Planetary Atmospheres

I A CONTINUING BIBLIOGRAPHY WITH INDEXES

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L UCCESSION NUMBER) Hard copy (HC) :N66 36130 (THRUI *L /95- - IPAGESI Microfiche (MF) /. rn 2

fl653 July 65 [NASA CR OR TMX OR AD NUMBER) ( ICATElZORYI This bibliography was prepared by the NASA Scientific and Technical Information Facility oper ated for the National Aeronautics and Space Administration by Documentation Incorporated I L NASA SP-7017(01)

PLANETARY ATMOSPHERES

A CONTINUING BIBLIOGRAPHY WITH INDEXES

A selection of annotated references to unclassified reports and journal articles that were introduced into the NASA Information System during the period February, 1965-May, 1966.

Scientific and Technical Information Division I NATIONAL AERONAUTICS AND SPACE ADMINISTRATION WASHINGTON, D.C. AUGUST 1966 This document is available from the Clearinghouse for Federal Scientific and Technical Information (CFSTI), Springfield, Virginia 221 51 for $1.50. .

INTRODUCTION

With the publication of this first supplement, NASA SP-7017(01), to the original issue of the Continuing Bibliography on “Planetary Atmospheres” (NASA SP-70 17), the National Aeronautics and Space Administration continues its program of distributing selected references to reports and articles on aerospace topics that are currently under intensive study. The references are assembled in this form to provide a convenient source of information for use by scientists and engineers who need this kind of specialized compilation. Continuing Bibliographies are updated periodically by supplements which can be appended to the original issue. With respect to particular subjects, the majority of entries in this publication pertain to investigations of Mars and Venus, and a large percentage of these references were produced as a result of the successful probes of the atmospheres of Venus (Mariner 11) and Mars (Mariner IV). In addition, a limited number of references to the atmospheres of Jupiter, Mercury, and Saturn is also included. The scope of coverage was defined to permit inclusion of references to such specific topics as the theory of planetary origins, extraterrestrial environment, planetary exploration and spacecraft reentry, and the physical properties of the planets. Pertinent references to the techniques of planetary observation and measurement, e.g., those involving photography, photometry, spectroscopy, astronomy, and meteorology, are also to be found in this bibliography. All references included in SP-7017(01) have been announced in either Scientific and Technical Aerospace Reports (STAR). International Aerospace Abstracts (IAA ) or the NASA Continuing Bibliography Aerospace Medicine and Biology (NASA SP-7011 and its supplements), and were introduced into the NASA information system during the period February, 1965-May7 1966.

Each entry in the bibliography consists of a citation and an abstract. The listing of entries is arranged in three major groups. Report literature references are contained in the first group and are subdivided according to their date of announcement in STAR. The second group includes journal and book references that have been announced in IAA. A third group is comprised of entries that were originally prepared by the Aerospace Medicine and Biology Bibliography Section of the Library of Congress (LC) for inclusion in Aero- space Medicine and Biology. A subject index and a personal author index are included.

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V TABLE OF CONTENTS

Page

1965 STAR Entries (N65-10000) ...... 1 1966 STAR Entries (N66-10000) ...... 18 1965 IAA Entries (A65-10000) ...... 33 1966 IAA Entries (A66-10000) ...... 68 1965 LC Entries (A65-80000) ...... 71 1966 LC Entries (A66-80000) ...... 73

Subject Index ...... 1-1 Personal Author Index...... 1-43

NASA SPONSORED DOCUMENT

N66-11138'# Consultants and Designers, Inc., Arlington. Va. MEASUREMENTS OF POLARIZATION AND OF BRIGHT- NESS TEMPERATURE DISTRIBUTION OF VENUS IN THE CORPORATE 10.6 cm WAVE [IZMERENIYA POLYARlZATSll I RASPRE- SOURCE DELENIYA YARKOSTNOY TEMPERATURY VENERY NA

ENGLISH from Dokl. Akad. Nauk SSSR. Astronomiya. v. 161. TITLE no. 3. 1965 p 551-553 (Contract NAS5-3760) PU BLlCATlON DATE

search conducted in 1962 at CALTECH radioastronomical observatory which consisted in experimental measurements of brightness distribution along Venus' disk in nonpolarized radiation. This pursuit took place near the 1964 lower conjunc- SALES AGENCY CONTRACT tion and included polarization measurements Author AND PRICE OR GRANT

REPORT NUMBER

vi .

vehicles. Uncertainties in the atmosphere composition and scale height are shown to preclude accurate prediction of the 1965 heating rates for an -unmanned probe entry. However. as expected, requirements for soft tandings are the most restric- STAR ENTRlES tive. Already difficult to satisfy because of low surface pressure. these requirements become extremely limiting because of the uncertainty in atmosphere structure. Author

N65-13519# General Electric Co.. Philadelphia. Pa. Space N65-14663'# New Mexico U.. University Park. Research Scienceslab. Center NORMAL SHOCK PARAMETERS FOR THE VENUSIAN AT- OBSERVATIONS OF THE RED SPOT ON JUPITER M OS PHER E Bradford A. Smith and Clyde W. Tombaugh 15 Apr. 1963 F. Bosworth. C. Cook. L. Gilbert, and S. Scala Dec. 1964 8p ref 6Op refs (Grant NsG-142-61) (R64SD65) (NASA-CR-50303; TN-557-63-21 OTS: HC $1.00/MF $0.50 Normal shock wave and stagnation point solutions for four Unfiltered photographs on blue plates were made of the Venusian atmospheric and chemical models are presented red spot on Jupiter between June 1962 and January 1963. which cover a range of flight speeds from loo00 to 4OOOO Two separate estimates of the average transit image on each fps. and a range of altitudes from 5OooO to 430000 ft. Singly ionized chemical species are included in the analysis and in of the plates were made and converted to the proper System II longitude of Jupiter. A red spot acceleration was observed the numerical solution of the thermochemical equations. around November 10. 1962. The longitude of the red spot Curves of dimensionless pressure. temperature. and density of increased at a rate of 0.025 0.008 degrees daily until the the shocked gas are presented as functions of flight speed for f middle of January 1963. A major. rapidly spreading disturb- constant altitudes. Author ance in the south equatorial belt was detected in September 1962 and made contact with the red spot in the first week of N65-1417'# National Aeronautics and Space Administration. November. No definite evidence was found that the red spot Marshall Space Flight Center. Huntsville, Ala. acceleration was directly related to the south equatorial dis- THEORETICAL MODEL ATMOSPHERES OF VENUS turbance. G.G. Robert B. Owen Washington, NASA, Jan. 1965 46 p refs (NASA-TN-D-2527) OTS: HC $2.00/MF $0.50 From a survey of past and present literature. a summation N65-14665'# Geophysics Corp. of America. Bedford, Mass. Of various models of the atmosphere of Venus is presented. THE EFFECT OF CLOUDINESS ON A GREENHOUSE It is shown how these models were formed and eliminated; MODEL OF THE VENUS ATMOSPHERE and a final model. apparently more consistent with recent ob- George Ohring and Joseph Mariano May 1963 33 p refs servations. is advocated. This model. one of the greenhouse (Contract NASw-704) variety. indicates more extreme surface conditions than were (NASA-CR-51176: GCA-TR-63-17-N) OTS: HC S2.00IMF Previously suspected. Author $0.50 In previous models of the greenhouse effect in the Venus N66-14828'# National Aeronautics and Space Administration. atmosphere. it has been assumed that infrared-absorbing Ames Research Center. Moffett Field, Calif. atmospheric gases provide the sole contribution to the infra- SOME EFFECTS OF. UNCERTAINTIES IN ATMOSPHERE red opacity of the Venus atmosphere. In the present study. the STRUCTURE AND CHEMICAL COMPOSITION ON ENTRY influence of an extensive cloud cover. opaque to infrared INTO MARS radiation. is also included in the greenhouse podel. The magni- Robert L. Mc Kenzie Washington. NASA. Jan. 1965 36 p refs tude of the greenhouse effect, which is defined as the ratio (NASA-TN-D-2584) OTS: HC $2.00/MF 60.50 of the surface temperature produced by the greenhouse to Provided are examples of the degree to which uncertain- the surface temperature of an atmosphereless Venus. is com- ties in the structure and composition of the Martian atmOS- puted as a function of infrared opacity of the atmosphere. phere affect various aspects of entry. The discussion contains and amount and height (actually ratio of cloud-top pressure the effects on manned-vehicle entry corridors, aerodynamic to surface pressure) of clouds. It is assumed that the Venus heating, including shock-layer radiation for an unmanned atmosphere is grey. the absorbing gas has a constant mixing probe-type entry. and vehicle design requirements for an ratio, and the temperature variation with altitude is linear. unmanned probe soft landing. The results indicate that current Calculations are made for two temperature lapse rates: the uncertainties in atmosphere scale height are significant in that adiabatic lapse rate, and nine-tenths of the adiabatic lapse they greatly decrease the entry corridor heights for manned rate. Author

1 t N65-14673

N65-14673' Israel Program for Scientific Translations. Ltd.. radiometry. and infrared spectroscopy were made. The result- Jerusalem. ing data include the measurements of the thickness of dust on THE NATURE OF THE PLANETS the floors of 16 lunar craters: the infrared radiometric tempera- V. V. Sharonov 1964 426 p refs Transl. into ENGLISH tures of Mercury. Venus. Mars. Jupiter. Saturn, and Uranus: of the book "Priroda Planet" Moscow. Gos. Izd. Fiz.-Mat. Lit.. and extensive photoelectric photometry of Mars. Some of the 1958 Published for NASA and NSF important conclusions that have been previously published (NASA-TT-F-77) OTS: $4.25 are included. Author The nature of planets and satellites in the solar system is comprehensivelv treated from the practical or observational N65-15370'# AVCO-Everett Research Lab., Everett. Mass. viewpoint. Topics covered include: (1) the solar system as THE SPECTRUM OF SHOCK-HEATED GASES SIMULAT- an object of physical investigation: (2) telescopic investigation ING THE VENUS ATMOSPHERE of the surface of planets and satellites. along with their geo- A. Fairbairn Jul. 1963 15 p refs Presented at the AlAA Conf. metrical and mechanical characteristics: (3) planetary cartog- on Phys. of Entry into Planetary Atmosphere. Cambridge, raphy and topographic descriptions of individual bodies in the Mass., 26-28 Aug. 1963 solar system: (4) integrated-light photometry. and photometry (Contract NASw-746) of planetary disks: (51 optics of planetary atmospheres, and (NASA-CR-51668: AVCO-Everett Res. Note-3711 OTS: physical conditions on planets and satellites. A bibliography HC $l.OO/MF $0.50 isgiven for each chapter. and the appendix lists the terminology Mixtures of 90% N2 plus 10% C02, and 80% N2 plus recommended by the Commission on Planetary Physics of the 20%C02 were heated by reflected shock waves to temperatures Astronomy Board at the U.S.S.R. Academy of Sciences. of about 8000" K and normal density. Photographic and photo- M.G.J. dectric measurements were made of the emitted radiation N66-15023 RAND Corp.. Santa Monica. Calif. in the region 0.23~to 1.2~.The CN radical is the most promi- ATMOSPHERES OF THE PLANETS nent radiator in these experiments. and the intensity of the G. F. Schilling Sep. 1964 30 p refs Submitted for Publica- emission may be used to derive transition probabilities for tion the violet and red systems of bands. Author (P-2964: AD -606026) Known facts and proposed theories about the atmospheres N65-15488'# Virginia Polytechnic Inst.. Blacksburg. of the various planets are presented in a general manner. CONFERENCE ON ARTIFICIAL SATELLITES, PART B In particular, an attempt is made to emphasize the causes and Aug. 1964 295 p refs Conf. held at Va. Polytech. Inst.. reasons why the planetary atmospheres still present a deep Blacksburg, 12-16 Aug. 1963 Its Bull.. Eng. Expt. Sta. Ser. mystery as to their existence and makeup. P.V.E. No. 156, Vol. 57. No. 8 (Contract NASr-2261 N66-16223*# Arizona U.. Tucson. Lunar and Planetary Lab. (NASA-CR-60132) OTS: HC $6.00/MF $1.50 COMMUNICATIONS OF THE LUNAR AND PLANETARY LABORATORY, VOLUME 2. NUMBERS 31-36: MARS CONTENTS: ISSUE Gerard P. Kuiper. T. C. Owen, Dale P. Cruikshank. and James SOLAR SPACE ENVIRONMENT V. Marshall 1964 98 p refs 1. THE ORBITING ASTRONOMICAL OBSERVATORY (Grant NsG-161) AND THE ORBITING SOLAR OBSERVATORY N. G. Roman (NASA-CR-60264) OTS: HC $3.00/MF $0.75 (NASA. Washington) 13 p (See N65-15489 06-30) Four papers on the atmosphere of Mars and one on 2. SOLAR AND STELLAR RADIATIONS ABOVE THE laboratory spectra of various gases are presented. In the EARTH'S ATMOSPHERE T. A. Chubb (Naval Res. Lab.) 48 p first paper. spectra of the planet Mars obtained from the (See N65-15490 06-29) 82-in. telescope of the McDonald Observatory are presented 3. THE ATMOSPHERE AND SURFACE FEATURES OF for the interval 1p to 2.5~.and the spectra are examined for MARS H. Spinrad (JPL) 20 p refs (See N65-15491 06-30) the presence of constituents other than COP. In the second 4. SOLAR FLARES AND THE ASSOCIATED EJECTION paper, the Mars spectra reported in the first paper are cali- OF PARTICLES E. Tandberg-Hanssen (High Altitude Observa- brated with laboratory spectra of pure COP and of mixtures tory) 9 p (See N65-15492 06-29) of C02 with N2 and Ar. and preliminary values are derived for the pressure of the Martian atmosphere and the total M ETEO LOG ICA L AN C 0 M M U N ICAT ION SATE LLITES amount of gases other than C02. The third paper presents R 0 D two independent determinations of the C02 content of the 5. TIROS-THE FIRST METEOROLOGICAL SATELLITE Martian atmosphere. derived from the Mt. Wilson plate ob- R. M. Rados (NASA. Goddard Space Flight Center) 55 p (See tained in 1964 by Kaplan. Munch. and Spinrad. The fourth N65-15493 08-31.) paper presents laboratory spectra of the region 1p to 2.5~ 6. THE NIMBUS SPACECRAFT SYSTEM H. Press for testing the presence of CH4. "3. N20. CO. and COS (NASA. Goddard Space Flight Center) 61 p (See N65-15494 in planetary atmospheres. A new investigation of the re- 06-31) ported presence of NO2 in the Martian atmosphere is dis- 7. PASSIVE COMMUNICATIONS SATELLITES W. J. cussed in the fifth paper, and it is concluded that the upper O'Sullivan. Jr. (NASA. Langley Res. Center) 49 p ref (See limit on a vertical column of NO2 on Mars is about 8 micron- N65-15495 06-31) atm. D.E.W. 8. ACTIVE COMMUNICATION SATELLITE SYSTEM D. Mitchell (Bell Terephone Labs.) 31 p (See-N65-15496 N66-15288# Lowell Observatory. Flagstaff, Ariz. 06-31 ) PHYSICAL RESEARCHES ON THE BRIGHTER PLANETS Final Report N65-15491' Jet Propulsion Lab., Calif. Inst. of Tech.. Pasa- William M. Sinton 30 Sep. 1964 20 p refs dena. (Contract AF lS(6041-5874) THE ATMOSPHERE AND SURFACE FEATURES OF MARS (AFC R L-64-926, AD-609547) Hyron Spinrad In Va. Polytech. Inst. Conf. on Artificial Satel- Observational studies of the planets and the moon through lites. Pt. 6. Aug. 1964 20 p refs (See N65-15488 06-31) the use of photography. photoelectric photometry. infrared OTS: HC $6.00/MF $1.50

2 . N65- 16776 A review is presented of earthbound observations of Mars. w. Jenisch, Jr. and D. Christensen 20 Jan. 1965 300 p refs An up-to-date description of the Martian surface is included, Its Rept.-2979 and it covers discussions of polar caps. dark areas. vibration (Contract NASB-11285) absorptions in the infrared spectrum. color. mountain areas, (NASA-CR-60469) OTS: HC $6.00/MF $1.50 canals. wave of darkening. propagation velocity. surface temper- This is a bibliography of documents that will be considered ature, and the equatorial temperature. The molecular atmos- in providing an accurate definition of the space, lunar, and plan- phere of Mars reveals only two positively identified gases- etary environments as they affect flight mechanics and the carbon dioxide and water vapor. A study of the estimates of aerodynamic aspects of space travel. Present knowledge of the these gases is presented. The cloud and blue haze patterns space environment is quantitatively incomplete. Concepts and are discussed in terms of absorption with photometric evidence. ideas develop and change rapidly. and continual updating of R.E.S. this bibliography is necessary to keep abreast of the ever- expanding understanding of the space environment. Each of N65-15938# Air Force Systems Command. Andrews AFB. Md. the documents contained herein will be considered and ana- Office of the Staff Meteorologist lyzed; this bibliography will be revised and updated. and only the NATURAL ENVIRONMENTAL DATA AND SUPPORT RE- most pertinent documents will be listed in the final report. QUIREMENTS Author 1 Aug. 1964 144p refs (AFSC-TDR-64-2: AD-451331) 11165-16468 Air Force Systems Command, Wright-Patterson Each of the systems divisions and test centers was re- AFB. Ohio. Foreign Technology Div. quested to comment on needs for natural environmental in- STUDY OF INTERPLANETARY GAS AND IONOSPHERES formation in terms of areas of environmental parameters. OF PLANETS WITH THE HELP OF TRAPS OF CHARGED kind of data used, adequacy or inadequacy of the data. pro- PARTICLES grams systems which require the data. future data require- or K. I. Gringauz In its Space 3 Sep. 1964 p 86-97 (See N65- ments. and accuracies required. The reports were divided 16463 07-30) into three groups: Group I includes those atmospheric Three electrode traps were established on all Soviet space parameters that have long been of concern in classical rockets to catch charged particles in order to study the inter- meteorology and are now of interest to great distances from planetary plasma. Experiments with these traps led to the con- the earth's surface; Group atmospheric parameters im- II. clusion that the free electrons of stationary interplanetary gas portant in near-earth phenomena which have recently be- did not influence the accuracy of radio navigation in space come of concern. such as micrometeorological diffusion or because their concentration is too small: however. the concon- acoustical propagation properties; and Group Ill. space tration of charged particles in solar corpuscular fluxes was parameters characteristic of the interplanetary medium as found to be larger than in stationary plasmas. Studies of the meteor%s charged particles, etc. Each report describes earth ionosphere revealed the existence of electron streams at the parameters. the current state of knowledge. and the distances of 55000 to 75000 km from the earths surface current and future requirements for information. R.E.S. with densities of 108 cm-* sec-' and of more than 200 eV energies. It is assumed that the most external belt of charged particles with its boundaries along the lines of force of the geomagnetic field of the earth consists of particles with less N65-15600# General Electric Co.. Philadelphia, Pa. Space energy that those in the radiation belts. G.G. Sciences Lab. LABORATORY SIMULATION OF HYPERVELOCITY HEAT TRANSFER PROBLEM DURING PLANETARY ENTRY NS5-18498'# AVCO Corp., Wilmington. Mass. Research and J. S. Gruszczynski. W. R. Warren. Jr.. and N. S. Diaconis NOv. Advanced Development Div. 1964 54 p refs Presented at the 15th Intern. Astronautical MARS-VENUS CAPSULE PARAMETER STUDY. VOLUME Congr.. Warsaw, 7-12 Sep. 1964 I: INTRODUCTION AND ANALYSIS (R64SD 73; AD -451664) 21 Mar. 1964 290 p refs Prepared for JPL Outlined are laboratory techniques for the simulation of (Contract J PL-950626) heat-transfer environments experienced by a space vehicle (NASA-CR-53674; RAD-TR-64-1. Vol. I. Rev. I) OTS: HC entering planetary atmosphere with superorbital velocity. $6.OO/MF $1.50 Partial results'are presented of 6-month study that was Stagnation point convective heat-transfer and high-temperature undertaken to obtain comprehensive information to be used gas radiance are studied in an electric discharge driven shock in the design. performance. and environment studies of Mars tube. in which flight velocity simulation up to 60000 ft/SeC and Venus entry capsules. By approximate methods. computer was attained. The investigation of the response of materials routines were compacted. computer calculation time was re- used for vehicle heat shields requires flow durations much duced, and the abiliw to deal with a broad scope of parameters longer than those obtained in the shock tube. Therefore. an was enhanced. The objectives of the studies of shapes. ele- electric arc facility in which the required stagnation point gas mental weights, and residual weight are described. The Scope properties are produced was employed in such a study. A new of the overall work is discussed in terms of the Mars vehicle test technique that permits the evaluation of material per- and the Venus vehicle. The computer program is described formance in an environment with high radiative and convective by blocks. and empirical data are treated by subject as well energy fluxes is described. Some results of heat transfer and as by source. Analytical methods are discussed in detail. with material response study in simulated atmospheres of Mars special attention giCn to the coefficients block, the heating and Venus are also presented. Author block, the trajectory block, the structure block. and the heat shield block. D.E.W.

N65-16086*# Aerojet-General Corp.. Azusa. Calif. Von N65-16776# Arizona Univ.. Phoenix. Lunar and Planetary Karman Center lab. SPACE ENVIRONMENT CRITERIA. SPACE ENVIRON- LABORATORY RESEARCH ON GASES OCCURRING IN MENT BIBLIOGRAPHY Semiannual Report, 1 Jul.-31 Dec. PLANETARY ATMOSPHERES Find Report. Jun. 1. 1963- 1964 May31.1964

3 % N65-17118

Gerard P. Kuiper [19641 10 p refs J. A. R. Samson and H. J. Liebl Washington, NASA. Sep. 1963 (Grant Nonr(G)-00014-64) 20p refs (AD-608352) (Contract NASw-395) The major effort of the research was concerned with the (NASA-CR-16; GCA-TR-62-8-N) OTS: HC $1.00/MF $0.50 atmospheres of Mars and Jupiter. A photographic spectrogram A light source was investigated that would emit radiation was calibrated using the 72-foot multiple-path absorption below loo0 A of comparable intensity to the high-voltage tube. and the abundance of COz in the Martian atmosphere pulsed type but which would operate from a dc supply. It was was derived. The result was 46 +20 meter atm for an assumed felt that with the combination of hot filament and axial mag- Martian atmospheric temperature of 200" K. Studies on the neticfield as found in the Duoplasmatron that the light intensity determination of atmospheric pressure and of abundances of would be comparable with the high-voltage pulsed light sources. other gases are also reported. The analysis of the photo- A preliminary measurement of the total intensity between 1050 graphic spectrum of Jupiter was extended to longer and to and 1350 A was made using a nitric oxide ion chamber with a shorter wavelengths. All of the planetary absorptions observed Duoplasmatron as an ion source. Spectrums are determined in the long wavelength region were due to either methane or for hydrogen between 1800 and 900 A and for argon from ammonia. Upper limits were set on the abundances of a num- 550 to 1100 A. Author ber of gases: acetylene. ethylene, ethane, methylamine. methyl deuteride. hydrocyanic acid. silane. and hydrogen deuteride. Low dispersion spectra of Saturn. Uranus. and Jupi- ter satellites lo and Ganymede were also studied. D.S.G. N66-17264*# Geophysics Corp. of America, Bedford, Mass. PLANETARY AERONOMY. V: VACUUM ULTRAVIOLET LIGHT SOURCES N66-17118'# National Aeronautics and Space Administration. J. A. R. Samson Washington, NASA Sep. 1963 59 p refs Ames Research Center, Moffett Field, Calif. (Contract NASw-395) A TECHNIQUE FOR DETERMINING PLANETARY ATMOS- (NASA-CR-17: GCA-TR-62-9-N) OTS: HC $3.00/MF $0.50 PHERE STRUCTURE FROM MEASURED ACCELERATIONS A study is made of photoelectric detectors, since they OF AN ENTRY VEHICLE provide a high degree of accuracy in the measurement of ab- Victor L. Peterson Washington, NASA. Feb. 1965 22 p refs sorption cross sections. As the intensity of radiation is often (NASA-TN-D-2669) OTS: HC $1.00/MF $0.50 the important factor in photoionization measurements. the A detailed procedure was developed for obtaining the degree of intenseness is defined as strong if, after dispersion density and pressure structure of a planetary atmosphere by a grating spectrograph, the radiant flux exceeds 108 from measurements of accelerations experienced by a vehicle. photons/sec at the exit slit. It appears that several light sources making an uncontrolled entry into the atmosphere. It was exist which produce useful continua from 3500 to 600 A of shown that simplification in the method is possible and a po- sufficient intensity to measure .(by photoelectric detection tentially large source of error is eliminated if the accelerom- techniques) the (a) absorption cross sections of gases and eters are carried by a spherically shaped vehicle. Sample crystals. and (b) reflectance and transmittance of thin films. calculations were made to illustrate how well extreme model Author atmospheres for Mars could be defined by this technique. Results of the calculations showed that accelerometers designed to measure over the entire range of expected accelerations with N66-17266*# Geophysics Corp. of America, Bedford. Mass. an accuracy of 0.1% would not provide sufflciently precise PLANETARY AERONOMY. I: ABSORPTION AND PHOTO- data. If, however. the time period over which large errors in IONIZATION COEFFICIENTS OF PROPYLENE AND BU- measured accelerations are encountered is reduced or the accel- TENE-1 IN THE VACUUM ULTRAVIOLET eration measurements are improved by resorting to a dual J. A. R. Samson, F. F. Marmo. and K. Watanabe Washington. system in which one set of instruments measures over the NASA. Sep. 1963 19 p refs Also published in J. Chem. Phys.. entire range of expected accelerations and the other over a v. 36.1962 more limited range.-then any of the model atmospheres within (Contract NASw-395) the extremes can be determined reasonably well. Author (NASA-CR-18; GCA-TR-64-4-N) OTS: HC $1.00/MF $0.50 The total absorption coefficient of propylene and butene- 1 vapors in the region from 1500 to 2000 A and the photo- N66-17216*# Geophysics Corp. of America. Bedford. Mass. ionization coefficient in the region 1050 A to the onset of MASS SPECTROMETER INSTRUMENTATION FOR THE ionization were measured by photoelectric methods. Pressures ANALYSIS OF THE MARTIAN ATMOSPHERE Final Re- ranging from 0.04 to 0.2 mm Hg were used for the total ab- Port sorption coefficient determination, and three pressures from R. F. K. Herzog and W. P. Poschenrieder 12 Dec. 1962 87 p 0.05 to 2 mm Hg were used for the photoionization absorption refs Prepared for JPL coefficient determination. Ionization potentials obtained directly (Contracts NAS7-100; JPL-950328) for the two vapors agreed with previously published data. (NASA-CR-60760; GCA-62-17-GI OTS: HC $3.00/MF $0.75 Author Ion sources. ion-orbits in an inversed magnetron gauge. permanent magnet design. and instruments to prove the basic feasibility of a mass spectrometer to analyze the ion beam gen- N66-17291*# General Electric Co.. Philadelphia., Pa. Missile erated by an inverted magnetron gauge are discussed. The ex- and Space Div. periments presented show that a simple mass spectra can be VENUS-MARS CAPSULE STUDY, VOLUME 11 obtained with the new instrument. However. resolution is below 1 Mar. 1963 741 p refs Revised Prepared for JPL the requirements for the Martian probe. Nevertheless, the in- (Contracts NAS7-100: JPL-950250) strument has important good features-uses very little power; (NASA-CR-50811; AD-441924) OTS: HC 810.41/MF $3.50 is simple; requires one voltage for ion source operation: and The equilibrium composition and thermodynamic proper- needs no filament. E.E.B. ties of the Venusian atmosphere have been calculated based on two proposed model compositions. The two model compositions were assumed to contain nine and twenty-five percent N66-17263'# Geophysics Corp. of America. Bedford. Mass. COz, respectively. The calculations cover the temperature PLANETARY AERONOMY. IV: THE DUOPUSMATRON range 200" + 15 OOO" K and the logto p/po range of -7.0 AS A VACUUM ULTRAVIOLET LIGHT SOURCE to 1.8 at 200°K and 0.4 intervals. An ideal gas mixture in

4 . N65-18918 chemical equilibrium is assumed. including the dissociation An intensive literature survey was made of the present and ionization calculations. At the higher temperatures. consensus on the surface and atmospheric conditions of Mars. T > 3000" K. thirty gaseous species have been included in the Knowledge of the gross features of the Martian surface appears mixture calculations. P.V.E. to be fairly complete. but there is sharp disagreement on the atmospheric conditions. While estimates of the surface temperature are in fairly close agreement and estimates of the N65-17404*# Stanford Research Inst., Menlo Park. Calif. surface pressure range from 10 to 150 millibars. other phe- LIGHTNING OBSERVATIONS FROM SATELLITES Final nomena such as the blue haze are inexplicable. Formal design RW criteria for entry vehicles cannot yet be finalized because of Arnett S. Dennis Dec. 1964 94 p refs the wide range of the environmental parameter values. Author (Contract NASr-49(18); SRI Proj. 4877) (NASA-CR-60806) OTS: HC $3.00/MF $0.75 The feasibility of observing lightning from satellites is N65-18098*# Melpar. Inc.. Falls Church, Va. examined in the light of the effects produced at satellite heights A DESIGN STUDY PROGRAM OF A POLAROGRAPHIC by a lightning flash and of the statistics of lightning occur- OXYGEN ANALYZER FOR OBTAINING DATA ON THE AT- rences. A sferics detector operating around 600 Mc could be MOSPHERIC COMPOSITION OF MARS Final Report, 16 used on a low-orbit satellite at. e.g., 1000 km, but could not May-15 Sw. 1962 be used on a satellite in a stationary orbit (at 37000 km) be- R. T. Foley and G. Halpert 119621 121 p refs Prepared for cause of the low signal-to-noise ratio. The short-period varia- JPL bility in flashing rates imposes a lower limit of about 20 (Con!racts NAS7-100; JPL-950284) flashes per resolution element per observation. This require- (NASA-CR-57085) OTS: HC $4.00/MF $1.00 ment. examined in the light of typical flashing rates and the A laboratory model gas phase polarographic cell was mechanics of satellite orbits, limits the spatial resolution of the constructed with an 0.5-mil Teflon membrane. a platinum optimum sferics satellite to some 150 km. To realize such polarized electrode. a silver-silver chloride reference (revers- resolution without the acceptance of severe limitations upon ible) electrode, and an aqueous methanol-potassium chloride coverage. it would be necessary to use direction-finding equip- electrolyte which was designed principally to conduct effec- ment. capable of watching several resolution elements simul- tively at lower temperatures. A single compartment cell was taneously. For an elementary system using a fixed antenna. constructed to provide a configuration which could be packaged 1000-km resolution would be more appropriate. The po- into a compact unit. The cell operated without difficulty when tential value of lightning observations from satellites in the subjected to the atmospheric conditions expected to be en- fields of meteorology. climatology. atmospheric electricity. countered during a Mars descent. A breadboard model was geophysics, and radio engineering is examined. It is con- designed and constructed including the polarographic cell; cluded that such observations would be of some value in the electrolyte injector and the accumulator. which allows the radio-noise studies but that their impact upon the other cell to be activated upon arrival at the planet; and the am- fields would be very slight. Author plifier, which converts current output to a voltage for trans- mina nce . R.L.K.

N65-17- Naval Research lab., Washington. D. C. RADIO ASTRONOMICAL OBSERVATIONS OF VENUS WITH N66-18512* National Aeronautics and Space Administration. HIGH RESOLVING POWER Washington. D. C. D. V. Korol'kov. Yu. N. Pariytkiy. G. M. Timofeava. and S. E. RESULTS OF SPECTROPHOTOMETRIC OBSERVATIONS Khaikin 119631 12 p refs Transl. into ENGLISH from Dokl. OF MARS DURING 1960-1961 Akad. Nauk (Moscow). v. 149, no. 1.1963 p 65-67 SSSR Ye. I. Didychenko. I. K. Koval'. and A. V. Morozhenko In its (NRL-TRANS-936; PB-63-11647: AD-602904) OTS: $0.50 Bull. of the Main Astron. Obs., Vol. V, Issue 1 Mar. 1965 During October-November of 1962 observations were p 48-69 refs (See N65-18507 08-30) OTS: HC $5.00/MF carried out of the radio emission from Venus on 3.02-cm wave- $1.00 length by means of a large Pulkovo radio telescope with a The results are presented of spectrograms of Mars obtained variable profile antenna. The purpose of these investigations by means of a spectrograph having a linear dispersion of 24 A/ was to evaluate the nature of the distribution of radio bright- mm in Hy. set up in the Cassegrain focus of the 70-cm reflector ness. by using high resolving power and high precision of of the Main Astronomical Observatory. Academy of Sciences. the coordinate measurements with a variable profile antenna. Ukrainian S.S.R. From the monochromatic values obtained for A divergence betwean the optical and radio methods cannot the visual albedo of various details of the planet, it was estab- be explained by the presence of high radiation belts as in the lished that (1) the visual albedo of the investigated formulations case with the Jupiter. Radio emission is practically absent of Mars (continents, polar caps. Wright clouds) gradually de- at a distance of 1.07 R from the center of the disk of the planet; creases from red to the violet end of the spectrum; and. (2) Le. the height of the radiation region does not exceed 420 km the polar caps were atmospheric formations during the period above the cloud cover of Venus. The results of measurements of the observations. Author of the effective dimensions of Venus are shown. An attempt to determine the phase variations of radio temperature with displacement of the center of gravity of radio emission led to a N65-18918*# Princeton Univ. Observatory. N. J. negative result. The Observations agree best of with the all HYDROGEN MOLECULE6 AND ASTRONOMY: A RMEW model over hot surface and cold atmosphere (Extracted). W. 8. !Somervil&. G. E. Fiald,and K. Dressler Jan. 1965 90 p Author refs (Grant NsG-414) (NASA-CR-571561 CFSTI: HC $3.00/MF $0.75 N66-17995.# National Aeronautics and Space Administration. Discussed are the kRorving topics: The Theory of the Hy- Marshall Space Flight Center. Huntsville, Ala. drogen Molecule-formulation. nuctear vibration and rotation. THE MARTIAN ENVIRONMENT the calculation of electronic wave functions. electronic states. Robert B. Owen 19 Nov. 1964 42 p refs the coupling of angular momentum vectors, symmetry, transi- (NASA-TM-X-53167) OTS: HC $2.00/MF $0.50 tions. correction terms to the energy. and the molecular ion

5 N65-18944

I+:; Hydrogen Molecules in Astrophysics-general considera- 1964 33 p refs Sponsored by NSF tions. planetary and stellar atmospheres, and interstellar space: Observations and calibration experiments on three tele- Spectroscopical@ Determined Term Values and Transistions in scopes are summarized. as well as progress in Aerobee rocket Hz-the language of molecular spectroscopists. the rotational sounding programs and theoretical consideration of planetary and vibrational structure of the ground state. and excited states atmospheric compositions from COz absorption data. E.P.V. and electronic transitions. G.G.

N65-19770*# Massachusetts Inst. of Tech., Cambridge. Re- N66-18944*# Stanford Univ.. Calif. Radioscience Lab. search Lab. of Electronics RESEARCH AT THE STANFORD CENTER FOR RADAR [GROUND-BASED OBSERVATIONS OF VENUS IN THE ASTRONOMY Semiannual Report, No. 4, 1 Jul.-31 Dec. WAVELENGTH RANGE FROM 0.90 TO 1.40 cm AND BAL- 1964 LOON-BORNE MEASUREMENTS OF MICROWAVE EMIS- V. R. Eshleman Jan. 1965 11 p refs SION FROM MOLECULAR- OXYGEN IN THE TERRESTRIAL (Grant NsG-377) ATMOSPHERE Finat Report, Jun. 1-Dec. 31,1964 (NASA-CR-57184) CFSTI: HC $l.OO/MF $0.50 Alan H. Barrett 4 Jan. 1964 5 p refs Research covered includes theoretical and experimental (Grant NsG-250-62) radio and radar studies of lunar and planetary ionospheres. (NASA-CR-57309) CFSTI: HC $l.OO/MF $0.50 atmospheres, and surfaces. and radar studies of the sun and Wavelength and brightness measurement values of interplanetary medium. Specific projects cover a radar-occulta- Venus radio spectra do not agree with those computed previ- tion method for the study of planetary atmospheres. possible ously. which considered nonresonant emission mechanisms models for the atmosphere of Mars. magnetohydrodynamic involving carbon dioxide and nitrogen as the model. However. waves in interplanetary space, a solar radar program, studies the observed values can be approximately matched by in- of cislunar gas, and data processing. D.E.W. cluding water in the atmospheric model because of the resonant line at 1.35 cm for water. It is also possible that the observations can be fitted with a model which includes microwave scattering with either resonant or nonresonant absorption. The measurement of the N = 9+ line of molecular oxygen during N66-18946*# Stanford Univ.. Calif. Radioscience Lab. ascent, at float. and during descent is also reported. E.E.B. THE BlSTATlC RADAR-OCCULTATION METHOD FOR THE STUDY OF PLANETARY ATMOSPHERES Scientific Report No. 6 G. Fjeldbo and V. R. Eshleman Feb. 1965 34 p refs (Grant NsG-377) General Electric Co.. Philadelphia. Pa. Space (NASA-CR-57178; SEL-65-010) CFSTI: HC $2.00/MF $0.50 N66-19884*# Theoretical studies were made of the characteristics of Sciences Lab. radio waves diffracted at the limb and refracted in the atmos- HYPERVELOCITY HEAT TRANSFER STUDIES IN SIMU- phere of a planet. Sample computations were made of atmos- LATED PLANETARY ATMOSPHERES Final Report pheric perturbations to the comdunication links to. and from J. S. Gruszczynski and W. R. Warren Mar. 1964 195 p refs a Mars flyby spacecraft having a trajectory that involves occulta- grepared for JPL . tion of the spacecraft by the planet as seen from the earth. (Contracts NAS7-100: JPL-950297) It is concluded that such a radio occultation experiment can (NASA-CR-57508) CFSTI: HC $5.00/MF $1.25 provide important new information on the atmospheric scale Stagnation point convective heat transfer was measured height and surface density of a planetary atmosphere, and when with a platinum calorimeter and thin-film gages in a simulated combined with other information. can help determine atmos- planetary atmosphere composed of 9% COz and 91% N2 over pheric constituents. Author a range of flight velocities up to 45000 ft/sec. It was found that the composition of the COz-Nz mixture does not have a large effect on experimental convective heat-transfer rates. Convective heat-transfer data obtained with gages of different N66-19405# AVCO Corp , Wilmington. Mass Research materials indicate that the state of the stagnation point boundary and Advanced Development Div layer can be such that the gage surface effects the observed LAMINAR AND TURBULENT CONVECTIVE HEATING ON heat-transfer rates. Stagnation point equilibrium total radiation CONICAL BODIES IN PLANETARY ATMOSPHERES measurements in 9% COz and 91% N2. for shock velocities Paul Sones Jan 1965 38 p refs between 22000 and 34000 ft/sec. were compared with the (RAD -TM -64-68. AD -454403) theoretical predictions of Breene, et al. The total radiation Methods were devised from existing techniques for the behind the incident shock for shock velocities between 20000 prediction of laminar and turbulent convective heat transfer and 30000 ft/sec and spectral distributions of equilibrium rates on cones in planetary atmospheres Comparison of these and nonequilibrium radiation were measured in a 25% C02- methods with experimental data from nitrogen-carbon dioxide 75% N2 mixture. D.E.W. mixtures was made to check their validity when applied to atmospheres other than air The laminar predictions are obtained from two methods a similar solution of the boundary layer equations and a reference enthalpy approach The ref- N66-20768'# Space Technology Labs, Inc . Redondo Beach. erence enthalpy approach is then further adapted for the turbu- Calif Quantum Physics Lab THEORETICAL INVESTIGATION; THE SCATTERING OF lent flow conditions The comparison of theory and experiment LIGHT BY A PLANETARY ATMOSPHERE Final Report, shows good agreement and indicates that the methods are valid 1 Jun.-1 Dec. 1964 for planetary atniosphes Author Robert S Fraser [ 19641 125 p refs (Contract NAS5-38911 (NASA-CR-57740, STL-4167-6002-RU-000) CFSTI HC N66-19648# Kitt Peak National Observatory. Tucson. Ariz. $400/MF $1 00 [FACILITIES AND EQUIPMENT FOR ASTRONOMY, PLANE- A theoretical-computational study IS presented on how TARY AND SPACE SCIENCES] Monthly Report specular reflection at the ground modifies the light scattered

6 . N65-22368 outwards from the top of a homogeneous Rayleigh atmos- N65-22203'# Jet Propulsion Lab.. Calif. Inst. of Tech.. Pasa- phere. The computations for this model are compared with com- dena. putations for a second modal. which is the same. except that VENUS, RECENT PHYSICAL DATA FOR its ground reflects radiation according to Lambert's law. When L D. Kaplan Jun. 1964 6 p refs Submitted for Publication their atmospheric optical thickness (71) IS not large (rl (NASA-CR-56851) CFSTI: HC $1.00/MF $0.50 < 1.0). the relative difference is small for the flux, increases Investigations of the planet Venus during the 1962 inferior for the specific intensity, becomes large for the maximum conjunction. including the measurements during the flight of degree of polarization. and is still larger for the neutral point Mariner 11. are reported. The microwave measurements showed positions. The neutral point characteristics for the two models unambiguouslythat limb darkening was present at 19-mm wave- are quite different for optical thickness smaller than 0.25. length; therefore the origin of the high thermal emission at The flow of the radiation is divided into several streams that centimeter wavelengths is at. or near. the surface of the planet. have physical significance and can be calculated separately. After eliminating the limb darkening and dividing the resulting Author brightness temperature by an assumed surface emissivity derived from earth-based radar measurements of reflectivity. a fairly uniform surface temperature of about 700" K was obtained. Among theother results reportedwere radiusof Venus. 6010*30 NS8-20799'# National Aeronautics and Space Administraticn. km; mass. 4.870 X ld'g. density, 5.36 g/cc; surface gravity, Goddard Inst. for Space Studies, New York. 900 cm/sec2: retrograde rotation period. 250140 days; sur- THE ATMOSPHERES OF MARS. VENUS AND JUPITER face pressure. 10*3bars: cloud top temperature. 200" K. J. I. Rasool and Robert Jastrow 119631 56 p refs Presented E.E.B at the Symp. on Extraterrestrial Bioi. and Org. Chem. at 4th COSPAR Meeting, Warsaw. 3-12 Jun. 1963 (NASA-TM-X-56223) CFSTI: HC $3.00/MF $0.50 Since composition, temperature. and pressure are the N65-22367'# National Aeronautics and Space Administration. three parameters which determine the structure of a planetary Ames Research Center. Moffett Field. Calif. atmosphere. these are discussed by considering the processes BLUNT BODY SOLUTIONS FOR SPHERES AND ELLIPS- by which the planetary atmospheres evolved. The reliable OIDS IN EQUlUBRlUM GAS MIXTURES physical data for the planet Mars are summarized. Considerably Mamoru lnouye Washington. NASA. May 1965 35 p refs less is known about Venus. However. the physical constants (NASA-TN-D-2780) CFSTI: HC $2.OO/MF $0.50 of the planet and the current hypotheses regardim its structure An inverse method was used to calculate the flow field are given. AGO. ~elatively~li~leiiknown about the structure of in the nose region of blunt bodies traveling at supersonic the atmosphere of Jupiter. Being five times farther removed speeds in equilibrium mixtures of gases that may be present from the sun than the earth. but having a comparable albedo in other atmospheres. Calculations were made for air. nitrogen, Of 0.47. the effective temperature of the planet is only 105" K. carbon dioxide. argon, and a mixture composed of 50% argon. The high surface gravity and low temperature together sug- 40% nitrogen. and 10% carbon dioxide. Speeds from loo00 gest that the gravitational escape of gases from the planet to 70000 ft/sec are covered for free-stream densities of should be extremely inefficient and the chemical composition lo-'. and times earth sea level values. Correlations of the atmosphere should still be primitive. containing large are presented for the shock standoff distance. surface pressure quantities of hydrogen and helium. E.E.B. distribution. and stagnation-point velocity gradient. Author

N65-21005'# Consultants and Designers. Inc., Arlington. Va. ON VENUS MODEL WITH "COLD ABSORBING ATMOS- PHERE [0 MODEL1 VENERY S "KHOLODNOY" POGLO- N65-22368'# National Aeronautics and Space Administration. SHCHAVUSHCHEY ATMOSFEROY] Langley Research Center. Langley Station. Va. A. D. Kuz'min 6 Apr. 1965 16 p refs Transl. into ENGLISH LONGITUDINAL STABILITY CHARACTERISTICS OF SEV- from In. Vysshikh Uchebn. Zavedenii. Radiotekhn. (Kiev). ERAL PROPOSED PLANETARY ENTRY VEHICLES AT v. 7. no. 6.1964 p 1021-1031 MACH 6.73 (Contract NAS5-3760) Peter 1. Bernot Washington. NASA. Apr. 1965 24 p refs (NASA-TT-F-9663; ST-LPS-10314) CFSTI: HC $l.OO/MF (NASA-TN-D-2785) CFSTI: HC $1.00/MF $0.50 SO. 50 Aerodynamic characteristics of several planetary entry ve- The possibility is considered of interpreting the observed hicles with different nose-bluntness ratios were obtained over Venus radio emission spectrum in centimeter and millimeter an angle-of-attack range from o" to 1W at Mach 6.73 and at bands by wave absorption in the atmosphere aerosol of the Reynolds numbers of 0.19 x Idand 0.25 x [email protected] an angle- planet. it is shown that the steep slope in the millimeter band of-attackof P , the flow about these configurations was charac- of the spectrum may be explained by absorption in trickle- terized by large-scale flow separation accompanied by shock- liquid aerosol at -300" K and containing 0.2 to 0.3 g of wave fluctuations, notably for the sharp-nose model. As angle polar liquid with 3.5-10-12 sec relaxation time. Such liquids ofattack was increased about lo". this separated-flow region on can be constituted by some functional derivatives of methane thewindward side of the model was swept aside with the result CHq. ethane C2Hg. benzol CsHg, and others. Oust aerosol. that large increases occurred in normal and axial force and, in consisting of rocks and volcanic formations. does not satisfy pitching moment. A high level of positive stability was ob- the experimental data. It is shown that the atmosphere model. tained for all the models at an ahgie of attack of o"; for the yielding to the observed radiospectrum. must be entirely non- tests at angles of attack greater than SO", the models showed transparent in the infrared and optical bands. Therefore. the no additional stable trim points. Positive stability was main- surface heating of the planet cannot be the resutt of direct tained for all models near an angle of attack of 0" as csnter-of- solar radiation. Surface heating by the planet's inner heat gravity location was varied longitudinally from 2096 to 90% is also considered, and the necessary heat flow is estimated. of the body length from the nose. Varying the location of the The possibility of explaining the measured Venus brightness center of gravity along the vertical axis as much as 7.5% of temperature decrease in decimeter band by wave absorption the base diameter resulted in small changes in trim angle of in relatively cold Venus ionosphere (-300" K) is indicated. attack. Increasing the nose-bluntness ratio decreased the Author axial-force coefficient and the stability. Author

7 N65-22579

N66-22679*# National Aeronautics and Space Administration. N66-23299# Space Technology Labs.. Inc.. Redondo Beach. Washington, D. C. Calif. CIRCUMPLANETARY EXPLORATION OF ATMOSPHERES HIGH TEMPERATURE THERMODYNAMIC PROPERTIES [EXPLORATION CIRCUMPLANETAIRE DES ATMOS- OF A 16% C0~86%N2 MIXTURE PHERES] J. T. Ohrenberger 5 Mar. 1964 12 p ref F. Link (Acad. of Sci.. Prague) 15 May 1962 8 p refs Transl. (STL-9990-6631 -TU-000) intoENGLlSH from the French paper presented at the COSPAR Thermodynamic properties of a 15% c02-85% N2 (b Symp., Washington, D. C.. May 1962 volume) mixture to 10OOO" K in the pressure range from 10- i (NASA-TT-F-8219) CFSTI: HC $1.00/MF $0.50 to 10 atm. calculated using a modified equilibrium chemistry The theory of using a spaceship to make photometric program, are presented. The composition chosen simulates observations of a star during its occultation by Venus or Mars a model planetary atmosphere. and the data presented are is discussed. and application of this theory for deriving the applicable to entry vehicle radiant heating and communications optical properties of these planetary atmospheres is described. blackout analyses. Curves presenting the following informa- The occultation's photometric curve for each case was com- tion are given: (1) the relation between enthalpy and pres- puted from the general transmission factor as a function of sure along lines of constant temperature. constant enthalpy. the luminous ray passing at a minimum altitude. the exponen- and constant 2 (molecular weight of original mixture divided tial atmosphere of low density. and the spaceship's position. by molecular weight of reacted mixture); (2) the relation be- Numerical examples relative to Mars and Venus are given. and tween the mole fraction of CN. CO. CO+, and temperature along the respective photometrical curves are shown on plots. Adapta- lines of constant pressure; and (3) the relation between the tion of a simple model of homogenous layer. from the ground electron concentration and temperature along lines of constant to the altitude of 50 km and with the optical density at zenith pressure. Equations of state. mass fraction conversions. and being 0.03, was used in a study of Mars' dust layer. It was exphssions for finding the number of particles per unit vol- found that the presence of the dust layer modifies the pattern ume are also given. M.P.G. of the occultation considerably. G.G.

N66-22689. # National Aeronautics and Space Administration. N66-23799. # National Aeronautics and Space Administration. Washington. D. C. Manned Spacecraft Center. Houston, Tex. POSSIBILITY OF EXISTENCE OF HIGH ELECTRON CON- VENUS ,AND MARS NOMINAL NATURAL ENVIRONMENT CENTRATIONS IN THE NIGHT ATMOSPHERE OF VENUS FOR ADVANCED MANNED PLANETARY MISSION PRO- VOZMOZHNOSTI SUSHCHESTVOVANIYA V NOCHNOY IO GRAMS ATMOSFERE VENERY VYSOKIKH ELEKTRONNYKH Dallas E. Evans, David E. Pitts. and Gary L. Kraus Washington. KONTSENTR ATSlY] NASA. 1965 52p refs A. D. Danilov and Yatsenko Jun. 1962 6 p refs Transl. S. P. (NASA-SP-3016) CFSTI: HC $2.00/MF $0.50 into ENGLISH from Geomagnetizm i Aeronomiya (Moscow). A compilation of numerical values for a nominal natural v. 2. no. 2. 1962 p 363-364 environment for application in studies for advanced manned (NASA-TT-F-8244) CFSTl: HC $1.00/MF $0.50 'planetary missions to Venus and Mars is presented. The goal The presence of high electron concentrations in the night is to provide a standard environment as a base for the various atmosphere of Venus was investigated in order to explain the missions and preliminary design studies, and to have a com- high temperatures of the emitting regions that were found mon basis for comparison of end results. G.G. bv radio observations in the IO-cm wavelength. A model of the Venus ionosphere was constructed on the basis of similar ionization and recombination processes in the terrestrial atmosphere. Comparison with the number of recombina- N65-24307'# RAND Corp.. Santa Monica. Calif. tions in the night ionosphere of the Earth led to the assumption INSTRUMENTATION TO MEASURE MARS' ATMOSPHERIC , that the same ionizing agent acts in the Venus as in the Earth's COMPOSITION, USING A SOFT-LANDED PROBE night atmosphere. The flux of that agent seems to be several R. 0. Woods and J. W. Ranftl Apr 1965 26 p refs times greater in the Venusian atmosphere. G.G. (Contract NASr-21(09))

(NASA-CR-62870; RM-4451-NASA) CFSTI. HC $2.00/MF- ~~ $0.50 N66-22739 Army Electronics Research and Development Ac- The most suitable method for determining the cornposition tivity. Fort Huachuca, Ariz of the Martian atmosphere, using a soft-landed probe. is NUMERICAL SOLUTION OF THE DISTRIBUTION OF WIND AND TURBULENCE IN THE PLANETARY BOUNDARY sought The methods considered include optical spectroscopy. mass spectrometry. gas chromatography. and other means of LAYER gas analysis. Of all the methods investigated. mass spec- J F Appleby and W D Ohmstede In Army Dept Army Sci trometry appears best suited to Martian atmospheric analysis. Conf Proc, Vol I [19641 p 85-99 refs (See N65;22732 Not only is the technique intrinsically well suited to the anal- 12-34) A planetary boundary layer model is presented which unifies ysis of an unknown mixture of fixed gases, but the output can micro- and macroscale measurements in meteorology The be telemetered with a minimum of processing. The construction and power requirements of mass spectrometers are readily two scales were used to measure different atmospheric phenomena The logarithmic wind profile equation relates the compatible with spaceborne applications. It is estimated that vertical distribution of wind speed immediately above the earth such an instrument would weigh about 5 to 8 pounds and surface to the momentum transport and roughness characteris- require 5 to 10 watts of power. Author tics of the surface. while the geostrophic wind equation is used to evaluate the horizontal field of wind in the free atmosphere from knowledge of the pressure distribution. Charac- N65-24310'# Stanford Univ., Calif. Radioscience Lab. , teristic of the planetary model is that in the free atmosphere BISTATIC-RADAR METHODS FOR STUDYING PLANE- the wind approaches the geostrophic wind, while in the surface TARY IONOSPHERES AND SURFACES Scientific Report boundary layer the wind profile is logarithmiic. Study of the No. 2 (Final) model was limited to the barotropic. adiabatic, steady-state Gunnar Fjeldbo Apr. 1964 95 p refs case, and requires extension to a broader class of situations. (Grants NsG-377; NSF G-21543) J.M.D. (NASA-CR-62823; SEL-64-025) CFSTI: HC $3.00/MF $0.75

8 N65-24480

The transmission of radio waves from the earth to a re- 6 Feb. 1964 245 p refs Transl. into ENGLISH from Kosmich. ceiver in a spacecrah that is moving behind a planet makes Issled. (Moscow). v. 1. no. 2. Sep.-Oct. 1963 p 195-334 it possible to observe the variations in the amplitude. phase (FTD-TT-64-42/ 1i- 2 +4; AD-429870) path. or group path caused by the planetary ionosphere. It is shown that measurement of any one of these quantities may CONTENTS: be used to determine the radial electron density distribution 1. CERTAIN PROBLEMS OF ASTRODYNAMICS AND in- that part of the planetav ionosphere which is probed by CELESTIAL MECHANICS G. N. Duboshin and 0. Ye. Okhot- the signal. Measurement of two of these quantities simul- simskiy p 1-29 (See N65-24476 14-30) taneously will reduce uncertainties due to changes in the 2. THE RADIATION OF THE SOLAR CORONA IN THE interplanetary medium or the earth's ionosphere during the SOFT X-RAY REGION Ye. P. Fetisov p 30-43 refs (See experiment. Separate radial electron density distributions N65-24477 14-29) can be obtained from the measurements during immersion 3. APPARENT MOTIONS OF THE EARTH IN THE and emersion and these are related to the spatial properties LUNAR SKY V. V. Shevchenko p 44-50 refs (See N65- of the atmosphere on the planet. It is shown that the lower 24478 14-30) atmosphere as well as the ionosphere of a planet can be studied 4. TWO-DIMENSIONAL PROBLEM OF ESTABLISH- by using so high a frequency that the signal is no1 influenced ING A TRUE INDICATRIX OF BRIGHTNESS BASED ON by the ionized component of the atmosphere. Author THE MEASURED SMOOTHED INTENSITY A. A. Dmitriev p 51-60 (See N65-24479 14-30) 5. SCATTERING OF LIGHT IN A SPHERICAL AT- N65-24338'# Aeronutronic. Newport Beach. Calif. MOSPHERE. 11. I. N. Minin and V. V. Sobolev p 61-73 refs DEVELOPMENT OF A HIGH TEMPERATURE BAlTERY (See N65-24480 14-30) W. J. Subcasky, T. M. Place. H. A. Parker-Jones. and W. G. 6. INVESTIGATION OF THE THERMAL RADIATION Anderson 20Apr. 1965 5Op refs FIELD OF THE STRATOSPHERE AND TROPOSPHERE IN (Contract NAS3-6002) THE INFRARED REGION OF THE SPECTRUM USING (NASA-CR-54404: U-4OOO) CFSTI: HC $P.OO/MF $0.50 GEOPHYSICALBALLOONS M. N. Markov, Ya. I. Marson. and Experimental cells with sodium anodes and CuCl cathodes M. P. Shamilev p 74-96 refs (See N65-24481 14-29) were discharged. Membranes used to separate anode and cath- 7. THE DEMAND FOR ACCURACY IN OBTAINING ode compartments were fabricated from a NaX zeolite or a high M ET E0 R 0 LOG ICA L INFORMAT1 0 N F R 0 M ART IF I C IA L sodium porcelain. Cell lives varied from 6 to 22 hours. Tests EARTH SATELLITES B. M. Novikov and V. A. Zyabrikov p 97- indicated attack of the membrane by molten alkali metals. 107 refs (See N65-24482 14-30) which substitution of a magnesium or magnesium alloy anode 8. ARGON IONIZATION IN THE UPPER ATMOS- with a LiCI-KCI anolyte for the sodium eliminated. Cell life PHERE A. D. Danilov p 108-115 refs (See N65-24483 was still erratic but in two cases cell lives approaching 70 14-29) hours under drain were achieved. Cracking of the zedite mem- 9. UPPER ATMOSPHERIC DETECTION OF O+ branes was ascribed to a volume change which occurred when IONS WITH HIGHER THAN THERMAL ENERGY V. G. lstomin the sodium ions in the zeolite were replaced with lithium ions p 116-127 refs (See N65-24484 14-30) from the anolyte. Cells constructed with other porous sepa- 10. MASS-SPECTROMETRIC MEASUREMENTS OF rators and molten CuCl cathodes had lives of the order of 15 He+, N+. O+. NO+, AND 0: ION DISTRIBUTION IN hours compared to cells with porous separators and solid THE EARTH'S ATMOSPHERE UP TO 430 km A. A. Pok- CuO cathodes which had lives in excess of 72 hours. Author hunkov p128-134 refs (See N65-24485 14-29) 11. EFFECT OF HIGH-ENERGY PROTONS ON SILI- CON PHOTOCELLS B. M. Golovin. G. M. Grigor'yeva. A. P. N65-24355'# RAND Corp.. Santa Monica. Calif. Landsman. and 8. P. Osipenko p 135-161 refs (See N64- MARS ENVIRONMENTAL MEASUREMENTS IN SUP- 23040 16-06] PORT OF FUTURE MANNED LANDING EXPEDITIONS 12. A SERIES OF MINIATURE MASS SPECTROMETERS W. H. Krase Apr. 1965 48p refs FOR INVESTIGATING THE COMPOSITION OF NEUTRAL (Contract NASr-21) AND IONIZED GASES IN THE UPPER LAYERS OF THE (NASA-CR-62872; RM-4437-NASA) CFSTI: HC $2.OO/MF ATMOSPHERE V. A. Pavlenko. A. E. Rafal'son. and M. D. $0.50 Shutov p 162-174 refs (See N65-24486 14-14) Measurement techniques to obtain data before manned 13. MINIATURE WIDE-BAND ELECTROMETER AM- landing expeditions on Mars are presented for any manned PLIFIER M. Ye. Slutskiy. B. I. Zarkhin. and M. A. Pushkina landing: a manned landing using aerodynamic braking from p 175-185 refs (See N64-23041 16-09) orbit; a manned landing using aerodynamic braking from hyper- 14. ENSURING RADIATION SAFETY DURING FLIGHTS bolic velocity. and a manned landing using a Mars-orbit-rendez- OF VOSTOK-3 AND VOSTOK-4 V. V. Antipov. Yu. I. Efre- vous flight profile with significant inclination of the rendez- mov. M. D. Nikitin, I. A. Savenko. and P. P. Saksonov p 186- vous orbit. A substantially different probe flight profile has to 195 refs (See N65-24487 14-29) be considered for .aerodynamic braking from hyperbolic speed 15. DOSE OF COSMIC RADIATION IN 610-UNITS OF at Mars than that considered for scientific probes. Desirable VOSTOK-3 and VOSTOK-4 V. N. Lebedev. V. S. Morozov. IneaSUrementS for unmanned probes in support of future G. F. Murin. M. D. Nikitin. and M. I. Salatskaya p 196-199 manned landings pertain to atmospheric pressure and tem- refs (See N65-24488 14-04) perature; atmospheric density; altitude measurements by a 16. EFFECT OF SPACE FLIGHT FACTORS ON THE radio altimeter in the law+- vehicle; mass spectrometry with VOSTOK-3 AND VOSTQK-4 ON THE MICROSPORES OF heat shield temperature instrument&on and-filter radiometry TRADESCANTIA PALUDOSA N. L. Delone, P. R. Popovich. of lander vehicle; surface load bearing capability: surface V. V. Antipov. and V. G. Vysotskiy p 200-224 refs (See slope: winds; mapping; radius of Mars; and oblateness of ~65-24489i4-04\ Mars. G.G.

N65-24480 Air Force Systems Command. Wright-Patterson N65-24475# Air Force Systems Command. Wright-Patterson AFB. Ohio. Foreign Technology Div. AFB. Ohio. Foreign Technology Div. SCAlTERlNG OF LIGHT IN A SPHERICAL ATMOSPHERE. COSMIC RESEARCH I1

9 N65-24526 .

I. N. Minin and V. V. Sobolev In its Cosmic Res. 6 Feb. 1964 N65-24908# National Academy of Sciences-National Re- p 61-73 refs (See N65-24475 14-29) search Council. Washington. D C Space Science Board Light scatt’er study in a planetary atmosphere taking into UNITED STATES SPACE SCIENCE PROGRAM, REPORT account the curvature of the atmospheric layer is continued TO COSPAR The case where the absorption coefficient is constant in the 1963 290 p refs Presented to the 6th Meeting of COSPAR. atmosphere is examined. An analytic solution of the basic equa- Comm on Space Res, Warsaw. 3 Jun 1963 tion determining the value of J is obtained. Light reflection from the surface of the planet is taken into account. Formulas CONTENTS are given for determining the intensity of radiation leaving 1 ASTRONOMY p 1-9 (See N65-24909 14-30) the atmosphere. The derived solution is applied to the case of 2 SOLAR PHYSICS p 10-16 (See N65-24910 14-29) the luminosityof a homogeneous sphere. A formula for determin- 3 ENERGETIC PARTICLES AND FIELDS p 17-35 ing the intensity of radiation leaving a homogeneous sphere (See N65-24911 14-29) after single diffusion is considered in detail. From this are 4 THE IONOSPHERE p 36-49 ref (See N65-24912 obtained asymptotic formulas for large values of the optical 14-13) radius of the sphere. Author 5 PLANETARY ATMOSPHERES AND METEOROLOGY p 50-71 ref (See N65-24913 14-30] 6 PLANETOLOGY p 72-84 (See N65-24914 14-30) 7 BIOLOGICAL STUDIES p 85-98 ref (See N65- N65-24526 Joint Publications Research Service. Washing- 249 15 14-04) ton, D. C. THE VENUS MODEL WITH A “COLD” ABSORBING AT- 8 CELESTIAL MECHANICS. TRAJECTORY STUDIES. MOSPHERE GEODESY. AND GRAVITY p 99-105 refs (See N65-24916 14-30) A. D. Kuz’min In its Izv. VUZov. Radiophys.. Vol. VII, No. 6, 1964 13 May 1965 p 1-16 refs (See N65-24525 14-071 9 LABORATORY ASTROPHYSICS AND RELATED SUBJECTS p 106-108 (See N65-24917 14-30) CFSTI: $7.00 10 COMMUNICATIONS SATELLITES p 109-1 12 (See The possibility of interpreting observed radiation spectrum of Venus in the centimeter and millimeter ranges by absorp- N65-24918 14-31) 11 NASA TRACKING AND DATA ACOUlSlTlON SYS- tion in the aerosol atmosphere of the planet is analyzed. It IS shown that the steep rise in the millimeter region of the spec- TEM NEW DEVELOPMENTS p 113-115 (See N65-24919 14-11) trum can be explained by absorption in the liquid-mist aerosol 12 INTERNATIONAL ACTIVITIES p 116-130 (See at about 300°K and containing 0.2 to 0.3 gm/cm2 polar N65-24920 14-30) liquid with about 3.5 X lo-’* sec relaxation time. Such liquids may be certain functional derivatives of methane, ethane APPENDIXES and benzene The aerosol dust. of mountainous and volcanic 13. SUMMARY OF LAUNCHING FOR 1962 AND origin, has not yielded satisfactory experimental data. It is PLANNED NASA FLIGHT SCHEDULE p 133-144 shown that an atmosphere with the given radiation spectrum 14. IGY ROCKET AND SATELLITE REPORT SERIES must be perfectly opaque in the infrared and visible region. p 145 Therefore. direct solar radiation cannot be the source from 15. JOURNALS IN WHICH U.S. SPACE RESEARCH which the planet surface is heated. Surface heating due to inner REPORTS ARE NORMALLY PUBLISHED p 146 heat of the planet is considered and heat flow necessary for 16. SPACE-RELATED RESEARCH SUPPORTED BY this estimated. It is pointed out that the measured decrease THE NATIONAL SCIENCE FOUNDATION p 147-148 in the brightness temperature of Venus in the decimeter range 17. BIBLIOGRAPHY ON SPACE SCIENCES 133 p may be possibly explained by absorption in the relatively cold (about 300°K) ionosphere of the planet The necessary conditions for this electron concentration in the porous ionosphere and the collision frequency in the semitransparent ionosphere are evaluated Author N65-24913 National Academy of Sciences-National Re- search Council. Washington, D. C. Space Science Board PLANETARY ATMOSPHERES AND METEOROLOGY N66-24896*# RAND Corp.. Santa Monica, Calif. Inits U.S. Space Sci. Program, Rept. to COSPAR 1963 p 50- USE OF RADIATION GAUGING METHODS TO MEASURE 71 ref (See N65-24908 14-30) ATMOSPHERIC DENSITY DURING MARTIAN ENTRY Distribution and structure of the ionized layers in the J. W. Ranftl Apr. 1965 81 p refs earth‘s atmosphere are described. Research in which the prin- (Contract NASr-2 1) cipal phenomena under study are concerned with energetic (NASA-CR-62971: RM-4434-NASA) CFSTI: HC $3.00/MF charged particles, fields and integjctions with extraterrestrial influences is presented. Aeronomical investigations are re- $0.75 Conclusions made on the basis of this study are these: ported, i.e . of temperature. density. neutral and ionic composition, aerosols, the time and space variations of all these. Except for the remoteness of the location and unknown factors in composition, the Martian atmosphere gaging problem is mass motions, and reactions with solar radiation; also meteoro- similar to that of gaging the density of the terrestrial atmos- logical studies defined as those emphasizing the larger-scale dynamical systems involving the interplay of the foregoing phere from a rapidly moving vehicle. (2) Of techniques available. X-ray backscattering with an electrically generated. continuously parameters through heat exchange. mass transport. over large geographical areas. ResJlts from planets other than the earth operating source of radiation appears most promising for gaging atmospheric density in the range to gm/cm3. are also reported if the data apply unquestionably and exclu- sively to their atmospheres. Author This range extends from those densities significant in entry effects (the lesser value) to the estimated near-surface density of Mars (the greater value). Use of an electron beam. generating soft X-rays (bremsstrahlung). is suspsted as an auxiliary technique for gaging in the range 10- to IO-’ gm/cm3. with N65-24983*# Jet Propulsion Lab.. Calif. Inst. of Tech.. Pasa- a possible extension to lo-’ gm/cm3 to overlap the X-ray dena. range. Author THE JOVIAN ENVIRONMENT

10 4 N65-27226

Lawrence M. Trafton 8 Mar. 1962 28 p refs Equilibrium gasdynamic charts suitable for use in con- (Contract NAS7-100) junction with shock tube experiments are presented for three (NASA-CR-63116; JPL-TM-33-77) CFSTI: HC $2.00/MF gas mixtures which are thought to represent the Martian at- $0.50 mosphere. The three mixtures are 65 percent COz + 35 Quantitative knowledge of the Jovian atmosphere and the percent A (Atmospheres G&H); 43 percent COz + 32 percent environment above the atmosphere is summarized. Topics A t 25 percent Nz (Atmosphere I); 11 percent CO2 + 13 covered include composition and structure of the atmosphere. percent A + 76 percent Nz (Atmospheres J&K). The charts photometric properties of the atmosphere. period of rotation, cover a range of shock velocities (Us) corresponding to stag- magnetic field. and the Jovian radiofrequency spectrum. nation temperatures greater than 4500" K and stagnation Author pressures greater than 0.1 atmosphere. Incident. reflected and standing wave. and stagnation point calculations are plotted for each mixture. A simulation plot of the stagnation point conditions in flight and in the shock tube is also presented. Author N65-24985'# Jet Propulsion Lab.. Calif. Inst. of Tech.. Pasa- dena. LOW SUBSONIC DYNAMIC-STABILITY INVESTIGATION OF SEVERAL PLANETARY-ENTRY CONFIGURATIONS N65-26075*# RAND Corp.. Santa Monica. Calif. IN A VERTICAL WIND TUNNEL. PART I NOTE ON THERMAL PROPERTIES bF MARS Jack E. Marte and Robert W. Weaver 1 May 1965 18 p refs C. bovy Apr. 1965 23 p refs (Contract NAS7-1001 (Contract NASr-21(07)) (NASA-CR-63117; JPL-TR-32-743) CFSTI: HC $l.OO/MF $0.50 (NASA-CR-63278; RM.4551 -NASA) CFSTI: HC $1.OO/MF C5cL-038 An exp_erimental investigation of the dynamic-damping 50.50 As measured by Sinton and Strong. the variation of-in- parameter. CmW for a series of possible Mars-entry configura- frared emission from the surface of Mars with local time on tions was performed in the Langley 20-ft free-spinning tunnel at low subsonic velocities. Several of the tested configurations Mars is here interpreted in terms of a simplified theory of exhibited satisfactory dynamic characteristics. including the diurnal temperature variations. in which the effect of the at- ability to recover from angular deflections up to 80". The effect mosphere is included. The results suggest a very low thermal of afterbody shape and maximum angle of oscillation on the conductivity for the upper few centimeters of the Martian dynamic stability of certain configurations was ascertained. ground. Such low conductivities appear to be possible only Drag and pitching-moment data were also obtained. Author if the material composing these layers is very fine powder having a characteristic size of not more than a few microns. If a linear relationship is assumed between convective heat transfer and surface temperature. the appropriate constant of N65-25246'# Parametrics. Inc., Waltham, Mass. proportionality is on the order of lo-' cat per cm2 sec deg. POTENTIAL PLANETARY ATMOSPHERE SENSORS: THE Author KRYPTONATE OXYGEN DETECTOR AND THE ALUMINUM OXIDE HYGROMETER Final Report 31 Dec. 1964 88 p refs Prepared for JPL N65-26255'# National Aeronautics and Space Administration. (Contract NAS7-100; JPL-950684) Langley Research Center, Langley Station. Va. (NASA-CR-63139) CFSTI. HC $3.00/MF $0.75 SOME CONSIDERATIONS ON THE USE OF ATMOSPHERIC An investigation of the characteristics of a kryptonate oxy- BRAKING FOR A TRANSFER INTO A MARTIAN ORBIT gen detector and an aluminum oxide hygrometer to be used as Jacob H. Lichtenstein Washington, NASA, Jun. 1965 57 p planetary atmosphere sensors is presented. Indirect heating of refs the detector sensor requires less power than resistive heating. (NASA-TN-D-2837) CFSTI: HC EZ.OO/MF $0.50 CSCL22C The Cu-Kr samples improve the oxygen sensitivity and allow An analytical investigation has been made into utilization a reduction in operating temperatures. A vacuum tested Cu- of the Martian atmosphere for braking in order to transfer kryptonate sample showed no decrease. in activity and retained from an approach trajectory into an orbit about Mars. The its sensitivity to oxygen. The oxygen sensitivity range was investigation was restricted to that combination of entry angles extended by using two sensors operating at different tempera- and velocities that would permit the vehicle to skip out of tures with separate Geiger tubes monitoring each sensor. The the atmosphere in order to establish an orbit about the Cu-kryptonate sensitivity to ozone could not be determined. planet. and the vehicle which was used was a blunt-faced .Geiger tubes are operable after sterilization but their electri- body typical of the Apollo spacecraft. The results show that cal characteristics are affected. Sterilization had no effect on for a ballistic vehicle the entry corridor is narrow. 3 nautical hygrometer performance. Water vapor sensitivity was retained miles, but with some lift (angle of attack approximately 20") after long term vacuum exposure but a slight shift in calibra- the corridor widens to about 30 nautical miles. Aerodynamic tions was observed. All major hygrometer elements were able braking can be utilized to reduce the approach velocity to to withstand high temperatures and high vacuum. The lucite orbital velocities without exceeding 10 Earth gravitational insulating layer was replaced with SiO. Elements were calibrated units and also .can be used to change the orbit plane abolrt to frost points of -100" C and there are indications that their 10". In the approach-velocity range of interest. an ablative heat Water vapor sensitivity extends to several orders of magnitude shield for aerodynamic braking was found to require con- below this. R.N.A. siderably less weight than the rocket fuel for thrust braking. Author

N65-25727# AVCO Corp.. Wilmington. Mass. Research and N65-27226 Joint Publications Research Service. Washing- Advanced Development Div. ton, D. C. SHOCKTUBE GAS DYNAMIC CHARTS, PART 2: MARTIAN ON THE THEORY OF THE RADIO EMISSION OF VENUS ATMOSPHERES (MODELS G, H, 1. J. AND K) A. S. Kuz'min In its IN. VUZov: Radiophys.. Vol. VIII. No. 1. K. Heron 21 May 1965 124p refs 1965 24 Jun. 1965 p 1-15 refs (See N65-27225 16-34] (RA D-TM-65-23) CFSTI: $6.00

11 . N65-27955 . We will give the analytical ratios connecting the brightness We have computed a number of models of the Martian temperature of the radio emission of a planet surrounded by thermosphere with various constants and boundary values in ,an absorbent atmosphere with the physical parameters of its the hydrostatic and heat-flux equations. The investigation is surface and atmosphere. For particular cases of the absorp- divided into two main parts. First, we have varied the basic tion by the entire thickness of the atmosphere and absorp- parameters, one or two at a time. to find to what extent an tion in homogeneous and parabolic layers. numerical solu- uncertainty in one of these fundamental parameters affects the tions have been obtained. The latter are used for an interpreta- derived exospheric temperature and other characteristics of tion of the results of radioastronomical measurements of Venus. the upper atmosphere. These models are physipally oversim- Author plified, but mathematically serve their purpose. Second, with selected specific chemical compositions. we have integrated the equations with allowance for diffusive separation and ab- N66-27966*# Geophysics Corp. of America, Bedford, Mass. sorption of sunlight in different spectral regions. A rather de- Technology Div. tailed and general discussion is included of the efficiency with STUDY OF THE .AVERAGE VERTICAL DISTRIBUTION OF which photon energy is converted into the kinetic energy of heat TEMPERATURE IN THE MARTIAN ATMOSPHERE Final in the neutral atmosphere. The computed models are thought Report to be fairly representative of an actual atmosphere with the George Ohring and Joseph F. Mariano Mar. 1965 81 p refs assumed compositions. Author (Contract NAS9-2423) (NASA-CR-65049: GCA-TR-65-3-N) CFSTI: HC $3.00/MF $0.75 CSCLO3B Theoretical computations of the vertical distribution of N66-28716# National Academy of Sciences-National Re- temperature in the Martian atmosphere are performed with the search Council, Washington. D. C. Space Science Board. use of a combined convective-radiative equilibrium model. UNITED STATES SPACE SCIENCE PROGRAM The model assumes'that the Martian troposphere is in con- [19641 355 p refs Submitted to COSPAR at its 7th Meeting. vective equilibrium and the Martian stratosphere is in radia- Florence, Italy, 8 May 1964 tive equilibrium. The height of the tropopause is a by-product A condensed compilation of reports on United States space- of the computations. Computations are performed for several science activities is presented which covers the fields of as- physical models of the Martian atmosphere to allow evaluation tronomy; solar physics; energetic particles and fields: iono- of the effect of present uncertainties in such parameters. as spheric physics: planetary atmospheres and meteorology: carbon dioxide content, surface pressure, tropospheric lapse- planetology; exobiology; the effect of the space environment rate, surface temperature, water vapor content. and distribution on man and other terrestrial organisms; celestial mechanics. ofabsorbing gas with height. On the basis of these calculations, trajectory studies. geodesy. and gravity; laboratory astrophysics a tentative model of the average vertical distribution of tem- and other supporting studies; communication satellites; inter- perature profile is based upon computations with an assumed national activities; and NASA tracking and data acquisition surface pressure of 25 mb. carbon dioxide amount of 55 m system-new developments. E.E.B. STP, water vapor amount of prec. cm. adiabatic lapse- rate in the troposphere, and surface temperature of 230" K. It is characterized by a tropopause at a height of about 5 km and an upper stratosphere temperature of about 145" K above 45 km. Author N66-28849" # National Aeronautics and Space Administration, Washington. D. C. PLANETARY ATMOSPHERES A Continuing Bibliography, N65-28631*# Geophysics Corp. of America. Bedford. Mass. Jan. 1962-Feb. 1966 SOME ASPECTS OF THE ATMOSPHERIC CIRCULATION Jun. 1965 '144 p refs ON MARS (NASA-SP-7017) CFSTI: MF $1.50 CSC! 038 Wen Tang Washington, NASA, Jul. 1'965 45 p refs A selection of annotated references to unclassified reports (Contract NASw-975) and journal articles on planetary atmospheres announced in (NASA-CR-262) CFSTI: HC $2.00/MF $0.50 CSCL 038 Technical Publications Announcements (TPA). Scientific and Inferences concerning atmospheric circulation features on Technical Aerospace Reports (STAR). and in lnternational Mars are made from analysis and interpretation of some ob- Aerospace Abstracts (IAA) is presented. Each entry in the bib- served Martian cloud systems and from application of meteoro- liography consists of a citation and abstract. The majority of logical theory to the Martian atmosphere. The trajectories of the references pertain to studies, measurements and discus- several cloud systems and the use of two different theoretical sions concerning the atmospheres of Mars, Venus and Jupiter. criteria suggest the presence of a wave type circulation regime but a limited number of references to the atmospheres of in the mean for the year on Mars Cloud observations also sug- Mercury and Saturn a,re also included. The scope of coverage gest the presence of sub-tropical high pressure centers, upper was defined to permit inclusion of references to such specific level meridional flow at equatorial latitudes. and frontal cloud topics as the theory of planetary origins, extraterrestrial en- phenomena at equatorial latitudes. Theoretical estimates of the vironment, planetary exploration and spacecraft reentry. and the mean large scale zonal and meridional wind velocities yield physical properties of the planets. All reports and amicles cited values greater than on earth. Theoretical estimates of the maxi- were introduced into the NASA Information System during mum surface wind suggest a value greater than 100 m sec-' the period January. 1962 to February. 1965. J.L.D. Computations of the vertical velocity profile. based upon a simplified "w" equation. indicate greater large scale vertical velocities than on earth, and a "dynamic" tropopause height of about 20 km Author N65-28960'# National Aeronautics and Space Administration. Marshall Space Flight Center, Huntsville, Ala. A PROPULSION ORIENTED STUDY OF MISSION MODES N66-28713# Kitt Peak National Observatory. Tucson, Ariz. FOR MANNED MARS LANDING Space Div. G. R. Woodcock 29 Jun. 1965 39 p refs STRUCTURE OF THE MARTIAN UPPER ATMOSPHERE (NASA-TM-X-53265) CFSTI: HC $Z.OO/MF $0.50 CSCLZlF Michael 8.Mc Elroy. Jean LEcuyer (Yerkes Obs.). and Joseph W. Results are given of a systems analysis of manned Mars Chamberlain [19631 32 p refs landing missions for a variety of mission modes. including

12 . N65-29509 chemical. nuclear. and electric propulsion. and aerodynamic N65-29458'# National Aeronautics and Space Administration. braking. Consistent ground rules and assumptions were used. Goddard Space Flight Center. Greenbelt, Md. The baseline mission requires 450 days for execution and HIGHLIGHTS OF RECENT SPACE RESEARCH places 4 men on the surface of Mars for 20 days. Advanced Robert Jastrow and A. G. W. Cameron 119641 65 p refs Sub- missions are discussed. Each mission was analyzed assuming mitted for Publication first Saturn V. and then a large reusable Post-Saturn ve- (NASA-TM-X-51903) CFSTI: HC $3.00/MF $0.75 CSCLO36 hicle to be available. in order to provide a co-mparison. A cost Space sciences is the collection of scientific problems to advantage was found for the reusable Post-Saturn for all but which space vehicles can make some specific contributions not very minimal planetary programs. Of the available technologies. achievable by ground-based experiments. At the present time the graphite nuclear rocket was found generally preferable this field includes broad segments of the traditional disci- to other systems for mission propulsion. Advanced nuclear plines of the earth sciences, physics. and astronomy. In later propulsion, such as ORION, was found to have great potential years the biological sciences will join this group in an im- for advanced missions. Author portant role. as our explorations of the moon and planets provide us with opportunities for studying the conditions under which physical life may have developed. The present article reviews some highlights of recent space research in the physical sciences. Author N65-29299'# NationalAeronautics and Space Administration. Ames Research Center. Moffett Field. Calif. ANALYSIS OF THE ERRORS ASSOCIATED WITH THE N65-29475*# California Univ.. Berkeley. Space Sciences Lab. DETERMINATION OF PLANETARY ATMOSPHERE STRUC- THE EVIDENCE FOR LIFE ON MARS: NATURE AND UN- TURE FROM MEASURED ACCELERATIONS OF AN ENTRY CE RTAINTIES VEHICLE D. G. Rea 119641 50 p refs Victor L. Peterson Washington. NASA. Jul. 1965 23 p refs (Grant NsG-101) (NASA-TR-R-225) CFSTl: HC $1.00/MF $0.50 CSCL 036 (NASA-CR-58430) CFSTI: HC $2.00/MF $0.50 CSCLO36 An analytic method is developed for estimating the errors A review of the current Martian environment and the ques- in the density and pressure structure of a planetary atmosphere tion of life on Mars is presented. Some of the physical prop- constructed from measurements of accelerations experienced ertiesof Mars are tabulated and include mass (0.646 X ld7g). by an entry body. Among the sources of error considered both diameter (6800 km). average density (3.96 g ~m-~).and mean singly and collectively are the measuring accuracy of the ac- distance from the sun (228 X lo6 km). Pressure. temperature. celerometers. the uncertainties in entry speed, entry angle, and gases present in the atmosphere are among other areas and aerodynamic coefficients. the frequency of data measure- discussed. but it is pointed out that no universal agreement ments. and the uncertainty of the attitude of entry bodies between scientists has been reached. Canals, vegetation, having nonzero lift-to-drag ratios. Results of sample cal- seasonal variations. dust clouds. and radiations are also dis- culations are presented to show the accuracy with which the cussed, with possible explanations relating to life on Mars extremes of a range of postulated model atmospheres for Mars presented. but again no universal agreement has been reached. can be defined upon measurements of accelerations experi- C.T.C. enced by a spherically shaped entry body. It is found that if the accelerometer method were used only over that portion of the atmosphere traversed at speeds greater than sonic speed. then N65-29509# National Academy of Sciences-National Re- any of the atmospheres postulated for Mars can be defined search Council. Washington. D. C. Space Science Board. reasonably well even when errors from all sources are com- UNITED STATES SPACE SCIENCE PROGRAM bined in the most unfavorable manner. Some of the results ob- 1965 316 p refs Submitted to the 8th Meeting of COSPAR. tained by the analytic method are compared with those from Euenos Aires. May 1965 more precise numerical calculations and the agreement is found to be excellent. Author CONTENTS: 1. ASTRONOMY pl-9 2. SOLAR PHYSICS p 1C23 3. ENERGETIC PARTICLESANDFIELDS p 24-31 4. ADVANCES IN PARTICLES AND FIELD RESEARCH N65-29433'# California Univ , Berkeley Space Sciences Lab IN THE SATELLITE ERA W. Hess. G. Mead, and M. P. Nakada CONSOLIDATED QUARTERLY PROGRESS REPORT 60p refs (See N65-29510 18-29) 27 Jul 1964 65 p Its Ser 5. Issue 37 5. IONOSPHERIC PHYSICS p 32-48 (Grants NsG-243-62 NsG-126 NsG-101. NsG-479, NsG-600 6. PLANETARY ATMOSPHERES AND METEOR- et al) OLOGY ~49-85 (NASA CR-59038) CFSTl HC $300/MF $075 CSCL 22A 7. PLANETOLOGY p 86-115 A broad multi-disciplinary program InvoKting the physical 8. LIFE SCIENCES p 116-123 biological engineering and social sciences is reported The 9. CELESTIAL MECHANICS. TRACKING. TRAJEC- studies in the social sciences cover a wide area of problems in TORY STUDIES. GEODESY, AND GRAVITY p 124-139 management operations analyses and decision making the 10. LABORATORY ASTROPHYSICS AND OTHER economic impact of the space program and the international SUPPORTING STUDIES p 140-148 import of the space program The projects in the physical bio- 11. INTERNATIONAL ACTIVITIES p 149-166 logical and engineering sciences group into areas of space science as follows Planetary A trnospheres, Lunar Structure. APPENDIXES Fields and Particles, Exobiology. Space Physiology, and Engi- 12. SUMMARY OF IAUNCHINGS FOR 1964: SATEL- neering Sciences Studies on detonation processes associated LITES. ROCKETS, AND BALLOONS p 168-181 with various types of fuels and shock waves in gases propulsion. 13. COMMUNICATIONS SATELLITES p 182-183 and reaction kinetics are also included Further a project on 14. SELECT LISTS OF RESEARCH PROJECTS AND kilovolt-ion sputtering has a twofold interest with respect to ASSOCIATED SUPPORTING AGENCIES p 184-197 space technology-the degradation of materials in space and 15. IGY ROCKET AND SATELLITE REPORT SERIES' ion propulsion The pro:ect combines solid state physics and the p 198 physics of plasmas and rarefied gases EEB 16. JOURNALS IN WHICH U. S. SPACE SCIENCE

13 N65-29722

RESEARCH REPORTS ARE NORMALLY PUBLISHED p 199 N65-30726*# Geophysics Corp of America Bedford Mass 17. BIBLIOGRAPHY ON SPACE SCIENCES 152 p (See PLANETA RY METEO RO LO GY N65-29511 18-30) George Ohring Wen Tang and Joseph Mariano Washington NASA Aug 1965 91 p refs (Contract NASw-975) N65-29722.# Geophysics Corp. of America. Bedford. Mass. (NASA CR 280) CFSTI HC $3OO/MF $075 CSCL 038 GCA Technology Div. Inferences concerning atmospheric circulation features STUDY OF EARTH’S ATMOSPHERE Final Report on Mars are made from analysis and interpretation of some R. Minzner Apr. 1965 98 p refs observed Martian cloud systems and from application of (Contract NASw-976) meteorological theory to the Martian atniosphere The tra (NASA-CR-6-8; GCA-TR-65-11-N) CFSTI: HC $3.001 MF jectories of several cloud systems and the use of two dif 60.75 CSCLWA ferent theoretical criteria suggest the presence of a wave A number of scientific problems relative to studies of the type circulation regime on Mars Cloud observations also Earth’s atmosphere were investigated and the results are suggest the presence of subtropical high pressure centers presented. Included are studies on atmospheric structure and upper level meridional flow and frontal phenomena at data. planetary atmospheres generated from solar radiation equatorial latitudes Radiative equilibrium temperatures are and absorption considerations, analytical investigation of the computed for the surface and atmosphere of Venus In the existence of successive isopycnic layers. temperature determi- model used for the computations it is assumed that the at nation from diffusion data, and proposed transition model mosphere and cloud cover are both gray in the infrared The atmospheres and problems associated with their generation. effect on the computed surface temperature of different values Two other studies are included in the appendix: low mesopaus of infrared emissivity height and thickness of the cloud temperatures over the Eglin test range deduced from density layer and infrared opacity of the gaseotis absorbers is data and temperature determination of planetary atmospheres. evaluated Equations are derived for the computation of the R.N.A. radiative equilibrium temperature profile in the nongray atmosphere above the Jovian cloud layer and circulation phenomena in the Jovian atmosphere is examined EEE

N65-30247# Hebrew Univ.. Jerusalem (Israel). Dept of Mete- orology. NUMERICAL STUDIES OF PLANETARY CIRCULATIONS IN A MODEL ATMOSPHERE Final Report N66-30733. # National Aeronautics and Space Administration. A. Huss Mar. 1965 159 p refs Goddard Space Flight Center. Greenbelt. Md. (Grant A F-EOAR -63- 108) A SURVEY OF THE METHODS DEVELOPED FOR THE IN- (AFCR L-65-350) VERSION OF THE RADIATIVE TRANSFER PROBLEM FOR The evolution of general circulation patterns has been PLANETARY ATMOSPHERES studied by means of two-level quasi-geostrophic models. Barney J. Conrath Washington, NASA, Aug. 1965 19 p refs Four different experiments were performed and compared (NASA-TN-D-2940) CFSTI: HC $1.00/MF $0.50 CSCL 04A to an earlier experiment in which the basic initial flow was Five of the methods developed for obtaining the thermal assumed to be constant at each pressure level and the Rossby profile of a planetary atmosphere from remote radiometric parameter did not depend on the latitude. The assumptions measurements are discussed and compared. An extension of made in the different runs were respectively: (1) Maximum the “variable slab” method of King is used in making an inver- zonal flow at the central latitude. (2) Maximum zonal flow sion calculation for a model atmosphere. The question of the south of the central latitude. (3)Constant zonal flow at each stability of the solutions of the basic integral equation of the pressure level and a latitudinal variation of the Rossby param- problem and its implications on the accuracy of the derived eter. (4) Maximum zonal flow south of the central latitude temperature profile are considered. It appears that some and a latitudinal variation of the Rossby parameter. The evolv- smoothing will have to be introduced. regardless of the method ing distribution of various field-variables was investigated used, in order to achieve a stable solution from a given set and compared to the actual distributions observed in the of observational data containing random errors. A considerable atmosphere The most significant results were obtained in amount of work remains to be done. including extension of the the third.run Specifically only in this case did the asymmetrical variable slab method to arbitrary band transmissions and the distributions of the field-variables around the central latitude performance of detailed error analyses of the various inversion tend to develop in the direction of the asymmetries observed methods. It also seems desirable to examine the problem from in the atmosphere. Author the point of view of the uses to be made of the derived thermal structure in order to ascertain whether the smoothed solutions retain sufficient physical information to be of value. Author

N65-30357’ California Univ San Diego Scripps lnst of Oceanography POSSIBLE OCEANOGRAPHIC AND RELATED OBSERVA- TIONS FROM SATELLITES N65-30746# Air Force Systems Command Wright-Patterson John D lsaacs In Woods Hole Oceanog lnst Oceanog from AFB, Ohio Foreign Technology Div Space Apr 1965 p 51 (See N65 30350 19 13) CFSTI HC CONCERNING THE DETECTION OF WATER IN THE AT- $7 45fMF $2 25 MOSPHERE OF VENUS Suggestions are made regarding observations of optical A Ye Salomonovich 7 Apr 1965 16 p refs Trans1 into phenomena made from satellites which would yield insight ENGLISH from Izv Vssh Ucheb Zaved . Radiofiz (Gor’kiy). into meteorological events on the earth and other planets v 7 no 1. 1964 p 51-58 Observations of the displacement of the specular image of the (FTD-TT 65 296/1+2. AD 614770) sun in ice clouds appear to be a direct measure of horizontal The question of the nature of the cloud layer of Venus and acceleration of the cloud and could provide a sounder basis the possibility of detecting water vapor in its atmosphere for the study of planetary atmospheres from earth, earth satel- is considered in the light of new data concerning the radiation lite. and flyby MWR spectrum of the dark side of the planet Author

14 L N65-321 14

N65-31047'# Geophysics Corp. of America. Bedford. Mass. atmosphere of the earth is discussed in terms of whether the PHYSICS OF PLANETARY ATMOSPHERES II: THE FLUO- amount of the rare gases present are derived by outgassing. by RESCENCE OF SOLAR IONIZING RADIATION capture from the primitive solar nebula. or by some other proc- A. Dalgarno and M. B. Mc Elroy May 1965 25 p refs ess. This problem is investigated by examining the isotopic (Contract-NASw-1283) composition of xenon. The composition of xenon extracted (NASA-C R-64424: GC A-TR -65- 15-N) C FSTI: HC $1 .OO/M F from the Murray carbonaceous chondrite is used as a standard $0.50 CSCL 20H to measure the deviations of xenon in other sources. M.R.W. The mid-day dayglow intensities arising from the fluorescence of solar ionizing radiation are calculated. The predicted overhead intensities above 120 km of the O+(2P-2D) lines at XX7319-7330A. the Meinel band system of N; the N6S-32025*# New Mexico State Univ., University Park. Ob- first negative system of N:. the first negative system of the 02. servatory. Hopfield emission system of and the second negative sys- 0; A RAPIDLY MOVING SPOT ON JUPITER'S NORTH TEM- tem of 0; are. respectively. 500 R-1 kR. 9 kR. 600 R. 2 kR. PERATE BELT R and R. Author 600 400 Elmer J. Reese and Bradford A. Smith Jul. 1965 20 p refs (Grant NsG-142-61) (NASA-CR-64568; TN-701-66-9) CFSTI: HC $l.OO/MF $0.50 N6S-31062.R' Geophysics Corp. of America, Bedford. Mass. CSCLWA GCA Technology Div. A very rapid drift in the longitude of a small dark spot on PHYSICS OF PLANETARY ATMOSPHERES. I: RAY- the south edge of Jupiter's North Temperate Belt (NTBs) was LEIGH SCATTERING BY HELIUM determined from 51 blue and ultraviolet photos. The spot made Y. N Chan (Queen's Univ.. Belfast) and A. Dalgmo Apc. 1965 seven complete circuits of the planet during 268 days of obser- 11p refs vation between July 1964 and April 1965. Mean daily rotation (Contract NASw-1283) period of the spot was calculated as sh49"18?5. The cent& of (NASA-CR-64187; GCA-TR-65-14-N) CFSTI: HC $1.00/MF the spot remained stationary near zenographic latitude +24'. $0.50 CSCLPOH withinthe probable error of the measures. This rpot was almost #variational method is used to calculate the Rayleigh scat- completely invisible to the visual observer: it represents the tering cross sections of helium as a function of wavelength. fifth observed outbreak of activity in the North Temperature The value at Lyman-a is 3.53 x cm2. Author Current. Rapidly rotating spots in this latitude seem to appem in 12-year intervals. G.G.

N65-31- Space Technology Labs., Inc.. Redondo Beach. Calif. SELECTIONS FROM THE TRW SPACE TECHNOLOGY N65-32082.U Geophysics Corp. of America. Bedford. Mass. LABORATORIES LECTURE SERIES, VOLUME TWO PLANETARY METEOROLOGY Quarterly Progress Report No. 1,21 Mar.- Jun. 1965 Thomas L. Branigan. ad. 1965 70 p refs 20 Jul. 1965 61 p refs CONTENTS: (Contract NASw-1227) 1. THE THEORY AND APPLICATION OF MASERS AND (NASA-CR-64432) CFSTI: HC $3.00/MF $0.75 CSCL 03A LASERS C. H. Townes (Mass. Inst. of Tech.) p 4-13 (See N65- Studieson the meteorology of Mars and Venus are reported. 31361 20-16) Included are data on the seasonal climatology of Mars. diurnal 2. THE BIOLOGICAL EXPLORATION OF MARS E. C. variation of the surface temperature on Mars. interhemispheric Levinthal (Stanford Univ.) p 14-21 ref (See N65-31362 20-23) transport of water vapor and the Martian ice caps. comparative 3. THE EFFECTS OF HIGH-ALTITUDE EXPLOSIONS studies of zonal wind velocities on Mars and Earth. atmospheric W. N. Hess (NASA. Goddard Space Flight Center) p 22-34 refs circulation in the Venusian atmosphere. and the composition (See N65-31363 20-29) of the Venusian clouds. S.C.W. .4. THE ABUNDANCE OF THE ELEMENTS H. C. Urey (Calif. Univ.) p 35-46 refs (See N65-31364 20-06) 5. THEORETICAL ASPECTS OF THE SPACE RELATIV- ITY-GYROSCOPE EXP5RIMENT L. I. Schiff (Stanford Univ.) p 47-50 refs (See N6Y-31365 20-23) N6632114*# National Aeronautics and Space Administration. 6. ENERGETIC SOLAR PARTICLES K. A. Anderson (Calif. Goddard Space Flight Center. Greenbelt, Md. Univ.) p 51-60 refs (See N65-31366 20-29) THE INFRARED INTERFEROMETER SPECTROMETER 7. THEORIGINOFPLANETARYATMOSPHERES A. G. W. EXPERIMENT (IRIS). VOLUME I: MARTIAN FLY-BY Cameron (NASA. Goddard Inst. for Space Studies) p 61-70 MISSION ref (See N65-31367 20-30) R. A. Hand and L. Chaney Jul. 1964 56 p refs (NASA-TM-X-55070; X-65064-204) CFSTI: HC $3.00/MF $0.50 CSCLO3A Theextraction of significant information on the atmosphere N66-31367 National Aeronautics and Space Administration. and surface of Mars from thermal emission of the planet is Goddard Inst. for Space Studies, New York. discussed. Also, the design of an infrared interferometer THE ORIGIN OF PLANETARY ATMOSPHERES capable of mea6uring thermal emission spectrum of the planet A. G. W. Cameron 3 Mar. 1964 In Space Technol. Labs.. Inc. is described; the requirements and constraints of the infrared Selections from the TRW Space Technol. Labs. Lecture Ser.. interferometer experiment on a planetary fly-by spacecraft Vol. 2 1965 p 61-70 ref (See N65-3136020-34) are documented. The information will be extracted from the Various processes are considered which might lead, to thermal emission spectrum within the interval of 2000 cm-' the formation of an atmosphere for most of the planets. Mech- to 500 cm-'. The experiment is aimed at a wide spectral range anisms for input of gases into an atmosphere. and for loss of to permit clear identification of many predictable spectral gases f;om an atmosphere are discussed. The structure of the features and to allow a search for unexpected phenomena. atmospheres of Jupiter, Mars. and Venus is illustrated. Micro- For a nominal fly-by distance of 5OOO km. the resolved area wave brightness measurements of Venus are interpreted. The will be a circle of 250-km diameter. E.E.B.

15 N65-32199

N65-32199*# Stanford Univ.. Calif. Radioscience Lab. N65-33556 National Aeronautics and Space Administration. THE TWO-FREQUENCY, BlSTATlC RADAR-OCCULTA- Washington, 0. C. TlON METHOD FOR THE STUDY OF PLANETARY IONO- THE ROLE OF REMOTE SENSING IN THE NASA MANNED SPHERES Scientific Reports No. 1 and No. 7 INTERPLANETARY PROGRAM AND VICE VERSA G. Fje1dbo.V. R. Eshleman, 0. K. Garriott. and F. L. Smith, Ill Rollin W. Gillespie In Mich. Univ. Proc. of the 3d Symp. on Apr. 1965 33 p refs Remote Sensing of Environment Feb. 1965 p 79-90 refs (Grants NsG-377; NGR-05-020-065) (See N65-33550 22-13) (NASA-CR-64460; SEL-65-044) CFSTI: HC $2.00/MF $0.50 The remote sensing of planetary and interplanetary envi- CSCL 038 ronments is essential to planning and establishing manned inter- A method for the study of planetary ionospheres is pre- planetary capability. while that capability will extend the op- sented which is based on the use of radio waves propagated portunities for remote sensing. Some engineering features of between the earth and a spacecraft on an occulting trajectory any possible manned interplanetary program are given as a beyond the planet. Phase path. group path, or amplitude guide in planning remote sensing experiments. It is urged that measurements made during spacecraft immersion into, and terrestrial and planetary applications of remote sensing should emersion from. the occulted zone could be used to deduce be integrated, at once. Author vertical electron density profiles at the two limb positions probed by the waves. By using two or more harmonically related frequencies, the ionospheric measurements would be self-calibrating, thus avoiding the extreme measurement and computational precision that otherwise would be required. N65-33835'# IIT Research Inst.. Chicago. 111. It is suggested that this simple technique would be particularly A REVIEW OF RECENT DETERMINATIONS OF THE COM- applicable for the initial exploration of planetary atmospheres. POSITION AND SURFACE PRESSURE OF THE ATMOS- Author PHERE OF MARS M. W. P. Cann. W. D. Oavies. J. A. Greenspan. and T. C. Owen Washington, NASA. Sep. 1965 186 p refs (Contract NAS5-9037) N66-32433. Jet Propulsion Lab., Calif. Inst. of Tech.. Pasa- (NASA-CR-298) CFSTI: HC $5.00/MF $1.25 CSCL 038 dena. Recent determinations of the Martian surface pressure ANALYSIS OF EQUILIBRIUM SHOCK-LAYER RADIA- are reviewed. The polarimetric work of Dollfus is discussed TION FOR ATMOSPHERIC.ENTRY TO MARS and a new value of the surface pressure, 63 mb. is derived F. Wolf and J. Spiegel In its Space Programs Sum:No. 37-33. from his data making use of more recent photometric data Vol. IV 30 Jun. 1965 p 99-103 refs (See N65-32410 and of a new treatment of the angular dependence of the 21-11) CFSTI: HC $7.00/MF $1.75 planetary surface brightness. A photometric argument by The gas radiance of mixtures simulating the Martian at- Musman is discussed and the general effects of aerosols and mosphere was calculated. The total equilibrium radiation in- various mixtures of gases on the pressure estimates are intensity of a 30% carbon dioxide and 70% nitrogen mixture vestigated. It is shown that these lead to a range of pressures behind the normal shock is given as a function of the free- depending on the assumptions made. and that this method of stream density with flight velocity as a parameter. The total pressure determination leads to indeterminate results. Several equilibrium radiative energy to the stagnation region was spectroscopic works are reviewed and a value of 45 k25 m-atm also determined for the same mixture. From the study it for the Martian Cop abundance is derived, corresponding to a appears necessary to compute equilibrium radiation at much mean Martian atmospheric temperature of 200" K. Using this lower density than where experimental data exist. The simple abundance. various methods for estimating the surface pressure procedure of normalizing to free-stream density appears to are reviewed, leading to surface pressures ranging from 13 introduce some problems. At a fixed velocity, density de- to 33 mb with relative errors on the order of +go%. The large pendence of radiation is acceptable for engineering estimates. uncertainty is due to the fact that the abundance determination The density dependence with velocity is significant. For more rests on the measurement of three weak lines in a single exact heat transfer predictions. a simple exponential density spectrogram. R.N.A. dependence should not be used. E.E.B.

N66-33919'# State Univ. of Iowa. Iowa City. Dept. of Physics and Astronomy. N65-32574'# National Aeronautics and Space Administration. ABSENCE OF MARTIAN RADIATION BELTS AND IMPLI- Washington. D. C. CATIONS THEREOF SPACE EXPLORATION-WHY AND HOW J. A. Van Allen. L. A. Frank. S. M. Krimigis. and H. K. Hills Edgar M. Cortwright [19641 22 p Aug. 1965 30p refs Its Rept.-65-30 (NASA-EP-251 CFSTI. HC $l.OO/MF $0.50 CSCL 22A (Grant NsG-233) The question "Why explore space when so much of our (NASA-CR-64870) CFSTI: HC $2.00/MF $0.50 CSCL 038 earth remains unexplored?" is answered in a paper based A system of sensitive particle detectors on Mariner IV on an address to the Norwegian Geographical Society. Main showed the presence of electrons of energy E, > 40 keV out Sections deal with the space around the earth, atmospheric to a radial distance of 165.000 km in the morning fringe of circulation and the weather. the earth. and the moon and the the earth's magnetosphere but failed to detect any such elec- planets Illustrations are included of the Orbiting Geophysacal trons whatever during the close encounter with Mars on July Observatory and schematics of the ionosphere and solar effects 14-15. 1965. for which the minimum areocentric radial dis- on the earth's atmosphere Also presented are pictures of tance was 13,200 km. This result is interpreted to mean that storms and fronts. the life cycle of a cyclone. and limitations the ratio of the magnetic dipole moment of Mars to that of the of satellite radar for measuring precipitation The Tiros, T~~~ earth MM/ME is surely less than 0.001 and probably less (USWB).and Nimbus meteorological satellites are diagrammed; than 0.0005. The corresponding upper limits on the equatorial and pictures of satellite photography are included. The signifi- magnetic field at the surface of Mars are 200 and 100 gammas. cance of high resolution lunar photography is Considered. and respectively. It appears possible that the solar wind interacts lunar photographs taken by Ranger VI1 are presented. M.w.R. directly with the Martian atmosphere, Author

16 . . N65-35976 N65-33962.# Consultants and Designers. Inc.. Arlington. Va. M. H. Davis and S. M. Greenfield In AFCRL Pocr.. 1964 STUDY OF THE ELONGATION OF HORNS OF THE VENUS AFCRL Sci. Balloon Symp. Jul. 1965 p 34-351 refs (See CRESCENT IN JUNE 1964 [ETUDE DE L'ALLONGEMENT N65-34804 23-20) DES CORNES DU CROISSANT DE VENUS EN JUlN 19641 The feasibility of Mars balloon operations are discussed. Audouin Dollfuss and Eric Maurice 21 Jun. 1965 8 p Transl. Estimates of the weight and volume requirements for such a into ENGLISH from Comp. Rend. Acad. Sci. (Paris). v. 260. balloon system are given. Two balloon types are considered: Groupe 3. 11 Jan. 1965 (1) A balloon to carry instruments from one point on the (Contract NAS5-3760) planet surface to another point nearby for which hydrogen- (NASA-TT-F-9685: ST-OA-10343) CFSTI: HC $1.00/MF filled balloons of the equal-pressure type are visualized. (2) $0.50 CSCLO3B A balloon to float at a fairly high altitude for long periods The photometry of the aureole prolonging the horns of carrying instruments designed to observe the atmosphere and Venus at inferior conjunction indicates that the atmosphere surface for which a ballasted equal-pressure balloon or the superpressure balloon is considered. Air-launched systems above the cloud layer remains charged of particles of approxi- are suggested for the Mars balloon. Equations are given for mately 1.5~in diameter. whose number decreases by a factor the ratio of balloon mass to total system mass. and the ratio oi 2 approximately every 2.8 km and whose diffusion coef- of payload volume to total system volume. Also. parameters ficient is 3.10-* stilb/phot per centimeter cube contrary to of the system are tabulated. No calculations made indicate the Sun at the level of the cloud layer. Author that the Mars balloon concept is invalid. E.E.B.

N65-34101# National Academy of Sciences-National Re- N65-34835 Observatoire de Paris (France). Section d'Astro- search Council. Washington. D. C. Comm. on Atmospheric physique. Sciences. DETECTION OF WATER VAPOR IN THE ATMOSPHERES THE ATMOSPHERIC SCIENCES, 1961-1971. VOLUME II: OF VENUS AND MARS SUMMARIES OF PLANNING CONFERENCES Audouin Dollfus In AFCAL Proc., 1964 AFCRL Sci. Balloon 1962 128p Symp. Jul. 1965 p 409-417 refs (See N65-34804 23-20) Balloon flights for the detection and measurement of (PUBL.-946) water vapor in the atmosphere of Venus and Mars are dis- Summaries are presented of the planning conferences cussed. A lightweight sealed cabin, and telescopic and spectro- on Atmospheric Physics and Chemistry; Atmospheric Dynam- scopic devices used to record the measurements are described. ics and Atmospheric Structures and Circulations; Eiome!eorol- Two lifting devices are mentioned. One type is composed of a ogy; Engineering Applications; and New Technologies. Specific cluster of 104 dilatable sounding balloons organized in 34 areas of aeronomy. planetary atmospheres. atmospheric com- groups of three balloons. one above the other. along a verti- position. cloud physics. climates. water resources. agriculture cal cable 1400 feet long. The second device uses a chaplet- meteorology, air pollution abatement. and data processing like cluster of 23 neoprene Darex 7000-gram balloons capa- and computing are among the subjects discussed in detail. ble of ascents to BOO00 feet. An observation was made from E.E.B. a high mountain site to determine. for calibration purposes. the amount of water vapor contributed by the earth's atmosphere. Reduction of data. including minor corrections and recalibration. yielded the following water vapor values: for N65-34244-n Aerojet-General Corp., Azusa, Calif. Venus. 0.7 X lo-' g/cm2. and for Mars. 1.5 x lo-' g/cm2. ENGINE OPERATING PROBLEMS IN SPACE: THE SPACE M.R.W. ENVIRONMENT D. Christensen Washington, NASA. Sep. 1965 227 p refs (Contract NAS7-98) N65-35792. # National Aeronautics and Space Administration. (NASA-CR-2941 CFSTI: HC $G.OO/MF $1.50 CSCL 22A Ames Research Center. Moffett Field. Calif. This volume presents a comprehensive definition of the EQUILIBRIUM THERMODYNAMIC PROPERTIES OF space environment as it is presently known. For the purpose THREE ENGINEERING MODELS OF THE MARTIAN of this program. this environment consists of the solar sys- ATMOSPHERE tem. excluding the earth and its inner atmosphere. Special Harry E. Bailey Washington. NASA. 1965 164 p refs emphasis is given to data on electromagnetic and particulate (NASA-SP-3021) CFSTI: HC $2.50/MF $1.00 CSCL 20M radiation. meteoroid flux, and the structure and composition Entropy. enthalpy, pressure. and sound speed of three car- of the planetary atmospheres. A list of 405 references is in- bon dioxide-nitrogen mixtures are presented graphically for cluded; many of these are annotated. Author wide ranges of temperature and density. The temperature range is 250" K 5 T 5 25000" K (AT = 250" K). The density range is -1.0 5 log p/po 5 +3.0 (Alog p/po = 0.2). The chemical compositions of the three mixtures correspond to N65-34804# Air Force Cambridge Research Labs.. Bedford. those selected as engineering models of the Mars atmosphere Mass. in NASA TN D-2525. Author PROCEEDINGS, 1964 AFCRL SCIENTIFIC BALLOON SYMPOSIUM N65-35976. # National Aeronautics and Space Administration. Arthur 0. Korn. Jr.. ed. Jul. 1965 439 p refs Its AF Surv. in Marshall Space Flight Center. Huntsville. Ala. Geophys. No. 167 DERIVATION OF PARAMETRIC VALUES FOR A GREEN- (AFCRL-65-486; AD-619695) HOUSE MODEL OF THE CYTHEREAN ATMOSPHERE Symposium papers are presented on advances in balloon Robert 8. Owen 7 Sep. 1965 77 p refs design. materials, instrumentation, meteorology. and scientific (NASA-7M-X-53327) CFSTI: HC $3.00/MF $0.75 CSCL 03A applications. For individual titles see N65-34805-N65-34836. Presented is a self-consistent model atmosphere for the planet Venus. with emphasis on parameters of general use in developing vehicle design criteria. Kern and Schilling's pro- N65-34830 RAND Corp.. Santa Monica, Calif. gram for generation of atmospheric parameter values is coupled THE MARS BALLOON-FEASIBILITY AND DESIGN with the most recent estimates of surface conditions in order

17 N6 5-36000

to derive the atmospheric environment at different altitudes The latitudinal bands of Jupiter are discussed as phe- A range of initial values is used to produce a parametric band nomena reflecting. in Jupiter's atmosphere, the particular most representative of actual conditions Because of the ex- tektonics of the planet. Physical relationships are established treme pressures and temperatures involved. it is felt that de- connecting the latitudes of the bands. the active formations, sign for such an environment presents an engineering prob- and the critical parallels-a relationship which can only arise lem of the first magnitude Author in the solid core of the planet through variation of the potential of deforming forces. The author comes to the conclusion that a volcanism is. perhaps, produced by changes in the rotational regime of the planet. N65-36000# Harvard Coll. Observatory. Cambridge, Mass. Author Meteor Dept. THE STUDY OF METEOR PHENOMENA, UPPER ATMOS- PHERE WINDS, AND TURBULENCE AND CHEMILUMI- NESCENCE IN THE UPPER ATMOSPHERES Final Report N66-10609*# Stanford Univ.. California. Radioscience Lab. Allan F. Cook, Richard E. Mc Crosky. and Fred L. Whipple RESEARCH AT THE STANFORD CENTER FOR RADAR 31 Dec. 1964 212 p refs ASTRONOMY Semiannual Report No. 5,l Jan.-30 Jun. 1965 (Contract AF 19(604)-51961 V. R. Eshleman Jul 1965 11 p refs (AFCRL-65-33; AD-616732) (Grant NsG-377) (NASA-CR-67794) CFSTI: HC $1.00/MF $0.50 CSCLO3B CONTENTS: Radar astronomy research is presented on cislunar gas 1. THE STUDY OF METEOR PHENOMENA A. F. Cook, studies, planetary atmospheres and ionospheres, detection of R. E. McCrosky. and F. L. Whipple 25 p refs (See N65-36001 interplanetary shock waves, solar radar studies. and polari- 24-30) zation of decametric radiation from Jupiter. R.N.A. 2. UPPER ATMOSPHERIC WIND FIELDS FROM ME- TEORIC TRAINS R. F. Hughes and A. F. Cook 117 p refs (See N65-36002 24-13) N66-10684'# Northrop Space tabs.. Hawthorne, Calif. 3. OPTICAL PROPERTIES OF SATURN'S RINGS, II: ENGINEERING STUDY TO DETERMINE FEASIBLE TWO-COLOR PHASE CURVES OF THE TWO BRIGHT RINGS METHODS OF SIMULATING PLANETARY ALBEDO AND F. A. Franklin and A. F. Cook 68 p refs (See N65-36003 RADIATION EFFECTS UPON THE THERMAL BALANCE 24-30) OF SPACECRAFT Final Report Constantino Cafaro, Mer1 K. Fairchild. Herbert J. Harris. Arnold P. Shlosinger. and Vincent M. Urban Jan. 1965 168 p refs Prepared for JPL N66-36391*# Hamilton Standard Div.. United Aircraft Corp.. (Contracts NAS7-100; JPL-95,0829) Broad Brook. Conn. (NASA-CR-67813: NSL-65-5) CFSTI: HC $5.00/MF $1.00 MARTIAN ATMOSPHERIC COMPOSITIONAL ANALYSIS: CSCL 20H ITS BIOLOGICAL SIGNIFICANCE First Quarterly Progress This report presents the results of an engineering study Report, 16 May-15 Aug. 1966 and analysis to determine the effects of planetary albedo and Dian R. Hitchcock and J. E. Lovelock (Houston Univ.) 119651 radiation from Mars and Venus on the thermal balance of 12p refs spacecraft orbiting these planets, and to study feasible methods (Contract NASw-871) of simulating Mars and Venus planetary albedo and radia- (NASA-CR-67354) CFSTI: HC $1.00/MF $0.50 CSCL 038 tion in a space simulation chamber. The existing literature for The potential biological significance of two types of atmos- Mars and Venus provides a multiplicity of planetary albedo pheric data is critically reviewed. These are the relationship values. This study used the range of published albedo values between the atmosphere and surface material. as revealed by to effectively bound the thermal effects on vehicles orbiting anexperiment designed to detect a free energy gradient between these planets. The results of the thermal analysis indicate that the two; and observations of the Concentrations of selected the effects of planetary albedo and radiation are significant. major and trace components of the atmosphere including Therefore. the albedo and radiation should be considered in the isotopic abundances. Discussed are studies relating to life design and test of spacecraft whose mission includes close detection by detection of chemical free energy in surface matter: orbit of these planets. The extreme variation of environment Martian atmospheric compositional analyses; and Martian for Mars and Venus and the conflicting simulation features de- biological atmospheric experiments. M.G.J. sired for planetary radiation simulations makes it impractical to devise one simulator system for both Mars and Venus. Simu- lator design should be tailored to the specific requirements of the spacecraft and its mission. Author

1966 N66-10836# McGill Univ.. Montreal (Quebec). Arctic Mete- orology Research Group. STAR ENTRIES THE BEHAVIOUR OF PLANETARY WAVES IN AN AT- MOSPHERIC MODEL BASED ON SPHERICAL HARMONICS Scientific Report No. 1 Andre Robert Jun. W65 93 p refs Its Publ. in Meteorol. No. 77 N66-10590# Defence Research Board. Ottawa (Ontario) (Contract AF 19(628)-49551 DIRECTORATE OF SCIENTIFIC INFORMATION SERVICES. (AFC R L-65-488: AD-62 1073) THE LATITUDE BOUNDARIES OF JUPITER'S BANDS The grid point method commonly used in numerical cal- M V Stovas Aug 1965 8p refs Trans1 into ENGLISH from culations presents serious problems in experiments that IGY Inform Bull, IGY Organizing Comm . Presidium of the require a global coverage of the meteorological variables, The Acad of Sci. Ukrain SSR. (Kiev). no 3. 1961 p 65-70 shape of the earth and the form taken by the meteorological (T-439-R) CFSTl HC $1 00/MF $0 50 equations in a system where longitude and latitude are the

18 N66-12974 basic coordinates. suggest the use of spherical harmonics for N66-11743*# Consolidated Systems Corp.. Monrovia, Calif. the horizontal specification of the variables. This method A FEASIBILITY STUDY OF THE MASS SPECTROMETER eliminates grid points and all the truncation errors due. to the INSTRUMENTATION FOR THE ANALYSIS OF THE MAR- finite difference approximations. It also permits the retention TIAN ATMOSPHERE Ficul Report of all the terms in the meteorological equations including those W. J. Whistler 7 Sep. 1962 277 p Prepared for JPL that would normally exhibit an anomalous behaviour near (Contracts NAS7-100: J PL-950327) the poles. A model based on five levels and 15 coefficients (NASA-CR-67959) CFSTI: HC $6.OO/MF $1.50 CSCL 14B was integrated for 200 days starting from an atmosphere at The feasibility of a mass spectrometer analysis of the rest. The integration was then continued for another 20 days Martian atmosphere was investigated. The mass spectrometer with 45 coefficients. Cioss-sections show a jet stream in each system must yield accurate analytical data in the presence of hemisphere and low level easterlies along the equatorial +It. imposing restrictions on instrument size. weight. power. and The amplitudes. the phase speeds and the structure of the magnetic fringe fmld; sample time and conditions; and trans- planetary waves in the model compare favourably with their mitting channel capacity. The proposed analyzer is the instru- atmospheric equivalents. The results of this integration indi- ment known as quadrupole mass filter. A general theoretical cate that spherical harmonics could be used profitably in analysis of the quadrupole analyzer was carried out discussing general circulation models and for the preparation of extended resolution, transmission efficiency. and power requirements. range forecasts. Author (TAB) Theoretical analyses were also performed on the electron bombardment and alpha ion sources; thermal and perfect imaging focal systems; Knudsen flow, getter ion pumping. 166-10996 Air Force Cambridge Research Labs., Bedford. electrometer detectors. anddata handling techniques. Author Mass. PLANETARY ENVIRONMENTS Roger A. Van Tassel and John W. Salisbury In its Handbook of N66-12248*# Geophysics Corp. of America. Bedord. Mass. Geophys. and Space Environment 1965 19 p refs (See N66- GCA Technology Div. 10976 02-13) EXPERIMENTAL AND THEORETICAL STUDIES IN PLANE- Brief descriptions and tabulated data are presented on the TARY AERONOMY F-l Repoft environments of Mercury. Jupiter, Saturn. Uranus. Neptune. F. F. Marmo Apr. 1965 133 p refs and Pluto. More detailed information is presented for Venus (Contract NASw440) and Mars and includes discussions on their atmospheres. thermal (NASA-CR-68106: GCA-TR-65-16-N) CFSTL: HC $4.OO/MF environments, magnetic fields, surface features, satellites. and other tabulated data. R.N:A. $1.00 CSCLO4A Detailed technical summaries are presented of published reports generated by investigations of the photochemistry of N66-10998 Air Force Cambridge Research Labs.. Bedford. planetary atmospheres. theoretical studies. exparimental Mass. studies in the vacuum ultraviolet (VUV) and extreme ultra- RADIO ASTRONOMY violet (EUV) spectral regions, and theoretical aeronomy. The N. H. Dieter, J. P. Castelli. and D. W. Ushakoff In its Handbook approach employed is discussed, and pertinent tables. figures. of Geophys. and Space Environment 1965 15 p refs (See and data analyses are included. Brief summaries are also N66-10976 02-13) presented on other phases of the continuing research effort Two aspects of radio astronomy. the sources of radiation to indicate the level of the research. the scope of the work and the effects produced by the terrestrial atmosphere on the involved. and the scientific direction and approach of future in- radiation received. are discussed. The discussion begins with vestigations. M.G.J. fundamental concepts and definitions used in radio astronomy. Atmospheric refraction. scintillation. and absorption effects are examined along with radio emission from the moon. planets. W-12611# Air Force Systems Command. Wright-Patterson background radiation, discrete sources. and radiation observed AFB. Ohio. Foreign Technology Div. in the hydrogen 21x117 line and OH 1Bxm line. Included are THE FREEWAY FROM OUTER SPACE background radiation maps ranging in frequency from to 38 960 A. Shibanov and F. Borisova 24 Jun. 1965 10 p Transl. into Mcp. and graphical and tabulated data on the spectra and flux ENGLISH from Tekhn. Molodezhi (Moscow). no. 9. 1963 density .wrsus frequency of the discrete radio sources Cass- P3-4 iopeia A, Cygnus A. Taurus A. Virgo A. and Centaurus A. (FTD-TT-65-741/ 1+2+4: AD-620975) R.N.A. A popularized account is given of atmospheric factors to be considered in space ftight. TAB N66-11136*# Consultants and Designers. Inc., Arlington. Va. MEASUREMENTS OF POLARIZATION AND OF BRIGHT- NESS TEMPERATURE DISTRIBUTION OF VENUS IN THE N66-12974. # California Univ.. Berkeley. Space Sciences Lab. 10.6 UTI WAVE [IZMERENIYA WLYARlZATSll I RASPRE- THE ATMOSPHERE AND SURFACE OF MARS A !hhtive DELENIYA YARKOSTNOY TEMPERATURY VENERY NA Review VOLNE 10.6 CM] D. G. Rea [19651 67 p refs Presented at the Lunar and Plane- A. D. Kuz'min and B. Dzh. Klark 14 May 1965 Transl. into tary Seminar, Calif. Inst. of Tech., Pasadena, 17 Sep. 1965 ENGLISH from Dokl. Akad. Nauk SSSR. Astronomiya. v. 161. (Contract NASr-220: Grant NsG-101) no. 3.1965 p 551-553 (NASA-CR-68136) CFSTI: HC $3.00/MF $0.75 CSCL 038 (Contract NAS5-3760) Recent significant developments in our knowledge and (ST-RA-LPS-10334; NASA-TT-F-9682) CFSTI: HC $I.OO/ understanding of the Martian atmosphere and surface are re- MF $0.50 CSCLO3B viewed. The surface pressure estimates using different tech- This work is the continuation in a broader fashion of the re- niques are roughly as follows: near infrared spectroscopy. search conducted in 1962 at CALTECH radioastronomical ob- 3 to 90 mb: ultraviolet albedo and spectrum, 3 to 30 mb. The servatory which consisted in experimental measurements of atmospheric abundances are: COz. 45 m atmo; HzO. 14p brightness distribution along Venus' disk in nonpolarized radia- precipitable H20. variable in time and space: no others de- tion. This pursuit took place near the 1964 lower coniunc- tected. Of the latter two of the most important are 02 and 03, tion and included polarization measurements. Author whose upper limits are 2 cm atm and 4p atm respectively. The

19 N66- 12992

atmosphere probably contains a semi-permanent load of sub- mission analysis. Evaluated were the Mars 1969 and 1971 micron particles (COS or H20 crystals. or dust) giving the orbiter, the Mars 1973 and 1975 back-up orbiter, the Mars "blue haze". The blue and white clouds are attributed to ice 1975 bus. the Mars 1969 lander. Mars landers after 1969. and 0: COP particles. The surface is characterized by-bright and Venus landers. G.G. dark areas. The former are covered with dust which is evidently a weathering product of the dark areas. The color is attributed to the ferric ion. but its concentration relative to silicon need not be higher than the relative solar abundance. Dust storms N66-13666*# Jet Propulsion Lab., Calif. Inst. of Tech.. Pasa- originate in the bright areas, indicating that the local winds dena. at an altitude of 1 meter are higher than 145 km hr-', and THE USE OF CONVENTIONAL WIND TUNNELS TO SIMU- may be as high as 300 km hr-', or higher. The dark areas LATE PLANETARY ATMOSPHERIC AERODYNAMICS consist of maria. oases. and canals. It is suggested that the Howard Koester and Norman Fox 15 Nov. 1965 14 p refs maria are extensive deposits of volcanic ash. the oases impact (Contract NAS7-100) craters of small asteroids. and the canals loci of small vol- (NASA-CR-68792; JPL-TR-32-762) CFSTI: HC $l.W/MF canoes oriented along crustal cracks connecting the oases $0.50 CSCL O1A with themselves and with the volcanoes. Author The aerodynamic effects of planetary atmospheric simulation have been experimentally investigated in wind tunnels. Admixtures of carbon dioxide into the conventional dried air N66-12992'# Southwest Center for Advanced Studies, Dallas. working fluid were used to simulate variations of the atmos- Tex. pheric properties. The performance of the wind tunnels. the techniquesused. and samples of the data obtained are presented. MULTI D lSCl P LINARY R €SEA RCH IN SPACE-R ELATE D The results obtained indicate that, within a given range. this SCIENCE AND TECHNOLOGY Semiannual Report approach will yield excellent data for planetary atmosphere entry 30 Sep. 1965 101 p refs vehicle design. Author (Grant NsG-269-62) (NASA-CR-68362) CFSTI: HC $4.00/MF $0.75 CSCL 04A Research activities from April through September. 1965 centered on various studies of planetary atmospheres, iono- N66-13673'# Smithsonian Astrophysical Observatory. Cam- spheric and radio physics, particles and fields. and planetology. bridge. Mass. This summary contains the following topics: History of earth THE ROTATION OF THE PLANET MERCURY atmopshere: atmospheric and ionospheric structure: plasmas; Giuseppe Colombo and Irwin I. Shapiro 15 Nov. 1965 27 p geomagnetic variations; energetic particles; auroral current refs Revised systems: planetary atmospheres and interplanetary physics: (Grant NSG-87-60) atmospheric chemistry; infrared studies; lunar investigations; (NASA-CR-68703; SA0 Special Rept.-l88-R) CFSTI: HC $2.00/ geochemistry: planetary structure; paleomagnetism; kinetic MF $0.50 CSCLO3C theory: spinors and cosmology: gravitational radiation: Reliable radar observations and some of the generally un- various mathematical calculations; and space technology reliable optical observations of Mercury are shown to be con- studies. G.G. sistent with its rotating in a direct fashion with a period just two-thirds of its orbital period. This possibility may be under- N66-13403*# General Electric Co., Philadelphia, Pa. Missile stood as a consequence of the combined solar torques exerted on tidal deformations and on a permanent asymmetry in Mer- and Space Div. VOYAGER DESIGN STUDY. VOLUME IV: SYSTEM DE- cury's equatorial plane, as suggested by Colombo. A simple SIGN model illustrating this superharmonic resonance phenomenon 15 Oct. 1963 566 p refs is developed in some detail; several alternative paths by which (Contract NASw-696) Mercury could have reached its present state of motion are discussed briefly. Author (NASA-CR-51839: DOC.-63SD801) CFSTI: HC $8.66/MF $2.75 CSCL 228 The following studies are reported: Entry Lander-design criteria and limitations, subsystem descriptions. basic trajec- N66-13681# RAND Corp.. Santa Monica. Calif. tories, configuration matrix. etc.; and Orbiter System Introduc- COMMENTS ON THE DETECTION OF WATER AND ICE tion-configuration selection and sequence of events, config- CLOUDS ON VENUS uration design and integration, thermal control, structural and D. Deirmendjian Oct. 1965 14 p refs Presented at the JPL/ dynamic criteria. and weight analysis. Considered were various CIT Conf. on the Moon and Planets, Pasadena, Calif.. 13-18 systems requirements for entry into the Venus or Mars atmos- Sep. 1965 pheres. G.G. (P-3245; AD-622987) CFSTI: HC $1.00/MF $0.50 Recent infrared spectroscopic evidence of the existence of ice clouds on Venus is verified by comparison with the spectra N66-13407*# General Electric Co.. Philadelphia. Pa. Missile of optically dense, terrestrial sunlit cirrus clouds. The un- and Space Div. certainties regarding the total water content of the planetary VOYAGER DESIGN STUDY. PART 11. VOLUME 111: SUB- atmosphere are pointed out. and an experiment is proposed SYSTEM DESIGN for the detection of possible water droplet clouds. otherwise 15 Oct. 1963 407 p refs obscured by the observed ice clouds. Author (TAB) (Contract NASw-696) (NASA-CR-51837; D0~.-63SD801)CFSTI: IHC $7.07/ MF $2.00 CSCL 228 N66-14057'# National Aeronautics and Space Administration. The following studies are reported. Guidance and Con- Washington. D. C. trol-guidance analysis. attitude control. Voyager lander high VOLCANIC ACTIVITY ON MARS (VULKANICHESKAYA gain antenna control. and alternatives: frOpUlSiOn-orbiter AKTIVNOST' NA MARSE] propulsion. lander propulsion. and attitude control propulsion: G. N. Katterfel'd Jan. 1966 18 p refs Transl. into ENGLISH Power Supply-system selection and basic studies. recom- from Priroda (Moscow). no. 8. 1965 p 103-109 mended and alternate Systems. power supply performance, and (NASA-TT-F-410) CFSTI: HC $l.OO/MF $0.50 CSCL 038

20 N66-14703

The Mars opposition occurred in March. 1965-the most Joseph W. Chamberlain (Kitt Peak Natl. Obs.), and Richard M. favorable time for observing its surface from the earth. Many Goody (Harvard Univ.) In it5 Space Res. Dec. 1965 p 96-107 astronomers pursued a great many studies at this time. which refs (See N66-14327 05-30) CFSTI: HC $4.00/MF $0.75 provided new information about Mars. Therefore. the present A priority system is set up for experiments dealing with article has become timely. The author of this article has uti- planetary upper atmospheres, and a bibliography is included for lized many data published during the last 55 years. primarily articles on the subject. Studies serving engineering require- data obtained by Japanese astronomers which are almost un- ments for support of exploration are considered urgent: pro- known to the Soviet reader. Author grams related to exobiology and the evolution of life are rated important: and research bearing on the origin and evolution of the solar system is classified as desirable. The general N66-14107' National Aeronautics and Space Administration. area of illuminating the comparative anatomy of atmospheres Goddard Space Flight Center, Greenbelt. Md. is considered as academic A recommended program for TELESCOPIC DESIGN FOR AN INTERFEROMETRIC SPEC- obtaining data considers topside sounders, airglow measure- TROPHOTOMETER ments. densities from drag data, magnetic fields, special Ernest Hilsenrath In its Goddard Summer Workshop Program Scans of resonance lines, Raman spectra, ultraviolet photometry 119641 2p (!5eeN66-1410104-14) CFSTI: HC $6.00/MF$1.50 and absorption from sunlight. far infrared emissions, and An infrared interferometer spectrometer for the explora- occultations. The bibliography lists articles according to (1 tion of the earth atmosphere and exploration of other terres- general reviews. (2) atmospheric evaporation and evolution, trial-type planets. Mars and Venus. is discussed. The spectrom- and planetary coronas, (3) composition and photochemistry. eter is the same for both missions except that the planetary (4) structurqof upper atmospheres and ionospheres. and (5) probe instrument will include a telescope. The instrument airglow andother optical measurements. Some of the references without the telescope has an acceptance of 8'. Therefore. for a are annotated. M.W.R. satellite such as Nimbus, the instrument would cover an area about 100 km across at the surface of the earth. However. the 8" acceptance angle is too large for a planetary flyby. The N66-14332. National Academy of Sciences-National Re- Mars probe is expected to pass about 5OOO km from the planet. search Council. Washington, D. C. Space Science Board. To cover 250 cm on the planet would require that the accept- ON THE CIRCULATION OF THE ATMOSPHERES OF JUP- ance angle of the instrument be reduced to 2.8" and this is the ITER AND SATURN purpose of the telescope. The interferometer spectrometer Raymond Hide (MIT) In its Space Res. Dec. 1965 p 107- and the telescope are described and the optics of the system 114 refs (See N66-14327 05-30) CFSTI: HC $4.00/MF isshown.The obscuration of the telescow is about 12% E.E.B. $0.75 By concentration on interpretation in terms of hydrodynam- ical theory of prominent visual features. certain key processes N66-14280# RAND Corp., Santa Monica. Calif. related to the atmospheres of Jupiter and Satqrn can be viewed SOME ASPECTS OF THE CIRCULATION OF MARS with a minimum of speculation. For Jupiter, it is pointed out, Conway Leovy Nov. 1965 27 p refs Presented at the Conf. there is the possibility that observations of visual markings on Exploration of the Planets. Blacksburg. Va.. 16-20 Aug. in combination with radio astronomical data can lead to informa- 1965 tion on the internal structure of the planet. Observations made (Contract NASr-21(07)) on Jupiter and Saturn are given and theoretical consideration (NASA-CR-68992) CFSTI: HC $2.00/MF $0.50 CSCL 038 is given to the atmospheric content of these planets. Parameters Estimates of the vertical temperature structure and heat required to characterize the dynamics of the planetary atmos- balanceof Marsare reviewed and compared with the correspond- pheres are discussed. The existence of rapid equatorial currents ing quantities on the Earth. The probable resulting circulation in the fluid layers of both Saturn and Jupiter is mentioned: and is discussed, and reasons for expecting a stronger solstice apparent variations in equatorial zone of Jupiter from 1908 circulation on Mars than on the Earth are given. The problem through 1947 are graphed.! Also shown are the longitudinal of thermally driven tides is reviewed. The amplitude of such wanderings of the Great Red Spot between 1831 and 1960: tides is likely to be small. Author and it is suggested that these variations may be manifestations of a gross torsional hydromagnetic oscillation. M.W.R.

N66-14281. Geophysics Corp. of America, Bedford. Mass. # N66-14334. National Academy of Sciences-National Re- Technology Div. search Council. Washington. C. Space Science Board PHYSICS PLANETARY ATMOSPHERES 111: THE TIME- D. OF INTERACTION THE SOLAR WIND WITH THE PLANETS DEPENDENT COUPLED HARTREE-FOCK APPROXIMA- OF Paul J. Coleman. Jr. (Calif. Univ.. Los Angeles) In its Space TION Res. Dec. 1965 p 127-139 refs N66-14327 05-30) G. A. Victor and A. Dalgamo Aug. 1965 12 p refs (See CFSTI: HC $4.00/MF $0.75 (Contract NASw-1283) A review is presented of observations of the properties of (NASA-CR-68991: GCA-TR-65-24-N) CFSTI: HC $1 .OO/MF the interplanetary medium: and the development of theoretical $0.50 CSCLO3B models of solar wind is summarized. Parameters typical of A coupled Hartree-Fock approximation for describing the the a quiet solar wind are calculated. Interaction of the solar wind effects of time-dependent perturbations on many-electron with the Earth's dipolar magnetic field is dewribad. and methods systems is presented. It is applied to the calculation of the are given for scaling observed effects for interactions with frequency-dependent refractive index of helium gas wtth results dipolar fields of different moments. Speculations are ofbred that differ by between 4% and 8% from the accurate values obtained by a refined variational calculation. Author about interactionof solar wind with planetary bodies not shielded by magnetic fields. M.W.R.

N66-14703*# National Aeronautics and Space Adrninistrar,un. N66-14331. National Academy of Sciences-National Re- Lewis Research Center. Cleveland. Ohio. search Council, Washington. D. C. Space Science Board. MANNED MARS LANDING MISSION BY MEANS OF UPPER ATMOSPHERES OF THE PLANETS H 10 H -TH R UST ROCKETS

21 N66- 15068

Roger W. Luidens. Richard R. Burley. Joseph D. Eisenberg. In the present paper, the density distribution within the Jay M. Kappraff. Brent A. Miller et al Washington, NASA. Martian atmosphere is derived as a function of altitude and the Jan. 1966 113p refs atmospheric parameters. The equations of motion of simple (NASA-TN-D-3181) CFSTI: HC $4.00/MF $0.75 CSCL 22A bodies are established and solved. The case of oblique entry An analysis of alternate mission profiles for a manned into the atmosphere is also treated. The second part discusses Mars landing mission in 1980 is presented. Considered were a sphere entering the atmosphere. It is assumed that the corpuscular radiation shielding. atmospheric entry, structures, center of gravity of the sphere does not coincide with its center. solar-flare protection. chemical and nuclear engines, trajectories, The diameter containing the sphere's center of gravity will be and life-support systems. Interactions between the various called its "axis." In the third part. the results obtained above subsystems were examined to assess the associated weight are compared with the exact solutions. For the exact solution, penalties and to develop those systems that can serve multiple a numerical integration of the equations of motion is carried purposes. High-thrust nuclear and chemical propulsion systems out taking into account all forces neglected above. It is seen were projected for manned landing missions of one to three that ?he new theory of motion is a considerable improvement years in duration. a table contains comparable data of inputs over the old theories. Author for the presented analysis and those of otheranelyses. G.G.

NO-16068*# Southwest Center for Advanced Studies. Dal- N66-16400'# Jet Propulsion Lab.. Calif. Inst. of Tech.. Pasa- las. Tex. dena. MULTIDISCIPLINARY RESEARCH IN SPACE-RELATED ULTRAVIOLET SPECTROSCOPY OF PLANETS SCIENCE AND TECHNOLOGY Smunn~~lRqmrt Charles A. Barth 15 Dec. 1965 261 p refs 30 Sep. 1965 108 p refs Supported in part by AF, Navy (Contract NAS7-100) and NSF (NASA-CR-67597; JPL-TR-32-822) CFSTI: HC $5.00/MF (Grant NsG-269-62) $1.00 CSCL 038 (NASA-CR-69137; EPS-65-2) CFSTl: HC $4.00/MF $0.75 The ultraviolet spectrum of a planet is produced by the CSCLO3B following physical processes: (1) dayglow. the scattering of A summary of studies is presented which were made to solar photons by atoms and molecules in the upper atmosphere develop an understanding of the earth and its atmosphere. and of the planet; (2) daylight. the combination of rayleigh scatter- the processes by which it reached its present state. This study ing of solar radiation and absorption by atmospheric constitu- also applies to the planets, the moon, and the interplanetary ents that produces the planetary albedo in the ultraviolet; and (31 or solar environment in which they are located. Consideration electron excitation. the excitation of atoms and molecules in is given to such areas sa atmospheric structure, plasmas, geo- the upper atmosphere by auroral electrons and by photoelec- magnetic variations, energetic particles, auroral current sys- trons. A quantitative description of each of these processes is tems. interplanetary physics. infrared studies, and kinetic theory. given. The atoms and molecules that are prominent in plane- C.T.C. tary ultraviolet spectra are listed. Calculations are given of planetary molecular emission spectra that are the result of optically thin and optically thick fluorescent scattering and of excitation by auroral bombardment and by photoelectrons. N66-16224'# Jet Propulsion Lab.. Calif. Inst. of Tech, Pasa- Rocket measurements of the dayglow spectrum of the Earth dena. are given for the spectral region between 2000 and 4000A. UTILIZING LARGE PLANETARY PERTURBATIONS FOR THE Author DESIGN OF DEEP-SPACE, SOLAR-PROBE, AND OUT-OF- ECLIPTIC TRAJECTORIES M. A. Minovitch 15 Dec. 1965 85 p refs (Contract NAS7-100) N66-16640'# Space Technology Labs.. Inc , Redondo Beach, (NASA-CR-69222: JPL-TR-32-849) CFSTI: H C $3.00/M F Calif. $0.75 CSCL 22C STUDY OF UNMANNED SYSTEMS TO EVALUATE THE This Report is concerned with three types of free-fall mis- MARTIAN ENVIRONMENT. VOLUME 111: UNMANNED sions that are primarily designed for unmanned vehicles. viz. SPACECRAFT DESIGN deep space. solar probe. and out-of-ecliptic missions. The ener- Robert L. Sohn and Paul Dergarabedian 23 Sep. 1965 152 p gies required to attain these trajectories are beyond present refs direct-transfer capability using available boosters. Solar-im- (Contract NAS2-2478) pact and 90-deg-inclination trajectories require launch ener- (NASA-CR-68742; STL-5303-6015-TU-000) CFSTI. HC gies so high that second-generation nuclear upper stages or SB.OO/MF $1.00 CSCL 226 ion engines would be absolutely necessary. By utilizing large Description of an unmanned spacecraft designed to evalu- planetary- perturbations. it is possible that a rocket like Titan ate the Martian and Cismartian environments in preparation for Il-Centaur with an extra kick stage can. by sacrificing a few subsequent manned Mars landing missions is presented. The extra pouhds for planetary approach guidance. obtain traiec- design concepts include orbiter/bus (or flyby) systems, entry tories that a nucleer Saturn V cannot obtain. Author capsules and survivable landers. In addition. a high resolution photo mapper package is defined Payloads .were selected on the basis of detailed requirements analyses reported in prior NO-16338'# Jet Propulsion Lab.. Calif. Inst. of Tech, Pass- phases of the present study contract and the launch capabili- dene. ties of several boost systems were examined to select the most TRANSLATIONAL AND ROTATIONAL MOTION OF A BODY effective Earth boost system for each of the precursor space- ENTERINO THE MARS ATMOSPHERE craft. M.R.W. Peter Hans Feitis 1 hc. 1965 47 p refs Presented at the Joint Ann. Meeting of the WGLR-DGRR. Berlin. 16 Sep. 1964 Submitted for Publication N66-16641'# Space Technology Labs.. Inc.. Redondo Beach, (NAS7-1001 Calif. (NASA-CR-69252: JPL-TR-32-845) CFSTI: HC $2.00/MF STUDY OF UNMANNED SYSTEMS TO EVALUATE THE $0.50 CSCL 038 MARTIAN ENVIRONMENT. VOLUME II: EXPERIMENTS

22 N66- 16207

Robert L. Sohn and Paul Dergarabedian 23 Sep. 1965 94 p utilizing the Mars orbiting rendezvous mode. Weight scaling laws refs were available for each of the designs so that the interactions (Contract NAS2-2478) of environmental factors on the system design could be readily (NASA-CR-68741. STL-5303-6014-TU-000) CFSTI: HC evaluated in terms of overall gross weight in the earth parking 83.00/MF 50.75 CSCL 22A orbit. M.R.W. Requirements for experiment programs for the measurement of Martian and Cismartian environmental factors by unmanned precursor missions, based upon the results of a preceding sensitivity analysis, are summarized. Consideration is N66-15807'# IIT Research Inst.. Chicago. 111. Astro ScknceS given to such facton as design feasibility, essential design Center. criteria. system weight. mission operation. and system develop- CRITICAL MEASUREMENTS ON EARLY MISSIONS TO ment. The priorities for the experiments in order of tbir im- JUPITER portance are: solar cosmic radiation environment. meteoroid J. M. Witting. M. W. P. Cann, and T. C. Owen Dec. 1955 127 p environment, and atmospheric properties. A list of instruments refs was prepared, including physical descriptions. to accomplish (Contract NASr-65(06)) the required experiments This list is divided into groups accord- (NASA-CR-69561; P-10) CFSTI: HC $4.00/MF $1.00 CSCL ing to mission mode requirements linterplanetery. orbiter or 22A capsule/lander). and spacecraft weight capability. It is apparent Existing knowledge of Jupiter's magnetosphere. iono- from the results of the study that the interplanetary environ- sphere. atmosphere, and interior is summarized and critical ment. particularly solar cosmic radiatkn and mefeoroid flux, measurements which can be made from *-by missions to are key factors in the design and operation of the manned Jupiter are indicated. Estimates place Jupiter's Surface m8g- mission. In contrast. uncertainties in the definition of the netic field strength at about 10 gauss. indicating the pr0SOIWS Martian atmosphere do not have a dominating impact on the of radiation belts with loo0 times greater partide densitk3 design of the manned system. Techniques for measuring the than those of Earth. The presence of an ionosphere was de- atmosphere are discussed. and limitations of experimants duced theoretically. assuming a model atmowhere. Spectral yielding indirect measurements delineated. M.R.W. analyses of Jupiter's atmosphere established the 7Of hydrogen. methane. and ammonia. Tem-re mewummentt at various wadengths showed a fluctuation from 125'K to 2WK in the wavdmgth range 8 fi to 3 cm. idiating !hat N66-lSS42g# Space Technology Labs.. Inc.. Redondo Beach, the thermal mission at daerent wadength comes from Calif. different depths in the Jovian atmosphere. Model studies of STUDY OF UNMANNED SYSTEMS TO EVALUATE THE Jupiter's interior indicated the possibh presence of dbc MARTIAN ENVIRONMENT. VOLUME IV: SUMMARY hydrogen and a hw coco new the center of ttm planet. Robert L Sohn and Paul Dergarabedian 23 Sep. 1965 24 p Several parameter measumpmts of the Jovian m.gnstem (Contract NAS2-2478) or atmosphere at future flv-by miss-- are suggested. G.G. (NASA-CR-68743: STL-5303-8016-TU-000) CFSTI: HC $1.00/ MF $0.50 CSCL 22A A study of the sensitivity of the manned Mars mission to the Martian and Cismartian environment. and a definition of the experiments and unmanned spacecraft to acquire the neces- N66-16151'# Jet Propulsion Lab, Calif. Inst. of Tech. Pasa- sary environment measurements. is reported. The general dena. goals of the study were to: identify those environmental factors THE MARINER II MICROWAVE RADIOMETER EXPERI- that can influence the planning and design of the manned Mars MENT mission: establish the sensitivity of the manned Mars mission Douglas Emron Jones 1 Jan. 1966 73 p refs system to uncertainty in the Martian and Cismartian environ- (Contract NAS7-100) ment; define experiments and instrumentation required to (NASA-CR-69916: JPL-TR-32-722) CFSTI: HC $3.00/MF make the necessary measurements of the significant environ- $0.75 CSCL 22A mental factors; and design unmanned systems to evaluate the A dual-channel microwave radiometer obtained three scans Martian and Cismartian environment. based on the priorities across the planet Venus at wavelengths of 13.5 and 19 mm. established from the sensitivity analyses. M.R.W. The relationship of the peak temperature values of the three scans supports a hot-surface model for the planet. Several atmosphere-surface configurations were assumed in an at- N66-16643'# Space Technology Labs.. Inc.. Redondo Beach. tempt to match the limb-darkening ratios and temperature Calif. values measured at both wavelengths. The model that agrees STUDY OF UNMANNED SYSTEMS EVALUATE THE TO best with the data consists of a specular surface and an iso- MARTIAN ENVIRONMENT. VOLUME I: SENSITIVITY thermal cloud-type layer at a temperature near 350°K. The ANALYSIS marked difference between the 13.5- and 19-mm temperatures Robert L. Sohn and Paul Dergarabedian 23 Sep. 1965 300 indicates the presence of an abrupt discontinuity in the micro- p refs wave spectrum of Venus that cannot be due to uncondensed (Contract NAS2-2478) water vapor and hence requires the presence of a molecule (NASA-CR-68740: STL-5303-6013-TU-000) CFSTI: HC or molecules in the atmosphere of Venus that condense or 87.00/MF 81.50 CSCL 228 polymerize into liquid form at T 2 350" K and exhibit line Results of a study devoted to establishing the sensitivity spectra in the vicinity of 13.5 mm and shorter. Author of the manned Mars system to uncertainties in the Martian and Cismartian environment are presented. These interactions were established by gathering and analyzing available data on the Martian and interplanetary environments. and plac- ing upper and lower bounds upon the environment data in N66-16207# Hebrew Univ.. Jerusalem (Israel). Dept. of Me- an effort to establish limits on the uncertainties in each environ- teorology. mental factor. A reference manned mission system &in was NUMERICAL STUDIES OF PLANETARY CIRCULATIONS selected based upon a design study conducted previously. and IN A MODEL ATMOSPHERE FIMI Report

23 N66-16208

Abraham Huss Bedford. Mass.. AFCRL. Aug. 1965 127 p refs This report presents a concise description of the study ap- (Grant AF-EOAR-64-76) proach results of manned system environmental sensitivity (AFCRL-65-771. AD-623662) CFSTI: HC $4.00/MF $0.75 analyses. and the resulting requirements for unmanned systems designed to acquire the environmental data necessary CONTENTS: to support the planning and design of manned Mars missions 1. NUMERICAL INTEGRATIONS OF A TWO-LEVEL Author QUASI- G EOSTRO P H IC MOD EL INCLUDING DlABATlC HEATING AND SURFACE FRICTION A. Huss 59 p refs (See N66-16208 07-13) N66-16463"# National Biomedical Research Foundation. 2. PRELIMINARY INTEGRATIONS OF A TWO-LEVEL Silver Spring. Md. QU ASI-G EOSTRO P H IC MOD EL INCLUDING WATER-VAPOR INVESTIGATION OF THERMODYNAMIC MECHANISMS A. Huss and E Doron 58 p refs (See N66-16209 07-13) FOR THE PRODUCTION OF COMPOUNDS ESSENTIAL FOR THE ORIGIN OF LIFE First Quarter Technical Report, Oct. l-Dec. 31,1965 NBB-18208 Hebrew Univ.. Jerusalem (Israel). Dept. of Me- Margaret 0. Dayhoff. Richard V. Eck. and Ellis R. Lippincott teorology. 11 9651 38 p refs NUMERICAL INTEGRATIONS OF A TWO-LEVEL QUASI- (Contract NSR-21-003-002) GEOSTROPHIC MODEL INCLUDING DlABATlC HEAT- (NASA-CR-69965) CFSTI: HC $2.00/MF $0.50 CSCL 038 ING AND SURFACE FRICTION From present information on the composition. pressures. Abraham Huss In its Numerical Studies of Planetary Circula- and temperatures of planetary atmospheres, we have calcu- tions in a Model Atmosphere Aug. 1965 59 p refs (See N66- lated the expected thermodynamic equilibrium composi- 16207 07-13) CFSTI: HC $4.00/MF $0.75 tion of the atmospheres of the Earth. Venus, Mars, and The evolution of general circulation patterns has been Jupiter. Departures from thermodynamic equilibrium must studied by means of a two-level quasi-geostrophic model in- be attributed to special mechanisms, including. on the Earth, cluding diabatic heating and surface friction. Results are shown biological activity. The major constituents of the terrestrial for integrations over a period of about 30 days. The Jacobian atmosphere are found to be in approximate thermodynamic equilibrium; while many minor constituents have abundances representing the advection of potential vorticity in the prog- exceeding their equilibrium values, there is a marked tendency nostic equations was approxi,mated in two ways: once by the for equilibrium to be restored. It appears that the atmosphere 4-point conventional finite difference analog and once by of Venus is in thermodynamic equilibrium. while that of Jupiter energy-consistent analog. The distributions of various field- is not. The evidence for Mars is less conclusive, although not in- variables were found to resemble the corresponding distri- consistent with thermodynamic equilibrium. For none of these butions in the atmosphere. as far as patterns and magnitudes planets is there a molecular species with a large predicted were concerned. Use of the energy-consistent Jacobian re- equilibrium abundance and spectroscopically accessible ab- sulted in a lower noise level at the conclusion of the run. in sorption features which has not been already identified. The higher zonal velocities, in lower energy transformations (ex- predicted equilibrium abundances of oxides of nitrogen are cept for the transform). and in a more pronounced oscil- [K.k] extremely low on all planets. Author latory evolution of various field variables. Author

NBB-18209 Hebrew Univ, Jerusalem (Israel) Dept of Me- N66-166@7'# Michigan Univ.. Ann Arbor. teorology INVESTIQATION OF QALACTIC AND PLANETARY RADIO PRELIMINARY INTEGRATIONS OF A TWO-LEVEL QUASI- ASTRONOMY Third Somiannual Sutur Roport, Jan.-Jun. GEOSTROPHIC MODEL INCLUDING WATER-VAPOR lS66 Abraham Huss and Eliyahu Doron In its Numerical Studies of Fred T. Haddock Jan. 1968 14 p Planetary Circulations in a Model Atmosphere Aug 1965 58 p (Grant NsG-572) refs (See N66 16207 07-13) CFSTI HC $4OO/MF $075 (NASA-CR-70152) CFSTI: HC $1.00/MF $0.50 CSCL 22A Water-vapor was introduced into a two-level quasi-geo- Progress is reported on studies in galactic and planetary strophic model The local change of the specific humidity was radio astronomy. During this period efforts on the galactic radio predicted by means of a continuity equation for the water vapor astronomy task were almost entirely devoted to the final prepa- Changes due to evaporation from the lower boundary (as- ration of the 11.03 rocket payload. culminating with its success- sumed to be an Ocean surface) and to precipitation were taken ful launching. Mechanical problems, the completion of payload into account Several integrations were performed with differ- and testing, and calibration of the radiometers are discussed. ent initial distributions of the specific humidity In the first Work performed on the kilometer weve orbiting telescope series of runs the flow pattern was assumed to develop with- studies is also presented. Efforts on the planetary radio astron- out being affected by the release of latent heat In the two last omy task were directed towards photochemical studies of the experiments latent heat was introduced into the thermody- C-0 complex, Martian ionospheric studies. and investiga- namic energy equation A rapid rise of the noise level was ob- tions of topside electron density profiles and forces on non- served in these cases and the integration had to be interrupted rigid bodies in space. R.N.A. after the passage of a few days Author

N68-16248'# North American Aviation. Inc , Downey, Calif NSB-16940'# National Aeronautics and Space Administration Space and Information Systems Div Ames Research Center. Moffett Field. Calif UNMANNED SYSTEMS TO EVALUATE THE MARTIAN AN ESTIMATE OF THE CHEMICAL KINETICS BEHIND ENVIRONMENT Condensed Summary Report NORMAL SHOCK WAVES IN MIXTURES OF CARBON M G Boobar and W G Landstrom Sep 1965 20 p DIOXIDE AND NITROGEN FOR CONDITIONS TYPICAL (Contract NAS2-2477) OF MARS ENTRY (NASA-CR-69997. SID-65.1173) CFSTI HC $1 OO/MF Robert L Mc Kenzie Washington. NASA. Feb 1966 67 p refs $050 CSCL 22A (NASA-TN-D-3287) CFSTI HC $3 OO/MF $0 75 CSCL 01A

24 N66-17290

The chemical kinetics behind normal shock waves in mix- polarimetry of the planetry atmospheres. microwave radiometry tures of carbon dioxide and nitrogen are studied. Particular and radar probing. charged particle detection in trapped radia- emphasis is placed on a shock speed of 8 km/sec in ambient tion belts, optical occultation experiments for Saturn's ring gas compositions containing 5. 10. and 50 percent CO, by system and atmospheric studies. rf occultation experiments volume. These conditions are typical of those anticipated for for atmospheric density determinations. and photography of entry into the Martian atmosphere. Ambient density is varied cloud structure and surface features CTC fmm to lo-' times that of the earth sea-level density. The species considered are C02. y.CO. NO, CN. 02. C. 02. C. 0. and N. A system of 17 reactions is initially assumed and later reduced to 9 by removing those found insignificant to the N66-17231'# National Aeronautics and Space Administration. gross thermochemical behavior. The methods used for estimat- Goddard Space Flight Center. Greenbelt. Md. ing exchange reaction rates are discussed in detail. and a RADIATIVE EQUlLl6RlUM IN PLANETARY ATMOSPHERES. scheme for correlating experimental activation energies is II: AN ANALYSIS AND INTERPRETATION OF SOME VENUS suggested. General features of the nonequilibrium chemistry OBSERVATIONS BASED ON A SINGLE REFLECTING CLOUD are presented followed by an analysis of the uncertainties due LAYER MODEL to possible errors in estimated reaction rates. Particular con- F. Bartko and R. A. Hanel Sep. 1965 68 p refs sideration is given to the kinetics of CN for shock speeds of 4 (NASA-TM-X-55392; X-622-65-436) CFSTI: HC $3.00/MF to 8 km/sec. The CN concentration is shown to rapidly over- $075 CSCLO3B The equilibrium temperature distribution, thermal emission shoot its equilibrium value for most ambient densities and spectrum. and limb function-of a nongrey N2-CO,-H,O model shock velocities anticipated during entry into the Martian atmos- atmosphere have been computed for a large variety of atmosphere. Author pheric parameters which are appropriate for the atmosphere of Venus in the vicinity of the cloud tops. Near infrared absorp- N66-16W8# Lockheed Missiles and Space Co.. Palo. Alto. tion by C4of direct and diffusely reflected solar radiation have Calif. Research Lab. been included. The important effects of the near infrared solar A MODEL FOR THE LOWER ATMOSPHERE OF MARS heating by CO, absorption. the water vapor amount, and the BASED ON MARINER IV OCCULTATlON DATA cloud top pressure level on the computed results are demon- Albert 0. Anderson Dec. 1965 34 p refs strated. Other conclusions resulting from a study of the water (LMSC-6-75-65-62 1 vapor abundance and thermal emission spectrum depend on The Mariner IV occultation experiment has resulted in the cloud composition. These results are based on the assump- low values for the neutral properties (temperature. pressure. tion of a single reflecting cloud layer. an assumed C02 con- and density) and the dominance of COz for the lower atmw- centration of 5% and a brightness temperature of 225°K for phere of Mars. Guided by these new results and theoretical the cloud tops in the 8-13~spectral interval. Author models of the Martian atmosphere, a neutral property model has been derived which takes into account surface air temperature variation. The neutral properties up to 50 km exhibit N66-17249.n National Aeronautics and Space Administration. strong dependence on the surface temperature. An isopycnic Goddard Space Flight Center, Greenbelt, Md. (constant density) level is manifested in the model at 10 km PRELIMINARY TRAJECTORY ANALYSIS OF A MARS where the density value is 5.77 x 10" gm cm-3 for surface PROBE temperatures ranging from 175 to 325' K. At 50 km. the density John Mc Nellis Oct. 1965 31 p ref variation for this same surface temperature range is a factor of (NASA-TM-X-55376; X-643-65-3901 CFSTI: HC $2.00/MF four. The height of the tropopause (boundary between convec- $0.50 CSCL22C tive and radiative equilibrium regimes), taken to vary linearly This report investigates the feasibility of the needle- with the surface temperature. is one of the principal uncertbin- nosed probe which is proposed as an experiment on a 1969 ties since the computed properties are sensitive to it. The ac- Voyager fly-by bus. The probe is to be separated from the curacy of the model appears to decrease with altitude. espe- buswithin 20 days prior to closest approach of the bus. It is cially above 30 km where the effects of CO2 photochemistry. to enter the Mars atmosphere and transmit atmospheric entry doppler broadening. and departure from local thermodynamic information back to the bus. Nine bus trajectories were used equilibrium start to become important. Author for generating probe trajectories. For a given bus trajectory a wt of probe trajectories (meeting the required constraints) was computed. Each of the trajectories in the set corresponded N66-17090'# IIT Research Inst.. Chicago, 111. Astro Sciences to a different separation time of the probe prior to closest Center. approach of the bus. For each probe trajectory the separation THE SCIENTlFlC OBJECTIVES OF DEEP SPACE INVES- velocity vector was varied to develop a subset of probe tra- TIGATIONS: SATURN, URANUS, NEPTUNE AND PLUTO jectories (with different entry times) for each separation time. P. J. Dickerman Jan. 1966 54 p refs It is shown that by choosing the separation time sufficiently (Contract NASr-65(06)) early (approximately 20 days prior to closest approach of the bus) the probe mission may be accomplished using a separa- (NASA-CR-70328; P-11) CFSTI: HC $3.00/MF $0.50 CSCL 03B tion velocity under Seven meters per second for all acceptable bus trajectories. Author A study was made of scientific obiectives for the four outer- most planets: Saturn. Uranus. Neptune. and Pluto. Differences between these planets and planets nearer the sun are shown in a general survey of their structure and composition. and in N66-17290*# Southwest Center for Advanced Studies. Dallas, detailed discussions of the individual bodies. Descriptions Tex. of the atmospheres are given. primarily with the aid of spectro- MULTIDISCIPLINARY RESEARCH IN SPACE-RELATED scopic and radiometric observations. and better known charac- SCIENCE AND TECHNOLOGY Semiannual Report, Period teristics are tabulated. Reasons for making probes to these Ending 31 Doc. 1965 planets are given. and proposed measurements are discussed. 31 Dec. 1965 28 p refs These include magnetic field determinations throughout the (Grant NsG-269-62) mission and in the region of the planets: spectrometry and (NASA-CR-70165) CFSTI. HC $2.00/MF $0.50 CSCL 148

25 N66- 1 761 7

Research activities during the period October 1965 through scattering and transmission functions. By a reduction developed December 1965 centered on planetary atmospherep. iono- by Sekera. this analysis is applied to Rayleigh scattering in- spheric and radio physics. particle and fields investigations. cluding the effects of polarization. Author (TAB) and planetological work. The development of the earth's atmosphere over geologicdl time was traced on the basis of geological evidence and photochemical constraints. Formu- NM-19497*# National Aeronautics and Space Administration. lation of a hydrodynamic solution to the problem of waves in a warm magnetoplasma was started. Some measurements Ames Research Center, Moffett Field. Calif. USE OF ENTRY VEHICLE RESPONSES TO DEFINE of plasma capacitance as a function of frequency were made THE PROPERTIES THE MARS ATMOSPHERE and showed good results. Analysis of ionospheric data obtained OF Alvin Seiff and David E. Reese, Jr. I19651 31 p refs Presented at occultation in terms of atmospheric properties established at the Am. Astronautical SOC. Symp. on Unmanned Explora- an exceedingly cold Martian atmosphere. Improvements in tion of the Solar System, Denver, 8-10 Feb. 1965 various test equipments and installations was also reported. (NASA-TM-X-56125) CFSTI: HC $2.00/MF $0.50 CSCL 038 G.G. Principles are developed by which the atmospheric properties of an unknown planetary atmosphere can be deduced from responses of a probe vehicle entering the atmosphere. NM-17617# Harvard Coll. Observatory. Cambridge, Mass. Experiments to determine atmospheric density and pressure HARVARD ASTRONOMICAL OBSERVATORY ANNUAL as functions of altitude, and to detect and determine quantities REPORT, 1965 of selected gases in the atmosphere are examined in detail. Donald H. Menzel 1965 16 p Probe geometries are discussed and take lift, drag coefficient. This activity report of the Harvard college astronomical Mach number. Reynolds number. gas composition, and angle observatory presents a very short review on all research activ- of httack into consideration. The approach to the detection of ities during the year 1964 through 1965. Research programs atmospheric species is by spectrometry of selected wavelengths dealing with astrophysical implications of autoionization in of emission from the hot atmospheric gases in the shock layer. atomic spectra, theoretical studies of atomic structures and Laboratory studies and theory show that very bright emission spectra. radio astronomy projects, solar phenomena and behind the bow wave in atmospheres of nitrogen and carbon their effects, evolutions of planetary atmospheres. and obser- dioxide is associated with the cyanogen radical. and detection vations on meteors and comets are very briefly outlined. G.G. of the violet band system would constitute direct evidence for nitrogen in the atmosphere. Other radiometers to measure the nitric oxide and argon radiations are discussed. C.T.C. Nee-17747 Israel Program for Scientific Translations, Ltd.. Jerusalem. THE SIQNIFICANCE OF ATMOSPHERIC OPTICS IN N66-19626'# National Aeronautics and Space Administration. ASTROPHYSICS (0 ZNACHENll ATMOSFERNOI OPTlKl Washington. D. C. DLYA ASTROFlZlKll SI0N IFICANT ACHIEVEMENTS IN PLANETARV ATMOS- V. G. Fesenkov In its Scattering and Polarization of Light in PHERES 1966-1964 the Atmosphere 1965 p 4-10 (See N66-17746 08-13) 1966 65 p refs CFSTI: HC $6.00/MF $1.50 (NASA-SP-98) GPO: HC $0.45; CFSTI: MF $0.75 CSCL 038 Studies in the field of atmospheric optics which have direct Recent advances resulting from satellite and rocket sound- bearings on astrophysics. particularly for the study of the phys- ings in the study of the Earth's atmosphere above 30 km. and ical nature of the planets and of the planetary medium are of Mars'. Venus,, and Jupiter's atmospheres are discussed. discussed. Studies in the following areas are considered: re- Among the findings reported about the Earth's atmosphere fractive properties of the atmosphere; atmosphere extinction: are: an isothermal temperature distribution above 300 km with terrestrial aerosols; physical nature of heat exchange in the diurnal and solar activity variations, the role of molecular diffu- surface layer of the atmosphere: determinations of the re- sion in the gravitational field in controlling constituent dis- flectance of the earth's surface: satellite radiation measure- tributions, the large atmospheric density variations. strong ments: influence of radiation on the motion of a continuous shear zones from 70 to 120 km. Discussed also are hydrogen medium; and the interaction of earth with high-altitude atmos- geocorona. auroral emissions excited by energetic electrons. pheric layers and the surrounding interplanetary medium. and micrometeoroid impact ratas and densities. An extensive bibliography is included. N.E.N. M.R.W.

N66-19628.# Stanford Univ.. Calif. Radio Science Lab. N66-19418# RAND Corp.. Santa M0nic.a. Calif RESEARCH AT THE STANFORD CENTER FOR RADAR MULTIPLE SCATTERING IN HOMOGENEOUS PLANE- ASTRONOMY Semiannual Status Report No. 6. 1 Jul.41 PARALLEL ATMOSPHERES D.c. 1966 T. W. Mullikin Dec. 1965 31 p refs V. R. Eshleman Jan. 1966 16 p refs (Contract AF49(638)-1700: Proj. RAND) (Grant NsG-3771 (RM-4846-PR: AD-626205) CFSTI: HC $2.00/MF $0.50 (NASA-CR-71090) CFSTI: HC $1.00/MF $0.50 CSCL 03A Steady-state multiple-scattering problems for homoge- Radar and radio studies of lunar and planetary ionospheres, neous plane-parallel atmospheres have been extensively atmospheres, and surfaces, and of the sun and interplanetary studied by means of the principles of invariance of Ambart- mediums were continued. In the cislunar gas studies, the sumian and Chandrasekhar. These nonlinear integral equa- ionospheric electron contents. determined by the Faraday tions have been used for computing intensities of radiation on rotation method. were subtracted from each radar deter- the faces of the atmosphere. Using linear integral-equation mination of total content, and the existence of two distinct theory. it is shown how one computes the source function regions beyond the ionosphere was reaffirmed. The simul- interior to an atmosphere with optical depth entering the com- taneous Doppler and Faraday lunar radar data showed that putation only parametrically. Intensities. throughout the at- these two methods produce similar conclusions about cislunar mosphere. are expressed by nonlinear combinations of the magnetospheric wake density. A digital radio polarimeter was computed source function. giving. on the faces, the familiar used to observe radio noise bursts at 22.2 Mc from Jupiter

26 N66-19930 and the sun. Jovian emission was felt to confirm the pre- that while we have several good ideas as to the origin of life, dominance of right hand polarization. and the solar burst much sophisticated research awaits before we arrive even at analysis showed no chage of either axial ratio or orientation a good set of hypotheses of how life occurred. Likewise. while of ellipse from burst to burst. A signal channel coding scheme we can detect many forms of life chemically. much more for additive noise channels with feedback was developed and sophisticated sensors are needed for space missions to help considered to operate successfully under a sizeable code decide whether a certain observed phenomenon may constitute book. Among the other programs mentioned are planetary "life." Finally. although we have demonstrated short-term surface mapping, planetary atmosphere and ionosphere life-support outside the atmosphere. the present crude auto- stud-. plasma effects on space probe tracking, and receiver matic control of a few gases and fluids will have to be re- construction techniques. N.E.N. fined greatly before we can, for example, establish a colony on the Moon. The advanced electronics for each of these pur- suits offers engineers one of the greatest practical challenges N66-19636*# Geophysics Corp. of America, Bedford. Mass. of an already challenging technology. Author GCA Technology Div. PHYSICS OF PLANETARY ATMOSPHERES. IV: GAS ANALYSIS BY PHOTOIONIZATION MASS SPECTROMETRY W. Poschenrieder and P. Warneck Jan. 1966 34 p refs Submitted for Publication N66-19901'# Arizona Univ . Tucson Field Emission and (Contracts NASw -1283; AF 19(628)-3849) Space Systems Lab (NASA-CR-71210; GCA-TR-66-1-Nf CFSTI: HC LZ.OO/MF DETECTION TECHNIQUES FOR TENUOUS PLANETARY $0.50 CSCLO3B ATMOSPHERES Fihh Six-month Report. 1 Jul.-30 0.E. A photoionization mass spectrometer featuring a special 1965 180-degree magnetic analyzer with inclined pole faces is Sturat A Hoenig and Jay Abramowttz [19661 211 p refs described and its usefulness as a gas analytical tool is ex- (Grant NsG-458) plored. The investigated range of ion source pressures was (NASA-CR-70934) CFSTI HC $6 OO/MF $1 25 CSCL 07D 0 to 150 microns. It was found that pressures up to 20 microns can be utilized for gas analysis. At higher pressures. CONTENTS ion-molecule reactions and increasing light absorption cause 1 DETECTION TECHNIQUES FOR TENUOUS PLANE- nonlinear ion current-pressure relationship. The major advan- TARY ATMOSPHERES Stuart A Hoenig and Jay Abram- tage of photoionization when compared to electron impact owitz 30 p refs ionization is the simplicity of fragmentation patterns, the 2 CHANGE IN THE THERMIONIC EMISSION CUR- major disadvantage, the lower sensitivity. At 20 microns RENT OF PALLADIUM DUE TO CHEMISORPTION OF pressure. spark or resonance light sources used in conjunc- ATOMIC AND MOLECULAR HYDROGEN M M Eisenstadt tion with a 1/2-meter monochromator produced peak ion 165 p refs (See N66-19902 10-06) intensities around 5X A. Although these ion intensities are higher than those reported previously. they are still considerably below the ion intensities commonly produced by electron impact ion sources. Author N66-19929# Tohoku Univ . Sendat (Japan) Faculty of Sci- ence SCIENCE REPORTS OF THE TOHOKU UNIVERSITY. Fifth 166-196768 Yale Univ.. New Haven. Conn. Series: GEOPHYSICS, VOLUME 16. NUMBER 1 SEARCH FOR PLANETARY OPTICAL EMISSION, AND Feb 1965 51 p refs STUDY OF FLARE ACTIVITY OF NEARBY STARS FiMl CFSTI HC $3OO/MF $050 R- R- Harlan J. Smith 3 Dec. 1965 5 p refs CONTENTS (Grant Nonr(G)-00043-62) 1 HEIGHT PROFILES OF DENSITY COMPOSITION. (AD-624895) CFSTI: HC $l.OO/MF $0.50 AN0 IONIZATION IN THE MARTIAN ATMOSPHERE H Ka- Jovian decameter radio noise storms arise from particles mtyama p 1-14 refs (See N66-19930 10-30) emitting essentially at gyrofrequencies near the Jovian mag- 2 ON A POSSIBLE MECHANISM FOK THE RULES netic poles. Parallel microwave radio studies indicate that OF POLARIZATION OF pc5 GEOMAGNETIC PULSATIONS Jupiter possesses very strong radiation belts. Results suggest Y Kat0 and T Tamao p 15-36 refs (See N66-19931 10- that clouds of ions focusing into Jupiter's magnetic poles 13) should also produce strong auroral activity. Detection of such 3 EVALUATION OF CLOUD SEEDING EFFECT BY auroras would provide a valuable test of the radio theories. STATISTICAL ANALYSIS OF SNOWFALL AMOUNT IN would give information on Jupiter's ionosphere. and would THE TOHOKU DISTRICT. 'JAPAN S Yoshida (Sendat Dis- permit a direct mapping of the near-surface magnetic field trict Meteorol Obs) p 37-47 refs (See N66-19932 10- configurations of the planet. Observational work is reported: 13) however, results have been inconclusive and equipment is required which is much more sophisticated than that available. E.E.B. Nb0-19930 Tohoku Univ.. Sendai (Japan). Geophysical Inst. HEIGHT PROFILES OF DENSITY, COMPOSITION. AND N66-19829 Radio Corp. of America, Princeton. N. J. Ra- IONIZATION IN THE MARTIAN ATMOSPHERE diation Physics Group. Hiroshi Kamiyama In its Sci. Rapt. of the Tohoku Univ. Feb. LIFE BEYOND THE ATMOSPHERE-ORIGINS, DETEC- 1965 p 1-14 refs (See N66-19929 10-13) CFSTI: HC TION, AND SUPPORT $3.00/MF $0.50 A. G. Holmes-Siedle In its Space Electron. [19651 6 7-13 With a particular assumption for the vertical temperature refs (See N66-19827 10-31) distribution and the chemical composition of the lower at- This paper discusses the existence and detection of life mosphere. a possible model of the Martian atmosphere is forms in the universe (with emphasis on our planetary system). deduced on the terrestrial analogy. On the assumption that. and the support of life in manned space travel. It is shown at the surface. the pressure is 85 mb and the air is composed

27 N66-20077 of 2 2% CO, and 97 8% NZ the photodissociation of CO, earth as a planet. and the flights of spacecraft in earth orbit takes place in the region above 128 km. and peaks of the con- and in cislunar space. It is shown that the results of such studies centration occur at 137 km for 0 and at 132 km for CO and can provide data in disciplines involving geophysics. planetary 0, Diffusion is considered to be important above 150 km atmospheres, solar physics. astronomy. and astronautics. Rigor- Two ionospheric layers are formed by the ionization of N, ous solutions of radiative transfer problems in a real atmos- 0. and 0, the lower layer being located at about 135 km and phere. however. still are beyond the capabilities of present the upper at a level between 600 km and 900 km The maxi- theory. Some preliminary quantitative results in the visible mum electron concentration is about 4x 104cm-3 in the lower range of the electromagnetic spectrum have been obtained layerand between9X104and 1 8x105cm-3 in the upper layer through the use of a semiempirical method. This technique The height variation of the ion composition is also described promises to become a useful tool in the fields of study dis- Author cussed. Author (TAB)

N66-20077'# TRW Systems, Redondo Beach. Calif. THEORETICAL INVESTIGATION: THE SCATTERING OF LIGHT BY A PLANETARY ATMOSPHERE Intorim Repott, N66-20131'# California Univ . Berkeley Space Sciences Lab 22 8ep.-22 Doc. 1966 BIOCHEMICAL ACTIVITIES OF TERRESTRIAL MICRO- Robert S. Fraser (19651 26 p refs ORGANISMS IN SIMULATED PLANETARY ENVIRON- (Contract NAS5-9678) MENTS Final Report (NASA- C R-70943; TRW-4520-6001~RO-000) C FSTl: H C I19641 14 p refs $2.00/MF $0.50 CSCLO3B (Grant NsG-126-61) A theoretical study of the characteristics of radiation (NASA-CR-71195) CFSTI HC $1 OO/MF $0 50 CSCL 06C scattering in a planetary atmosphere was conducted. It is The major effort of this research program was directed shown that the lower boundary of the atmosphere reflects toward environmental conditions that might serve as con- radiation specularly according to Fresnel's law. The follow- straints upon the evolution or development sf microorgan- ing investigations are reported: (1) the accuracy of the com- isms on the surface of anaerobic planets such as Mars Studies puted x and y functions of Chandrasekhar: (2) the albedo of on low temperature freezing and thawing of microorganisms. diffuse sky light from both smooth and rough water surfaces; on alternatives for atmospheric oxygen. and on ultraviolet and (3) the characteristics of the neutral points which refer radiation as an environmental constraint are discussed R N A to the directions where the degree of polarization of light from the atmosphere vanishes. D.T.

N60-21229'# National Biomedical Research Foundation, Sil- N66-20080'# Litton Systems. Inc.. St. Paul. Minn. Applied ver Spring, Md. Science Div. DESIGN AND DEVELOPMENT OF AN AIR-EJECTOR THERMODYNAMIC EQUILIBRIA IN PLANETARY AT- POWERED PNEUMATIC SURFACE SAMPLING SYSTEM MOSPH E R E8 L. W. Rees and M. J. Grundtner Dec. 1965 97 p refs Pre- Ellis R. Lippincott (Md. Univ.). Richard V. Eck. Margaret 0. pared for JPL lrs Rept.2930 Dayhoff. and Carl Sagan (Harvard Univ.) I19651 38 p refs (Contracts NAS7-100.: JPL-950771) CFSTI: HC $3.00/MF Prepared in cooperation with Md. Univ. and Harvard Univ. $0.75 CSCL 13G (Grant NGR-21-003-002) A pneumatic surface sampling system for use under simu- (NASA-CR-69829) CFSTI: HC $2.00/MF $0.50 CSCL 20M lated Martian environmental conditions was designed. fabri- From present information on the composition. pressures, cated and tested. The unit relies upon the phenomena of air and temperatures of planetary atmospheres. the expected blast dislodgment of surface particles by an external. travers- thermodynamic equilibrium composition of the atmospheres ing sampler head. pneumatic.transport of particulate material of the Earth, Venus, Mars, and Jupiter is calculated. Depar- to the main sampler body. and subsequent centrifugal separa- tures from thermodynamic equilibrium must be attributed to tion by a cyclone collector. It is capable of operation with special mechanisms, including, on the Earth. biological ac- particles as large as 800 microns diameter at ambient pres- tivity. The major constituents of the terrestrial atmosphere sures as low as 5 millibars and at ambient temperatures down are found to be in approximate thermodynamic equilibrium; to -60°C. In tests with sandy soils the collection rate of this while many minor constituents have abundances exceeding device is on the order of 15 grams per minute for periods up their equilibrium velues, there is a marked tendency for equi- to 10 minutes Biological assessment has shown the acquired librium to be restored. It appears that the atmosphere of samples are representative of the environment. Author Venus is in thermodynamic equilibrium, while that of Jupiter is not. ,The evidence for Mars is less conclusive, although not inconsistent with thermodynamic equilibrium. For none N66-20124# RAND Corp Santa Monica Calif of these planets is there a molecular species with a large ON THE SCATTERING OF SUNLIGHT INTO PLANETARY predicted equilibrium abundance and spectroscopically ac- SHADOW CONES R C Moore and G F Schilling Dec 1965 27 p refs Pre- cessible absorption features which has not been already sented at the Symp on Interdisciplinary Aspects of Radiative identified. The predicted equilibrium abundances of oxides of Energy Transfer Philadelphia 24-26 Feb 1966 nitrogen are extremely low on all planets. The measured (P-3282. AD-625260) CFSTI HC $2 OO/MF $0 50 upper limits on the abundances of Cytherean CH4. "3. and Refraction and multiple scattering of solar radiation in a CO are a11 inconsistent with the possibility of elemental car- planetary atmosphere cause the propagation of appreciable bon or organic molecules in contact with the atmosphere of amounts of radiative energy into the planet's geometric shadow Venus either on the surface or as clouds. The porsibility of cone The implications of this atmospheric phenomenon to re- small quantities of oxygen on Mars is not excluded. It is sug- seerch in various fields are discussed Examples are studies of gested 'that the colored materials at the Jovian clouds are lunar eclipses. the presence of the Venus ring near inferior con- organic molecules. produced by non-equilibrium procesaes (unction. the astronomical problem of the appearance of the in a reducing environment. Author

28 N66-23493

NW-21687 International Business Machines Corp.. San jective grating spectrograph on an Aerobe rocket. The data Jose. Calif. Research Lab. indicate a reflectivity of 0.04 to 0.08 in the ultraviolet. in- EQUATIONS OF MOTION FOR ELASTIC BODIES EN- creasing toward shorter wavelength according to a Rayleigh TERING A PLANETARY ATMOSPHERE Law. The data can be represented by an N2:C02:A model P. K. C. Wang and N. E. Langlois In its Papers on the Con- atmosphere with a surface pressure of about 5 to 20 milli- trol ot Distributed Parameter Aeroelastic Systems Nov. 1965 bars. The photographic appearance of the planet in the blue p 5-28 refs (See N66-21666 11-01) CFSTI: HC $S.OO/MF is interpreted as a loss of surface contrast and reflectivity $1 .00 rather than by absorption in the atmosphere by the "blue The equations governing the motion of elastic bodies haze". ;The model predicts the general appearance of the during their entry into a planetary atmosphere at hypersonic planet in the photographic ultraviolet, blue, visible, and red. velocities were derived under reasonable physical assump- There are serious biological implications since the model tions. The results are applied to the derivation of a mathe- predicts that ultraviolet radiation (2000-3000 Angstroms) matical model for a simplified flexible aerodyanmic re-entry will reach the surface. Author vehicle. Author

-?,2466# Aeronutmnic. Newport Beach. Calif. ASEORPTION BY COt 6EWEEN 8OOO AND 1O.ooO Cm-1 N66-21767'# Geophysics Corp. of America. Badford. Mass. (1-126 MICRON REGION) GCA Technology Div. Darmll Burch. David A. Gryvnak, and Richard R. PatW 6 Aug. CONTRIBUTIONS TO PLANETARY METEOROLOGY E. 1965 37p refs Find Roport (Contract Nonr-3560(00); ARPA Order 273) George Ohring. Wen Tang. Frederick B. House. and Joseph (U-3200; AD-626316) CFSTI: HC $2.00/MF $0.50 Mariano Mar. 1966 87 p refs The absorption by COz in the 9300 to 9650/cm region (Contract NASw-1227) (NASA-CR-71627; GCA-TR-66-8-N) CFSTI: HC $3.00/MF and eo00 to 8325/cm region were studied. Spectra were ob- $0.75 CSCL 038 tained for four srmples of C02 in the 1.0 micron region at Reports are given on meteorological investigations of a pressure of 2.5 atmospheres and path lengths up to 933 Mars and Venus. The steady state. axially symmetric case of meters. Spectra were obtained for ten samples of COz in the the general circulation of the Martian atmosphere was con- 1.2 micron region at pressures as high as 15 atmospheres sidered. It was concluded that the symmetrical regime cannot for path lengths up to 32.9 meters and pressures as high 8s remain stable. A simple theoretical model was formulated to 2.50 atmospheres for path lengths up to 933 meters. The investigate the Martian latitudinal and seasonal variation of strengths of the important bands and the half-widths of sev- the surface and mean atmospheric temperatures. and the eral lines have been measured. Tables of transmittance ver- atmospheric heat transport effect on the temperature climate sus wavenumber a+ included for both regions as well as is discussed. The water vapor mixing ratios near the cloud- photographs of most of the specrra. Also presented are tables tops of Venus were studied, assuming a water vapor mixing of the. integrated absorptance versus wavelength for both ratio which decreases with altitude at rates comparable to regions. Author (TAB) those in the earth's upper troposphere. It was concluded that some of the observed amounts of water vapor are compatible N66-2##6'# Joint Publications Research Service, Washi& with the presence of aqueous clouds. A diffusion model was ton, D. C. developed to study the interhemispheric water vapor transport SOVIET-BLOC RESEARCH IN GEOPHYSICI). ASTRONOMY. and the Martian ice caps. It is suggested that this transport AND SPACE. NO. 130 requires a large scale eddy diffusion coefficient, and that this 18 Apr. 1966 76 p refs Transl. into ENGLISH from Russian size coefficient leads to meridional speeds of water vapor (JPRS-35095; TT-66-11147-130) CFSTI: $3.00 isopleths that are in good agreement with the observed speed Abstracts are presented for Sino-Soviet-bloc research of darkening wave propagation. N.E.N. studies dealing with astronomy. meteorology. oceanography, terrestrial geophysics. and the upper atmosphere and space. Also included are news articles and several reports of schn- tific conferences. M.W.R. N68-22218'# National Aeronautics and Space Administration. NM-23052 Texas Univ.. Austin. Dept. of Astronomy. Goddard Inst. for Space Studies, New York. THE ATMOSPHERIC ENVIRONMENTS OF MARS AND THE GREENHOUSE EFFECT IN A GRAY PLANETARY AT- VENUS MOSPHERE Rupert Wildt 3 Jun. 1965 16 p refs Submitted for Publica- G. de Vaucouleurs /n Southwest Res. Inst. Bioastmnautics tion and the Exploration of Space Dec. 1965 p 59-76 refs (%e (NASA-TM-X-56621) CFSTI: HC $l.OO/MF $0.50 CSCL 038 N66-23048 12-04 CFSTI: HC $9.40/MF $2.50 Hopf's analytical solution is illustrated for several values Current knowledge of the Mars and Venus atmospheres of the greenhouse parameter. Le.. the ratio of gray absorption is stfrfmarized. This incorporates discussions of the atmos- coefficients for insolating and escaping radiation. assumed pheric pressure. violet layer. structure and temperature, and to be constant at alldepths. Author clouds and winds. C.T.C.

NM-23493'#' Stanford Univ., Calif. Radioscience Lab. MODELS FOR THE ATMOSPHERE OF MARS BASED NW-22239*# National Aeronautics and Space Administration ON THE MARINER IV OCCULTATION U(PER1MENT Goddard Space Flight Center, Greenbelt, Md Scisntific Report Nos. 2 and 16 OBSERVED ULTRAVIOLET REFLECTIVITY OF MARS Gunnar Fjeldbo. Wencke C. Fjeldbo. and Von R. Eshleman Jan. Dennis C Evans [1965] 18 p refs Submitted for Publication 1966 36 p refs (NASA-TM-X-56654) CFSTI HC $1 00/MF $0 50 CSCLO3B (Contract pGR-05-020-065; Grant NsG-377) CFSTI: HC $2.00/MF $0.50 Ultraviolet spectrograms of Mars (2400-3500 Angstroms. (NASA-CR-74152; SEL-66-007) -50 Angstrom resolution) have been obtained using an ob- CSCL 03B

29 N66-23536

Several possible atmospheric models are investigated Measurements were made of the 6190 A absorption based on data from the radio occultation experiment, and one band intensity in the spectra of the equatorial zone and two is shown to be more likely than the others. Profiles in height temperate zones of Jupiter in 1959-61. The Observations of the constituent number densities. electron number density, were made in order to detect the possible variations in the temperature. pressure. and mass density are derived. The anal- intensity of the band as a function of time and the position ysis indicates that Mars has a tenuous carbon dioxlde lower of the investigated zone on Jupiter's disk. It was established atmosphere with a temperature of about 180°K near the sur- that the width of the 61 90 A band was the same for all of the face, and an atomic oxygen upper atmosphere with a tempera- investigated zones of Jupiter. There is an indication of small ture of only about 80°K. Frozen carbon dioxide particles may variations in the band intensity from one night to another. be an almost permanent feature of the atmosphere at inter- These variations are not associated with solar activity or with mediate altitudes. The main daytime ionospheric layer has its the longitude of the central meridian of the planet. The pos- peak density at 120 km. and is most likely a Bradbury (F2) sible reasons for these variations are as follows: the change layer with the principal ion (O+)being lost through O++ in the thickness of the pure gas layer which is over the cloud CO2'-92++CO. The atmospheric mass density decreases layer and photochemical processes in the atmosphere of nearly ten orders of magnitude from the surface to the base Jupiter. The first reason seems more likely. Author of the exosphere at 140 km. thus remaining several orders of magnitude below the density of the earth's atmosphere at N66-23674'# National Aeronautics and Space Administration. corresponding altitudes despite the lower gravity. Author Marshall Space Flight Center, Huntsville, Ala. A COMPARISON OF TWO GREENHOUSE MODELS FOR THE N66-23636'# National Aeronautics and Space Administration CYTHEREAN ATMOSPHE~RE Washington. D. C. Robert B. Owen 4 Dec. 1963 24 p refs STUDY- OF THE EARTH-TYPE PLANETS (IZUCHENIYE (NASA-TM-X-57375: MTP-AERO-63-82) CFSTI: HC $1 .OO/ PLANET TlPA ZEMlLll MF $0.50 CSCL 038 I. K. Koval Mar. 1966 13 p Transl. into ENGLISH from Surface temperatures of Venus appear to be comparable to Zemlya i Vselennaya (USSR). vol. 1. no. 6. 1965 p 53-55 a red-hot oven on the basis of a comparison of two Green- (NASA-TT-F-9898) CFSTI: HC $l.OO/MF $0.50 CSCL 03F house models for the Cytherean atmosphere which are de- The article discusses work by the USSR Academy oi scribed in the literature. Temperature estimates as high as Sciences commission on Planetary Physics in 1964 and 1965 750°K and surface pressures of over 30 atm are estimated. Atmospheric pressure investigations by photometric and pol- Temperature of the dark pole has been established by Drake to arimetric means were conducted. Aerosol influence is con. be 540°K: and possible polar seas may contain liquid benzene. sidered. Values for the Mars and Venus atmospheres are pre. acetic acid, butyric acid. and phenol. If the pressure exceeds sented. Various individual studies were presented by theit 60 atm. the seas may contain a bit of liquid water. It is con- authors. Author cluded that if the described model is valid, a surface landing presents very complex engineering problems. M.W. R.

N66-23638'# National Aeronautics and Space Administration. Washington. D. C. BRIQHTNESS DISTRIBUTION IN THE LIMB ZONE OF MARS N66-23682*# Geophysics Corp. of America. Bedford. Mass. [RASPREDELENIYE YARKOSTI V KRAYEVOY ZONE MARSA] TEMPERATURE DETERMINATION OF PLANETARY AT- L. A. Bugayenko. 0. I. Bugayenko, I. K. Koval'. and A. V. MOSPHERES Morozhenko Mar. 1966 11 p refs Transl. into ENGLISH Raymond A. Minzner. Bernard 0. Sauermann. and Lennart from Fiz. Luny i Planet (Kiev). 1964 p 54-57 R. Peterson Jun. 1964 46 p refs (NASA-TT-F-10018) CFSTI: HC $1 .OO/MF $0.50 CSCL 03A (Contract NASw-976) The results of photoelectric observations of Mars by the (NASA-CR-71862; GCA-TR-64-9-N) CFSTI: HC $2.00/MF method of cross sections are presented. The observations were $0.50 CSCL 038 made in the Cassegrain focus of the 70 cm reflector at the A method is presented whereby accurate temperature. Main Astronomical Observatory of the Academy of Sciences altitude profiles of planetary atmospheres may be determined of the Ukrainian SSR. In the opposite of 1963. the brighlness from the number-density profiles of two inert gases having distribution along the apparent radius of the planet was trqced markedly different molecular weights M. In the earth's at- up to r=0.97R 8. The data, averaged and corrected fur turbu- mosphere, such gases would preferably be helium and argon. lent scintillation of the image and for the finite size of the dia- In contrast to previous methods in which mass-density pro- phragm (0=0".35). are tabulated. It was found that for files permitted the calculation of only the ratio T/M at altitudes X<390 nm the atmosphere of Mars possesses an appreciable sufficiently below the highest altitude of density data, the two- true absorption. while for longer wavelengths scattering pro- gas method yields values of kinetic temperature T. not only at vides the main contribution. Author low altitudes where number-density data for both gases exist, but also up to the greatest altitude for which the light-gas number-density data have been measured. The method depends upon recently developed mass spectrometers with de- NW-23010'# National Aeronautics and Space Administration. tection sensitivities of the order of '106 particles per cubic Washington. D. C. centimeter. A rigorous error analysis predicts the accuracy INTENSITY OF METHANE ABSORPTION IN 6190 A BAND of the resulting temperatures on the basis of sensor and ON JUPITER'S DISK [OB INTENSIVNOSTI METANO- telemeter tharacteristics. and allows for optimizing any actual VOQO POQLOSHCHENIYA V POLOSE CHq 6190 A NA experiment as far as range and number of measurements are DISKE YUPITERA] concerned. Author V. G. Teyfel' and N. V. Priboyeva Apr. 1966 28 p refs Transl. into ENGLISH from Izv. Akad. Nauk Kaz. SSR. Ser. Fix.-Mat. N66-23713*# Michigan Univ.. Ann Arbor. Radio Astronomy Nauk (Alma-Ate). v. 16. no. 1. 1963 p 61-73 Observatory. (NASA-TT-F-10062) CFSTI: HC $2.00/MF $0.50 CSCL INVESTIGATION OF GALACTIC AND PLANETARY RADIO 038 ASTRONOMY status Report. Jut.-Dec. 1986

30 N66-23797

Fred 1. Haddock Mar. 1966 10 p refs NW-23787*# Ball 8x1s. Research Corp.. Boulder. Colo. (Grant NsG-572) ENGINEERINQ BREADBOARD MODEL. WOLF TRAP (NASA-CR-74173) CFSTI: HC $l.OO/MF $0.50 CSCL 03A .UlCROBE DETECTION DEVICE Final Ropolt A preliminary report is presented which discusses a sound- D. E. Buckendahl. L. Ried. Jr.. and E. Lemberg 8 Sep. 1965 ing rocket flight to measure cosmic radiation intensity on three 55 p refs Prepared for Rochester Univ. frequencies, 0.75. 1.225. and 2.0 Mc/s. No data was received (Grant NsG-209) at 0.75 Mc/s because of a lack of sensitivity: however. pre- (NASA-CR-74214; F65-6) CFSTI: HC $3.00/MF S0.50 liminary analysis of data at 1.225 and 2.0 Mc/s seems to CSCL 068 confirm a sharp fall in the spectrum. A discussion of some An experimental microorganism detection device, in- points in connection with the 0.75 Mc/s measurement is pro- tended eventually for a Mars landing, is described, The vided. Studies were also conducted of the Martian atmos- breadboard model optically monitors organism growth in an phere and ionosphere. A model constructed from data derived enrichment culture. Collection of an aerosolized dirt in- from the Mariner IV flight. was extended to include detailed noclum is accomplished by a gas operated suction pickup. photoionization and heat balance factors. Some conclusions Checkout equipment is described which provides automatic regarding the atmosphere above the subsolar region are given. control and data readout. Ability of the device to withstand H.S.W. high temperature sterilization is shown. Recommendations for engineering improvements are made. Author

N66-23776'# Lowell Observatory. Flagstaff. Ariz. . N66-23797'# Geophysics Corp. of America. Bedford. Mass. THE ATMOSPHERIC PRESSURE AT THE SURFACE OF MASS SPECTROMETER INSTRUMENTATION FOR THE MARS ANALYSIS OF THE MARTIAN ATMOSPHERE Final Report: Karl D. Rakos [1965] 15 p refs It5 Bull. No. 131. Vol. VI. R. F. K. Henog and W. P. Poschenrieder 12 Dec. 1962 96 p No. 12 refs Prepared for JPL (Grant NG R-03-OO3-OO3) (Contracts NAS7-100: JPL-950328) (N4SA-CR-71312) CFSTI: HC $1.00/MF $0.50 CSCL 038 (NASA-CR-71916: GCA-TR-62-17-G) CFSTI: HC $3.001 Photometric observations of eclipses of Phobos by Mars MF $0.75 CSCL 2OC were carried out by a new photoelectric scanning technique A mass spectrometer which uses a hetero-energetic ion for the purpose of estimating Martian atmospheric pressure source without need of any specific deflection field is e- on the surface of the planet. An upper limit of 30 mb for the scribed. The instrument is very simple and is of great value pressure at a mean temperature of 200°K was obtained. The for applications where high reliability. small size. small weight. observations show strong evidence of particle absorption at and low power consumption are of prime importance: and high levels in the atmosphere. The data suggest that the where a moderate resolution is adequate. The ion source is of absorption level which causes the so-called "blue haze" is the inversed magnetron type. and consists of two electrodes. not higher than 10 km above the surface of the planet. The an anode cylinder which is concentric and surrounded by a can- question as to what value should be adopted for the surface shaped cathode on ground potential. The ions are under the pressure on Mars can be solved by first answering the ques- influence of a radial electric and axial magnetic field which tion as to what distribution of solid particles in the atmosphere confines the electrons in a potential well. Special kinds of is the most Drobable. Author orbits which occur if the magnetic field is weak and if the ions follow essentially the straight lines of the electric force are investigated. Computations were carried out for axial symmetrical and other set-ups. A plane geometry was found to provide higher resolution along with other advantages. It was shown that under certain field conditions. velocity focus- General Electric Co.. Philadelphia. Missile Nm-23779'# ing can be achieved which permits the us8 of the hetero-ner- and Space Div. getic ion source as a mass spectrometer. Results of experi- USE OF A MASS SPECTROMETER TO DETERMINE THE ments with several test model instruments are presented. COMPOSITION OF THE UNDISTURBED MARTIAN AT- and evaluated. Although it was shown that simple mass spec- MOSPHERE FROM A HYPERSONIC ENTRY VEHICLE tra can be obtained with the instrument. resolution is far blow Final Report the requirements for the Martian probe. L.S. M. H. Bortner. R. P. Fogaroli. H. L. Friedman. H. W. Gold- stein, R. E. Simons et al 25 Oct. 1965 105 p refs (Contract NAS5-9602) (NASA-CR-71307) CFSTI: HC $4.OO/MF $0.75 CSCL 22A The use of a mass spectrometer aboard a hypersonic entry vehicle. to determine the chemical composition of the Martian atmosphere. was studied by application to minimum and maximum engineering models of the atmospheric medium. First. the heating of the entry vehicle was calculated throughout the entry and the results were applied to find the correspond. ing thermal response of the graphite in mass losses and ten perature changes. The quantity of the ablation products W-L then estimated and added to the chemical kinetic information to determine the gas flow composition thatenters the mass spectrometer. Thus, the factors that influenced the accuracy of the analysis were established and related to the chemical composition of the atmosphere; final model atmospheric compositions containing N2 N. COZ CO. C2N2. CN. 0,. 0. c~ and C are shown in tables. G.G.

31 A65- 1 5454

is significantly greater than that for air at similar flight copditiop.. To coyer the possibility that the Martian atmosphere coptlim argon, the COZ-N study was extended to deter- the effect of argon dilution. Tke measurements and C.~CU~~~OMshw Little change in mpectral emiasive power for a density survey taken at 7.5 km/sec. Results of the investigation are summarired .pd compared with other theoretical computatiow and reported mhock- tube measurement. . (Author) F.R.L. A6Sl436S # THE EFFECT OF FIRM DEFINITION OF THE MARS ATMOSPHERE OF THE PAYLOAD CAPABUTY OF ADVANCED MARTIAN ON MARS. D. G. Rea (California, University. Space Sciences Laboratory. LANDERS.~. E. J. Merr (General Electric Co., Missile ud Space Div., Re- Berkeley, Calif. 1. Nature, voL 201. Mar. 1964, p. 1014, 1015. refs. entry Systems Dept., Philadelphi.. Pa. ). 7. 7 Grant No. NsG 101-61. American Institute of Aeronantics ud ktronautics, Aerospace Paper dealing with a recent communication of the author con- Sciences Meeting. 2nd. New York, N.Y., Jan. 25-27, 1965. Pwar cerning the evidence for life on Mars and. in particular. the 65-22. 15-r- n. 5 refs.~~- Members. SO. 50; nonmembers, $1.00. seasonal wave of darkening and associated changes in the polarization of the dark areas. An improved rationale for a previous Description of improvements which could be attained in the model (the principal feature of which is the seasonal transport designed payload capabilities of advanced Martiaa mtrylhder of dust and the dark areas) explaining these phenomena is vehicle. if the Mar. atmosphare could be defined more precisely on off proposed. P. thm the present 11 to 30 mb estimated range. To illustrate the v. improvement att8inable. UI advanced lander syntem using tlm Saturn V launch vehicle as a booster is discussed, together with A65-15342 #t key system trade-offs. For this Mer, two systems are syntbe- CLOSE APPROACH METEOR STREAMS AND COMETS TO sired, one based on an ll-mb atmosphere only and the othsr on a OF MARS' ORBIT. 30-mh atmosphere only, both of which offer significant weight savings over the design presently dictated by the imprecision in J. K&o& (Czechoslovak Academy of Sciences, Astronomical Institute, Ond;ejov, Czechoslovakia). defining the Mars atmosphare. The results indicate the importance Astronomical Institutes of Czechoslovakia, Bulletin, vol. 15, no. 6, of an early entry probe to Mars to determine atmospheric denmity. 1964, p. 230-232. 8 refs. gradient, comtituents. adother characteristics. P. K. Calculation of the heliocentric longitudes at which a number of comets and meteor strearns have intersected the orbit of Mars at distances of less 0.3 AU. A comparison of the dates the A65-14107 than of close apprcaches with the dates the blue clearing Mars' atmo- INFRARED ASTRONOMY BY BALLOON. of of sphere, given by Kdr, shows correlation. More accurate John Strong (Job Hopkins University, Baltimore. Md.). 2s no results are seen to await improved data on the height of the planet's Scientific American, vol. 212, J=. 1965, p. 28-37. violet 1a)er. W.M.R. Description of the Feb. 21. 1964, and the Oct. 28. 1964. unmanned balloon flights designed to determine the water vapor content of the atmosphere of Venw. Sponsored by the IISAF, the A65-15368 project employed a helium-filled polyester balloon to lift a combina- LISTENING IN ON SPACE. tion Schmidt telescope and IR diffraction-grating spectrometer to G. W. Swenson (Jllinois. University, Urbana, Ill. 1. altitudes above 80, 000 ft. The telescope had a 16-in. primary LEEE Student Journal, vol. 2, May 1964, p. 2-9. 6 refs. mirror ~ichwas effectively stopped down to 11 in. The coarse Review of the field of astronomy as carried out with wave8 of and fine tracking systems. which are designed to enable the radio wavelengths. Radio astronomy makes possible the exploita- telescope to remain pointed at Venus for intervals of several hours, tion of wavelengths between about 5 Mc and 30 Gc. In the study of are described. Comparison of the spectra obtained with the IR solar radiation, the expansion of the observable spectrum by over spectra of several materials including liquid water, solid GOz. and 11 octaves has increased the acquisition of data manyfold. Study a cloud of ice crystals revealed a close match with the ice-crystal of such wavelengths helps to reveal the structure of the solar atmo- spectra. Future projects are being planned and the use of an IR sphere, makes possible the observation of physical processes in telescope of 48411. aperture is anticipated. D.H. high-temperature, fully-ionized gases, and contributes greatly to the problem of solar-terrestrial relationships. Use of radio waves A65-1SOOO .# has permitted the detailed mapping of the Galaxy, and has assisted THEORETICAL AND EXPERIMENTAL STUDIES OF EQUILIBRIUM in the interpretation of its hydrogen-line model. Radio astronomy's AND NONEQUILIBRIUM RADIATION TO BODIES ENTERING task in support of cosmological research is to discover many thou- POSTULATED MARTIAN AND VENUSIAN ATMOSPHERES AT sands of weak radio galaxies, and to measure their strengths a8 HIGH SPEEDS. accurately as possible. Results of radio-telescopic examination Junes 0. Arnold, Victor H. Reis. and Henry T. Woodward (NASA. of Jupiter are discussed. Problems of radio astronomy are angular Am+. Research Center. Moffett Field, Calif.). resolution and sensitivity, and their solution requires complex American Imtitute of Aeronautics and Astronauticm, Aerospace antennas, and utilization of the best low-noise receiving techniques. Science. Meeting, 2nd. New York. N.Y., Jan. 25-27. 1965, Paper Continuous efforts must be made to increase signal power. The 6%. 12 p. 27 refs. science has also contributed some of the most essential data for Members, $0.50; nonmembers. $1.00. the engineering of communications systems. F. R. L. Preaentation of new theoretical predictioru and extended measurements of spectral and total radiation from shock layerr Of vehicles traveling at hypersonic apeeda into 9% and 25% COz. A65-154154 * balance N~ and 16% cOZ. 48% N~,and 36% A gas mixtures. Spectra THEORETICAL MODELS OF CYTHEREAN AND MARTIAN UPPER computed for the COZ-NZ mixtures show CN violet to be the ATMOSPHERES. 1 - DISSOCIATION LAYERS. predomi-papt !pectrd feature for velocities from?. 0 to 9.5 knlsec. Mikio Shimizu (Ochanomizu University, Dept. of Physics, Tokyo, Comparison of the predictions with obaervations of shock Gyers Japan). formed about small gun-launched blunt models shows good agree- Progress of Theoretical Physics, vol. 31, June 1964. p. 1153-ll55. ment. Measurements at high ambient densities show the shock 13 refs. layer to be in thermochemical equilibrium. At lower demities. Investigation of solar-planetary relationships, particularly excessive radiation was obmerved and interpreted to be due to upper atmosphere phenomena such as ionospheres and aurorae, nonequilibrium procesaea. CN violet radiation dominates the 11011- on the basis of data from ground-based and space-probe observa- equilibrium spectra. Further, the total nonequilibrium radiation tions. Tables show the following: (1) upper atmo'spbere models

33 A65- 1 5610 and heights of the dissociation layers of Venus and Mars, and (2) of N2 contents. The critical level temperature is found to be rela- the amounts of CO on Venus. It is stated that the calculations have tively low as a result of a heat flux from the illuminated hemi- shown that the Uncertainties of scale heights and temperatures do sphere into the obscured hemisphere, despite the intensive ionizing not cause serious changes to the results. The existence of small radiation. The upper content level in the planet's atmosphere for amounts of CO on Mars and of O2 on both planets hardly affects CO, NZO, NH3. and CH4, and the relative energy distribution in them. On the other hand, the substitution of effective temperature the planet's spectrum are estimated. V.Z. for solar radiation from 4700 to 5000°K nearly doubles the quantities of CO and 0. They also depend considerably on the values of the recombination rates. The effect of atmospheric density is only to change the heiKhts of the dissociation layers. M.M. A65-15691 NEW OBSERVATIONS OF THE INFRARED SPECTRUM OF VENUS (A= 1.2 - 3.8 p). V. I. Moroz (Gosudarstvemyi Astronomicheskii Institut. Moscow, A65-15610 THEORETICAL PERFORMANCE OF METALS BURNING NITROGEN USSR). (Astronomicheskii Zhurnal, vol. 41. July-Aug. 1964, p. 711-719. ) FOR PROPULSION IN THE MARTIAN ATMOSPHERE. Soviet Astronomy. vol. 8. Jan. -Feb. 1965, p. 566-572. 24 refs. J. Q. Weber and K. H. Mueller (North American Aviation, Inc., Translation. Rocketdyne Div., Canoga Park, Calif. ). Discussion of some of the results of observations of the infrared IN: CHEMICAL ENGINEERING TECHNIQUES IN AEROSPACE. spectrum of Venus conducted in the wavelength regions of hl. 2-2.5 Edited by D. J. Simkin. and 2. 8-3. 8p. using two spectrometers with cooled lead-sdlhide Chemical Engineering Progress, vol. 60, Symposium Series. photocells attached to a 125-cm reflector. Both wavelengths and no. 52. [A65-15607 06-28] equivalcnt widths of the planetary absorption bands are measured. New York, American Institute of Chemical Engineers, 1964, It is found that some weak absorption bands could not be identified. p. 17-22. The intensities of "hot" C02 bands show that the temperature in the Different techniques by which Martian nitrogen might be used region of their formation is less than the laboratory temperature. as a propellant with primary emphasis on: (1) liquefaction and sub- Estimates are made of the C02 abundance, total pressure above sequent use as a rocket oxidizer or working fluid, and (2) use as the cloud layer, the coefficient of volume scattering in the cloud the oxidizer and working fluid in a ramjet. Theoretical rocket layer. and concentration of scattering particles. The presence of performance of liquid nitrogen with boron, aluminum, beryllium, and nitric-acid beryllium were calculated and found to fall in the a band at about 2.35 p, apparently due to CO. is confirmed. The albedo of Venus at 3.3b comprises about 1%. Absorption observed range 200 to 280 sec (Pc = 250 psia and I 40). Of the above in the region A > 3 b is probably responsible for a strong greenhouse fuels, boron was found to give the best ramjet performance. A effect which heats the planetary surface. theoretical analysis is presented of the ramjet performance over J. R. a mixture ratio range of 4 to 32 (NZ/B) and a Mach-number range of 2 to 6. Fuel-based impulses ranged from 550 to 1350. (Author) W. M.R. A65-15763 # X-RAYS IN THE AURORAL ZONE>. A I. Ershkovich (Akademiia Nauk SSSR. Institut Fiziki Atmosfery, A65-1 5619 Moscow, USSR). THERMAL PROBLEMS OF ABLATIVE MATERIALS IN VARIOUS (Geomagnetizm i Aeronomiia, vol. 4, Mar. -Apr. 1964, p. 412-414. ) PLANETARY AThLOSPHERES. Geomagnetism and Aeronomy, vol. 4. no. 2, 1964, p. 324, 325. R. M. Lurie. S. Georgiev, and P. Levine (Avco Corp., Research 7 refs. Translation,- and Advanced Development Div., Wiknington, Mass. ). Derivation of expressions for calculating the intendity of X- IN: CHEMICAL ENGINEERING TECHNIQUES IN AEROSPACE. radiation in the regions of aurorae polaris on the assumption that Edited by D. J. Simkin. the atmosphere is practically transparent. It is noted that measure- Chemical Engineering Progress. vol. 60, Symposium Series, ments of the intensity of X-ray radiation In the regions of aurorae no. 52. [A65-15607 06-28] polaris of a planet can be used to determine its magnetic moment. New York, American Institute of Chemical Engineers, 1964, p. 91-98. Study of heat shield requirements and heat transfer phenomena AM-1 5944 * on contact of a probe with the atmospheres of Earth, Mars, and A MARS SKIP-OUT CAPSULE FOR IN-FLIGHT ATMOSPHERIC Venus. Unmanned exploration of Mars a6d Venus, now in the plan- MEASUREMENTS. ning stage. pones the problem of entry velocities into these planets Haim Kennet and John F. Wayne (Boeing Co., Aero-Space Div., as high as 45,000 fps and re-entry into the Earth's atmosphere at Flight Technology Dept., Seattle, Wash. ). speeds up to 75,000 fps. Two promising heat shield materials are American Institute of Aeronautics and Astronautics. Aerospace described:' dense carbon-reinforced charring resins are particular- Sciences Meeting, Znd, New York, N. Y., Jan. 25-27. 1965. ly effective against high radiative heating rates, while low-density Paper 65-23. 16 p. 17 refs. char-forming resins have especially low thermal conductivities. Members, $0.50; nonmembers. $1.00. These materials also show mechanical and thermal properties that Discussion of the use of a ballistic skip-out capsule, considered are compatible with apace and pre-entry environmental requirements. to be a feasible method of determining.the characteristics of the The preliminary results are presented of solar furnace experhents Martian stratosphere. The capsule would be injected into the atmo- W. on these materials. M. R. sphere from either a fly-by bus or an orbiter. On-board accelerometers, a densitometer. a radar altimeter and a mass spectrometer provide the desired information concerning the density-altitude pro- A65-15676 #t file in the stratosphere as well as ambient composition. The capsule. INFRARED SPECTRUM OF MERCURY (A 1.0 - 3.9 p) [INFRA- though sterilized by the best available techniques to avoid biological KRASNYI SPEKTR MERKURTIA (A 1.0 - 3.9 p)]. contamination of th? planet, is designed to exit the atmosphere ~.. ~~~ .- ~~ . ~ V. I. Moroz (Moskovskii Gosudarstvennyi Universitet, Astronomi- hyperbolically. Furthermore, as ahadded prtcaution, a nonahlating cheakii Inqtitut, Moscow. USSR). structure is used. and all propulsion maneuvers are accomplished Astronomicheskii Zhurnal, vol. 41. Nov. -Dec. 1964, p. 1108-1117. well outside the sensible atmosphere. The deposition of either ahla- 15 refa. In Russian. tion or engine exhaust products on the planet is thus avoided. Capsule Observation, in October 1963, of the Mercury spectrum in the performance has been investigated parametrically, considering all region 1.0 - 3.9 p, by means of a 125-cm reflector and two IR pertinent mission phases. namely: injection, penetration, and post- spectrometers with PbS-photoresistances cooled with solid coz or encounter. The studies included propulsion requirements, configura- liquid N2. The CO 2 -lines are found to be more pronounced in tion requirements, trajectories, entry dynamics. entry loads and Mercury's atmosphere as compared to the telluric lines, and a heating. communication and power requirements. as well as the C02 content of 0.3 to 7 gm,km'2 is established. A model of effects of atmosphere uncertainties. From these, system and mission Mercury's atmosphere is designed. assuming 10% of CO2 and 900f0 parameters have been established, including (1) optimum injection

34 A65- 1 6989

points (from highly elliptic orbits about Mars) that minimize propel- interaction of electromagnetic waves under the effect of a quasi- lant weight; (2) magnitude and direction of the required total impllse; transverse magnetic field; the calculation of this interaction by (3) minimum capsule nose radius; (4) optimum capsule ballistic coef- means of phase integrals; the interpretation of solar radio emission ficient; (5) optimum total system weight; (6) antenna beam-width in terms of the wave interaction effect in the region of a quasi- requirements; (7) thermal protection and structural weights. and (8) transverse magnetic field in the corona; and the problem of the capsule configuration requirements. On the basis of the parametric ejection of charged particles from the corona. Chapter 7 deals with studies, an optimum skip-out capsule has been conceptually designed the generation and absorption of electromagnetic waves in the solar for a typical mission and its performance determined for both nominal corona. including: the emission and absorption of electromagnetic and off-design conditions. (Author) F. R. L. waves in an equilibrium plasma; the transport equation of radiation; the emission of electromagnetic waves by individual particlea; the absorption of electromagnetic waves in an isotropic and in a A4S-1- #t magnetoactive plasma; the gyroresonance absorption in the solar EARTH RE-ENTRY SIMULATION OF PLANETARY ENTRY EN- corona; and the emission, absorption, and amplification of electro- VIRONMENT. magnetic waves in a nonequilibrium plasma. Chapter 8 outlines the theory of thermal solar radiation. It reviews the theory of the H. Kennet and R. A. Taylor (Boeing Co., Aero-Space Div., Flight Technology DeDt.. Seattle. Wash. ). radiation of the quiet Sun, and the mechaniam of this radiation; the theory of the B-component for a simple model of corona and the Americ&&st&e of Aeronautics 'and Astronautics and NASA, the Flight Testing Conference. Huntsville, Ala., Feb. 15-17. 1965. chromosphere; the interpretation of the peculiarities and the Paper 65;2;. 16 p. 12 refs. distribution of radio brightness over the solar disk on the basin of Members 50; nonmembers. $1.00. a complex model of the corona and chromosphere; and the origin of Study of the feasibility of "-ai& re-entry through the Earth's the slowly varying component of s+r radio emiasion. Chapter 9 atmosphere to simulate the entry environment for a Mars or Venus reviews the theory of nonthermd solar radiation, including the generation of sporadic continuum-type radiation; the origin of entry vehicle. The key subsystems associated with the entrv Dhase and of the intensive radio emission associated of unmanned Mars or Venus~eGlorationsyG& and -the emiron- microwave bursts. with the sunspots; the generation of Type-I, Type-33, Type-III mental characteristics influencing them are examined, and all similitude relationahips which must be fulfilled to ensure a simula- bursts; and the mechanism of these bursts. Chapter 10 examines the origin of the radiation from the planets and the Moon. It tion of the planetary entry environment are derived. It is found that the simultaneous simulation of those entry environmental char- discusses the hypothesis of the mechanism of the sporadic radiation from Jupiter; the "storm" hypothesis; the mechanism of natural acteriatics that are independent of ambient atmosphere composi- plasma oscillations; the origin the continuous radiation from tion. such as deceleration. aerodynamic loads, and convective of heating, is feasible. and does not impose unrealistic requirements. Jupiter and Saturn; the radiation belts as a source of the decimeter radiation from Jupiter; the radio sources of Venus; and the theory In addition, the total radiative heat load can be simulated exactly. of the radio emismion of the V.P. and the radiative heating history clomely. Ablative mass losses Moon. of the thermal protective system can also be simulated, aa cau communication blackout. P. K. A65-16981 ASTROCHEMISTRY - THE UNG-DISTANCE SCIENCE. A6S-16909 Francis 0. Rice (Notre Dame University, Radiation Laboratory RADIOEMISSION OF THE SUN AND PLANETS [RADIOIZLUCHENIE and Dept. of Chemistry. Notre Dame, Ind. 1. SOLNTSA I PLANET]. Chemical and Engineering'hws. vol. 43, Feb. 15, 1965, p. 88-%, V. V. Zhelezniakw. 96-102. Moscow. Izdatel'stvo Nauka. 1964. 560 p. In Russian. General outline of conceivable chemical dents in outer space, This monograph presents the results of worldwide radio- covering occurrence. state. and behavior of the elements on the telescopic studies of the emission from the Sun, Moon. and planets planets and the Moon. Meteorites are discussed as a tangible of the solar system. and discusses the problems of the mechanism source of astrochemical information. and the physical and astro- of these radio emissions. Chapter 1 reviews the physical conditions nomical characteristics of the planets, the escape speed of the on the Sun, the Moon. and the planets Mercury, Venus. Mars, constituent molecules of a planet's atmosphere, and some chemical Jupiter, and Saturn. Chapter 2 outlines. the basic features of figures for meteorites are tabulated. Free radicals are mentioned extraterrestrial radio emission and the methods used to study this as a possible source of the colored zones on Jupiter. The atmo- emission. The following are covered the frequency spectrum of spheric chemical and temperature profile, the atmosphere as a radio emission; the antenna temperature and the eifective tempera- participant in life cycle, the Ranger pictures of the lunar surface, ture of radio emission; multichannel radio receivers and radio and extraterrestrial life are other topits. v. 2. spectrographs; the requirements posed to antenna systems in radio astronomy; paGabolic antennas; the iwo-element interferometer; the MUS cross; the polarization of radio emission; the effect of the A65-16W9 # Earth's atmosphere on the nature of the observed radio emission; DEFINING MARS' ATMOSPHERE - A GOAL FOR THE EARLY the absorption of radio waves in the troposphere and ionosphere; MISSIONS. the effects associated with the refraction of radio waves in the Alvin Seiff and David E. Reese. Jr. (NASA, Ames Research Center, atmosphere; and the change in palarization of radio emission in the Vehicle Environment Div., Moffett Field, Calif,). passage through the ionosphere. Chapter 3 gives the results of Astronautics and Aeronautics, vol. 3. Feb. 1965, p. 16-21. 9 refs. observations of the radio emission from the quiet Sun. The Technique for measuring the atmospheric properties of planets following are covered the frequency spectrum and intensity of through the response of an mtry vehicle to the atmosphere. This this radio emission; the dependence of solar effective temperature response can be sensed in many forms - in the deceleration. pitching upon wavelength; and the distribution of radio brightness over the oscillation, heating, and radiation exposure, among others - and it solar disk. Chapter 4 presents the result8 of observations of the can be analyzed to define the properties of the atmosphep encoun- sporadic radio emission of the Sun, including: the slowly varying tered. It is deemed necessary to define the profile of atmosphetic ' component; microwave bursts; solar storms; Type-II. Type-XII. density aa a function of altitude in order to guide the design of pay- Type-IV, and Type-V bursts; rapidly drifting decimeter bursts; load-landing vehicles and to provide a firm base for long-range continuous storms; short-lasting broadband bursts; and double studies of manned entry systems. Integration of the density profile. bursts wit3 inverse frequency drift. Chapter 5 gives the results of once obtained, also permits the definition of static pressure profile observations of the radio emission from the Moon and planets, and the RT product profile. These and atmospheric temperature including the sporadic radiation of Jupiter, and the continuous serve to define the atmospheric structure. Atmospheric composi- radiation of planets. Chapter 6 examines the propagation of radio tion can also affect the aerodynamics of certain entry-vehicle waves in the solar corona. It covers: the propagation of electro- configurations and the he+ing', especially the radiative heating. magnetic waves in an isotropic and a magnetoactive coronal plasma. The primary experiment of this kind proposed for the Mars atmo- and in a homogeneom plasma in the presence of a constant magnetic spheric probe involves measuring nitrogen, as yet only assumed to field; the polarization of the emission from a coronal plasma; the be a principal constituent of the Mars atmosphere, and its mole

35 A65-17 164 fraction. , This can be done by measuring the intensity history of is seen to lie in its ability to demonstrate, in actual operation, the the prominent cyanogen violet bands. The possibility of detecting validity of the concept of atmosphere -sensing instrumentation sys- trace amounts of water vapor remains undemonstrated. W .M.R tems, in its proofing of the operation of aerodynamic retardation systems, and in its demonstration of communications link operation under actual conditions of vehicle motion and plasma sheath A65-17164 blackout. Limitations are found to include an oversimulation of the STUDY OF THE ELONGATION OF THE HORNS OF THE CRESCENT Mars-entry heating profile, brought about by the relatively high OF VENUS IN JUNE 1964 [ETUDE DE L'ALLONGEMENT DES Earth-entry convective heat flux, and the high costs of full-scale CORNES DU CROISSANT DE VENUS EN JUIN 19641. tests of large entry systems. A brief discussion of the suitability Audouin Dollfus and Eric Maurice (Paris, Observatoire. Section of available launch vehicles and a hypothetical test program for a d' Astrophysique, Meudon, Seine-et-Oise, France). small Mars atmospheric probe illustrate the applications of Earth- Acadehie des Sciences (Paris), Comptes Rendus. vol. 260, no. 2. entry tests to presently hypothesized Mars-entry hardware. Jan. 11, 1965. p. 427-430. In French. (Author) W. M.R. Discussion of a photometric study of the aureole which elongates the horns of Venus at the time of inferior conjunction. Evidence indicates that the atmosphere above the cloud layer is charged with A65-17422 particles of about 1-p diameter whose number decreases by a factor SYSTEM ASTROPHYSICS. of 2 about every 2.8 km and whose coefficient of diffusion per cm3 SOLAR J. C. Brandt (Kitt Peak National Observatory. Space Div., Tucson. at the opposition of the Sun has a value of about 3.10-8 stilb/phot at Arie.) and Hodge (California, University, Dept. Astronomy. the level of the cloud layer. F. R. L. P. W. of Berkeley, Calif. ). New York, McGraw-Hill Book Co., Inc., 1964. 457 p. A65-17189 $12.50. AN UPPER LIMIT TO THE MOLECULAR OXYGEN CONTENT OF Intended for use as a text in advanced undergraduate or graduate THE VENUS ATMOSPHERE. courses in solar system astronomy and space physics. the work is Hyron Spinrad (California. University, Berkeley Astronomical considered also of nlue to workers in various fields of space re- Dept., Berkeley; California Institute of Technology, Jet Propulsion search as a fairly high-level introduction to the astrophysics of the Laboratory, Pasadena, Calif. ) and E. H. Richardson (Dominion solar system. The book discusses the basic principles of celes- Astrophysical Observatory, Royal Oak, British Columbia, Canada). tial mechanics, and presents a few applications appropriate to other Astrophysical Journal, vol. 141, Jan. 1, 1965. p. 282-286. 16 refs. solar system problems. Basic solar data are renewed, and the Presentation of an improved determination of the upper limit methods of determining the internal structure ofthe Sunare outlined. to the 02 content of the visible Venus atmosphere. obtained with the as well as the present knowledge of its formation and evolution. The Doppler-shift technique and a curve-of-growth analysis. It is stated fourth and fifth chapters discuss the,physical conditions in its atmo- that the lack of displaced Cytherean O2 lines near the tail of the sphere and the sixth chapter deals with the wide variety of solar ac- telluric A-band leads to a limit of 57 cm-atm 02. less than the ter- tivity. while.in the seventh chapter, which discusses observations of restrial abundance by a factor of 2800. This result is said to be in the solar spectrum. the properties of the terrestrial atmosphere a* disagreement with the tentative detection of Venus oxygen lines they affect solar radiation are also examined. Further on, the claimed by Prokofiev and Petrova. These spectrograms include a physics of the interplanetary gas is considered. Comets, meteors, contribution of light scattered from fairly deep in the Venus atmo- meteorites. asteroids, and interplanetary dust each have chapters sphere, as evidenced by total pressure measured from nearby C02 to themselves. The fourteenth chapter briefly introduces the sub- line widths. The relative abundance of Venus oxygen is less than ject of the planets and two subsequent chapters discuss planetary 8 x 10-5. This negative result is interpreted, and the possibilities interiors and planetary surfaces. The atmospheres of the Jovian of future attempts to detect Cytherean molecular oxygen from space planets and of the terrestrial planets are described and discussed. are briefly discussed. (Author) M. M. The concluding chapter deals with the Moon and other satellites. Bibliographical notes are given at the end of each chapter. A subject index is presented. The text is illustrated with numerous dia- A65-17213 * grams and photographs. F. R. L. A THEORETICAL INVESTIGATION OF JOVIAN UPPERAT- MOSPHERE. I - 1ONIZATION AND DISSOCIATION. Mikio Shimizu (Ochanomizu Women's University, Dept. of A65-17992 Physics, Tokyo, Japan). NITROGEN OXIDES ON Progress of Theoretical Physics, vol. 32. Dec. 1964, p. 977-979. MARS. 9 refs. Carl Sagan (Harvard University, Harvard College Observatory; Smithsonian Institution. Smithsonian Astrophysical Observatory, Investigation of the effect of the solar ionizing radiation on the Jovian upper atmosphere. Jupiter's microwave radiation may be Cambridge, Mass.), Philip L. Hanst (Avco Gorp., Research and Advanced Development Div. , Wilmington, Mass. ), and Andrew T. separated into three components: (1) the 130°K thermal radiation; (2) the nonpolarized, nonthermal radiation (possibly due to a Jovian Young (Harvard University, Harvard College Observatory, ionosphere); and (3) the polarized nonthermal radiation (possibly Cambridge, Mas s . ). 51 refs. due to the aynchrotron radiation of electrons in a Jovian Van Allen Planetary and Space Science, vol. 13, Jan. 1965, p. 73-88. Comprehensive analysis the case for the presence belt). The results of the calculation of hydrogen and electron den- of of sity distribution in the Jovian upper atmosphere are presented in nitrogen oxides on Mars. Analyses of observations at a variety of wavelengths place a firm upper limit on the Martian NO2 abundance graphical form. F. R. L. of 1 mm-atm. Nitrogen dioxide is a highly photolabile gas and will be photodissociated by visible and ultraviolet radiation on Mars. The photochemical equilibria of nitrogen oxides on Mars have been A65-17398 # computed from the observational upper limits on the NO and O2 EARTH ENTRY FLIGHT TEST OF MARS ENTRY VEHICLES. abundances. The same procedure gives consistent results for the F. G. Beuf. G. D. Kate. and R. J. Kern (General Electric Co., Earth, at locales free from urban pollution. The corresponding Missile and Space Div., Re-entry Systems Dept., Philadelphia, theoretical upper limit to the abundance of NO2 on Mars is 1 mm- Pa. ). atm. when reactions with water are neglected. When reactions with American Institute of Aeronautics and Astronautics and NASA, water are considered. the NO2 abundance 1s further diminished. Flight Testing Conference, Huntsville, Ala., Feb. 15-17, 1965, These low abundances are regarded as inadequate to account for Paper 65-219. 16 p. the Martian observables discussed by Kiess et al. The one Martian Members, $0.50; nonmembers, $1. 00. phenomenon in which it is suggested that nitrogen peroxide may Systems studies to assess the degree to which Martian-entry play a role is the blue haze, where 1 rnrn-arm may help to explain conditions can be simulated in an Earth-entry test program,and an not only the general blue and violet opacity, but also the dependence estimate of the launch vehicle. tracking, cost. and schedule re- of the opacity on time and position. The required abundance of NO quirements for such a test series. The value of the test program must then be > 50 cm-atm. (Author) A. B. K.

36 A65-18479

A65-1- lunar comparisons and a limited set of laboratory calibrations. MOLECUM SPECTROSCOPY AND ASTROPHYSICAL PROBLEMS. The iR spectra are examined for the presence of constituents other G. Herzberg eational Research Council. Div. of Pure Physics. thmCO2 (COS CH "3. HzS, NO, N2O. HCHO. and COS), md Ottawa. Canada). for the presence of4'isotopic bands of C02. The Om isotopic band (Optical Society of America. Ives Medal Award Lecture, New York. at X 2.15 p is definitely present in the Martian spectra and allows N. Y., Oct. 9. 1%4.) a provisional determination of the d8/0l6ratio relative to the Optical Society of America, Journal, vol. 55. Mar. 1965. Earth. The evidence is strong, though not yet conclusive. that this P. 229-238. 99 refs. ratio is larger on Mars than on the Earth. The other gases listed Consideration of molecular problems of astrophysics - such as are all below the threshold of detection, with the upper limits given the question of the presence of molecular hydrogen in planets and in the text. The Martian spectral intensities are also expressed in the interstellar medium, or the question of the composition of in terms of those derived for the Moon; the ratio spectra SO oh- Comets - which have stimulated a good deal of laboratory and tbe- tained for Mars are summarized graphically. In the introductory dretical work in molecular spectroscopy. It is stated that, con- parts of the paper a discussion is given of the types of atmospheric versely. advances in molecular spectroscopy have made possible particles detected in the Martian atmosphere and the information a better understanding of many astrophysical phenomena. Exam- that may be derived therefrom. A rough value of the atmospheric ples for this mutual cross-fertilization are discussed. pressure (10 to 20 mb) is thus derived. (Author) D.H. (Author) M.M.

A65-18223 HOT SHADOWS OF JUPITER. AM-1-n # Robert L. Wildey (Carnegie Instltution of Washington and California A DETERMINATION OF -THE COMPOSITION AND SURFACE Insatute of Technology. Mount Wilson and Palomar Observatories; PRESSLIRE OF THE MARTIAN ATMOSPHERE. T. C. Owen Witt Peak National Observatory; Arizona, University. California Institute of Technology, Div. of Geological Sciences, Pasadena. Calif. ). Lunar and Planetary Laboratory, Tucson, Ariz. ) and Science. vol. 147. Feb. 26. 1965, p. 1035. 1036. G. P. Kuiper (Arizona, University, Lunar and Planetary Labora- Presentation of photometric observations of Jupiter. On the tory, Tucson, Ariz. ). evenings of 26 Oct. and 15 Dec. 1962, while the disk of Jupiter was IN: COMMUNICATIONS OF THE LUNAR AND PLANETARY being scanned for thermal emission in the 8- to 14-micron wave- LABORATORY. VOLUME 2 (Numbers 31-35). length region, a large enhancement was discovered in the ermssion Tucion, University of Arizona Press. 1964, p. 113-132. Grants No. NsG 61-161; No. 223-61; No. Nonr (G)-0050-62; from shadows cast on Jupiter by the Jovian satellites Ganymede NwG and Europa. However. on the eveplng of 14 Dec. 1964. the shadow NO. ONR-00014-64. of satellite io was observed and no enhancement was detected. It Calibration of 1 to 2.5 p Martian spectra using laboratory is concluded that the effect is thus variable with time. spectra of pure GO2 and mixtures containing C02. N2. and Ar. (Author) M, M. Pathlengths up to 3.6 km are used and presmrei down to 4 mm. With the aid of the total C02 content (based on the Mt. Wilson spectrum) preliminary values are derived for the pressure in the A65-18475 Martian atmosphere and the total amount of gases other than GOz. COMMUNICATIONS OF THE LUNAR AND PLANETARY The values obtained are 17 f 3 mb (13 mmHg) and (N2 t Ar)/C02=6. LABORATORY. VOLUME 2 (Numbers 31-35). Arguments are given indicating that the Ar/NZ ratio is probably Tucson, University of Arizona Press, 1964. 173 p. similar to that for the Earth atmosphere (z10-2) and that the O2 content is probably less than 7 an-atm. (Author) D.H. CONTENTS: INFRARED SPECTRA OF STARS AND PLANETS. N -'THE SPECTRUM OF MARS, 1-2.5 MICRONS, AND THE STRUCTURE AM-lU78 * OF ITS ATMOSPHERE. Gerard P. Kuiper (Arizona, University. A DETERMINATION OF THE MARTJAN CO ABUNDANCE. Tucson. Ariz. ), p. 79-112. 33 refs. [See A65-18476 08-30] T. C. Owen (Arizona, University, Lunar a& Planetary Laborato- A DETERMINATION OF THE COMPOSITION AND SURFACE ry; Kitt Peak National Observatory, Tucson. Ariz. ). PRESSURE OF THE MARTIAN ATMOSPHERE. T. C. Owen W: COMMUNICATIONS OF THE LUNAR AND PLANETARY (Kin Peak National Observatory; Arizona, University. Tucson. LABORATORY. VOLUME 2 (Numbers 31-35). Ariz. ) and C. P. Kuiper (Arizona, University. Tucson. Ariz. 1, Tucson. University of Ariwna Press, 1964, p. 133-140. 7 refs. p. 113-132. [See A65-18477 08-30] ONR Contract No. NR 046-791. A DETERMINATION OF THE MARTIAN C02 ABUNDANCE. Presentation of two independent determinations of the C02 T. C. Owen (Arizona, University; Kitt Peak National Observatory. content of the Martian atmosphere derived from the Mt. Wilson Tucson. Ariz. ), p. 133-140. 7 refs. [See A65-18478 08-30] plate obtained by Kaplan, Miinch, and Spinrad. Observations and LABORATORY SPECTRA FOR TESTING THE PRESENCE experimental procedures are described and solar observations and OF MINOR CONSTITUENTS IN PLANETARY ATMOSPHERES. laboratory calibrations are discussed. An appendix on atmospheric I - CH4, "3. N20, CO, COS, REGION 1-2.5 p. Gerard P. temperature and the L 05-p C02 bands and a note added in proof Kuiper and Dale P. Cruikshank (Arie~~,University. Tucson, are included. D. H. Ariz. ), p. la-165. [See A65-18479 08-30] IMPROVED TEST FOR NO2 ON MARS. James V. Marshall (Arizona. Univeriity. Tucson, Ariz. ), p. 167-173. 8 refs. [See A65-18480 08-30] 165-18479 * LABORATORY SPECTRA FOR TESTING THE PRESENCE OF MINOR CONSTITUENTS IN PLANETARY ATMOSPHERES. I - A65-18476 # CH4, "3, N20, CO, COS, REGION 1-2.5 p, INFRARED SPECTRA OF STARS AND PLANETS. N - THE Gerard P. Kuiper and Dale P. Cruikshmk (Arizona, University, SPECTRUM OF MARS, 1-2.5 MICRONS, AND THE STRUCTURE Lunar aud Planetary Laboratory, Tucson. Ariz. ). OF ITS ATMOSPHERE. IN: COMMUNICATIONS OF THE LUNAR AND PLANETARY Gerard P. Kuiper (Arizona, University. Lunar and Plrnetary LABORATORY. VOLUME 2 (Numbern 31-35). -hboaatory. Tucion, Ariz. 1. Tucson, University of Arizona Preis, 1964. p. 18-165. (NASA, 6%&r~c~Oct.l, 2, 1963, Washiton. D. C. ). Grant No. NsG 161-61. IN: COMMUNICATIONS OF THE LUNAR AM) PLANETARY Presentation of five reference spectra obtained with a PbS LABORATORY. VOLUME 2 Mumbers 31-351. spectrometer operating in part of the region here rotation- Tucson, University of Arizona Press, 1964, p. 79-112. 33 refs. vibration bands occur. The laboratory spectra presented were Grant No. NsG 161-6L made with the PM spectrometer described previously by Kuiper presentation of 1 to 2. 5 u spectra of the planet Mars obtained at al. Absorption cells of various lengths were made of glass with the 82-in. telescope of the McDonald Observatory, including tubing; the light source was an incandescent laboratory lamp.

37 A65- 18480

The spectra show, in addition to the absorption of CH4, "3, [PRIBLIZHENNOE RESHENIE ZADACHI 0 DIFFUZNOM OTRAZHE- NZO, CO, and COS, absorptions caused by CO2 and H20 in the NII I PROPUSKANII SVETA ATMOSFERAMI PLANET PRI spectrometer and the laboratory (with some enrichment of COz PROIZVOL' NO1 INDIKATRISE RASSEIANIIA]. E. G. Ianovitskii, due to evaporating dry ice). The total path in the spectrometer p. 92-110. 20 refs. [See A65-18975 09-30] and laboratory was about 3 m. D. H. AUTOMATIC POLARIMETER OF THE MAIN ASTRONOMICAL OBSERVATORY OF THE ACADEMY OF SCIENCES OF THE UKRAINIAN SSR [AVTOMATICHESKII ELEKTROWLIARIMETR A65-18480 # GAO AN USSR]. 0. I. Bugaenko, p. 111-125. 5 refs. [See A65-18976 09-14] IMPROVED TEST FOR NOZ ON MARS. [TIPY KOMETNYKH KHVOSTOV]. James V. Marshall (Arizona, Universlty. Lunar and Planetary TYPES OF COMET TAILS A. A. Demenko, p. 126-138. 70 refs. [See A65-18977 09-30] Laboratory, Tucson, Ariz. ). IN: COMMUNICATIONS OF THE LUNAR AND PLANETARY LABORATORY. VOLUME 2 (Numbers 31-35). Tucson, University of Arizona Press, 1964. p. 167-173. 8 refs. A65-18971 Grant No. NsG 161-61. * STUDY OF OPTICAL PROPERTIES OF THE ATMOSPHERE AND Derivation, on the basis of new laboratory tests and micro- SVOISTV photometer traces of Mt. Wilson coudd spectra, of an upper limit SURFACE OF MARS [K IZUCHENIIU OPTICHESKIKH ATMOSFERY 1 POVERKHNOSTI MARSA]. of 8 micron-atm of NO2 in a vertical column of the Martian at- I. K. Koval'. mosphere. This 1s two orders of magnitude less than the previous PHYSICS OF THE MOON AND PLANETS [FIZIKA LUNY I limit and appears to remove empirical arguments for the presence IN: PLANET]. of this gas in the (normal) Martian atmosphere. (Author) D.H. Edited by I. K. Koval' . Kiev, Naukova Dumka, 1964, p. 46-53. 12 refs. In Russian. A65-18553 4# Study of the problem of brightness distribution along the visible A MICROWAVE RADIOMETER AND MEASUREMENT OF JUPITER radius of Mars. Results obtained by other authors for narrow re- RADIATION [RADIOMETR DETSIMETROVOGO DIAPAZONA I gions of the spectrum over a range of 400 to 900 m IJ are discussed. IZMERENIE SOBSTVENNOGO IZLUCHENIIA IUPITERA]. It is c'oncluded that, within this range of wavelengths, the Martian atmosphere possesses mainly scattering properties. The darkenlng 0. N. Rzhiga. G. I. Slobodeniuk, V. N. Titov, and Z. G. Trunova of the limb has its maximum at about 650 mu. A decrease in the (Akademiia Nauk SSSR, Institut Radiotekhniki i Elektroniki, Moscow, USSR). limb darkening to the left of this wavelength is due to a scattering To the right of thls wave- Radiotekhnika i Elektronika, vol. 10, Feb. 1965, p. 364-367. similar to that of the molecular type. 12 refs. In Russian. length, this decrease is attributed to the. scattering by large dust Description of a modulation microwave radiometer used to particles constantly present In larger or smaller quantities in the Martian atmosphere. J. R. measure the intensity of Jupiter radiation at a frequency of about 700 Mc in October 1963. A block-diagram of the instrument is included. The value of the average Jupiter temperature obtained from a series of observations was 12,000°K. The results are shown to confirm the law of intensity variations in Jupiter radiation A65-18972 with wavelength. J. R. BRIGHTNESS DISTRIBUTION IN THE MARGINAL ZONE OF MARS [RASPREDELENIE IARKOSTI V KRAEVOI ZONE MARSA]. L. A. Bugaenko. 0. I. Bugaenko, I. K. Koval', and A. V. A65-18967 Morozhenko. PHYSICS OF THE MOON AND PLANETS [FIZIKA LUNY 1 PLANET]. IN: PHYSICS OF THE MOON AND PLANETS [FIZIKA LUNY I Edited by I. K. Koval' . PLANE TI. Kiev, Naukova Dumka, 1964. 140 p. In Russian. Edited by I. K. Koval' . Kiev, Naukova Dumka, 1964, p. 54-57. In Russian. CONTENTS: Presentation of the results of photoelectric observations of POLYCHROMATIC POLARIMETRY OF SOME LUNAR AREAS Mars by the method of cross sections. The brightness distribution [MNOGOTSVETNAIA POLLAFtIMETRIIA NEKOTORY KH UCHASTKOV along the visible radius of the planet was traced up to r = 0. 97 of LUNY]. V. V. Avramchuk, p. 3-15. 16 refs. [See A65-18968 09-30] the Mars radius. The results. averaged and corrected for tur- SPECTROPHOTOMETRY OF DETAILS ON THE LUNAR SUR- bulent vibration of the image and for the dimension of the diaphragm FACE [SPEKTROFOTOMETRIIA OB' EKTOV LUNNOI POVERKH- (D = 0". 35), are tabulated. It is found that for A< 390 m u. the at- NOSTI]. M. N. Mironova, p. 16-29. 9 refs. [SeeA65-18969 09-30] mosphere of Mars possesses a considerable true absorption, while SPECTRAL INVESTIGATIONS OF THE LUNAR SURFACE at large wavelengths the main role is attributed to scattering. [SPEKTRAL' NYE ISSLEDOVANIIA LUNNOI POVERKHNOSTI]. J. R. A. N. Sergeeva, p. 30-45. [See A65-18970 09-30] STUDY OF OPTICAL PROPERTIES OF THE ATMOSPHERE AND SURFACE OF MARS [ K IZUCHENIN OPTICHESKIKH A65-18974 SVOISTV ATMOSFERY I POVERKHNOSTI MARSA]. I. K. Koval' , METHOD AND RESULTS OF DETERMINATION OF OPTICAL p. 46-53. 12 refs. [See A65-18971 09-30] PARAMETERS OF THE MARTLAN ATMOSPHERE AND SURFACE BRIGHTNESS DISTRIBUTION IN THE MARGINAL ZONE OF [METODIKA I RESUL'TATY OPREDELENIIA OPTICHESKIKH MARS [RASPREDELENIE IARKOSTI V KRAEVOI ZONE MARSA]. PARAMETROV ATMOSFERY I WVERKHNOSTI MARSA]. L. A. Bugaenko, 0. I. Bugaenko. I. K. Koval, and A. V. A. V. Morozhenko and E. G. Ianovitskii. Morozhenko, p. 54-57. [See A65-18972 09-30] IN: PHYSICS OF THE MOON AND PLANETS [FIZIKA LUNY I RESULTS OF POLARIMETRIC OBSERVATIONS OF MARS PLANET]. FROM 1962 TO 1963 [REZUL' TATY POLIARIMETRICHESKIKH Edited by I. K. Koval' . NABLIUDENII MARSA V 1962-1963 GG]. A. V. Morozhenko, Kiev, Naukova Dumka, 1964, p. 81-91. 20 refs. In Russian. p. 58-80. 19 refs. [See A65-18973 09-30] Presentation of a method for determining the optical parameters METHOD AND RESULTS OF DETERMINATION OF OPTICAL of the atmosphere and surface of Mars, based on data from absolute PARAMETERS OF THE MARTIAN ATMOSPHERE AND SURFACE photometry. In particular, the method is shown to make possible [METODIKA I RESUL' TATY OPREDELENIIA OPTICHESKIKH a rapid and reliable determination of both the optical thickness and PARAMETROV ATMOSFERY I POVERKHNOSTI MARSA]. the absorbing power of the atmosphere. On the basis of the results A. V. Morozhenko and E. G. Ianovitskii. p. 81-91. 20 refs. obtained, it is concluded that,in the range of wavelengths from 450 [See A65-18974 09-30] to 840- mLo, the Martian atmosphere is purely diffusive. Beginning APPROXIMATE SOLUTION OF THE PROBLEM OF DIFFUSE with A -450 mi, the true absorption increases with a decrease in REFLECTION AND TRANSMISSION OF LIGHT BY ATMOSPHERES wavelength. In the range of wavelengths from 360 to 450 mu the OF PLANETS FOR AN ARBITRARY DISPERSION COEFFICIENT optical thickness of the Martian atmosphere can vary within very

38 A65- 1 9520

broad limits, frequently exceeding unity. L the infrare n ultra- Norm diffusion esti shes the pre minance c itomic oxygen in violet regions of the spectrum, the albedo of the Martian su ice the upper thermosphere, and it is concluded that the less-abundant varies much more slowly with wavelength than in the visible region. elements in the homosphere end up by dominating the nitrogen and the J. R. oxygen, and creating belts of helium and hydrogen, before escaping under one form or another from the exosphere. F.R.L. A&-18975 *- APPROXIMATE SOLUTION OF THE PROBLEM OF DIFFUSE A65-19505 # REFLECTION AND TRANSMISSION OF LIGHT BY ATMOSFWERES BUOYANT PROBES INTO THE VENUS ATMOSPHERE. OF PLANETS FOR AN ARBITRARY DISPERSION COEFFICIENT F. R. Gross (Goodyear Aerospace Corp., Akron, Ohio). [PRIBLIZHENNOE RESHENIE ZADACHI o DIFFUZNOM IN: AIAA UNMANNED SPACECRAFT MEETING, LOS ANGELES, OTRAZHENII I PROPUSKANLl SVETA ATMOSFERAMI PLANET CALU?. , MARCH 1-4, 1%5 (AIAA PUBLICATION CP-12). PRI PROIZVOL'NOI INDIKATRLSE RASSEIANILA]. [A6 5-1 9498 09- 311 E. G. lanovitskii. New York, American Institute of Aeronautics and Astronautics. IN: PHYSlCS OF THE MOON AND PLANETS [FIZIKA LUNY I 1%5, p. 76-87. 16 refs. PLANET]. Preliminary study directed toward selecting expandable drag Edited by I. K. Koval' . bodies capable of withstanding entry into the Venus atmosphere Kiev, Naukova Dumka, 1964, p. 92-110. 20 refs. In Russian. and remaining in static equilibrium at the higher altitudes to sup- Presentation of an approximate solution to the problem of port instruments for the exploration of Venus. The study is based diffuse reflection and transmission by a flat layer of a planetary on Kaplan's Venus atmosphere.which is discussed. The payloads atmosphere with true absorption. Approximate formulas are de- considered are limited30 those which can be ptinto a 1000-mi rived for the Ambartsumian functions with the simplest nonspher- circular orbit around Venus. The payload of a Saturn launch vehicle, ical dispersion coefficient. This curve can be used to calculate then, would be a Voyager-type probe with a detachable instrument the intensity of-diffuse-reflected and diffuse-transmitted radiation capsule. The capsule would enter and stay for an extended time by the layer, both with and without an isotropically reflecting sur- period in the Venus atmosphere and send scientific information back face adjoining to the layer. Sobolev's method is used to obtain ap- to the Voyager, which would then relay the information back to proximate formulas for the brightness coefficients of the diffuse- Earth. The entry into Venus atmosphere is considered. The reflected and diffuse-transmitted radiation with an arbitrary dis- necessary instrumentation would be supported by a Ballute-type persion coefficient. It is noted that the formulas presented may balloon capable of entry into, and of static equilibrium within, the be used for both the interpretation of observations planets and of Venus atmosphere. The Ballute design, construction, and for studying the diffusion of radiation in the Earth' a atmosphere operation are discussed. Scientific experiments possible mth the and in the sea. J. R. Voyager probe are noted. M.L.

A65-19314 ACCURACY REQUIRED FOR SPACE VEHICLE RECOVERY AM-19518 # TRAJECTORIES [PRECISIONS REQUISES POUR LES TRAJEC- THE AUTOMATED BIOLOGICAL LABORATORY - THE SCIENTIFIC TOIRES DE RETOUR D'ENGINS SPATIAUXL AND ENGINEERING OBJECTIVES. L Moulin (Centre de Formation en ACrodynamique Erp6rimentale. Temple W. NeumaM (Philco Corp., Aeronutronic Div., Newport Rhode -Saint -Genb se, Belgium). Beach, Calif. ). IN: INTERNATIONAL ASTRONAUTICAL CONGRESS. 13TH. IN: AIAA UNMANNED SPACECRAFT MEETING, LOS ANGELES, VARNA, BULCARIA, SEPTEMBER 1962. PROCEEDINGS. VOL- CALIF., MARCH 1-4, 1%5 (AIAA PUBLICATION CP-12). UME 2. [A65-19311 09-30] [A65 -19498 09- 311 Edited by Nicolas Boneff and Irwin Hersey. New York. American Institute of Aeronautics and Astronautics, Vienna, Springer-Verlag. 1964. p. 523-554. In French. 1965. p. 224-229. Analysis of recovery trajectories extending from a given Review of the present technological capability of the US space initial orbit to the top of the atmosphere. The propulsion is re- program of exploring the planets, particularly Mars, for extra- duced to an impulse; the trajectories considered lie in the plane of terrestrial life. Specifically, the Automated Biological Laboratory the initial orbit; a spherical nonrotating Earth is the only center (ABL). a planetary landing payload concept currently under study of attraction. Analytical expressions are derived for the velocity by the Aeronutronic Division, Philco Corp., under contract to the increment and its orientation at the departure from the initial orbit. Office of Bioscience Programs, NASA, is reviewed. The scientific first for the case of a circular orbit and then for the general case. objectives. techniques for the detection and classification of extra- Optimization of the fuel consumption is analyzed in two instances: terrestrial life, and the system problems are discussed. The most the search for an absolute minimum and rocket braking outside the difficult single problem in the design of the ABL is identified as atmosphere. Expressions are also given for the accuracy re- the selection of the most meaningful characteristics of life. The quirements on vehicle attitude, velocity increment, and determina- importance of the program from the plilosophical. scientific, and tion of the initial orbit. (Author) W. M R. engineering viewpoints is considered to be apparent. An integrated ABL is suggested as the optimum approach to such a search. It is concluded that no fundamental technological barrier appears to A-19485 # exist that would prevent the U.S. from accomplishing this mission STRUCTURE OF THE TERRESTRIAL HETEROSPHERE [LA in the early 1970's. M. L. STRUCTURE DE L'HETEROSPHERE TERRESTRE]. M. Nicolet (Centre National d@Etudes et de Recherche. Agronau- tiques, Brussels, Belxium). A65-19520 # (Astronautica Acta, vil. 10, no. 1. 1964. p. 24-34.) PLANETARY ATMOSPHERIC DETERMINATION UTILIZING A Institut Royal Mit;orologipue de Belgique. Contributions. no. 96, SEMIPASSIVE PROqE. 1964. p. 24-34. InFrench. Frank S. Holman and Haim Kennet (Boeing Co., Aero-Space Ev., Discussion of results of observations obtained from satellites Seattle, Wash.). and rockets, which leads to consideration of the problem of the lN: AIAA UNMANNED SPACECRAFT MEETING, LOS ANGELES, heterosphere under new aspects. The thermal balance must first CALIF., MARCH 1-4. 1965 (AIAA PUBLICATION CP-12). be obtained by introducing into the thermosphere the effect of [A6 5 -1 9498 09-31] variable uv solar heating in the course of an eleven-year cycle of New York, American Institute of Aeronautics and Astronautics, activity, and that of the cooling which is basically related to Con- 1%5, p. 236-245. 9 refs. ductive heat transfer. Thus, the photodissociation of molecular Presentation of an experiment to provide highly accurate oxygen constitutes the essential source of oxygen atoms. Further- knowledge on the densityhltitude and pressurelaltitude profiles more, gas diffusion in the gravity field keeps the molecular constitu of planetary apnospheres. notably those of Mars and Venus. The cuts above those normal limits which unite the dissociation balance. experiment is to consist of a small, lightweight spherical probe

39 A65- 19668

injected into the planetary atmosphere either from a flyby space- of the Earth. In particular, circulation of air masses in the craft prior to planetary encounter or from a planetary orbiter prior Martian atmosphere, water content in the inert air masses, and to orbit injection. Information on the probe's entry flight-path angle distribution of thermal flows are considered. J. R. and its velocity history before and after communications blackout is to be obtained through a two-way doppler measurement by the Deep Space Instrumentation Facility (DSIF), Aero-Space nv. , A65-19902 Boeing Co. To demonstrate the concept's validity, the application MARS - THE ORIGlN OF THE 3.58- AND 3.69-MICRON h4INIMA of such an experiment to determining the atmosphere of Mars is IN THE INFRARED SPECTRA. presented. The mission profile of the probe, as well as the current D. G. Rea, B. T. 0' Leary (California, University. Space Sciences and future capability of the DSIF to provide the required data, is Laboratory, Berkeley, Calif. ), and W. M. Sinton (Lowell Obser- discuasedfirst. The techniques for converting the doppler data vatory, Flagstaff, Ariz.). into knowledge of the Martian atmospheric density and pressure Science, vol. 147, Mar. 12, 1965, p. 1286-1288. 12 refs. profiles are then developed without a priori assumptions about the Contract No. NASr 220. atmosphere. It is shown that with Earth-based astronomical ob- Analysis of the 3- to 4-p spectra of Mars recorded in 1958 servations, augmented by theoretical climatology considerations, with the 200-in. Hale telescope, in order to determine if the mini- the analysis can be Simplified without loss of accuracy. Using ma at 3.58 and 3.69 p are due to terrestrial HDO molecules, rather simulated DSIF data furnished by the NASA Ames Research Center, than to substances on Mars as previously indicated. Solar spectra. both generalized and simplified analysis techniques are applied. together with water-vapor abundances derived from radiosonde The density profiles thus predicted are shown to be in remarkable flights, obtained during the observing period are studied. There agreement with those used by Ames in generating the simulated appears to be a correlation between the intensities of the 3.58- and data. A conceptual design suitable for incorporation into a modified 3.69-~features and the amount of terrestrial water vapor in the Mariner spacecraft is presented. (Author) M. L. optical path. Thus, the data considered are no evidence for the presence on Mars of substances absorbing at these wavelengths. P.K.

A65-19668 OPTICAL PROPERTIES OF THE MARTIAN ATMOSPHERE IN THE A65-20563 # ULTRAVIOLET. AN ANALYTIC SOLUTION FOR ENTRY INTO PLANETARY ATMO- V. I. Garazha and E. G. Ianovitskii (Khar'kovskaia Astronomi- SPHERES. cheskaia Observatoriia. Kharkov; Akademiia Nauk Ukrainskoi SSR, S. J. Citron and T. C. Meir (Purdue University, School of Aero- Glavnaia Antronomicheskaia Observatoriia. Kiev, Ukrainian SSR). nautical and Engineering Sciences, Lafayette, Ind. ). (Antronomicheskii Zhurnal. vol. 41, Sept. -0ct. 1964, p. 942-950.) AIAA Journal, vol. 3, Mar. 1965, p. 470-475. 15 refs. Soviet Astronomy, vol. 8, Mar. -Apr. 1965, p. 754-760. 21 refs. Derivation of approximate closed-form Solutions for inclination Translation. angle and density or altitude as a function of velocity, for a body -Proof that the optical thickness of the atmosphere of Mars in entermg a planetary atmosphere. The method of solution used the X = 360 mp region of the spectrum was appreciably greater than assumes that the atmospheric density may be expanded in a power unity during the great 1956 opposition. Suggestion is made that the series in terms of the logarithm of the velocity. Termination Of "UV layer" of the atmosphere of Mars consists of a gas-aerosol the series after the first three terms is shown to be equivalent to a mixture. The particle albedo of the mixture is 0.50 in the event of result obtained by Loh on the basis of observations that a certain single scattering. The indicatrix of light scattering for the spectrum combination of the entry variables may be considered constant. region and the mean aerosol particle radius are determined using The approximate solution obtained is compared with the exact the Rocard theory to interpret atmospheric indicatrices. The solution and with other approximate solutions obtained by Loh and concentration of aerosol particles in the UV layer is found to be Allen and Eggers, over wide regions of lift-to-drag ratio, entry very high. v. z. velocity, and entry-inclination angle. Good agreement is found over all regions except those corresponding to certain skipping- type trajectories. For this critical case. the nolution Of Loh is also A65-19676 t# inaccurate. It is stated that, in general, the solution obtained A MODEL OF VENUS WITH A "COLD" ABSORBING ATMO- yields the same accuracy as the second-order theory of Loh, SPHERE [oMODELI VENERY s W-~OLODNOI" POGLOSHCHA~U- although it is somewhat simpler to apply. (Author) M.M. SHCHEI ATMOSFEROI]. A. D. Kuz'min (Akademiia Nauk SSSR, Fieicheskii Institut, Moscow, USSR). A65-20633 7. 22 Radiofizika. vol. no. 6, 1964, p. 1021-1031. refs. In Russian. A RE-EVALUATION OF W. H. WRIGHT'S PLATES OF THE 1924 Study the possibility interpreting the observed spectrum of of AND 1926 OPWSITIONS OF MARS. of Venus radio emlesion in the centimeter and millimeter wavebands R. A. Wells (London, University. University College, Dept. of as absorption into the atmospheric aerosol the planet. of It is Physics, London, England). shown that the steep slope of the millimeter band of the spectrum Planetary and Space Science, vol. 13, Mar. 1965, p. 261-263. 12 can be explained by the absorption into a liquid aerosol with a tem- refs. perature of about 300°K and containing 0.2 to 0.3 gcm-2 of the Grant No. NsG 101-61. polar liquid with a relaxation time 3.5 x sec. It is shown of Re-examination of Wright's original plates of the 1924 and 1926 that the model of atmosphere yielding such a spectrum is absolute- oppositions Mars. from which he first deduced that Mars photo- ly nontransparent in the infrared and optical regions the spec- of of graphed on IR has a smaller diameter than when photographed on trum. Therefore a direct solar radiation cannot be the source of UV plates. The plates are analyzed by both a micrometer measur- surface heating of the planet. Surface heating by the inner heat of ing engine and a microphotometer. A wide difference found between the planet is considered. and the required heat flux is estimated. the measurements by the two methods is explained on the basis that The possibility is indicated of explaining the observed decrease in the microphotometer picked up faint extensions of the atmosphere the brightness temperature of Venus in the decimeter waveband that the eye could not distinguish. The diameter the Martian as absorption into the relatively cold Venus ionosphere. of J.R. surface is deduced to be 6682 km. Problems in the photographic determination of planetary diameters are discussed, including those arising from the optical system and tracking and from the A65-198s # photographic plates. P. K. SOME PROPERTIES OF THE ATMOSPHERE OF MARS [NE= OSOBINE MARSOVE ATMOSFERE]. Dragoslav Ekainger. Vasiona, vol. 12. no. 1. 1964. p. 4-6. In Croatian. A65-21854 Brief discussion of some of the basic properties of the atmo- COMPARISONS OF LABORATORY AND PLANETARY SPECTRA. sphere of the planet Mars which distinguish it from the atmosphere II -THE SPECTRUM OF JUPITER FROM 9700TO 11200 1.

40 A=-22205

Tobiaa Owen (Illinois Inatitute of Tecblogy, Research Institute. arises from the increase of temperature with atmospheric depth. htrosciences Center, Chicago, Ill. ; Arizona. Univeraity. Lanar In Model B. both the (T -+) relation arid the dependence of emissivity and Planetary Laboratorv. Tucson. Ariz. \. ~ ~~- on the angle of emergence contribute to the limb-darkening. Each htrophysical JO-I. vi~la, Feb. 15, i965. p. 444-456. 33 refs. model can be made to agree with observation. with an appropriate Contract No. NRO 46-791 specification of atmospheric and cloud parameters. With the Comparison of absorption spectra of several gaaes with the spec angular resolution available from the vicinity of the Earth. a trum of Jupiter in the region 9700-WOO 1. All nanaolar absorptions discrimination among these models is difficult to achieve. But a occurring in this region of the phet' a apectrum are identified LS Venus fly-by or orbiter performing only somewhat better than due to NH3 or CHe Upper limit. are set on the abundances of HCN Mariner II can potentially determine uniquely the cause of the liinb- and CzHz, and previous limits on CH3D. CH "2, md the DIH r8t.b darkening and provide significant new information on the structure are rwaed. The 3 bnd of CH4 rt ll057 fin the spectrum of and composition of the atmosphere and clouds of Venus. Jupiter ia analysed kioretidy and empirically to derive Inpup (Author) A. B. K. atmoapheric temperature of 200 f 25°K. This result appear1 consistent with a model of the Jovian cloud deck which require. the presence of considerable vertical atructure. (Author) D.H. AM-22120 # BIOLOGICAL PRECURSOR MISSIONS TO MARS.

Temple W. Neumann (Philco Corp., kronutronic Div. ~ Newport A6S-2l8SS Beach, Calif.). DECAMETER-WAVELENGTH OBSERVATIONS OF JUPITER - THE APPARITIONS OF 1961 AND 1962. MUG. Smith, G.R. Lebo, N.F. Six, Jr., T.D. Carr (Florida. University, Dept. of Physics aud Astronomy, Gainesville, Fh. ), Heins Bollhagen. Jorge May. and Jorge Levy (Chile, Univeraity. MaiG Radioastronomical Observatory. Mai& Chile). Brief review of studies ofmanned miasiolu to Mars performed Astrophysical Journal, voL 14, Feb. 15, 1%5. p. 457-477. 26 refs. to date by NASA, and demonstration, by several examplea. of the Army-Navy-NSF-aupported research. dependence of such missiona on our knowledge of the phyaical Final reduction of extenaive observationa of Jupiter conducted environment of Mars. A knowledge of the biological parameter. on during 1961 and 1962 in the radio-frequency range 5 to 31 Yc. Both Mars is ahown to be of equal or greater importance. The evidence probability-of-emisaion and intenaity atudies have been made of the for life on Mars is reviewed. Effect. which such life can ham on the factors of crew contamination during surface operations. air several decametric "SOUZC~S. $9 it appurs that a change in the apparent rate of rotation of the source. occurred in 1%0. Both the lock, and decontamination operations, material degradation, ad overall Jovian activity .nd the apprent width. ofthe sources have spacecraft and Earth back-contamination by returned crew members, increased aa the aolar cycle declined, although the groaa source ge- equipment, and samples. are specifically reviewed. Poasible ometry remains much the aame aa in previoua year.. Televiaion advantages of indigenous life forms in support of future manned techniques have bem uaed in a search for optical activity correlated operations on Mars are also pointed out. The importance of early with the Jovian outbursts. Venus and Mars have ahoan no detectable biological precursor missions to obtain the required data is apparent 3ecametric activity, while Saturn remains. ad before, a dubious from these possible interactiolu. Esaential differences are shown source. (Author) D. H. to exist, however, between procedure. used for apace phyaica 5- perimentation and those required to obtain meaningful biological data. It is demonstrated that these differences Lad to the concepts being employed in an automated biological laboratory (ABL) currently A6522097 # under atudy. (Author) M. M. A QUANTITATIVE MEASUREMENT OF WATER-VAPOR IN THE ATMOSPHERE OF VENUS. ~65.11135 Mark Bottema. William Plummer, and John Strong (JobHopb PLANETARY ENVIRONMENTS. University. Baltimore, Md. 1. LUNAR AND John Eggleatm. Dallas E. Evans, and John W. Harris lSymposium sur les Observations Astronomiques Faites Bord de M. (NASA, Manned Spacecraft Center. Houston. Tex.). Vehiculee Spatiaux. 23rd, Likge, Belgium, hug. 17-20, lq64.1 IN: TOWARDS DEEPER SPACE PENETRATION; PROCEEDINGS Annales d'llstrophysique, vol. 28. Jan. -Feb. 1965, p. 225-228. OF AAS SYMWIU'M AS PART OF 13lST MEETING Contract No. 191628)-202. AN HELD OF AF THE AMERICAN ASSOUATION FOR THE ADVANCEMENT OF Description of the method of observing Venus water-vapor SCIENCE. MONTREAL, CANADA. DECEMBER 29, 1964 (AS absorption in the 1.13-# band. Certain aspects of the data- Science and Technology Series. Volume 2). [ASS-ZUU 12-30] recording system. the data reduction, and the interpretation of the Edited by E. R. Van Driest. results are discussed in the light of present knowledge of the atmo- North Hollywood. Western Periodicals Co.. 1964, p- 7-53. 35 refa. nohrre of Venw. A. B. K. -r---- ~- . Description of the lunar and planetary "natural" avironmsnta currently used by the Manned Spacecraff Center of NASA for manned A6522098 #: missim planning and design. A natural envircmment is defined an SPACECRAFT OBSERVATION OF VENUS INFRA-RED LIMB- that eDvironm'&tMis thakght to exist without the induced effects DARKENING. -raft and sensors. Although there are mauy theoriea Carl Sagan (Harvard University; Smithsonian Institution, Smithsonian and interpretations of the data, with consequent uncertainties. oply Astrophysical Observatory. Cambridge, Mass.) and James B. a few of these affect spacecraft and mission deaign. The lunar Pollack (Harvard University, Harvard College Observatory. natural environment is covered in terms of (1) the lunar respmse Cambridge, Mass.). throughout the electromagnetic spectrum, (2) the topography and engineering properties, (3) the atmosphere. and (4) the external radiation and meteoroid environment. The planetary envircmment 1~ .- ~~ ?s d'Astrophysique. vol. 28. Jan. -Feb. is covered by firsistatingtlxrphuetsinto eaMge.r&&rPbcpn- Ision, p. 233. sidering primarily those which are of interest to manned misnona. Comparison of the limb-darkening laws predicted for several Of these. Mars appears to be moat interesting. and primary attan- models of the atmosphere and clouds of Venus with limb-darkening ti- is paid to the natural environment of this planet. observatione in the 8- to 13-c( interval made from the ground and (Author) F.R.L from Mariner II. Model A attributes the limb-darkening to pure molecular absorption by the atmosphere above the Cytherean cloud A65-22105 layer; Model B attributes it to multiple scattering by cloud particles 11-CY OBSERVATIONS OF THE TEMPERATURE OF MERCURY. of arbitrary albedo and altitude distribution. In each model, the K. I. Kellermann (Coommonaealth Scientific and Induatrial Research temperature regime is considered to be specified alternatively by Orgmiutioo, Radiophyaics laboratory. Sydney. Australia). convective and radiative equilibrium. In Model A, limb-darkening E.-1. 205. Mar. 13, 1%5, p. 1091. 1092. 6 refa.

41 A65-22598

Determination of the temperature distribution at the surface has been described in detail in a number of other papers. The of Mercury, based on measurements of the mean disk temperature electron-density curves, however, show a singularity for rx 0, over a wide range of plase angles as the planet moves in its orbit and, since stellar atmospheres also have a maximum of electron around the Sun. Observations were made on ten separate days density coinciding with the center of symmetry, this kind of radio during May and June 1964 at a wavelength of 11 cm for planetocentric propagation is treated predominantly. Attention is also paid to the phase angles I3 from 29O to 149O (eis the angle between the Sun separation of rather irregular ionized layers or clouds in order to and the Earth as seen from Mercury). The observations were made obtain a precise ray path. (Author) D. H. by scanning back and forth in declination over a range of about 45 min of arc approximately centered on the declination of Mercury. It is found that the nurface temperature doen not exhibit the strong dependence on phase angle that it wan expected to. In particular, A~S-WIB~ the observationn at large phase angles. where only 10 to 15% of the SURVIVAL AND GROWTH OF TERRESTRIAL MICROORGANISMS visible disk wan illuminated by the Sun. indicate a temperature of IN AMMONIA-RICH ATMOSPHERES. about 250°K on the dark hemisphere. This, taken with other con- S. M. Siege1 and C. Giumarro (Union Carbide Corp., Research sideration.. seems to indicate that atmospheric convection plays Inatitute, Tarrytown, N. Y. ). an important role in determining the temperature dintribution on ea.vol. 4. Apr. 1%5, p. 37-40. 9 refn. the surface Mercury. P. K. of Contract No. NASw-767. Demonstration that varioun bacteria and ascomycetes have ~65-2259a#: grown on specimens of Euphorbia xylophylloides and other xero- SOLAR-WIND MEASUREMENTS NEAR VENUS. phytes after two months in atmonpheres containing NHJ with CH4, Marcia Neugebauer and Conway W. Snyder (California Institute of Hz. or air. NH3 leveln of at least 50,000 ppm far exceeded con- Extreme per- Technology, Jet Propulsion Laboratory, Pasadena. Calif. ). ventional upper safe limits for hu.man toxicity. Journal of Geophysical Research. vol. 70, Apr. 1, 1965, p. 1587- formance was nhown by a stress-adapted Penicillium brevi-com- It considered 1591. 18 refn. pactum which grew slowly in 95% NH3/5% CH4. is Determination of the velocity, temperature, and density of the that these obserntions are significant with reference to the origin protons in the solar wind for the period when Mariner 2 wan near and current existence of microbial life on Jupiter. (Author) F. R. L. Venun. From these data, it is concluded that: (1) Mariner 2 never penetrated any magnetosphere associated with Venus. (2) Mariner 2 was probably also outside any shock front associated with the muper- ~65-2~~ sonic motion of the nolar wind paat Venus, (3) the solar-wind INFRARED REFLECTIVITY OF Fe203'nHZO- INFLUENCE ON intensity was not especially great during the time of Venus en- MARTIAN REFLECTION SPECTRA. counter, and (4) any shock wave surrounding Venus was probably W. A. Hovis, Jr. (NASA, Goddard Space Flight Center, Greenbelt, closer than about 25,000 to the center the planet at the sub- km of Md. ). solar point. (Author) D. H. Icarus, vol. 4, Apr. 1965, p. 41, 42. Measurement of the IR reflectivity of limonite and Fe203.nH20 ~65-2309a from 1 to 5 M. A strong reflection minimum due to water of hydra- A DETECTOR FOR THE ARGON ABUNDANCE IN THE MARTIAN tion in shorn. The influence of the measured reflectivities on It is considered possible that, by ATMOSPHERE. Martian spectra is discussed. F. B. Harrimon, W. Bernatein, and J. L. Vogl (Space Technology combining measurements of water vapor in the atmosphere made in Laboratories, Inc., Redondo Beach, Calif. ). other spectral regions with measurements in the 2 to 4 u region an JNuclear Science Sympomium, llth, Inmtrumentation in Space and estimate of the degree of hydration of the Martian surface may be made. F. R. L. Laboratory, Philadelphia, Pa., Oct. 28-30, 1%4. IEEE Tranmactionm on Nuclear Science, vol. NS-12. Feb. 1965, ..- p. 103. A65-23491 Demcription of an inmtrument conlilting of a cylindrical ioniza- AN EXPLANATION OF KOZYREV'S HYDROGEN EMISSION LINES tion chamber containing an Fe 55 X-ray mource, to be used aboard IN THE SPECTRUM OF MERCURY. a capsule descending through the Martian atmosphere to detect the .~ Hyron Spinrad and Paul Hodge (California. University, Berkeley atmompheric argon content: The atmomphere of Mars is aisumed to W. Astronomical Dept., Berkeley, Calif. ). consist of a mixture of argon. nitrogen, and carbon dioxide with vol. 4, Apr. 1965, p. 105-108. other gaaen appearing only in trace amounts. A capsule descending w, Examination data obtained from several high-resolution near- through the Martian atmoaphere, containing instruments to measure of spectrograms Mercury taken through the 120-in. coudd the the presmure, density, and temperature, would make pommible the IR of of Lick observatory. It was found possible to place quantitative upper determination of the total pressure and mean molecular weight. One more measurement would then be necemmary to determine the limits on possible gaseous constituents of the Mercurian atmosphere. A microphotometer tracing is presented which was made of the partial preamurei Of the three gaaem. Thim meanurement could be made with an ionization chamber containing an Fe 55 X-ray source. spectrum. A strong IR Ca II line 18542 is shown, and double ab- In much a chamber the current would be linearly related to the sorption peaks are clear. If the significance of a sky component to the Mercury spectrum were not realized, the hump between the argon content of the atmosphere. (Author) D.P.F. two absorption lines might well suggest an emission core feature, and therefore this splrious core "emission" between the two absorp- A6S-23429 ## tion components of all strong Fraunhofer lines may be the source RADIO PATH FORMULAE FOR RADIOASTRONOMY AND ASTRO. of Kozyrev's claim of an accreted atomic hydrogen atmosphere. NAUTICS. F. R. L. E. Chvojkovi (Csechoslovak Academy of Sciences, Astronomical Inntitute, Prague, Caechoslovakia). Amtronomical Inmtitutes of Czechoslovakia, Bulletin, vol. 16, A65-23521 # no. 1, 1965, p. 5-10. 9 refm. OZONE AND CARBON DIOXIDE HEATING IN THE MARTIAN AT- Summary of the previously derived radio-path formulas for MOSPHERE. amtronomical and astronautical purposem. The formulas are first C. Prabhakara (NASA, Goddard Space Flight Center, Goddard applied to planetary ionompherem and mtellar atmompheren. As Institute for Space Studies, New York, N. Y. ) and Joseph S. Hogan, long am the ionized regions poemearn a spherical symmetry. the ray Jr. (New York University, New York, N. Y. ). path is eamily determined by a quami-conic equation since the whole Journal of the Atmospheric Sciences, vol. 22, Mar. 1965, p. 97-109. region can be divlded into thinner spherical layera in which the 40 refa. electron-density variation is defined in terms of the radiua of mrn- Examination of the radiative equilibrium temperature structure ture. The applicability of the electron-density equation and the of the atmosphere of the planet Mars. The absorption of nolar ener- quasi-conic equation to planetary ionospheren - in mpite of their gy in the UV and visible by Oz and O3 and in the near IR by C02 in importance in astronautics - is mentioned only in brief becaume it included in the calculation of atmospheric heating. The transmission

42 A65-2 5226

functions of CO2 are theoretically calculated making use of a "sta- A6S-24803 * tistical" model for band absorption. These transmission functions THE THEORY OF RADIO EMISSION OF VENUS [K TEORII are then used to evaluate the absorption of solar energy in the near RADIO12 LU CHENIIA VENERY]. IR and to iwestigate the radiative transfer in the far IR. The theo- A. D. Kuz'min (Akademiia Nauk SSSR, Fizicheskii Institut, retical hand parameters involving the line intensity and the mean Moscow. USSR). ratio of line half-width to line spacing are derived using the trans- Radiofizika, vol. 8, no. 1, 1965. p. 7-18. 13 refs. In Russian. mittance tables of C02 presented by Stull, Wyatt and Plass. The Derivation of analytical expressions relating the brightness basic photochemical theory of 03 production is used to determine temperature of the radio emission of the planet surrounded by an a vertical O3 distribution consistent with the radiative equilibrium absorbing atmosphere to the physical parameters of its surface temperature structure. The equation of radiative transfer is and atmosphere. Numerical solutions are obtained for the special numerically integrated, avoiding the empirical relationships com- cases of absorption by the entire thickness of the atmosphere and monly involved in the pressure dependence of C02 absorption. The absorption in homogeneous and parabolic layers. These solutions IR flux transmittance is also calculated without any simplifying as- are used in interpret- the results of radio-astronomical measure- aumptions.'8adiative equilibrium temperatures are calculated from menta of Venus. (Author) A. B. K. the surface of the planet to the 100-km level. For surface temperatures ranging from 230° to 270°K, surface pressures from 10 to 50 mb. and C02 amounts from 40 to 70 m atm. the "tropopause" is found at levels below 10 km. Within these limits of sur- A65-25020 # face temperature and pressure and C02 amounts, the temperature OZONE DISTRIBUTION IN THE ATMOSPHERE OF MARS. above the tropopause steadily decreases toward a value of - 155% F. F. Marmo. Shardanand. and Peter Warneck (GCA Corp., &the upper layers. The results indicate that no temperature Bedford, Mass. ). maximum is produced by the absorption of solar energy in the UV Journal of Geophysical Research, vol. 70. May 1, 1965, by 03 or in the near IR by C02 in the Martian atmosphere. The p. 2270-2272. 12 refs. maximum 03 number density is found at the surface of Mars with Analytical attempt to reconcile the conflict between the results a gradual decrease upward. The total amount of 03 present is of Marmo and Warneck (1961). who found a monotonic increase in about one-tenth of the amount found in the Earth's atmosphere ozone concentration with decreasing altitude and those of Paetzold (- 0.3 cm atm). The total UV energy absorbed in the Martian atmo- (1963), who suggested the existence of an ozone concentration peak sphere by O2 and 03 is comparable to the near IR energy absorbed at an altitude of about 40 lan. There is agreement that the basic by C02. However, the vertical distribution of absorbed energy photochemical reactions involved in the atmosphere of Mars are: shows that, below - 30 km. O2 and O3 absorption is comparable to (1) 0 t hu - 0 t 0, A I2400 1; (2) 0 t 02 t M - O3 t M; (3) 1 CO2 absorption. while above this level C02 absorption becomes 0 t 63 - O2 t 02; (4) 03 t hu 7 02 t 0. A 5 3000 1; (5) considerably larger. (Author) A. B. K. OtOtM-O2tM;(6)COzthv-COtO. AS175OH;and (7) CO t 0 - CO2. The overriding discrepancy factor is seen to be that Marmo and Warneck included Eq. (5) which Paetzold ignored. It is concluded that the existence of an ozone layer in the atmosphere of Mars can be denied. W.M. R. A65-2391 8 THE AERODYNAMIC PROBLEMS OF THE HYPERSONIC FLIGHT OF SPACE PROBES THROUGH PLANETARY ATMOSPHERES [DIE A65-25099 # AERODYNAMISCHEN PROBLEME DES HYPERSONISCHEN FLUGES CHAMBER SIMULATING MARTIAN CONDITIONS FOR WCRO- VON RAUMSONDEN DURCH PLANETARISCHE ATMOSPmEN]. BIOLOGICAL INVESTIGATIONS [KAMERA, IMITIRUIUSHCHAIA Ernst Adams (Deutsche Versuchsanstalt Mr Mt- und Raumfahrt, USLOVM MARSA, DLLA MIKROBIOLOGICHESKIKH ISSLEDOVA- hstitut fur angewandte Mathematik und Mechanik, Freiburg im =I. Breisgau, West Germany). A. I. Zhukova and I. I. Kondrat'ev. (Deutsche Gesellschaft fur Raketentechnik und Raumfahrtforschung. Kosmicheskie Issledovaniia, vol. 3, Mar. -Apr. 1965. p. 330-333. and Wissenschaftliche Gesellschaft fur Ut- und Raumfahrt. Annual 6 refs. In Russian. Meeting. Berlin, West Germany, Sept. 1964.) Description of a chamber (lo0 x 150 x 180 un) and the electrical 36 refs. Raumfahrtforschung, vo1. 9, Apr. -June 1965. p. 66-75. circuit used to simulate the environment on Mars (temperature drop In German. from :+Q to -6OOC; composition of the atmosphere 95.5% N, 0.25% A discussion of the flight corridor through an atmosphere, which Cq. 0.25% Ar) with the exception of the gravitatiod, magnetic- is bounded on the one hand by the deceleration factor in the range field, and charged-particle-radiation effects. Preliminary observa- of flight due to the effect of lift and on the other by small aerodynamic tions of the growth of various cultures of fungi and bacteria(Asprgil- drag, based the two-body problem in celestial mechanics. Thermo- on lus niger, Mucor plumbeus. Strain 1339. Micrococcus aurantircua, chemical effects and the effects of more rarefied atmospheres in the Bacillus subtilis. etc.) in the chamber are reported. W.M.R. flow'field around the vehicle are discussed, and the methods for calculating pressure distribution are given. After a brief qualitative review of the causes of aerodynamic heating, quantitative estimates A65-25226 of ita order of magnitude are presented. The conduction of heat by SPECTROSCOPIC OBSERVATIONS OF MERCURY. convection and by radiation is considered, and numerical data on heat Hyron Spinrad. George B. Field, and Paul W. Hodge (California. flow are included. Finally,evaporation cooling and thertnal protec- University, Berkeley Astronomical Dept. , Berkeley, Calif. ). tion are discussed. D. P. F. Astrophysical Jqurnal, vol. 141, Apr. 1, 1965, p. ll55-ll60. 27 refs. Review of evidence for a Mercurian atmosphere. New high- 1\65-2441 5 dispersion spectra of the planet Mercury in the near-infrared EXPLOSIONS IN RAREFIED ATMOSPHERES. make it possible to place upper limits on the abundance8 of COz (< 57 meter'-atmospheres), 1 meter-atmosphere). and G. W. Stuart (General Dynamics Corp., General Atomic Div., O2(e John Jay Hopkins Laboratory for Pure and Applied Science, San HzO (< 30 u precipitable). The strength of the 1.6-p absorption Diego. Calif.). bana of COz found by Moroz can bee%p=ned only if M-ercury Physics of Fluids. vol. 8, Apr. 1%5, p. 603-606. 5 refs. possesses a considerable atmosphere (Ps > 3. 3 mb) which can An investigation of explosions in cold, homogeneous atmospheres. pressure-broaden that band. While this lower limit and the ob- in which, initially, th.e mean free path of an explosive product atom tained upper limit are marginally compatible with a pure COz at- through the atmosphere is much longer than the dimension of the mosphere of about 4-mb surface pressure, such an atmosphere expanding material. On the basis that a uniform expansion persists would he accompanied by a Rayleigh scattering which would lead for all time, a snowplow model is derived from the virial theorem to a polarization six times larger than the amount detected by and is used to describe the expansion. To illustrate the method, a Dollfus. Admixture of other constituents would be consistent with chemical explosion in the Earth's atmosphere at 150 km is analyzed. both spectroscopic observations. and argon in particular would give (Author) D. P. F. the smallest discrepancy with Dollfus' polarization observations.

43 A65-25228

The relationship of the pressure estimates obtained to the require- meteor shower activity. This result. combined with the optical prop- ments of the theory which attributes surface features to meteoritic erties of the Martian atmosphere and the close resemblance be- erosion are discussed; it is considered possible that the tenuous tween the characteristics of the blue haze and those of the terrestrial atmosphere of Mercury may be time-variable. (Author) W. M.R. noctilucent clouds. suggests that variable amounts of interplanetary dust are suspended in the Martian atmosphere and that the occasion- al clearings of thd blue haze are caused by a diminishing influx of these dust particles. (Author) D.P.F. A65-25228 THE ATMOSPHERE OF VENUS NEAR HER CLOUD TOPS. Joseph W. Chamberlain (Kitt Peak National Observatory. Tucson, A65-26042 Ariz. ). OBSERVATIONS OF JUPITER'S RADIO SPECTRUM AND POLARI- Astrophysical Journal, vol. 141, Apr. 1, 1965, p. 1184-1205. ZATION IN THE RANGE FROM 6 CM TO 100 CM. '67 refs. J. A. Roberts and M. M. Komesaroff (Commonwealth Scientific Theory of line formation and some conclusions concerning and Industrial Research Organization, Radiophysics Laboratory. Venus' atmospheric structure and composition near the top of the Sydney, Australia). cloud cover. It is argued that the absorption bands of GO2 are Icarus. vol. 4, May 1965, p. 127-156. 36 refs. produced through multiple scatterings in an optically thick at- Data relative to an extensive series of complete determination. mosphere and that, consequently, current knowledge of thc Cytherean of the linear polarization of Jupiter' m radio emission at wavelength. atmosphere is much less precise than is commonly believed. The of 6, 10, 11, 21, 74, and 100 cm. A search for circular polarization visual data are reviewed to obtain an estimate of the properties of at a wavelength of 31 cm is reported. Recording0 of a lunar Occulta- the cloud particles. Then, thermal-infrared observations are used tion of the source are also given. The rocking of the plane of polari- to derive some idea of the temperature T and its variation with op- zation with rotation of the planet is shown to be asymmetric in form. tical depth 7 in the cloud; the degree of uncertainty in these pa- probably reflecting some asymmetry in the radiation belt. The beam- rameters is considerable, but it is concluded that the cloud tops ing of the radiation is used to infer the pitch angle distribution of the are almost certainly cooler than the region where CO2 absorption electrons in the belt. The distribution appears to change with ener- occurs. From the T(? ) dependence combined with the rotational gy, relatively more of the higher-energy electrons being in very flat temperature of carbon dioxide, the mean depth <+ > of band for- helices. The flux density of both the polarized and unpolarized non- mation is deduced. The radiative-transfer theory of line formation thermal radiation is shown to be essentially independent(Author) of wavelength D. P. F. is used to relate to the albedo w" for single scattering. The vver the range from 6 to 74 cm. C02 equivalent widths and the line profiles are discussed as a means of deriving the amount of collisional broadening and thence the C02/total-gas ratio. Spinrad' s important conclusion that car- A65-26212 # bon dioxide is a minor constituent of the Venusian atmosphere is PRESSURE AND GO2 CONTENT OF .THE MARTIAN ATMOSPHERE- confirmed. For the phase variation of band strength. an error in A CRITICAL DISCUSSION. an earlier paper is corrected, and it is shown that for weak bands Joseph W. Chamberlain and Donald M. Hunten (Kitt Peak National the temperature should change very little with phase. Taking Observatory, Tucson, Ariz. ). Spinrad' s data literally, it is concluded that the near-infrared GO2 Reviews of Geophysics, vol. 3, May 1965. p. 299-317. 25 refs. bands are formed mostly within the first scale height (about 8 h) NASA-supported research. below the cloud tops. Kuiper's conclusion thatthe carbon and oxygen Review of the principal techniques that have been used to es- isotopes are in about the same ratios as on Earth is reaffirmed. timate the surface pressure on Mars. The basic physics behind each W. M. R. technique is outlined and illustrated with simplified examples. An attempt is made to evaluate the reliability of each technique and its A65-25632 ?Y use to date. The problem is outlined, the older techniques RADIO EMISSIONS FROM THE PLANET JUPITER. (polarimetry and photometry) are examined, and the spectroscopic D. McNally (London. University, Observatory, Mill Hill, Middx., method, in which at least two GO2 absorption bands are used to England). derive both the CO abundance and the surface pressure, is re- Science Progress, vol. 53, Apr. 1965, p. 257-262. viewed. The concfusions are princlpally: (1) that the polarimetric and photometric techniques are not nearly reliable as has been Results Of the detection of radio emission from Jupiter. ~t is so considered that the radiation is nonthermal incharacter. It has been generally supposed; and (2) that, although the spectroscopic method suggested that Jupiter has a magnetosphere similar to that possessed should ultimately settle the problem, the data thus far available do by the Earth, with belts of trapped charged particles similar to the not yield good accuracy in either the GO2 content or the total pres- (Author) W. R. van Allen belte; with this assumption, it is possible to explain why sure. M. the decametric radiation is confined to narrow beams. F.R. L. A65-26272 LUNAR AND PLANETARY SURFACE CONDITIONS (Supplement 2 AM-25694 * Edited PHOTOGRAPHIC POLARIMETRY OF VENUS [FOTOCRAFICHE- to ADVANCES IN SPACE SCIENCE AND TECHNOLOGY). SKALA POLIAElIMETRIIA VENERY]. by F. 1. Ordway, 111 (NASA, Marshall Space Flight Center, V. A. Gagen-Torn. Huntsville, Ala. ). bningradskii Gosudarstvennyi Universitet, Aatronomicheskaia N. A. Weil (Cummins Engine Co., Inc., Research Div., Columbus, Ind. ). Observatoriia, Trudy, vol. 21. 1964, p. 95-98. In Russian. Investigation of the distribution of polarization over the Cvtherean New York, Academic Press, Inc., 1965. 222 p. disk for phase angles 52.5 and 53O. 5. The degree of polarization is $10.00. This book is a collection of available theoretical knowledge and found to increase with distance from the center of the planet. The plane of vibration is seen to coincide with the intensity equator. experimental evidence on the surface conditions obtaining on the Moon and on the terrestrial and outer planets. Exinting knowledge (Author) W. M.R. of these conditions is critically reviewed, the moat probable alter- A65-26040 natives are identified, and new hypotheses are advanced where they THE BLUE HAZE OF MARS. are considefed warranted. Because there exists a close associa- A. Palm and B. Bamu (California, University. Space Sciences Labo- tion between the space scientist and the technical specialist who ratory. Berkeley. Calif. 1. must place a functioning data-collection system on these planetary Icaru., vol. 4, May 1965, p. 111-118. 24 refs. surfaces, the author has attempted to compose the text so that it Grant No. NsG 243-62. can be used with equal facility by scientific or professional per- Investigation of the extent of blue clearings as a function of the sonnel engaged in space research, by educators, or by graduate number of the meteor showers Intersecting the orbit of Mars at 100 students in aerospace dilciplines. In an introduction, the prevalent intervals of heliocentric longitude. A rank correlation method has hypotheses on the origin and age of the solar syntem are presented; been employed. The analysis indicates a small but statintically sig- these are followed by a brief description of the methods of acquiring nificant negative correlation between the extent of blue clearing and lunar and planetary data, either frorh fixed terremtrial observatories

44 A65-26945 or from instrumented or manned space probes. In the chapter de- Symposium sponsored by the International Astronautical Federa- voted to the Moon. sections deal sequentially with the atmosphere, tion. International Academy of Astronautics, UNESCO. Interna- temperature conditions. subsurface stratification. field intensities tional Atomic Energy Agency. International Telecommunication (gravitational. electric, and magnetic), and with the biological con- Union, World Health Organization, and World Meteorological ditions existing on the lunar surface. New information is prenented Organization; Grant No. NsG 101-61; Contract No. NASr-220. on the density of the lunar atmosphere under quiesc.ent or high-flux Discussion of the theory underlying infrared spectroscopy transient conditions. on the topography of the lunar surface. and on md summary of the remote infrared observations made of Mars. the probable proportion of crater-covered areas in the highlands The emission and absorption characteristics of liquids, solids, and on the maria. A critical examination is mlde of the surface- and gases renulting from the electromagnetic dipole, rotational. forming mechanisms on the Moon, with prediction. for the stratifica- and vibrational properties of their molecules are outlined. Infra- tion. temperature profile, and composition (both chemical and red Spectroscopy has provided infomation on the atmospheric meteoritic) of subsurface layers. The question of indigenous lunar composition. presnure.and other parameters which are vital in life is reviewed and discarded. Equally detailed treatments ue the designing of a lander to explore the surface of Mars for evi- given of the surface conditions of the terrestrial planets, the Jovian dence of life. Infrared radiometry has been used to measure the planets. and Pluto. When these planets are situated at vast dis- surface temperatures for the entire disk during the various sea- tances. are not easily observable, or possess cloud-mantled at- sons. The possibilities afforded by a spacecraft orbiting Mars mospheres, information about their nurfaces is less complete than and by a landed vehicle in the search for life on that planet are information about the surfaces of the Earth's nearer planetary detailed. S.H.B. neighbors. D. H.

Am-263 A65-26719 INFRARED SPECTRUM OF MERCURY (A 1.0-3.9 bd. THE MARINER 4 OCCULTATION EXPERIMENT. V. I. Moroz. (Moshvskii Gosudarstvebnyi Univsrsitet. Astrono- Arvydas J. Kliore, Dan L. Cain, Gerald S. Levy (California micheskii Institut , Moacow, USSR). Institute of Technology, Jet Propulsion Laboratory, Pasadena, (Astronomicheskii Zhurnal, vol. U, Nov. -Dee. 1964, Calif. ), Von R. Eshleman, Gunnar Fjeldbo (Stanford University. p. iiOE-ni7. i Stanford Center for Radar Astronomy, Stanford, Callf. 1, and Soviet Astronomy, vvl. 8, May-June 1965, p. 882-889. 15 refs. Frank D. Drake (Cornel1 University, Center for Radiophysics and Translation. Space Research. Ithaca, N.Y.). [For abstract see Accession no. A65-15676 06-30] Astronautics and Aeronautics, vol. 3, July 1965, p. 72-80. 13 refs. Discussion of the Mariner IV occultation experiment, intended to improve knowledge of the atmosphere and ionosphere of Mars. A65-26914 Approximately one hour after its closest approach to Mars. the PLANETARY ATMOSPHERES. spacecraft will be occulted by the limb of the planet and will R. Jastrow (NASA. Goddard Space Flight Center, Goddard Inntitute for Swce Studies, New York. N. remain in occultation for approximately 50 min. Immediately Y. 1. before and immediately following occultation. the 2300-Mc tracking Societh Italiana di Fisica, Scuola Internazionale di Fisica Enrico and telemetry signal of the spacecraft will traverse the atmosphere kermi, Corso 24, Varenna. Italy, June 4-16, 1962. and ionosphere of Mars, The changes caused in the frequency, phase, and amplitude of the spacecraft signal by passage through RICERCHE SPAZIAI-I E IL SISTEMA S0~1. Edited by B. Rossi. these media will constitute the raw data of the experiment. The New York. Academic Press. Inc., 1964, p. 236-297. geometry of occultation is described, and the instrumentation and Discussion of the currently accepted picture of the origin and accuracy of the experiment are discussed. Problems of data analysiti and interpretation of results are examined. F. R.L. development of planetary atmospheres, beginning with the theory Of stellar evolution. An approximate table is constructed of the atmospheric lifetimes (times in which a fraction 1 - e-1 of the original content of the atmosphere is lost by gravitational escape) of con- A65-26720 # stituents of interest on the Moon. Mars, Earth, Venus, and Jupiter. A SUBSURFACE MARINE BIOSPHERE ON MARS? These include the lightest gases, hydrogen and helium; atomic Hubertus Strughold (USAF, Systems Command, Aerospace oxygen, representing the C, N. 0 group; and finally argon, as a Medical Div. , Brooks AFB, Tex. ). representative of the heavier gases. but occurring in special Astronautics and Aeronautics. vol. 3, July 1965, p. 82-86. abundance by virtue of the steady source provided throughout the 18 refs. life of the planet by the decay of radioactive potassium in the crust. Examination of the theory that the water of Mars may be A great deal of attention is given to problem in the identification of locked beneath layers of dust and ice, supporting there a variety the major nources of energy for the Earth's upper atmosphere. By of chemosynthetic organisms. The theory first advanced by numerical integration of the heat conduction and hydroatatic blrnce Baumann and developed by Davydov assumes that planetary mate- equationa, tables are conetructed of the temperature, density, rials from which Mars evolved include water in approximately the pressure. scale height, mean molecular weight, and the concen- same proportion to the total mass as did those from which the trations of Nz, 02, C, He, and H for altitudes from 120 to 2050 km. Earth was formed. Because of the greater distance between Mars They were unfortunately prepared before the presence of a helium and the Sun. however, most of this water is now frozen and layer wan confirmed and do not allow for this. but in other respectB covered with dust from the frequent dust storms that sweep the they are seen to provide a realistic summary of atmospheric proper- planet. It is considered that if liquid water is found in substantial ties. W.M.R quantities below the surface of Mars, beneath a layer of ice measuring 0.5 km or more, the water may constitute a potential biosphere; the mechanism by which life could have originated and A65-269a continue to exist is discussed. F.R.L. vIsmu POLARIZATION DATA OF MARS. D. G. Rea and B. T. 0' Leary (California, University, Space Sciences Laboratory, Berkeley, Calif. ).

A65-26729 f Nature, vol. 206. June 12, 1965. p. 1138-ll40. 6 refs. THE ROLE OF INFRARED SPECTROSCOPY IN THE BIOLOGICAL Grant No. NsG 101-61. EXPLORATION OF MARS. Discussion of the discrepancy in values derived by different D. G. Rea (California. University, Space Sciences Laborbtory, methods for the surface pressure of Mars. A value of 90 mbar Berkeley. Calif. ). for this pressure, based on visible photometric and polarimetric International Symposium on Basic Environmental Problems of work, has generally been accepted. Recently, however, a value Man in Space, 2nd. Paris. France, June 14-18, 1965. Preprint of 25 mbar has been derived by Kaplan, Munch, and Spinrad from -no. 9. 47 p. 31 refs. a curve-of-growth analysis of pressure-broadened carbon-dioxide

45 A65-27015

vibration-rotation lines in the near IR Martian spectra. It is sug- taken from eight observatories which. after an evaluation process, gested that this discrepancy can be accounted for by the presence showed the regular appearance of a dark spot shaped like a recumbent of aerosol particles in the Martian atmosphere contributing an Y. Additipnal evidence is cited from the Paris Observatory in the appreciable component to the observed brightness and polarization form of a series of measurements of radial velocities at different of Mars. Calculations are given indicating the feasibility of this points on the disk of the planet. made by means of a sensitive inter- explanation. P. K. ferential spectrograph which inhcate, by Doppler effect, a four-day retrograde rotation. Certain irregularities in the observed period A65-27015 of rotation are considered to be due to meteorologlcal effects in the LACK OF EFFECT OF IO ON JOVIAN 3.75-CM EMISSION. Venusian atmosphere. F.R.L. John R. Dickel (Illinois, University, Observatory, Urbana, Ill. ). -Nature, vol. 206, June 19, 1965, p. 1241, 1242. Investigation of the effect Io on the synchrotron emission of A65-27669 generated within the radiation belts in Jupiter's atmosphere. The STRUCTURE OF THE MARTIAN UPPER ATMOSPHERE. position Io was plotted against the results of observations at of Michael B. McElroy, Joseph W. Chamberlaln (Kitt Peak National 3. 75 cm, taken with a polarimeter on the 85-ft telescope at the Observatory, Tucson, Ariz. ), and Jean L'Ecuyer (Chicago. University of Michigan. After correcting for the effects of the University, Yerkes Observatory. Williams Bay, Wis. ). planet's rotation, no correlation was detected between the position Astrophysical Journal, vol. 141, May 15, 1965, p. 1523-1535. 26 refs. of Io and degree of polarization, flux density, or position angle Computation of a number of models of the Martian thermosphere of the polarized radiation. It is concluded that, although Io has with various constants and boundary values in the hydrostatic and been observed to have an effect on the localized regions respon- heat-flux equations. The investigation is divided into two main sible for decameter bursts, it does not influence the overall parts. First, the basic parameters are varied, one or two at a structuie the Jovian magnetosphere, which is responsible for oi time, to find to what extent an uncertainty in one of these fundamental the nonthermal emission at centimeter wavelengths. A. F. R. parameters affects the derived exospheric temperature and other characteristlcs of the upper atmosphere. These models are physi- A65-27098 cally oversimplified but mathernatlcally serve their purpose. Secondly, POSSIBLE ALTERNATIVE CHEMISTRIES OF LIFE. with selected specific chemical compositions, the equations are V. A. Firsoff. integrated with allowance for difhsive separation and absorption of Spaceflight, vol. 7, July 1965, p. 132-136. 11 refs. sunlight in different spectral regions. A rather detailed and general Discussion of chemical elements and compounds suitable for di8cussion is included of the efficiency with which photon energy is prolonged biomolecular evolution and chemical selection in light converted into the kinetic energy of heat in the neutral atmosphere. of varying planetary conditions of environment and temperature. The computed models are thought to be fairly representative of an The most salient chemical features of life are discussed as algebraic actual atmosphere with the assumed compositions. It appears that terms without the substitution of any definite chemical species for CO vibrational excitation is not so important as a thermostat as was symbols. An important feature of the molecular structures' occurring previously suggested, but the rotational levels of CO, and to a in biology is that of a state of labile equilibrium, under which they smaller extent the fine-structure levels of the ground term of 0, respond to stimuli in chemical terms but revert to original constitu- may cause appreciable radiation loss. Direct observation of the tion once the disturbance is over. A solvent is necessary for chemi- Martian corona in the A 1302 resonance radiation of 0 I should be cal interchange and exchange; this and other considerations restrict possible and would allow the main present uncertainties to be any given life system to a fairly narrow temperature range. It is removed. (Author) W. M. R. shown that the elements which exhibit the phenomena of catenated hydride formation and ready polymerization are those which are included in thecroups I11 to V of the periodic table. Reasons are given which show that boron is not suitable as an independent A66-27771 catenant, but that the elements in Group IV, including C, Si, and * RADIOASTRONOMICAL OBSEHVATION AND THE IONOSPHEAE OF Geare. Hydrosilicons or silanes and germanes are described. VENUS [RADIOASTRONOMICHESKIE ISSLEDOVANIL4 I IONOSFERA Nitrogen is discussed as a suitable catenant, with particular refer- VENERY]. ence to the B-N series compounds which form polymers analogous of A. D. Danilov (Akademiia Nauk SSSR, Institut Prikladnoi Ceoflziki. to some of the hydrocarbons such as borazole, the analog of benzene. Moscow, USSR). Various possible solvents are investigated in terms their suitabil- of Akademiia Nauk SSSR, Doklady, vol. 162, June 1, 1965, p. 774-777. ity for such catenant systems at differing environmental tempera- 17 refs. In Russian. tures. "3, and HgBr3 are all possibilities. depending on HF, F20 Survey of some results obtained by different authors in the the planetary temperatures. Catenant systems based on atoms of course of the past year concerning the origin of Venus radio emission the noble gases which are polarized in the presence strong dipole of and its relation to the Venus ionosphere. Partlcular attention is solvents, such as FZO, are discussed as being applicable to very given to results which indicate the presence of a dense ionosphere cold planets such as Pluto. D.P.F. surrounding Venus and that radioastronomic observations may be influenced by this ionosphere. It is seen that this circumstance A65-27146 * should be taken into account in the interpretation of observation A MICROWAVE RADIOMETER AND MEASUREMENT OF THE data, irrespective of the type of model used to explain the total NATURAL RADIATION OF JUPITEh. brightness-temperature spectrum of Venus radio emission. V. P, 0. N. Rzhiga, G. I. Slobodeniuk, V. N. Titov, and Z. G. Trunova (Akaderniia Nauk SSSR, Institut Radiotekhnlki 1 Elektroniki, Moscow, USSR). (Radiotekhnika i Elektronika, vol. 10, Feb. 1965, p. 364-367. ) Radio Engineering and Electronic Physics, vol. 10, Feb. 1965, AM-20200 p. 306-309. 12 refs. Translation. SIGNS OF LIFE - CRITERION-SYSTEM OF EXOBIOLOGY. [For abstract see Accession no. A65-18553 08-30] Joshua Lederberg (Stanford University, School of Medicine, Dept. of Genetics, Palo Alto, Calif. ). Nature, vol. 207, July 3. 1965. p. 9-13. AM-27650 # Systematic criticism of the theoretical basis and operational STUDIES OF THE ROTATION OF VENUS [RECHERCHES SUR LA methods of exobiology, the study of extraterrestrial life. The dis- ROTATION DE VENUS) cussion in this case is limited to the possibility of life on Mars and C. Boyer. is based on the supposition that the three evolutionary stages char- L'Astronomie, "01. 79, June 1965, p. 223-228. 5 refs. In French. acterizing the earth's history have their counterparts in the develop- Discussion of telescopic observatlons of Venus made from 1957 ment of Mars. Various approaches which might prove to be fruitful to the present which are considered to indicate that the planet in determining the present stage of evolution of Mare are suggested. rotates in a retrograde sense during a period of approximately four The launching of a Mars-orbiting observatory is considered an es- days. The conclusion was reached on the basis of UV photographs sential prerequisite to an actual landing on Mars. A.B.K.

46 A65-29491

A65-2-54 X vehicle having a halt-cone angle of 18' and an (L/D)max =l.lb was RECENT SPACE MEASUREMENTS STRATOSPHERIC BAL- WITH studied to determine the effect of initial entry velocity on vehicle LOO" [RECENTS RESULTATS SPATIAUX PAR BALLONS heat-protection weight. The indications suggested by the results STRATOSPHERIQUES]. of this analysis are provided. R. Zander (Liage. Universitl, Institut d' Astrophysique, Likge, Belgium). Ciel et 'Ierre. vol. 81. May-June 1965, p. 155, 156. In French. A65-28940 Discussion of the data concerning the composition of the STRATGSCOPE 2. Venusian clouds. which appear to be formed of ice crystals. based M. Blavet. on telescopic observations of the planet Venus with helium-filled Electronique. June 1965, p. 245-249. In French. stratospheric balloons. The experimental data were obtained at an Stratoscope 2 is a balloon-elevated optical system capable of altitude of 26 km where absorption by the residual terrestrial at- making astronomical observations of planets, nebulae, and other mosphere does not exceed 2% of its total value. A 30-cm automatic celestial objects at an altitude of 80,000 feet. The system, which telescope was used, coupled to a spectrometer for measuring ab- weighs 3 tons. is essentially free of the absorption and distortion sorption spectra. Two series of observations were made, one in caused by atmospheric water vapor and dust. The optical equipment February, one in October 1964. Based on the absorption spectra includes: (1) a primary mirror 90 cm in diam., weighing 200 kg, of the sun's IR radiations in the 1.6-3.4 p range, the latter obser- and constructed with a precision of 1/100,000 of a nun; (2) a control vations indicate that the clouds which mask the surface of Venus system; (3) a 64-cbaMel system of telemetry for long-distance con- are composed of water in the form of ice crystals. D. P. F. trol; (4) a guidance system with a precision of 0.02" of arc; and (5) a suspension syatem which allms the telescope to be displaced about multiple axes. There is a TV camera which is aligned with A65-28839 # the principal optical axis of the telescope. The optical system is AERODYNAMIC BRAKING TRAJECTORIES FOR MARS ORBIT also equipped for spectrophotometry in the IR spectrum. D.P.F. ATTAINMENT. Thomas W. Finch (Douglas Aircraft Co., Inc., Missile and Space Systems Div., Santa Monica, Calif.). A65-29113 (American Institute of Aeronautics and Astronautics, Annual Meeting, SOLAR SYSTEM SCIENCE - 1964 LITERATURE SURVEY. 1. 1st. WashinKton. D. C., June 29-July 2, 1964, Paper 64-478. ) Edna O'Connell (RAND Corp., Santa Monica, Calif. ). Journal of Spacecraft and Rockets, vol. 2. July-Aug. 1%5. Icarus, vol. 4, July1965, p. 319-333. p. 497-500. 5 refs. Bibliography containing 275 entries on various astronomical NASA-supported researcy. subjects, published in the year 1964, and referring to 11 US, Examination of the problems associated with aerodynamic British, and Soviet technical publications. The entries are dis- braking into a Martian orbit from the standpoint of vehicle and tributed among 11 main subject headings: atmospheric physics, trajectory Capability. Mars entry corridors for lifting vehicles cosmogony, interplanetary physics, planetary biology, meteorites, are presented. Trajectories are developed which minimize the planetary geodesy, planetary geology, planetary physics. solar propulsive orbit injection velocity increment. The magnitude of physics, solar-system dynamics, and solar-terrestrial relations. the propulsive velocity increment is examined for these trajecto- D. P. F. ries as a function of orbit altitude, vehicle lift/drag ratio, and A65-29288 * lift parameter, and entry velocity and peak load factor. It is RECENT OBSERVATIONS OF SATURN. stated that, since the minimum propulsive velocity trajectories Patrick Moare. are found to be impractical due to extreme sensitivity and lack British Astronomical Association, Journal, vol. 75, June 1965, of control capability, a class of trajectories is proposed which p. 215, 216. minimizes these difficulties. These alternate trajectories are Study of the ring system and atmosphere of Saturn. Searches found to require larger propulsive velocities for orbit injection. for Ring D were made and proved negative. In 1962. an interesting Propulsive velocity increments are again examined as functions feature was a vague white spot in the equatorial zone. In 1963, the of orbit altitude, vehicle lift/drag ratio and lift parameter, and chief feature of the early part of the apparition was the brightness entry velocity and peak load factor. It is noted that, since the of the south polar zone. Observations in 1964 showed that the whole alternate trajectories provide orbital plane rotation capability, equatorial zone was chrome or brownish in hue. Because similar the magnitude of the orbital plane rotation possible through aero- but more striking color phenomena had just been seen on Jupiter, dynamic maneuvering is examined as a function of the vehicle it was difficult to avoid speculating whether solar influence might be lift/drag ratio. responsible. M.F.

A65-28841 * A65-29289 ## SPACECRAFT HEAT-PROTECTION REQUIREMENTS FOR MARS A POGSIBLE CLOUD ON MARS? AERODYNAMIC BRAKING. Patrick Moore. G. M. Hanley and F. J. Lyon (North American Aviation, Inc., British Astronomical Association, Journal, vol. 75. June 1965, Space and Information Systems Div., Flight Sciences Dept., p. 217. Downey, Calif.). Observation of clouds on Mars. During the present apparition (American Institute of Aeronautics and Astronautlcs, Annual Meeting, of Mars, conditions have been generally poor, but one or two possible 1st. Washington, D.C., June 29-July 2, 1964, Paper 64-479.) clouds have been detected. The most interesting of these was seen Journal of Spacecraft and Rockets, "01. 2. July-Aug. 1%5. on Feb. 27, 1965. A fairly well-defined white cloud was seen, placed p. 508-515. 13 refs. approximately over the western end of the Deucalionis Regio. Un- Contract No. NAS 9-1748. fortunately the weather conditions for the next few nights were quite Determination of the feasibility of decelerating a spacecFaX6y hopeless, and when the area was next seen, there was no sign of the aerodynamic braking to establish an orbit about the planet Mars. cloud. The only other cloud phenomenon was seen on Mar. 28-29 The effect of vehicle shape on heat-protection weight at a nominal in the area of Thymiamata. However this was by no means so clear entry velocity of 27, 600 fps, and the effect of initial entry velocity as that of Feb. 27. The observations were made with a 12-112-in. on heat shielding of a selected configuration for entry velocities reflector at 46Ox. M.F. between 27.600 and 39,000 ips are studied. It is stated that, because of the wide spread in current estimates of the constituents and density of the Martian atmosphere. their effect on the maximum heat- A65-29491 F protection weight and entry corridor depth is presented. The study THE BISTATIC RADAR-OCCULTATION METHOD FOR THE STUDY results are said to indicate that gas radiation is a major source Of OFPLANETARYATMOSPHERES. gasdynamic heating during atmospheric braking, even for entry at G. FJelaDo and V. R. Eshleman (Stanford University. Center for 27,600 fps. Consequently. blunt shapes, such as the Apollo con- Radar Astronomy, Stanford, Callf. ). figuration, have higher heat-protection weight requirements than Journal of Geophysical Research. vol. 70. July 1. 1965. p. 3217- finer shapes such as the M-2 and high LID delta wing shapes. As 3225. 7 refs. a consequence of these initial study results, a modified conical NASA-sponsored research.

47 A65-29684

Theoretical studies of the characteristics of radio waves Naval Research Laboratory, Washington, D. C. ), p. 1-4. [See diffracted at the limb and refracted in the atmosphere of a planet. A65-29983 19-32] Sample computations have been made of atmospheric perturbations REPORT OF CHAIRMAN - WEIGHTLESSNESS COMMITTEE. to the communication links to and from a Mars-flyby spacecraft Richard Lepper (Northrop Corp., Hawthorne, Calif. ), p. 5. having a trajectory that involves occultation of the spacecraft by the ANAPPROACHTOTHEPROBLEMOFCREATINGACONTROL- planet as seen from the earth. It is concluded that such a radio LABLE TEMPERATURE PULSE IN A MOVING AIR STREAM. W. occultation experiment can provide important new information on Richard Vollmar (U.S. Naval Air Turbine Test Station, Trenton, the atmospheric scale height and surface density of a planetary N.J.), p. 7-16. 7 refs. [SeeA65-29984 19-11] atmosphere. and, when combined with other information, can help ENVIRONMENTAL TESTS OF SATURN S-IIIB STAGES FUEL determine atmospheric constituents. (Author) F.R.L. PRESSURIZATION STORAGE SPHERES. Larry V. Clarkson and Robert W. Claunch (Chrysler Corp., New Orleans, La.), p. 17-22. [See A65-29985 19-31] A65-29684 ' A USER ORIENTED 15,000 FORCE POUND ELECTRODYNAMIC THE FEASIBILITY OF A VEHICLE USING ATMOSPHERIC BRAKING SHAKER. Frederick C. Hunt (Ling-Temco-Vought, Inc., Anaheim. TO LAND ON THE PLANET MERCURY. Calif.), p. 23-27. [See A65-29986 19-11] Gerald M. Roth and Herbert S. Shaw (General Electric Co., Missile PROBLEMS IN GETTING CONSISTENT RESULTS IN VIBRATION and Space Div., Re -Entry Systems Dept., Philadelphia, Pa. ) . TESTING. Peter C. Calcaterra (Barry Wright Corp., Watertown, Mass.), p. 29-31. [See A65-29987 19-32] INTERNATIONAL TEMPERATURE AND HUMIDITY STANDARDS. Samuel Greenberg (American Instrument Co., Inc., Silver Spring. Postulation of atmospheres based on Kozyrev's observations of Md.). p. 33-36. a possible hydrogen-rich composition to investigate the feasibility of using atmospheric braking to land a payload on Mercury. The CONTROL OF LIQUID ENTRAINMENT AT VENTING. D. A. atmospheres are compared to an atmosphere composed of such Smith (Douglas Aircraft Co., Inc., Santa Monica, Calif.) and heavy inert gases as krypton and argon, which, until recently, were J. Majoros (Douglas Alrcraft Co., Inc., Huntington Beach, Calif.). believed to comprise the planet's atmosphere. Entry trajectory p. 37-48. 12 refs. [See A65-29988 19-31] analysis indicates that a high-drag lander configuration such as a AN INTRODUCTORY GUIDE TO AN ELECTROMAGNETIC Langley Research Center Tension Shell entering the hydrogen atmo- COMPATIBILITY PROGRAM. W. A. Wilson (Honeywell, Inc., splere can achieve impact velocity values of approximately one-half St. Petersburg, FLa. ), p. 49-53. [See A65-29989 19-09] the initial entry velocity for a low W/C+ (- 1 to 3 psf) and entry path EFFECTS OF COMBINED HEAT AND NOISE ON HUMAN angles te I - 60°. It is further shown that by using this atmospheric PERFORMANCE, PHYSIOLOGY, AND SUBJECTIVE ESTIMATES braking in a grazing trajectory coupled with a retardation system. OF COMFORT AND PERFORMANCE. Robert D. Dean and Carl L. the descent velocity can be reduced sufficiently to allow safe impact McGlothlen (Boeing Go., Seattle, Wash.), p. 55-64. 29 refs. of an instrument payload. (Aubor) F. R. L. [See A65-29990 19-05] EVALUATION OF SELECTED METHODS FOR DETECTING CONTAMINANTS WITHIN SEMICONDUCTORS. L. D. Clark, A65-29766 # AERODYNAMICS OF PLANETARY ENTRY CONFIGURATIONS IN J. C. Burrus. and R. D. Clark (Texas Instruments, Inc., Dallas, AIR AND ASSUMED MARTIAN ATMOSPHERES. Tex. ), p. 65-71. [See A65-29991 19-09] SERVO-CONTROLLED PNEUMATIC ISOLATORS AN Leland H. Jorgensen (NASA, Ames Research Center, Moffett Fleld, - Calif. \. ADVANCED CONCEPT FOR VIBRATION ISOLATION. Serge Kunica (Barry Wright Corp., Watertown, Mass.), p. 73-79. [See A65- American Institute of Aeronautics and Astronautics, Annual Meeting, 29992 19-15] 2nd. San Francisco, Calif., July 26-29, 1965, Paper 65-318. . 14 p. LL__ refs. Members, $0.50; nonmembers, $1.00. TESTING ELECTRICAL COMPONENTS FOR THE SNAP Use of approximate and characteristics methods to predict the ENVIRONMENT. William G. Long (North American Aviation, InC. Canoga Parks p' 81-84' [See A65-29993 I9-O9] effect of gas composition on the forces and static stability of entry- COST REDUCTIONS IN TESTING TO MIL-STD-202. Vernon L. type vehicles at speeds from 1.5 to 14 kmlsec. A constant stratosphere temperature of 180°K and a density range from 10-5 to 10-1 Bradfield (Collins Radio Go., Newport Beach, Caltf.), p. 85-92. times earth sea-level density were assumed. Two types of configura- LSee A65-29994 19-09] tions have been considered: (I) those that are short and blunt, and HIGH-SPEED, SOLID STATE, AUTOMATIC SIGNAL ATTENUA- (2) those that consist of a blunt nose followed by a cylinder and TION AND ITS APPLICATIONS. William T. Farrell (Radio stabilized by a flare. For short blunt vehicles the predicted force Corporation of America, Princeton, N. J.), p. 93-96. [See A65- and moment characteristics at any angle of attack and in any carbon 29995 19-09] dioxide-nitrogen composition are very close to those in air. For USE OF LH2 CRYOPUMPING FOR FLOW RAREFACTION AND blllnt-nosed flred-cylinder vehicles, the predicted stability is sensl- BOUNDARY LAYER CONTROL IN A LOW DENSITY NOZZLE. tive to gas composition, particularly at probable flight speeds below B. H. Shirley (Lockheed Aircraft Corp. , Sunnyvale. Calif. ), P. 97- about 12 km/sec. In a carbon-dioxide atmosphere the stability 104. 21 refs. [See A65-29996 19-12] might be as low as 60 to 70% that in air. However, in an atmo- of A NEW METHOD OF EVALUATING THE ACOUSTIC RESPONSE sphere in which there is considerably less carbon dioxide than OF PIEZOELECTRIC ACCELEROMETERS. Rex B. Peters nitrogen - e.g., a 0. 2C@2-. 8N2 composition - the stability should lEndevco Gorp., Pasadena, Callf.), p. 105-112. 5 refs. [See A65- be reasonably close to that in air. For these predictions the dynamic pressure at the flare was complted by the blunt-body characteristics 29997 19-14] ~ THEORETICAL MODEL ATMOSPHERES OF VENUS. Robert method of Lomax and Inouye, and real-gas thermodynamic prop- B. Owen (NASA, Marshall Space Flight Center, Ala.), p. 113-122. erties were used. (Author) M.M. 34 refs. [See A65-29998 19-30] A LOW COST 20°K REFRIGERATOR. George K. Sneden (Air A65-29982 Reduction Co. , Inc. , New York, N. Y.), p. 123-128. [See A65- INSTITUTE OF ENVIRONMENTAL SCIENCES, ANNUAL TECHNICAL 29999 19-11] MEETING, IITH. CHICAGO, ILL., APRIL 21-23, 1965, PRO- VIBRATION ISOLATION AND ATTENUATION FOR PAYLOADS CEEDINGS. OF ROCKET SLED VEHICLES. Wilfred E. Baker (Southwest Mount Prospect, 111. , Institute of Environmental Sciences, 1965. Research Institute, San Antonio, Tex.) and Joseph E. Montalbano 648 p. (Aircraft Armaments, Inc., Cockeysvllle, Md. ), p. 129-137. Members, $9.00; nonmembers, $14. 30 refs. [See A65-30000 19-11] REPRESENTATION OF TRANSIENT SINUSOIDS IN THE CONTENTS: ENVIRONMENTAL VIBRATION TESTS FOR SPACECRAFT. INTRODUCTION, p. ii. Sherman A. Clevenson, Dennls J. Martin, and Jerome Pearson PRESENT STATUS OF INTERNATIONAL STANDARDS FOR INASA. Langley Research Center, Va.). p. 139-144. 5 refs. [See SHOCK AND VIBRATION SPECIFICATIONS. Irwin Vigness (u.s.

48 A65-29982

ENVIRONMENTAL ASPECTS OF NUCLEAR SPACE PROPUL- LABORATORY SIMULATION OF THE COMBINED ACOUSTIC- SION. Wade E. Selph (Ling-Temco-Vought. Inc., Dallas. Tex. ), VLBRATION ENVIRONMENT OF LAUNCH VEHICLE ONBOARD p. 145-150. ll refs. [See A65-30002 19-22] ELECTRONIC EQUIPMENT. Arnold W. Mueller and Philip M. THERMALLY CONTROLLED VACUUM-ULTRA VIOLET Edge. Jr. (NASA. Langley Research Center. Va. ), p. 299-303. SYSTEMS FOR MATEFUALS TESTING. W. E. Jamison and W. J. [See A65-30022 19-ll] Courtney (Illinoielmtitute of Technology. Chicago, Ill. ), p. 151- A MULTI-PURPOSE HIGH CAPACITY HELIUM REFRIGERA- 154. [See A65-30003 1941 TOR-LIQUEFIER. W. A. Snow. A. R. Winters. andR. B. Currie A SMALL CAPACITY NEON REFRIGERATOR FOR CRYO- (Air Products and Chemicals, Inc. , Allentown. Pa. ), p. 305-314. PUMPING APPLICATION. Joseph P. Ryan (General Dynamics [See A65-30023 1941 Corp., Chicago, Ill. ), p. 155-160. 22 refs. [See A65-30004 19-lll STATIC EQUALIZATION FOR RANDOM WAVE VIBRATION RELATIVE ACCURACY OF OSCILLOGRAM AND MAGNETIC- TESTING. Manny Greenhouse (North American Aviation, Inc., TAPE RECORD ANALYSES. H. F. Alma and% E. Lee (U.S. Anaheim, Calif. ), p. 315-320. [See A65-30024 19-32] Navy, Washington, D.C.), p. 161-167. 9 refs. [See A65-30005 A METHOD OF DETERMINING EFFECTIVE SKY TEMPERA- 19-14] TURE FOR THE CALCULATION OF RADIATION HEAT TRANSFER PERFORMANCE REPORT - MAN RATED HIGH VACUUM AT THE EARTH'S SURFACE. K. R. Hanson and W. E. Krauss SPACE SIMULATOR. Carl 3. Schmock (F. J. Stokes CO., (Martin Marietta Gorp. , Orlando, Fla.), p. 321-324. 9 refs. [See Philadelphia, Pa. ), p. 169-175. [See A65-30006 19-11] A65-30025 19-33] A UNIFIED METHOD FOR OBTAINING THE MECHANICAL INPUT AND OUTPUT POWER CHARACTERISTICS OF A IMPEDANCE OF VIBRATORY SYSTEMS. Joseph I. Schwartz LARGE ELECTRO-PNEUMATIC TRANSDUCER USED FOR (U.S. Navy, Annapolis. Md.). p. 177-184. [See A65-30007 19-32] ACOUSTIC ENVIRONMENTAL TESTING. Frank M. Tdlou. Jr. PROBLEMS IN TRANSLATING ENVIRONMENTAL DATA INTO (Ling-Temco-Vought, &nc. , Anaheim, Calif. ), p. 325-336. [See A TEST SPECIFICATION. W. R. Forlifer (NASA, Goddard Space A65-30026 19-11] Flight Center, Md.), p. 185-188. 13 refs. [See A65-30008 19-32] DESIGN OF ELASTOMERIC MOUNTING SYSTEMS FOR A PROCEDURE FOR SELECTION OF RANDOM VIBRATION ISOLATION OF VIBRATION ENVIRONMENTS. Edward L. Meyer DATA ACQUISITION/ANALYSIS EQUIPMENT. Robert Lochner (Radio Corporation of America. Princeton. N. J.), p. 337-342. (Honeywell, Inc., Minneapolis, Minn. ), p. 189-192. [See A65-30027 19-15] UPGRADING UNMANNED SPACECRAFT QUALITY AND AN INVESTIGATION OF HEAT TRANSFER AT HIGH ALTI- RELIABILITY THROUGH ENVIRONMENTAL TESTING. Kenneth R. TUDES. E. Robert Wilson (Martin Marietta Corp., Denver. Colo.). Mercy and Albert R. Timmins (NASA, Goddard Space Flight Center, p. 343-352. [See A65-30028 19-33] Md.), p. 193-200. [See A65-30009 19-31] A 200,000 FORCE POUND, 22 FOOT DIAMETER VIBRATION THE DEVELOPMENT OF A 150. ooo LITER~SECOND ION- SYSTEM FOR TESTING OF MAJOR SATURN STRUCTURES. GETTER PUMP FOR CONTINUOUS REMOTE OPERATION. Ronald DavidR. Reese (Wyle Laboratories, Inc., Huntsville, Ala.). p. 353- D. Olmstead and Raymond A. Wolf (Ultek Corp., Palo' Alto. Calif.), 363. [See A65-30029 19-11] p. 201-207. 5 refs. [See A65-30010 19-11] A METHOD OF TESTING DRY FILM LUBRICANTS IN AN MEASUREMENT OF GAS TEMPERATURE AND THE RADIA- ULTRA-HIGH VACUUM. Robert N. Hager. Jr. (General Dynamics TION COMPENSATING THERMOCOUPLE. Glenn E. Daniels (NASA. Corp., San Diego, Calif.): p. 365-368. [See A65-30030 19-15] Marshall Space Flight Center, Ala.). p. 209-218. 18 refs. [See CROSS-AXIS "G" CONTROL IN INSTRUMENT LINEAR A65-30011 19-14] VIBRATION. Kenneth R. Jackman (General Dynamics Gorp., DESIGNING TRAVELING WAVE TUBES TO WITHSTAND POmOM, Calif. ), p. 369-385. [See A65-30031 19-11] MLLITARY AIRBORNE AND SHIPBOARD ENVIRONMENTS. MAINTAINING ENVIRONMENTAL CONTROL REQUIREMENTS Stanley W. Corbett and James E. Mitchell (Microwave Electronics FOR FABRICATION AND ASSEMBLY OF STERILE SPACE Corp., Palo Alto, Calif. 1, p. 219-223. [See A65-30012 19-09] VEHICLES. Fred W. Thomas, Jr. and Myron H. Bengson (General Electric Co., New York. N.Y.), p. 387-391. [See A65-30032 19- DEVELOPMENT OF A PILOT UNIVERSAL COUCH FOR 051 ACCELERATION. VIBRATION, AND SHOCK. L. M. McClernan EFFECTIVE RADIATIVE PROPERTIES OF SURFACES IN and William S. Thayer (Aircraft Armaments, Inc., Cockeysville, SPACE SIMULATION FACILITIES. William Clausen (General Md. ). p. 225-240. 21 refs. [See A65-30013 19-05] Dynamics Corp. , San Diego, Calif. ). p. 393-400. 10 refs. [See HUMAN ANGULAR MOTION CAPABILITY IN THE ZERO A65-30033 19-17] GRAVITY ENVIRONMENT. William S. Thayer (Aircraft Armaments MAGNETIC SHIELD SIMULATOR. S. H. Levine and R. Lepper Inc., Cockeysville. Md.). p. 241-250. 7 refs. [See A65-30014 (Northrop Corp., Hawthorne, Calif. ), p. 401-408. 11 refs. [See 19-05] A65-30034 19-11] SHOCK CAPABILITIES OF ELECTRO-DYNAMIC SHAKERS. ENSURING THE ACCURACY OF SHOCK AND VIBRATION James M. McClanahan and John R. Fagan (Radio Corporation of MEASUREMENTS. R. R. Bouche (Endevco Corp., Pasadena, America. Princeton. N. J.), p. 251-256. [See A65-30015 19-11] Calif. ), p. 409-415. 13 refs. [See A65-30035 19-32] DESIGN OF A LARGE ION-GETTER PUMPED SPACE SIMU- A PRACTICAL APPROACH TO NUMERICAL RESULTS IN NON- LATION FACILITY. Max Baron (F. J. Stokes Co., Philadelphh. LINEAR DYNAMICS PROBLEMS. Robert M. Mains (General Pa. 1, P. 257-261.. [See A65-30016 19-ll] Electric Co., Schenectady, N. Y.), p. 417-423. [See A65-30036 SHOCK ANALYSIS AND SYNTHESIS. Jorge S. Forte (Ling- 19-23] Temco-Vought. Inc., Anaheim, Calif. ), p. 263-269. . [See A65- HIGH INTENSITY SHOCK SIMULATION. D. E. White. R. L. 30017 19-32] Shipman. and W. L. Harvey (Martin Marietta Corp., Denver, Colo. ), p. 425-431. [See A65-30037 19-11] THE SIGNIFICANCE OF FAILURES IN SHOCK AND VIBRATION A DRIVEN PLATFORM (SOFT TEST STAND) FOR VIBRATION TESTS. Richard T. Othmer (Sandra Corp., Albuquerque, N.Mex.), ENVIRONMENT SIMULATION. Russell C. Jouett and Frank H. p. 271, 272. Rezavy (International Busmess Machines Corp. , San Jose. Callf. ), TRANSPORTATION ENVIRONMENTS REVISITED, Anthony s. p. 433-443. [See A65-30038 19-11] Baran and Arthur R. Schilling (Radio Corporation of America. AN APPARATUS FOR THE INVESTIGATION OF COLD WELDINI Princeton. N. J. ), p. 273-275. [See A65-30018 19-11] IN A SIMULATED SPACE ENVIRONMENT. Allan Juster (Republic A UNIFIED PHILOSOPHY OF SHOCK AND VIBRATION Anation Corp., Farmlngdale. N.Y.). p. 445-448. [See A65- TESTING FOR GUIDED MISSILES. Ernest F. Small (Boemg CO., innin 10 trl >"">7 Seattle, Wash.). p. 277-282. 5 refs. [See A65-30019 19-32] L7-*>, A MANNED REVOLVING SPACE STATION SIMULATOR. E. A. VALUES OF EXTREME SURFACE PRESSURE FOR DESIGN Harrs. Jr. and B. D. Newsorn (General Dynamics Corp., San CRITERIA. Glenn E. Daniels (NASA, Marshall Space Flight Center. Diego. Calif. ), p. 449-453. [See A65-30040 19-11] Ala. ), p. 283-288. 5 refs. [See A65-30020 19-21] PROBLEMS IN GETTING CONSISTENT RESULTS IN SHOCK PREDICTION OF SOUND INDUCED VIBRATIONS OF A VTOL TESTING. Harold M. Forkois (U.S. Naval Research Laboratory. AIRCRAFT - BELL X-ZZA. Werner Fricke and Paul Kehler (Bell Washington, D.C.). p. 455-457. 10 refs. [See A65-30041 19-11] Aerospace Corp., Buffalo, N. Y.), p. 289-297. 7 refs. [See A65- ULTRA-HIGH VACUUM WITH EXTREMELY HIGH PUMPING 30021 19-32] SPEED. Robert J. Piper and James A. Craig (North American

49 A65-29998

Aviation, Inc., Canoga Park. Calif.), p. 459-463. 8 refs. [See DESIGN AT THE ROYAL AIRCRAFT ESTABLISHMENT. H. A. J. A65-30042 19-11] Prentice and J. Porter (Ministry of Aviation, Royal Aircraft INTEGRATED TESTING - YES OR NO. Tim B. Seman (Lockhee Establishment, Farnborough, Hants. , England), p. 633-643. Aircraft Corp., Sunnyvale, Calif. ), p. 465-468. [See A65-30043 15 refs. [See A65-30062 19-31] 19-11] AUTHOR'S INDEX, p. 647, 648. DIGITAL RANDOM VIBRATION ANALYSIS TECHNIQUES. Claude E. Green (NASA, Huntsville, Ala.) and Thurman L. Pitts A65-29998 (Brown Engineering Co., Huntsville. Ala. ),. p. 469-472. [See A65- THEORETICAL MODEL ATMOSPHERES OF VENUS. 30044 19-32] Robert B. Owen (NASA, Marshall Space Flight Center, Huntsville, REDUCTION OF COMPLEX SINUSOIDAL VIBRATION TEST Ala. ). DATA. Luis M. Zervigon (Chrysler Corp., New Orleans, La.), IN: INSTITUTE OF ENVIRONMENTAL SCIENCES, ANNUAL p. 473-480. 9 refs. [See A65-30045 19-32] TECHNICAL MEETING, ILTH, CHICAGO, ILL., APRIL 21-23, EXPLOSION CHARACTERISTICS OF DUST. Joseph P. Gillis 1965, PROCEEDINGS. [A65-29982 19-11] (Fenwal, Inc., Ashland. Mass. ), p. 481-484. Mount Prospect, Ill. , Institute of Environmental Sciences, 1965, SOLAR SIMULATOR PERFORMANCE PARAMETERS - PRO- p. 113-122. 34 refs. POSED SPECIFICATION AND INSTRUMENTATION. L. L. Young anc Consideration of several theoretical model atmospheres of the Francis H. Webb, Jr. (Technical Explorations Co. ), p. 485-488. planet Venus and their modification or elimination, with the exceptio [See A65-30046 19-11) of Greenhouse Model "B. 'I According to this latest model, the GAS FIRED ENVIRONMENTAL HEATING. Joseph N. Steinmetz. bright-side surface temperature of Venus is 750°K, and that of the Jr. (Lockheed Aircraft Corp., Sunnyvale, Calif. ), p. 489-491. dark side is 640°K; the derived surface pressure is at least 30 [See A65-30047 19-11] atmospheres. It is assumed that under these conditions no CONTROL OF MULTIPLE SHAKERS. James Gay Helmuth significant water vapor exists. Since the melting points of tin, (Chadwick-Helmuth Co., Inc., Monrovia, Calif.), p. 493-496. lead, aluminum, magnesium, bismuth, and zinc might be reached [See A65-30048 19-11] on the bright aide, molten pools of these metals could cover much ANIMAL BEHAVIOR IN FIELDS OF SIMULATED GRAVITY. of that area. Temperature at the dark pole has been estimated to K. 0. Lange and A. B. Broderson (Kentucky, University, Lexington. be 540°K; with the high surface pressures, possible constituents of Ky.). p. 497-509. [See A65-30049 19-05] the lower atmosphere may condense out in that region. Therefore, DYNAMIC COMPARISON CALIBRATOR FOR HIGH RANGE seas around the dark pole may contain benzine, acetic acid, butyric PRESSURE TRANSDUCERS. Robert I. Morefield (Bolt Beranek acid, and phenol in the liquid state. B. B. and Newman, Inc., Los Angeles, Calif. ), p. 511-515. [See A65- 30050 19-14] ELECTRICAL POWER TRANSMISSION TO GIMBAL MOUNTS A65401 10 # IN HIGH VACUUM. Marshall K. Kingery (USAF. Arnold Air Force FORECASTING HUMIDITY [0 PROGNOZE VLAZHNOSTI]. Station, Tenn.), p. 517-527. 8 refs. [See A65-30051 19-11] Sh. A. Musaelian. IMPROVING SHAKER RELIABILITY THROUGH PRACTICAL IN: HYDRODYNAMIC LONG-RANGE WEATHER FORECASTING DESIGN MODIFICATIONS. Ralph M. Oliva (North American [GIDRODINAMICHESKU DOLGOSROCHNYI PROGNOZ POCODY]. Aviation, Inc., Canoga Park, Calif.), p. 529-537. [See A65- Edited by E. N. Blmova. 30052 19-11] Moscow, Izdatel'stvo Nauka, 1964, p. 62-74. 8 refs. In Russian. A METHOD FOR EXPERIMENTAL DETERMINATION OF THE Solution of the problem of humidity transport in the atmosphere EFFECT OF THERMAL RADIATION FROM THE ATMOSPHERE. in planetary-scale processee. A nonlinear equation for forecasting R. W. Porter and Donald W. Boekemeier (Bendix Corp., Mishawaka specific humidity is linearized by the method of small perturbations. Ind.), p. 539-544. [See A65-30053 19-33] The linearized humiaity equation is averaged with respect to time, THEORETICAL ERROR ANALYS~S APPLIED TO SPACE AS and the time-averaged vertical-velocity fields are determined. The CHAMBER ENVIRONMENTAL THERMAL ANOMALIES. Morton working formulas of the problem are derived. A method of deter- Jacob Rosenberg (Martin Marietta Corp., Baltimore, Md. ), p. 545- mining certain constants figuring in the solution is described. 561. [See A65-30054 19-11] A.B.K. ISOLATION OF SUSCEPTIBLE ELECTRONIC COMPONENTS FROM MISSILE LIFTOFF VIBRATION AND ACOUSTIC ENVLRON- A6540119 MENT. H. L. Obertreis (General Dynamics Corp., San Diego. INFRARED ASTRONOMY. Calif. ), p. 563-567. [See A65-30055 19-09] Bruce C. Murray and James A. Westphal (California Institute of NUCLEAR EFFECTS FACILITIES AT WHITE SANDS MISSILE Technology, Pasadena, Calif. ). RANGE. Glenn E. Elder (U.S. Army, White Sands Missile Range, Scientific American, vol. 213. Aug. 1965, p. 20-29. N.Mex.). p. 569-572. [See A65-30056 19-11] General survey of IR astronomy, methoda of detecting IR radia- REPORT ON WORKING GROUP NO. 7 OF IEC/TC 50, ON tion, and an evaluation of the results obtained from observations of DUST AND SAND TESTS. David Askin (U.S. Army, Frankford the moon and the planets. The earth's atmosphere is transparent Arsenal. Philadelphia, Pa. ), p. 573-576. to radiation in the range from 0.7 to 5.2 b, opaque from 5. f to 8 p, AN APPROXIMATE METHOD OF SIMULATING MECHANICAL transparent again from 8 to 14 u, opaque from 14 to 17p. and trana- IMPEDANCE IN VIBRATION TESTING. C. E. Nuckolls (Sandia parent again from 17 to 22 p range. From 22 to 1000 p the earth's Corp.), p. 577-581. [See A65-30057 19-32] atmosphere does not transmit because of the absorption bands USE OF GAMMA RAYS TO MEASURE THE PROTON SHIELD caused by water vapor, which are broadened by-the effect of atmo- EFFECTIVENESS OF THE APOLLO COMMAND MODULE. Ridhard spheric pressure. The development of IR detectors is described C.Ross and Aaron Krumbein (Unlted Nuclear Corp. ), p. 583-591. beginning with the primitive thermocouple, then followed by the [See A65-30058 19-22] Golay cell, the Low cryogenic bolometer. and terminating with the CHRONIC WEIGHTLESSNESS SIMULATION IN BIOLOGICAL present-day sensitive semiconductors. Sinton's observations on RESEARCH. Charles C. Wunder (Iowa, State University, Iowa the planet Mars are discussed, together with his work on Venus, City, Iowa). p. 593-602. 37 refs. [See A65-30059 19-05] Jupiter, and the moon. D. P. F. THE PLANNING OF AEROSPACE VIBRATION TESTS AND PROGRAMS. Roy W. Mustaxn (Douglas Aircraft Co., Inc., Huntington Beach, Calif.), p. 603-613. I9 refs. [See A65-30060 A65-30237 # 19-32] THERMAL EMISSION OF JUPITER [0 TEPLOVOM IZLUCHENII CONTRASTS IN ENERGY BALANCES BETWEEN INDIVIDUAL IUPITERA]. LEAVES AND VEGETATED SURFACES. Kenneth R. Knoerr A. P. Naumov and I. P. Khizhniakov (Gor'kovskii Cosudarstvennyi (Duke University, Durham, N.C.). p. 615-623. Universitet, Radiofizicheskii Institut, Gorki, USSR). THE METHODOLOGY OF TEST PLANNING APPLIED TO AN Astronomicheskii Zhurnal, vol. 42, May-June 1965, p. 629-638. EXPERIMENTAL STUDY. Arthur R. Anderson (Cook Electric Co., 29 refs. In Russian. Morton Grove, Ill,), p. 625-631. [See A65-30061 19-18] Calculation of the optical thickness of the isothermal atmo- ENVIRONMENTAL TESTING IN SUPPORT OF SATELLITE sphere (130°K) of Jupiter in the 1.3-mm to 3-cm band,. assuming

50 b A65-30683 from spectroscopic data that the planet's atmosphere consists of Investigation of the survival of terrestrial microorganisms in Hz. CH+ and "3. Thermal emission levels and the brightness a simulated Martian environment. The ultimate objective is to es- temperature of the planet are determined using nonisothermal atmo- tablisb whether earth organisms can contaminate Mars. In addition. spheric models for various temperature gradients and trqospheric any demonstration of survival and grotvth in a simulated Martian en- heights hc. The difference between the brightness temperature Tb vironment will provide information relating to the biology of Mars. and the IR temperature of the cloud layer at = 36.9 km (A LI 1.25) In the experimental design, exhaustive consideration was given to the is given as z 7OoK for a temperature gradient of -2.01%/km. The duplication of the known and the theoretical environmental parame- wavelength A 1.05 to 1.54 cm is found to Ee most convenient for a ters of Mars. These included composition of the soil and the atmo- comparison of theoretical and experimental results. V.Z. sphere, barometric pressure, moisture content, solar radiation, and diurnal temperature extremes. Baaed on these considerations. a simulated Martian summer environment was defined and used in A6530238 * the experiments. One group of microorganisms was selected from NATURE OF TRANSFORMATIONS ON THE SURFACE OF JUPITER culture collections on the basis of their known characteristics. The [O PRIRODE IZMENENII NA POVERKHNOSTI IUPITERA]. other group was made of microorganisms isolated from soils. The S. K. Vsekhsviatakii (Kievakii Gosudarstvennyi Universitet, soil samples were obtained from the Antarctic, from New Mexico Kafedra Astronomii, Kiev, Ukrainian SSR). and California deserts, and from the Colorado tundra. The studies Astronomicheskii Zhurnal, vol. 42, May-June 1965, p. 639-644. showed that a number of microorganisma can survive the simulated 14 refs. In Russian. Martian environment. However. no substantial growth under such Interpretation of conspicuous, rapid phenomena observed since conditions could be demonstrated. The ability of microorganisms 1462 on the surface of Jupiter by Soviet and other astronomers to form spores as a mechanism for survival is discussed. Also, whicb'appear to require a revision of accepted concepts concerning experiments utilizing augtnented environments to establish minimum the nature of the processes on the planet. A tentative estimate gives environmental conditions which will permit growth are describsd. the minimum amount of ash particles in the planet' s atmosphere as (Authar) M.M. loa to 1022 g, and the theory is advanced that the dark bands are ash particle accumulations resulting from gigantic volcanic erup- tions. From the integral brightness attenuation, the albedo of a A6540682 dark equatorial band observed in 1961 is found to be 0.06. Further ON ARTIFICIAL MARTIAN CONDITIONS REPRODUCED FOR systematic studies of the integral brightness and surface changes MICROBIOLOGICAL RESEARCH. are urged. V.Z. A. I. Zhukova and I. L Kondratiev (Academy of Sciences, Moscow, USSR). (COSPAR. Meeting, 7th, and International Space Science Symposium, 5th. Florence, Italy, May 8-20. 1964, Paper. ) A65-303ZI IN: LIFE SCIENCES AND SPACE RESEARCH. VOLUME 3; INTER - TRANSLATIONAL AND ROTATIONAL MOTION OF A BODY NATIONAL SPACE SCIENCE SYMPOSIUM, 5TH.5TH, FLORENCE. ENTERING THE MARTIAN ATMOSPHERE [TRANSLATIONS- UND ITALY, MAY 12-16, 1964. [A65-30671 19-04] ROTATIONSBEWEGUNG EINES IN DIE MARSATMOSP~RE Symposium sponsored by COSPAR. EINTAUCHENDEN K&PERS], Edited by Marcel Florkin. Peter Hans Feitia (California Institute of Technology, Jet Propulsion Amsterdam, North-Holland Publishing Co. ; New York. John Wiley Laboratory, Pasadena, Calif. ). and Sons. Inc., 1965. p. 120-126. (Wissenschaftliche Gesellschaft fur Luft- und Raumfahrt. and Approach to the .oli&cm of probGms-regar&g &e character Deutsche Gesellschaft mr Raketentechnik und Raumfahrt, of life on Mars, by simulating Martian conditions by means of data Jahrestagung.. Berlin, West Germany. Sept. 14-18. 1%4. Paper. ) obtained from astrophysics. Experiments are describsd in which Raumfahrtforschq, wl. 9, July-Sept. 1965. p. 124-131. InGerman. pure cultures of fungi and bacteria have been used, as listed in Derivation the atmospheric paramGters the density &a table. Short-time exposure has mabled conclusions 01 the viability distribution within the Martian atmosphere as a function of altitude, of 22 strains of microorganisms under chambr conditions when the The equations motion assuming that the perfect-gas law holds. of insolation source is switched on. It is concluded that: (1) spores of simple bodies are established and solved. The solution consists of mold fungi are more stable than spores of bacterial cells, and of equations for the velocity. acceleration, and time as explicit (2)not all tested forms of microorganisms are capable of retaining functions of altitude. The case of oblique entry into the atmosphere viability under conditions imitated in the installation. is also treated. It is shown how the altitudes at which acceleration and heating have their maximum can be calculated. A sphere entering the Martian atmosphere is considered, assuming that the center Ab540683 of gravity of the sphere does not coincide with its geometric center. ABIOGENIC SYNTHESIS ON MARS. The diameter containing the sphere's center of gravity is called its Richard S. Young, Cyril Ponnamperuma, and Barbara K. McCaw axis. First, the rotational motion of the sphere is considered. (NASA, Ames Research Center, Moffett Field, Calif. ). assuming that its axis is initially inclined with respect to the IN: LIFE SCIENCES AND SPACE RESEARCH. VOLUME 3; INTER- trajectory. The axis oscillates in a plane with an amplitude which NATIONAL SPACE SCIENCE SYMPOSIUM, STH, FLORENCE. first decreases and then increases after maximum acceleration is ITALY, MAY 12-16, 1964. [A65-30671 19-04] reached. When the sphere is spinning it performs a camplicated Symposium sponsored by COSPAR. precessional motion around the velocity vector, The precession Edited by Marcel Florkin. angle first converges and then divergea. Amsterdam, North-Holland Publishing Co. ; New York, John Wiley and Sons, Inc., 1965. p. 127-138. 7 refa. Discussion of atmospheres capable of producing organic com- A6540676 pounds under primitive conditions in the light of recat experimen- RESPONSE OF MICROORGANISMS TO A SIMULATED MARTIAN tal evidence. The atmosphere of Mars io conbidered and in par- ENVIRONMENT. ticular, the observations of Sinton of reflection spectra with feature Ervin J. Hawrylewics, Charles A. Hagen, and Richard Ehrlich at 3.45. 3.58. and 3.69 (r. which are attributed to C-H bands and (Illinois Institute of Technology, Research Institute. Life Sciences to the presence of organic molecules. Colthup interprets these Div., Chicago, Ill. ). features as being representative of organic aldehydes and suggests. 1N: LlFE SCIENCES AND SPACE RESEARCH. VOLUME 3; INTER- specifically, acetaldehyde. Many works have considered these ob- NATIONAL SPACE SCIENCE SYMPOSIUM, 5TH. FLORENCE. servations as being indicative of life on Mars. Rea has offered al- ITALY, MAY 12-16. 1964. [A65-30671 19-04] ternative hypotheses. Experimental evidence is presented of yet Symposium sponsor+d by COSPAR. another possible explanation: that organic compounds are being Edited by Marcel Florkin. produced in the Martian atmosphere. and may be responsible for Sinton's observations. The influence of such syntheses possjble Amsterdam, North-Holland Publishing Co. ; New York. John WfieY on Martian organisms is discussed. Various possible Martian atmo- and Sons. Inc., 1965, p. 64-73. 14 refs. NASA- supported re search. spheres were irradiated with ultraviolet light as well a6 with other

51 A65-3 1 247 possible energy sources. and a variety of organic end products were identified. Martian atmospheres plus acetaldehyde as a starting A65-32321 # point were also used and end-products analyzed. Possible abiogenic A PROPOSED SOLUTION TO ENTRY VEHICLE DESIGN PENALTIES MARS ATMO- pathways for Mars are discussed. (Author) M. M. CAUSED BY LACK OF KNOWLEDGE OF THE SPHERE. George M. Levin (NASA, Goddard Space Flight Center, Advanced Missions Analysis Group, Greenbelt, Md. ) . American Institute of Aeronautlcs and Astronautics. Annual Meeting, A65-31247 # 16 p. TWILIGHT STUDIES OF PLANETARY ATMOSPHERES FROM 2nd. San Francisco, Calif., July 26-29, 1965, Paper 65-493. SPACECRAFT [0 SUMERECHNYKH ISSLEDOVANIIAKH PLA- 12 refs. Members, $0. 50; nonmembers, $1.00. NETNYKH ATMOSFER S KOSMICHESKIKH KORABLEI]. Proposed solution to the tremendous weight penalty in any entry- G. V. Rozenberg (Akademiia Nauk SSSR, Institut Fiziki Atmosfery, Moscow. USSR). vehicle design due to lack of knowledge of atmospheric properties of Izvestiia, Fizika Atmosfery i Okeana, Mars. The "stepping stone" concept of planetary exploration using Akademiia Nauk SSSR, a nonsurviving needle-nosed probe is discussed. The small probe vol. 1, Apr. 1965, p. 377-385. InRussian. would provide the needed atmospheric data for the efficient design Proposed use of an observer situated at great height above a Three sets of measurements would be planetary surface for the investigation of the planet's atmosphere of larger entry vehicles. from its twilight phenomena. Crepuscular events can be observed made during entry: (1) dynamic and static pressure encountered by at greater distances and with better resolution than daylight events. the probe to provide pressure and density profiles, (2) deceleration of the probe to provide independent density data, and (3) atmos- W. M. R. pheric composition measured with a mass spectrometer. Externally, the probe configuration will consist of a 9O half-angle conical nose. a cylindrical midsection. an 18O half-angle skirt, and a hemispherical A65-3 1267 # afterbody. The sharp-nose. low-drag design is employed to minimize THE TWO-FREQUENCY BISTATIC RADAR-OCCULTATION plasma interference with communication and permit continuous METHOD FOR THE STUDY OF PLANETARY IONOSPHERES. transmission of data (from the probe to a fly-by spacecraft or G. Fjeldbo, V. R. Eshleman, 0. Garriott, andF. L. Smith, K. III orbiter for subsequent relay to the earth) throughout the entire (Stanford University, Center for Radar Astronomy and Radioscience interval from initial atmospheric penetration to surface Impact. Laboratory, Stanford, Calif. ). The probe's overall length and total weight (not including separation Journal of Geophysical Research, vol. 70, Aug. 1. 1965, p. 3701- mechanism) are 48 in. and 60 lb,respectively. The configuration 3710. 8 refs. will permit delivery of two or more probes from a single spacecraft. Grants No. NsG-377; No. NsC-30-60; No. NGR-05-020-065. depending on overall mission definition. (Author) B. B. Method for the study of planetary ionospheres which is based on the use of radio waves propagated between the earth and a spacecraft on an occulting trajectory beyond the planet. Phase path, group path, or amplitude measurements made during spacecraft immersion A65-32416 into, and emersion from, the occulted zone could be used to deduce BEHAVIOR OF PLANTS UNDER EXTRATERRESTRIAL CONDI- vertical electron density profiles at the two limb positions probed by TIONS - SEED GERMINATION IN ATMOSPHERES CONTAINING the waves. If two or more harmonically related frequencies are NITROGEN OXIDES. used, the ionospheric measurements are self-calibrating; thus the S. M. Siegel, Constance Giumarro, and Richard Latterell (Union extreme measurement and computatlonal precision that otherwise Carbide Research Institute, Tarrytown, N.Y.). would be required are avoided. Furthermore. the use of more than National Academy of Sciences. Proceedings, vol. 52, July 1964, one frequency makes it possible to separate dispersive ionospheric p. 11-13. effects from the nondispersive refractive effects of the neutral Contract No. NASw-167. atmosphere. so that both neutral and ionized regions of the atmo- Experimental demonstration that seeds of common plant speciea sphere could be studied in some detail. It is suggested that this can be germinated in rarefied nitrogen atmospheres containing high simple technique would be particularly applicable for the initial proportions of individual nitrogen oxides (NzO, NO, NOZ) or their exploration of planetary atmospheres. (Author) M.F. mixtures. A buffering substratum of CaC03 is especially beneficial, and the best responses thereto were given by rice and norghum in the presence of certain nitrogen oxides as compared with nitrogen alone. Cell division in the aorghum shoot in N2/N0 was demon- A65-31279 * strated. Nitrogen dioxide was inhibitory under anaerobic conditions, ON THE INTERPRETATION OF THERMAL EMISSION MAPS OF but much less when O2 was present. It is concluded that if ordina- JUPITER. so ry terrestrial flora unselected for tolerance to the oxides of nitrogen Robert L. Wildey (California Institute of Technology, Div. of Geological Sciences; Carnegie Institution of Washington and California are taken as a model, their prospects for growth in a nitrogen oxide- Institute of Technology, Mount Wilson and Palomar Observatories. rich atmosphere would be good provided the nubstratum prevents excess acidity and that NO2 is not present in excessive quantities. Pasadena. Calif. ). F.R.L. Journal of Geophysical Research, vol. 70, Aug. 1, 1965, p. 3796, 3797. Study of mapping procedures for Jupiter. Because of the limitations on the accuracy of present mapping procedures, importanl A65-32620 discrimination must be made between structural features of maps SELECTIONS FROM THE TRW SPACE TECHNOLOGY LABO- which are obviously noise and those which are good candidates for the RATORIES; LECTURE SERIES. VOLUME 2. extraction of theoretical implications. The peculiar nature of the Edited by T. L. Branigan (Space Technology Laboratories. Inc., noise warrants an elaboration of this discriminatory procedure. The Redondo Beach, Calif. ). sources of noise are primarily photometric error and secondarily Redondo Beach, Calif., Space Technology Laboratories, Inc., tracking error. Map noise of sufficient magnitude to appear as a 1965. 70 p. pneudo-Jovographic feature betrays its presence by its tendency to form troughs and ridges which align themselves parallel to the CONTENTS: general scanning direction. This tendency is seen to be highly THE THEORY AND APPLICATION OF MASERS AND LASERS. variable from night to night, and examination of the signal tracings Charles H. Townes (Massachusetts Institute of Technology, shows it to be correlated with the magnitude of that component of Cambridge, Mass. ), p. 4-13. [See A65-32621 21-16] noise in the system which is nonstationary. With stationany noise THE BIOLOGICAL EXPLORATION OF MARS. Elliott C. photometric accuracy can be increased more or less mdefinitely by Levinthal (Stanford University. Stanford, Calif. ), p. 14-21. [See decreasing the rate of scan while increasing the system time A65-32622 21-30] constant. because the aky level to be subtracted from the signal THE EFFECTS OF HIGH-ALTITUDE EXPLOSIONS. trace in a rigid constant which can be well determined simply by lone Wilmot N. Hess (NASA. Goddard Space Flight Center, Md. ), measurement time. M.F. p. 22-34. 34 refs. [See A65-32623 21-29]

52 A65-33292

THE ABUNDANCE OF THE ELEMENTS. Harold C. Urey CONTENTS: (California, University. La Jolla. Calif. ), p. 35-46. 33 refs. PREFACE. P. J. Brancazio (NASA. Goddard Space Flight [See A65-32624 21-30] Center, New York; Brooklyn College. Brooklyn, N.Y.) and A. G. THEORETICAL ASPECTS OF THE SPACE RELATNITY- W. Cameron (NASA, Goddard Space Flight Center; New York GYROSCOPE EXPERIMENT. L. I. Schiff (Stanford Universitv. University, New York, N.Y. ), p. v-viii. Stanford. Calif. ), p. 47-50. 10 refs. [See A65-32625 21-23] GEOLOGIC HISTORY OF SEA WATER. William W. Ruby ENERGETIC SOLAR PARTICLES. Kinsey A. Anderson (California, University. LOBAngeles. Calif.), p. 1-63. (California, University, Berkeley, Calif. ), p. 51-60. 23 refs. CONVECTION W THE EARTH'S MANTLE. Peter J. Brancario [See A65-32626 21-29] (NASA, Goddard Space Flight Center, New Yorki Brooklyn College, THE ORIGIN OF PLANETARY ATMOSPHERES. Brooklyn, N.Y.), p. 64-73. 21 refs. [See A65-33290 21-13] A. G.. W. Cameron (NASA, Goddard Institute for Space Studies, DEGASSING OF ARGON AND HELNM FROM THE EARTH. New York. N.Y.). p. 61-70. [See A65-32627 21-30] Karl K. Turekian (Yale University, New Haven, Conn.), p. 74-82. 11 refs. [See A65-33291 21-13] COMMENTS ON THE OUTGASSING OF THE EARTH. G. J. A6532627 * Wasserburg (California Institute of Technology, Pasadena, Calif. ), THE ORIGIN OF PLANETARY ATMOSPHERES. p. 83-85. A. G. W. Cameron (NASA, Goddard Institute for Space Studies, ON THE CHEMICAL EVOLUTION OF THE TERRESTRIAL New York. N. Y. j. AND CYTHEREAN ATMCSPHERES. Heinrich D. Holland (Princeton IN: SELECTIONS FROM THE TRW SPACE TECHNOLOGY LABO- University, Princeton, N.J.), p. 86-100; Discussion, p. 100, 101. RATORIES; LECTURE SERIES. VOLUME 2. 11 refs. [See A65-33292 21-30] Edited by T. L. Branigan. THE HISTORY OF GROWTH OF OXYGEN IN THE EARTH'S Redondo Beach, Calif., Space Technology Laboratories, Inc., ATMOSPHERE. L. V. Berkner and L. C. Marshall (Southwest 1965. p. 61-70. Center for Advanced Studies, Dallas, Tex.), p. 102-124; Dimcussion. Discussion of the mechanisms explaining the origin of planetary p. 124-126. 53 refs. [See A65-33293 21-13] atmospheres as due to outgassing or capture from a primitive solar THE ESCAPE OF HELIUM FROM THE EARTH',S ATMOSPHERE nebula or solar wind. Atmospheres can be lost by reverse processe Gordon J. F. MacDonald (California, University, Los Angeles. such as thermal evaporation, sweeping action of the solar wind, Calif.). p. 127-182; Discussion, p. 182. 97 refs. [See A65-33294 chemical reactions with surface materials, and the hypothetical case 21-13] of excess planetary rotational velocity. On the basis of meager data PRZMORDLAL RARE GASES IN METEORITES. Peter Signer that are available for the giant planets, it is reasonable to suppose (Minnesota. University, Minneapolis, Minn.). p. 183-190; Dis- that the bulk of their atmospheres was captured from a primitive cussion, p. 190. 12 refs. [See A65-33295 21-30] solar nebula with the 5-e composition as the sun. Hydrogen and R. 0. Pepin (California, helium would be the dominant elements. It is shown that the action ISOTOPIC ANALYSES OF XENON. University, Berkeley, Calif. ), p. 191-233; Discussion. p. 233, 234. of the solar wind would strip the moon of any atmosphere within a matter of months. Mercury can only have an atmosphere containing 28 refs. [See A65-33296 Zl-301 A. G. W. substantial amounts of molecules which can radiate efficiently. Lack INTERPRETATION OF XENON MEASUREMENTS. of knowledge about the escape mechanisms for Mars precludes any Cameron (NASA, Goddaid Space Flight Center, New York, N.Y.), [See A65-33297 21-30] definite conclusion about that planet's atmospheric composition. Ex- p. 235-247; Discussion, p. 247. 248. perimental evidence seems to indicate that the Venusian atmosphere OUTGASSING PROCESSES ON THE MOON AND VENUS. is about two orders of magnitude greater in mass than earth's. The Thomas Gold (Cornell University. Ithaca, N.Y.), p. 249-255; Discussion. p. 255, 256. [See A65-33298 21-30] latter's atmosphere is discussed in terms of the origins Of aha- spheric xenon. D. P. F. OBSERVATIONS OF WATER VAPOR ON MARS AND VENUS. A. Dallfus (Paris, Observatoire. Meudon, Seine-et-Oine. France), [See A65-33299 21-30] A6532654 p. 257-266; Discussion. p. 266-268. THE ATMOSPHERE OF MERCURY. G. Field (Princeton ABSOLUTE INTENSITY MEASUREMENTS IN THE EXTREME University. Princeton, N. J.), p. 269-276; Discussion, p. 277, ULTRAVIOLET SPECTRUM OF SOLAR RADIATION. 278. [See A65-33300 21-30] H. E. Hinteregger (USAF, Office of Aerospace Research, Cambridge THE ATMOSPHERE OF VENUS. Carl Sagan (Harvard Uni- Research Laboratories, Bedford. Mass. ). versity, Cambridge, Mass. 1, p. 279-288. Space Science Reviews, voL 4, June 1965, p. 461-497. 50 refs. THE ATMOSPHERE OF MARS, Richard M. Goody (Harvard Review of experimental results and problems of absolute intensit) University. Cambridge, Mass. ), p. 289-296; Discussion, p. 296- measurements of solar electromagnetic radiation in the EUV and 298. 6 refs. [See A65-33301 21-30] soft X-ray region of the spectrum (designated cumulatively an ARE THE INTERIORS OF JUHTER AND SATURN HOT? P. "XUV" for brevity). The numerous practical problems are divided J. E. Peebles (Princeton University, Princeton. N.J. ), p. 299- into two major areas - (11 general problems of heterochromatic 303. 5 refs. [See A65-33302 21-30] absohte XUV spectrophotometry in the laboratory and (2) specific THE ATMOSPHERE OF JUPITER. R. Wildt (Yale University. problems characteristic requirements of solar physics, the of New Haven. Corn.), p. 304, 305; Discussion, G. Field (Princeton physics of planetary atmospheres, and existing restrictions of space University. Princeton, N. J.) and G. J. Wasserburg (California technology. Within the first area, emphasis is placed on recent Institute of Technology, Passadena. Calif.). p. 305, 306. [See progress toward vstified reliance on ionization detectors without A65-33303 21-30] necessary connection to source standards. For the second area, INDEX, p. 307-314. emphasis is placed on the immediate need to have existing ex- ploratory observations followed by a new phase of more systematic experimmts of increased accuracy. (Author) M. F. A6543292 f ON THE CHEMICAL EVOLUTION OF THE TERRESTRML AND CY THEREAN ATMOSPHERES. A6533289 Heinrich D. Holland (Princeton University, Princeton, N.J.). THE ORIGIN AND EVOLUTION OF ATM-PHERES AND IN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND OCEANS; PROCEEDINGS OF A CONFERENCE, NASA, OCEANS; PROCEEDINGS OF A CONFERENCE. NASA, GODDARD GODDARD SPACE FLIGHT CENTER, GODDARD INSTITUTE SPACE FLIG~T CENTER, GODDARD INSTITUTE FOR SPACE FOR SPACE STUDIES, NEW YORK. N.Y., APRIL 8, 9, 1963. STUDIES, NEW YORK. N.Y.. APRIL 8, 9, 1963. [A65-33289 21-30] Edited by P. J. Brancazio (NASA, Goddard Space Flight Center, Edited by P. 3. Brancazio and A. G. W. Cameron. Goddard Institute for Space Studies, New York; Brooklyn College, New York, John Wiley and Sons, Inc., 1964. p. 86-100; Discussion. Brooklyn. N.Y.), and A. G. W. Cameron (NASA, Goddard Space p. 100, 101. 11 refs. Flight Center, Goddard Institute for Space Studies; New York Brief review of the history of the terrestrial atmosphere University, New York, N.Y.). and consideration of a model. mwhfied somewhat from the New York. John Wiley and Sons, Inc.. 1964. 314 p. terrestrial model. which seems to account for the presently 512.50. accepted data concerning the chemical composition of the atmoephere

53 A6 5- 3 329 8 of Venus. The data on the abundance of the nonvariable and variable A6543300 # constituents of our present atmosphere are summarized in tabular THE ATMOSPHERE OF MERCURY. form. The ratio of Xe to Si in the earth was found to be lower by G. Field (Princeton University, Princeton, N. J.). six or seven orders of magnitude than the ratio of Xe to Si in the IN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND cosmos. As it is difficult to see how the Xe in the earth's atmo- OCEANS; PROCEEDINGS OF A CONFERENCE, NASA, GODDARD sphere could be reduced by a factor of IO6; it is more reasonable SPACE FLIGHT CENTER, GODDARD INSTITUTE FOR SPACE to assume that at an arbitrary starting point, t = 0, there was STUDIES, NEW YORK, N.Y., APRIL 8, 9, 1963. [A65-33289 21-30] essentially no atmosphere. The lack of a time trend in the ratio of Edited by P. J. Brancazio and A. G. W. Cameron. ferrous to ferric iron in ancient basalts and diabases suggests that New York. John Wiley and Sons, Inc., 1964, p. 269-276; Discussion, there has been no change in the oxidation state of volcanic gases p. 277, 278. during the past 1.8 billion years. On the other hand, it is probable Description of evidence that the planet Mercury has an atmo- that the chemistry of volcanic gases was quite different very early sphere. and a tentative interpretation of this evidence. It was in the earth' s history. for a period which lasted for less than 0.5 thought that no atmosphere would exist because the escape velocity billion years, when methane, ammonia, and especially N were the of such a body (with a radius 30% greater than that of the moon, but predominant gases. There is geologic evidence that 02 was not with 4.2 times more mass) is small and the high surface tempera- abundant in the atmosphere during the second period which lasted ture approaches the critical value for the exospheric escape of light for some 1-112 billion years. During the third stage, which began dance of this element in the earth's atmosphere and its concentra- some 2 billion years ago and continued to the present, 02 content tion per gram of meteorite investigated. The phenomena relative increased chiefly due to photosynthetic processes. Similar lines to neutron capture are examined to determine in what way this of thought are developed to explain what is known about the atmo- observed discrepancy could be accounted for, and neutrons produced sphere of Venus. D.P.F. as a result of deuterium formation in the sun could account for the earth' s xenon concentration through interaction of the solar wind with the terrestrial magnetosphere. A mechanism which.captures solar xenon with great efficiency but rejects neon, helium, and other # A6543298 elements is described, based on the mass-to-charge ratio. OUTGASSING PROCESSES ON THE MOON AND VENUS. D.P.F. Thomas Gold (Cornel1 University, Ithaca, N.Y.). IN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND OCEANS; PROCEEDINGS OF A CONFERENCE, NASA, GODDARD SPACE FLIGHT CENTER, GODDARD INSTITUTE FOR SPACE STUDIES, NEW YORK, N.Y.. APRIL 8, 9, 1963. [A65-33289 21-30] A6543301 # Edited by P. J. Brancazio and A. G., W. Cameron. THE ATMOSPHERE OF MARS. New York, John Wiley and Sons, Inc.. 1964, p. 249-255; Discussion Richard M. Goody (Harvard University. Cambridge, Mass.). p. 255, 256. IN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND Analysis the phenomena related to outgassing processes on of OCEANS; PROCEEDINGS OF A CONFERENCE, NASA, GOODARD Venus and the moon. Using a terrestrial analogy for investigating SPACE FLIGHT CENTER, GODDARD INSTITUTE FOR SPACE the atmospheric conditions on Venus it is shown that the present- STUDIES, NEW YORK, N.Y., APRIL 8, 9, 1963. [A65-33289 21-30] day earth's atmosphere is really only a small by-product the of Edited by P. J. Brancazio and A. G. W. Cameron. gases that have come out of the ground; the outgassing of C02 or New York, John Wiley and Sons, Inc.. 1964, p. 289-296; Discussion, other carbon-containing gases is still in process. Applying the p. 296-298. 6 refs. analysis to Venus, the consequences of a rise in surface tempera- Discussion of information on the composition of the Martian ture to the boiling point of water are considered and it is shown that atmosphere, including data available at the time of the Goddard the greenhouse effect could lead to thermal equilibrium. Howeyer, Institute Conference. Polarimetric observations are described, surface temperature is not related to the escape of gases from the and indications of the relative abundance of CO2 were obtained by top of the Cytherean atmosphere because of the cold trap which comparing spectra of Mars and the moon. restricts the upward diffusion of water vapor. With respect to the The contributions made by Dollfus, Kaiper, de Vancouleurs, and others to the field of moon and other small bodies with no magnetic field, the effect of Martian atmospheric investigation are considered. the solar wind would effectively rule out the formation of any D.P.F. permanent atmosphere by interior-degassing phenomena. D. P. F.

A6543299 # OBSERVATIONS OF WATER VAPOR ON MARS AND VENUS. A6543302 # A. Dallfus (Paris, Obaervatoire. Meudon, Seine-et-Oise, France). ARE THE INTERIORS OF JUPITER AND SATURN HOT? IN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND P. J. E. Peebles (Princeton University, Princeton, N.J. ). OCEANS; PROCEEDINGS OF A CONFERENCE. NASA, GODDARD LN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND SPACE FLIGHT CENTER, GODDARD INSTITUTE FOR SPACE OCEANS; PROCEEDINGS OF A CONFERENCE, NASA, GODDARD STUDIES, NEW YOU, N.Y., APRIL 8, 9, 1963. [A65-33289 21-30] SPACE FLIGHT CENTER, GODDARD INSTITUTE FOR SPACE Edited by P. J. Brancazio and A. G. W. Cameron. STUDIES, NEW YORK, N.Y., APRIL 8. 9. 1963. [A65-33289 21-30] New York, John Wiley and Sons, Inc., 1964, p. 257-266; ,Discussion, Edited by P. J. Brancazio and A. G. W. Cameron. p. 266-268. New York, John Wiley and Sons, Inc., 1964, p. 299-303. 5 refs. Methods used for verifying the quantity of water vapor on Mars Investigation qf the temperatures of the interiors of Jupiter and and Venus and an analysis of the results obtained. Water vapor was Saturn based on the examination of the composition and physical measured with a 20-in. telescope and the H20 absorption band was states of their atmospheres. Information on the general structure detected by photometric rather than spectrographic methods; a bire- of the latter can be obtained from the known gravitational multipole fringent monochromatic filter was used. By tuning the filter to moments J and K. It is assumed that both Jupiter and Saturn con- give a particular transmission. the background intensity could be sist of a high-density core surrounded by a uniform mixture of H2 determined. When the transmission was changed 20 times per and He. Interpolation from the ideal gas law to the calculated second, modulation was obtained and the intensity comparisons properties of the ground states gives fairly reliable estimates of could be made photoelectrically. The intensity of the 1.4-i( band is the equations of state of hydrogen and helium. According to Aller, 80 great that in order to observe it unsaturated by terrestrial water if the planets were taken to be completely cold, the density of hy- vapor, balloon and high-mountain observations were made. For drogen in the upper layers would be so high according to the assumed Mars, the deduced and corrected value of water vapor was 1.5 x equation of state that the calculated value of the gravitational multi- 10-2 gmIcm2. FOI Venus a transmission band was chosen which pole moment for Saturn would be too large, while the indicated would completely absorb the intense C02 bands. Corrected, abundance of H2 in Jupiter would greatly exceed cosmic and solar ground-based observations on water vapor for Venus indicated a abundances. An adiabatic model with a temperature of 150°K at probable value of about 1 x 10-2 gmlcm2. with a probable error of 3 atm is considered, and sources of discrepancy between observed a factor of 2. D.P.F. and predicted K' s are suggested. D.P.F.

54 A65-34745

A6543303 t# particles suggests an explanation of a phenomenon that must be THE ATMOSPHERE OF JUPITER. accounted for by any satisfactory model of the Venus atmosphere: R. Wildr (Yale University, New Haven, COM.). the temperature at the Venus cloud surface lies near -4OOC. The IN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND positive identification of the cloud particles as water and ice OCEANS; PROCEEDINGS OF A CONFERENCE, NASA, GODDARD requires that all knowledge of terrestrial clouds be applied to the SPACE FLIGHT CENTER, GODDARD INSTITUTE FOR SPACE discussion of Venus. particularly in relation to the anomalously STUDIES, NEW YORK. N.Y., APRU. 8, 9. 1963. IA65-33289 L1-301 high microwave brightness. Terrestrial observationa show that Edited by P. J. Brancazio and A. G. W. Cameron. clouds emit nonthermal microwave radiation. M.F. New York. John Wiley.and Sons, Inc., 1964. p. 304, 305; Discussion G. Field (Princeton University. Princeton, N.J.) and G. J. Wasaer- burg (California Institute of Technology, Pasadena, Calif. 1, p. 305. 306. Ah44433 Discussion of certain aspects of Jupiter' s atmosphere, such THE INFRARED LIMB DARKENING OF VENUS. as the differential rotation between the NH3 gas and the' cloud ma- James B. Pollack (Harvard University, Harvard College Observatory. terial first discovered by Spinrad in 1962. Spectra of Jupiter taken Cambridge, Mass.) and Carl Sagan (Harvard University; Smithsonian at Victoria in 1954 also showed (as noted by Spinrad) an inclination Institution. Smithsonian Antro@ysical Observatory. Cambridge. indicative of a differential rotation of 4 km/sec, with the NH3 ro- Ma... ). tating slower than the clouds. New spectra taken recently, hwever, Journal of Geophysical Research. vol. 70, Scpt. 15, 1965, p. 4403- showed that no effect was present, which indicates that this phe- 4426. 28 refs. nomenon is time-variable. In 1963 Spinrad determined the equivalent Proposal of three general categoric. of models of the atmo- widths of a few quadripole lines of the HZ molecule in the near infra- sphere and clouds of Venus in orper to explain the observed IR limb red, which enabled the total amount of molecular H2 above the cloud darkening. In the 8- to 13-micron interval and over the observed layers to be determined. Spinrad and Trafton' s proposed working range of the cosine of the Venus smith angle, this darkening can be composition for the Jovian atmosphere is discussed. D.P.F. expressed as p , *ere p is the cosine of the zenith angle and (according to two independent seta of measurements) a is approximately equal to 0.5. For ea+ model, convective and then radiative A6543549 # equilibrium is assumed. In Models A, limb darkening is attributed MARS ROUND-TRIP MISSION ANALYSIS FOR THE 1975-1985 to de temperature gradient in an unknown. approximately gray ab- TIME PERIOD. aorber above the visible cloud deck. Other properties of the absorber. D. N. Lascody (Douglas Aircraft Go., Inc., Santa Monica, Calif. 1, required 80 that a P 0.5, render theae models rather unlikely. In E. D. Thorson, H. W. Hawthorne, and G. Markus (Douglas Air- Modela B. limb darkening is attributed to a combination of the tem- craft Co., Inc., Missile and Space Systems Div., Santa Monica, perature gradient and the angular dependence of the emissivity in Calif. ) . approximately gray multiply scattering clouds, initially with inotropic (American Institute of Aeronautics and Astronautics, Annual phase functions. In convective Model B1, agreement with observation Meeting. lst, Washington. D.C.. June 29-July 2. 1964, Paper ia secured for moderate values of do, the albedo for IR single scat- 64-403.) tering, if the douda are diffuse by terrestrial standards; high Jo Journal of Spacecraft and Rockets, vol. 2. Sept.-at. 1965, imflies more compact cloud.. The temperature range with depth, p. 775-780. 6 refs. prticle number demity. and composition of the doudsis discussed. Contract No. NAS8-11005. Moderate variation of the extinction coefficient with de@ in the Review of an analysis of the energy and gross weight require- douda has little effect on the predicted limb darkening mrthe range ments of vehicle systems whose objective is the manned exploration in p reliably observed, but closer to the limb, and for low duesof of Mars during the 1975 to 1985 period. It is seen that promising Oo, such variation may signjficzmtly influence the limb darkening. missions, selected on the basis of minimum gross-weight in Earth In radiative Model B2, high values of &lo 1.ead to predictions d the orbit. are available with long duration class transfers (800 to 1000 planetary bolometric albedo in conflict with obaervatim. Moderate days) during the entire period, but are restricted to the 1980's if dues of C0 lead to the observed limb-darkening law if the 8- to short duration (360-600 day) missions are desired. The concept of 13-micron opacity is about 2.5 thee the mean opacity, which is a multi-mission vehicle design is considered,& the vehicle's property of silicate clouds. The preceding delsare extardad to capability is determined for several synodic period.. This vehicle, anisotropic phase functions and to other values of a. An anisotropic with a constant structural weight and tank sire. is capable Of per- +sa function of the form Oo(l+ com e) increases the contribution forming round-trip missions of various durations during several of the emissivity to a by about 20%. In Modela C, the clouds coherent- synodic periods. Weight-saving techniques, such as utilizing ellip- ly redistribute radiation emitted by the underlying atmosphere. The tical orbits at Earth departure. and at Mars. planetary atmospheric absence of marked apectral features in 8- to 13-p Venus spectron- braking, and high-speed Earth entry, are evaluated with regard to copy leads to the rejection of Model C. Methods are described feasibility. weight, and cost. It is seen that resulting weight savings for removing the remaining ambiguity among the modela. are not sufficient to justify the extra complexity required in the (Author) M. F. mode of operation. A6534745 ATMOSPHERIC ELECTRICAL STUDIES OF OTHER PLANETS. A6533692 # Robert E. Holzer (California. University, Ixutitute of Geophysics THE COMPOSITION OF THE VENUS CLOUDS AND IMPLICATIONS and Planetary Physica. Los Angeles. Calif.). FOR MODEL ATMOSPHERES. IN: PROBLEMS OF ATMOSPHERIC AND SPACE ELECTRICITY; Murk Bottema. William Plummer, John Strong, and Rodolphe Zander INTERNATIONAL CONFERENCE, 3RD. MONTREUX. SWITZER- (Johns Hopkins University, Laboratory of Astrophysics and Physical LAND, MAY 5-10. 1%3. PROCEEDINGS. [A65-34713 23-13] Meteorology, Baltimore. Md. ). Conference spomored by the hternatiod Association of Meteorology Journal of Geophysical Research, vol. 70, Sept. 1, 1965. p. 4401, and Atmospheric Physics, and International Association of Geomag- 4402. 15 refs. netism and Aeronomy of the Iniernational Union of Geodesy and USAF-supported research. Geophysica. Extension of previous work on balloon observations of the atmo- Edited by S. C. Coroniti. sphere of Venus. The balloon-telescope flight of Feb. 21, 1964, Amaterdam, Elsevier Publishing Go., 1965, p. 573-576; Discussion. using reflected radiations near 1.1 p. showed that the upper Venus p. 587-596. atmosphere contains water vapor in amounts comparable to those in Dimcussion of the possibility of obtaining advance information similar levels of the earth's atmosphere. Solar radiation reflected about the electrical condition8 prevailing in the atmoapheres of by the Venus clouds in the IR spectrum region 1.7 and 3.4 c was other planets by studiea of the electromagnetic radiation emitted by measured on a subsequent flight. From the similarity between the much planets. Theme investigations would use mpcecraft outaide of curves of the Venus spectrum and of the reflection spectrum of a the ionoaphere. Obtaining much advance information on the natum laboratory ice cloud, it is concluded that Venus clouds are composed and electrical problem8 of planetary atmoapherem other than that of of ice crystals. The identification of the Venus clouds as ice the earth is necessary in view of the fact that direct electrical

55 A65-34922 measurementi on such planets are likely to be possible only within A6545112 # a number of years. D. P. F. SYSTEM DESIGN OF AN AUTOMATED LABORATORY AND ASSO- CIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORA- TION. C. E. Anderson and F. G. Beuf (General Electric Co.. Missile and Space Div., Re-entry Systems Dept., Philadelphia, Pa. ). A6544922 # International Astronautical Federation, International Astronautical~ TWILIGHT STUDIES OF PLANETARY ATMOSPHERES FROM Congress, lbth, Athens, Greece, Sept. 13-18, 1965, Paper. 34 p. SPACE SHIPS. Outline of some of the results of a company-sponsored study G. V. Rozenberg (Akademiia Nauk SSSR. Institut Fiziki Zemli. Moscow, USSR). of an integrated laboratory system which might be landed on Mars from a rocket of the Saturn V class, with a brief description Of a jAkademiia Nauk SSSR, Izvestiia, Fizika Atmosfery i Okeana. conceptual design of an entry vehicle for carrying it dmthrough vol. 1, Apr. 1965, P. 377-385.) the Martian atmosphere to a safe landing and deployment on the Academy of Sciences, USSR, Izvestiya, Atmospheric and Oceanic planetary surface. The following conclusions are drawn: (1) it ap- I, Apr. 1965, p. 223-227. Translation. pears reasonable to assume that the carrier vehicle and the AMEL see Accession no. A65-31247 20-301 (Automated Mars Exploration Laboratory) support subsystems can be developed in time for a 1973 launch date; (2) using these subsystems and a Saturn V launch vehicle, a laboratory containing up to 2400 Ib of instruments and process control equlpment could be A6544959 k landed safely on the Martian surface; (3) the surface life of the A SATELLITE METHOD FOR PRESSURE AND TEMPERATURE laboratory should be at least 2 earth years, to permit operation during one complete cycle Martian seasons; (4) in order to sample BEMW 24 KM. of most effectively, the AMEL should be capable of limited mobility on Frederick F. Fischbach (Michigan, University, High Altitude the Martian surface; (5) if Saturn V is used for this mission, it would Engineering Laboratory, Ann Arbor, Mich. ). be desirable to use its large weight-lifting capability to launch at (American Meteorological Society. Annual Meeting. 45th. New York. least two laboratories per rocket shot, thus strongly enhancing N.Y., Jan. 25-28. 1965, Paper.) mission reliability; and (6) definition the measurements which Amer,can Meteorological Society, Bulletin, vol. 46, Sept. 1965, of must be made and development of the required automated instru- 0. 528-532. ments and processing equipment appear to k among the most criti- NASA-sponsored research: cal long-lead problems. M.M. Description of an accurate and economical satellite method for measuring atmospheric pressure and temperature over the globe for altitudes below 24 km. The satellite, put into a circular polar A6545268 orbit which is sun-synchronous in a day-night plane, measures the MEASUREMENTS OF POLARIZATION AND DISTRIBUTION OF atmospheric refraction of light from various given stars. The BRIGHTNESS TEMPERATURE OF VENUS AT 10.6 CM. manner in which the resulting data can be used for density and A. D. Kuz'min and B. G. Clark (Akademiia Nauk SSSR. Fizicheskii temperature calculations is described. The sources of error in the hstitut. Moscow, USSR; California Institute of Technology. Owens method are examined, and the limitations of the system are Valley Radio Observatory. Calif. ). evaluated. P. K. (Akademiia Nauk SSSR. Doklady, vol. 161. Mar. 21, 1965, p. 551-553.) Soviet Physics - Doklady, vol. 10, Sept. 1965, p. 180, 181. Trans- lation. Detection of differential polarization of radiation emitted by dif- A6545022 ferent parts of the visible disk of Venus. Measurements of the COMPARISONS OF LABORATORY AND PLANETARY SPECTRA. brightness distribution over the surface of the planet in polarized III - THE SPECTRUM OF JUPITER FROM 7750 TO 8800 A. radiation were carried out at a wavelength of 10. 6 cm. The results Tobias Owen (Illinoin Institute of Technology. Research Institute, are shown in a graph of the difference between the visibility functions Astro Sciences Center, Chicago, Ill. ; Arizona, University. Lunar for polarization perpendicular and parallel to the effective base of and Planetary Laboratory, Tucson. Ariz. 1. the interferometer, as a function of the resolution of the inter- Astrophysical Journal, vol. 142, Aug. 15,-1965, p. 782-786. 14 refrr. ferometer. The existence of differential polarization in the radio Contract No. NRO-46-791. emission of Venus is thus established. It thus appears that most of Comparison of laboratory spectra of methane and ammonia with this emission in the 10-cm band is from a continuous medium, which a spectrum of Jupiter obtained by Kuiper and wavelengths tabulated is thought to be the surface of the planet. R. A. F. by Kiess, Corlise, and Kiess which ha8 indicated that these gases can account for a11 unidentified planetary absorptions in the spectral region 7750 to 1. 8800 A methane band that overlaps the 7900-1 A65-35360 ammonia band in the spectrum of Jupiter is held to be responsible THE ABSORPTION INTENSITY OF THE 5U3 BAND OF CARBON for the mimidentiflcation ammonia in the spectrum of Saturn. The of DIOXIDE, AND THE MARTIAN C02 ABUNDANCE AND ATMO- assignment of vibrational frequencies to the observed methane bands SPHERIC PRESSURE. remain. uncertain. (Author) M.F Philip L. Hanst and Paul R. Swan (Avco Corp., Research and Advanced Development Div., Wilmington, Mass. ). Icarus, vol. 4, Sept. 1965, p. 353-361. 9 refs. A65-35025 Recalculation of the atmospheric pressure of Mars. The THE 8-14-MICRON APPEARANCE OF VENUS BEFORE THE 1964 surface pressure of the Martian atmosphere strongly affects the CONJUNCTION. design and payload capabilities of Mars entry vehicles. The J. A. Weotphal. R. L. Wildey. and B. C. Murray (California current most widely accepted value of this surface pressure is Inititute of Technology. Paaadena, Calif. ). 25 mb. This value was determined by Kaplan, Mhch, and Spinrad Aitrophyaical Journal. vol. 142, Aug. 15, 1965, p. 799-802. based on their observations of C02 absorption lines near 8700 A Deacription of the mapping of the 8 to 14-1, radiation from and on Sinton' s ana Kuiper' s C02 observations at 2.06 Z. It 1s Venus during the period from Dec. 15, 1963 to June 6, 1964, using noteworthy that their estimated value of 25 mb is a factor of 3 or the ZOO-in. Hale telemcope. Detailed map6 for six days 6how the 4 below estimates determined both by photometric and by polari- morphology of the upper-atmosphere brightness temperature and metric techniques. A laboratory redetermination of the integrated illumtrate a number Of anomalous features near the cusps. The absorption intensity of the 5 U3 band of COz near 8700 A has been problem of atmospheric extinction and the derived brightness tern- made with a long-path technique and photomultiplier detection. perature is diacumed. The detailed brightness-temperature -ming This has resulted in a revision of the calibration used by Kaplan, of Venus in the 8 to 14-u region is maid to indicate a complex Miinch, and Spinrad. In view of the importance of the surface temporal variation in the thermal radiation from the Cytherian pressure to current studies of Mars probes, a recalculation of the atmompher e. A. B. K. pressure utilizing the new laboratory measurements is carried out.

56 .

A65-36325

The results of the analysis give a revised value of (31 f 13) m-atm that bas been reflected from the ground at least twice are hard to for the Martian COz abundance under the assumption of an effective compute, but this stream contributes less than 0. 01 to the flux and temperalure for the Martian atmosphere of 2OOOK. The surface intensity at the top of the atmosphere. If the flux and intenaity are pressure is now estimated, using this abundance value. to k (51 * compared with the corresponding quantities computed for the model 25) mb. (Author) M. F. of a Rayleigh atmosphere and Lambert ground reflection, the fluxes for the two models differ by less than 0.05, if the solar zenith angle is less than 78O; but the intensity differences become large at optical MU73 thickness less than 0.5. (Author) M.F. SOLAR SYSTEM SC~ENCE- 1964 LITERATURE SURVEY. n. Edna 0' Cannell (RAND Corp. a Santa Monica. Calif. ). Icarus. vol. 4. Sept. 1965. p. 444-459. Bibliography containing 290 entries on various astronomical subjects. The articles, the great majority of which are in English. were published in 1964 in 18 technical publication.. The entries are A6535841 # distributed among 11 main subject headings: atmospheric physic., RADIO EMISSION OF SATURN ON A WAVELENGTH OF 8 MM cosmogony. interplanetary physics. planetary biology, meteorite.. [RADIOIZLUCHENIE SATURNA NA VOLNE 8 MM]. planetary g'. Aesy, planetary geology, planetary phyaics. solar B. G. Kutuza, B. Ik Losovskii. and A. E. Salomonovich physics, solar-system dynamics, and solar-terrestrial relations. (Akademiia Nauk SSSR. Fizicheskii Institut and Institut Radio- R.A.F. tekhniki i Elektroniki. Moscow, USSR). Akademiia Nauk SSSR, Doklady. vol. 161, Apr. 21, 1965, p. 1301. 1302. 10 refs. In Russian. A6545583 Measurement of the luminance temperature of Saturn in the ULTRAVIOLET REFLECTIVITY OF MARS. millimeter range. The experiment was conducted during July and Dennis C. Evans (NASA. Goddard Space Flight Ccnter, Greenbelt. August, 1964, using a radio telescope with a normal modulation Md. 1. radiometer at 8 mm. To protect against error, the experimenters Science, vol. 149, Aug. 27, 1965. p. 969-972. 24 refs. simultaneously recorded the radio emission of Jupiter. The value Analysis of UV spectrograms of Mars (2400 to 3500 1, ... 50-A obtained for the luminance temperature of Saturn at a wavelength resolution) obtained with an objective gratiq spectrograpb cm an of 8 nun is 132 i FK. This is considered to agree well with pre- Aerobee rocket. The data indicate a reflectivity of 0.04 to 0.08 in vious values obtained for luminance temp -rature at other wave- the UV. increasing toward sbrter wavelength according to 8 Ray- lengths. R. A. F. leigh law. The data can be representcd hy a model having an atmosphere of nitrogen, carbon dioxide, and argon. and a surface prea- sure of about 5 to 20 mbar . The photographic appearance of the planet in the blue is interpreted as a loas of surface csntrast and reflectivity rather than an absorption in the atmoaphere by the "blue he." The model permits predictim of the general appearance of the planet in the photographic UV, blue. visible, and red. There A6536523 are serious biological implications since the model suggest. that MARINER IV MEASUREMENTS NEAR MARS - INITIAL RESULTS. UV radiation (ZOO0 to 3000 A) wiU reach the surface. Hugh R. Anderson (California Institute of Technology, Jet Propulsior (Author) F.R.L. Laboratory, Pasadena, Calif. ). Science, vol. 149, Sept. 10, 1965, p. 1226-1228. 6 refs. Description of the Mariner IV spacecraft and of its encounter A6545585 sequence during its approach and occultation of Mars on July 14 SATURN'S RING AND THE SATELLITES OF JUPITER - INTER- and July 15, 1%5. Measurements made of the magnetic field and the PRETATIONS OF INFRARED SPECTRA. various particle fluxes near Mars during the timn preceding picture Tobias Owen (Arizona, University, Lunar and Planetary Laborato- transmission are described, and an experiment is discussed in which ry; Kin Peak National Observatory, Tucson, Ark.). the behavior of the radio signal transmitted by the spacecraft as it -Science, voi. 149. Aug. 27. 1965, p. 974. 975. 7 refs. was occulted by Mars is used to infer properties of the planet's Contract No. NR-046-791. atmosphere. B.B. Infrared observation of Saturn's ring and the Galilean satellite. of Jupiter to extend the study of the spectra of these bodies to longei wavelengths: U. 000 1 in the caae of Saturn, and 9700 1for the Joe Satellites. The results are seen to support Kuiper' a suggestion for the composition of the ring - i.e.. thrt it is composed of water ice. The absence of the strong absorption at 8873 A in the spectra of Io, Ganymede. and Callisto leads to a new upper limit for the abundrnci A65-36325 of methane in possible atmosnheres of these satellites. F.R.L. SEARCH FOR TRAPPED ELECTRONS AND A MAGNETIC MOMENT AT MARS BY MARINER IV. J. J. O'Gallagher and J. A. Simpson (Chicago, University. Enrico Fermi Institute for Nuclear Studies. Dept. of Physics. Chicago. A6545711 # Ill. ). EFFECT OF SPECULAR GROUND REFLECTION ON RADIATION Science, vol. 149, Sept. 10, 1965, p. 1233-1239. 16 refs. LEAVING THE TOP OF A PLANETARY ATMOSPHERE. Grants No. NsG179-61; NO. AF AFOSR 521-65; Contract No. JPL- Robert S. Fraser (Thompson Ramo Wooldridge. Inc., Redondo 950615. Beach, Calif. ). Analysis of the attempt of the Mariner IV spacecraft to find American Institute of Aeronautics and Astronautics. Tbermophysics trapped electross and a magnetic moment at Mars during ita flyby Specialist Conference, Monterey. Calif. , Sept. 13-15, 1965, Paper of that planet on July 14-15. 1965. No evidence of charged-particle

65-664.~ ~. 8 n. radiation was found in the bow-shock, magnetospheric boundary, or - ~ c- Members, $0.50; nonmembers, $1.00. transition regions. In view of these results, an upper limit is NASA-supported research. established for the Martian magnetic moment, provided it is Computation of the wtward flux and intensity of scanered assumed that the same physical processes leading to acceleration radiation for the top of a i!ayleigh atmosphere that lies above a and trapping of electrons in the earth's magnetic field would be smooth water surface, which reflects radiation according to Fresnel's found in a Martian magnetic field. Accordingly, the upper limit for law. The polarization characteristics of the radiation are taken into the Martian magnetic moment is found to be 0.15 of that of the earth account. The albedo of the water is less than 0.10, if the solar for a wide range of postulated orientations with respect to the zenith angle is less than 65O. The flux and intensity at the top of rotational axis of Mars. The implications of these results for the the atmosphere are giva for several streams that compose the physical and biological environment of Mars are briefly discuamcd. radiation field. The characteristics of the stream of radiation B.B.

57 A65-36328

A65-36328 A66-15777 OCCULTATION EXPERIMENT RESULTS OF THE FIRST DIRECT * - EMISSION AND ABSORPTION OF RADIANT ENERGY IN A MODEL MEASUREMENT OF MARS'S ATMOSPHERE AND IONOSPHERE. PLANETARY ATMOSPHERE. Arvydas Kliore, Dan L. Cain, Gerald S. Levy (California Institute H. G. Myer, J. T. Ohrenberger, and T. R. Thompson (Thompson of Technology, Jet Propulsion Laboratory, Pasadena, Calif, ), Ramo Wooldridge, Inc., TRW Systems Group, Aerophysics Dept., Von R. Eshleman. Gunnar Fjeldbo (Stanford University. Center for Redondo Beach, Calif. ). Radar Astronomy. Stanford, Calif.). and Frank D. Drake (Cornel1 AlAA Journal, vol. 3, Dec. 1965, p. 2203-2210. 19 refs. University, Dept. of Astronomy, Ithaca, N. Y. ). Radiation charts are developed for a model planetary atmosphere Science, vol. 149, Sept. 10, 1965, p. 1243-1248. 8 refs. composed of 15% C02 and 8570 N2 by volume. At this time such a Grants No. NGR-05-020-065; No. NsG-377. cornposition is considered representative of the Martian atmosphere. Description of the use of coherent radio transmission to probe The effect of varying CO2 concentration in a C02-N2 atmosphere and the atmosphere and ionosphere of Mars. The refractivity and the effect of percentage of argon are studied for a specific flight con- density of the atmosphere near the surface. the scale height in the dition. Self-absorption of radiation within the gas is examined and atmosphere, and the electron density profile of the Martian iono- is found to be of considerable significance in limiting the total amount sphere are estimated. It is concluded that the atmospheric density, of radiation leaving a volume of gas. The results are applied to a temperature, and scale height are lower than previously predicted, large spacecraft for which radiant heating is determined during a as are the maximum density, temperature, scale height, and braking maneuver within the Martian atmosphere. (Author) altitude of the ionosphere. B.B.

A66-15915 # NUCLEIC ACID AND THE ORIGIN OF LIFE. Alan E. Slater. International Astronautical Federation, International Astronautical 1966 Congress, lbth, Athens, Greece, Sept. 13-18, 1965, Paper. 4 p. Calculation of the probability of a nucleic acid molecule re- producing itself in a favorable natural environment. It is seen that IAA ENTRIES the odds on the development of life on the earth arising as pure happenstance cover the range from 1041 to 1 in favor to to 1 against. depending on the initial assumptions. It is concluded that, even if the universe is finite (in size, duration or both) the possibility A66-15288 of life's beginning somewhere cannot be ruled out altogether, and THE 5U3 BAND OF CARBON DIOXIDE-R-BRANCH INTEGRATED that the fact that there is life on the earth can be logically accounted INTENSITY. for. R.A.F. Robert W. Boese, Jacob H. Miller. and Edward C. Y. Inn (NASA, Amen Research Center, Space Sciences Div., Moffett Field, Calif. ). Astrophysical Journal, vol. 142, Oct. 1, 1965, p. 1272, 1273. A66-16039 Determination of the intensity of the R-branch lines of the 5 U3 SOME EFFECTS OF THE MARTIAN ATMOSPHERE ON ELECTRO- band of C02 from the integral of the absorption coefficient. From MAGNETIC RADIATION FROM MARINER IV. measurements of the rotational lines J I 0 to J = 48 in the R-branch, H. D. Cubley and A. H. LaGrone (Texas, University. Dept. of using path lengths of 100. 200, and 400 m at a pressure of 3.1 atm Electrical Engineering, Austin, Tex. ). and a temperature of 291°K, a mean value of 0. 381 crn-lkm-lamagat- IEEE Transactions on Antennas and Propagation, vol. AP-13, is obtained. A. B. K. Nov. 1965, p. 985, 986. Grant No. AF AFOSR 766-65. A66-15415 # Investigation of the diffraction effects to be expected when the LIGHT SCATTERING IN THE ATMOSPHERES OF THE PLANETS 2300-Mc telemetry signal from Mariner IV is attenuated by the [O RASSEIANII SVETA V ATMOSFERAKH PLANET]. Martian atmosphere and blocked by the planet itself. The refractivi- I. N. Minin. ty N derived for two extreme versions of the Martian atmosphere Leningradskii Gosudar stvennyi Universitet. Astronomicheskaia (the upper and lower limits) is tabulated. The Martian ionosphere Obnervatoriia, Trudy, vol. 22, 1965, p. 39-43. 5 refs. In was considered (and found) to have negligible effect at 2300 Mc. R,,."i%". The variation in field strength observed on earth due to the occula- Derivation of approximate formulas for light passage through tion of Mariner IV by Mars was solved analytically. The determina- planetary atmospheres of finite optical thickness. taking into account tion of some of the properties of the Martian atmosphere by com- pola'rized 1iBhGcattering by aerosols and the light polarization due paring the observed and predicted diffraction curves is discussed. to reflection from the atmospheric "bottom. The formulas are M. F. suggested for use inthe ntudy of the optical properties of the Martian atmoiphere. v. 2. A66-16323 # AUTOMATED LIFE DETECTION. A66-15759 Richard S. Young (NASA, Ames Research Center. Exobiology Div., PLANETARY ATMOSPHERES. Moffett Field, Calif. ). R. Jastrow and S. I. Rasool (NASA. Goddard Space Flight Center, Astronautics and Aeronautics, vol. 3, Oct. 1965, p. 70-76. Greenbelt, Md.). Consideration of optimization criteria applicable to a choice of IN: INTRODUCTlON TO SPACE SCIENCE (Professional Edition). experiments designed to verify the existence of life on the planet Edited by W. N. Hens. Mars. The latest data relative to the Martian atmosphere and sur- New York, Gordon and Breach Science Publishers. Inc.. 1965, face conditions are reviewed. The existence bf life can be charac- p. 669-699. 16 refs. terized by growth, movement, irritability, reproduction, and Study of the properties and characteristics of the atmospheres metabolism. In view of the conditions assumed to be prevalent on of the planeta and their composition. The effect Of gravitational Mars (extreme diurnal temperature changes). it is shown that escape on the compoeition of a planet' e atmosphere is examined chemistry, metabolism. and reproduction seem to be the most in terms of density distribution in the exosphere. Temperature, suitable criteria upon which an experimental life-detection program density, and composition are the basic atmospheric data. Of these could be based. The problems related to chemical life-detection temperature is the most important because it directly reflects the tests are discussed; one of the main problems in the design of processes of absorption of solar energy which in turn determine metabolic experiments will be the selection of substrates. Heat as atmospheric structure. The probable compoeition and properties a by-product of metabolism may prove to be a more useful criterion, of the atmospheres of Mercury, Mars, Venus, and Jupiter are de- The problems connected with the identification of reproduction as a scribed. D.P.F. criterion for life are discussed. D. P. F.

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A6616404 A6617247 ATMOSPHERE OF MARS. REMARKS ON THE SHAPE OF A SPECTRAL LINE IN THE RADIA- F. S. Johnson (Southwest Center for Advanced Studies. Earth and TION DIFFUSED BY A PLANETARY ATMOSPHERE [REMARQUES Planetary Sciences Laboratory. Dallas, Tex. ). SUR LA FORME D'UNE RAIE SPECTRALE DANS LE RAYONNE- Science, vol. 150. Dec. 10. 1965, p. 1445-1448. 8 refs. MENT DIFNSE PAR UNE ATMOSPHERE PLANETAIRE]. Grant No. NsG-269-62. iacqueline Lenoble (Lille. Universite: Dgpartement de Physique. The Martian ionospheric observations made by Mariner N Laboratoire d' Optique Atmosphgrique, Lille. France). are interpreted in terms of an atmospheric model. The ion peak is Acadgmie des Sciences (Paris), Compte6 Rendus. vol. 261. no. 22, identified as an F2 peak, that is. as a maximum whose profile is Nov. 29, 1%5. p. 4633-4636. In French. controlled by ambipolar diffusion. The principal features of the Calculation of the spectral distribution of the albedo and the resulting atmospheric model are that the atmosphere consists luminance at the center of the disk for a diffusing and absorbing at- mainly of carbon dioxide, the temperature is very low, and there is mosphere. From a study of three absorption lines of various strengths, no thermosphere. Surface temperature is 210%. The tropopause using two different diffusion laws to exemplify isotropic and aniso- occurs at an altitude of 14 kilometers and has a temperature of tropic diffusion, it is found that the maximum attenuation and the line 140%. Above the tropopause, the temperature decreases with al- shape vary rapidly with the observation conditions and the diffusion titude at the rate of 0.64OC km-l, following the solid carbon dioxide law. It is emphasized that great precautions must be taken when ab- vapor-pressure curve up to 100 h,where the temperature is 85°K; sorption lines appearing in the spectrum of a planet wlth a diffwsing at higher altitudes the temperature is isothermal. (Author ) atmosphere are used to evaluate temperature or pressure. A. B. K.

A616436 THE ELECTROMAGNETIC PROPAGATION CHARACTERISTICS OF VENUS AND MARS. Charles E. Francis (Bell Aerospace Gorp., Bell Aerosystems COO. A6617891 # Tucson Research Laboratory, Tucson, Arie.). EXPERIMENTAL ASSESSMENT OF THE EFFECT OF LARGE IEEE, Proceedings, vol, 53. Sept. 1965, p. 1216-1221. 24 refs. AMOUNTS OF ARGON IN A PLANETARY ATMOSPHERE ON Examination of the information available about Mars and Venus. STAGNATION-POINT CONVECTIVE HEATING. and their atmospheres, to determine the electromagnetic propaga- T. E. Horton and T. L. Babineaux (California Institute of Technol- tion characteristics of the two planets. Consideration of some ogy. Jet Propulsion Laboratory, Pasadena, Calif. 1. preliminary model atmospheres indicates that the electromagnetic American Inshtute of Aeronautics and Astronautics. Aerospace propagation effective radius of Venus is between 7400 and 13,900 Sciences Meeting, 3rd. New York. N. Y., Jan. 24-26. 1%6, km. Other models, which give even larger effective radii and lead Paper 66-29. 16 p. 27 refs. to the limit of a plane surface, are discussed. The troposphere Of Members, $0.50; nonmembers, $1.00. Mars, because of its low density, is shown to have essentially no Hypersonic stagnation-point convective-heat-transfer data effect on the propagation loss between points on the surface or near were obtained utilizing an arc-heated shock tube to simulate flight the surface. An examination of the knowledge of the dielectric velocities ranging from 18.000 to 34,000 fps. The mixtures in- constants and conductivities of the surface revealed considerable vestigated consisted of 65% C02-35% A, 30% CO2-40% N2-30% A. and uncertainties. Measured values of the dielectric constant are 9% C02-90% N2-1% A. In addition. tests were conducted in air to between 2.2 and 7.1 for the Venusian surface. The conductivity establish a base to which the heating rates in the above mixtures is probably 10-3 mhoslmeter or less for both the Venusian and could be compared. The results of this investigation indicate an Martian surfaces. if they have compositions similar to dry terrestrial increase in heat transfer in the atmospheric mixtures containing soil. No measurement of the dielectric constant of the surface of large amounts of argon for the flight range where ionization be- Mars has been published. Mars and Venus are strongly believed to comes significant. For the 30% C02-40% N2-30% A mixtures this have ionospheres in their atmospheres, but only crude estimations increase, above the values obtained in air, was about 10%; while, are available for the electron densities and the altitudes of these for the 65% C02-35.% A mixture the values of the heat-transfer ionospheres. (Author) parameter were about 251.above those of air and 15% absve'theoretical values. In the Martian entry range below 25,000 fps, the ionization is not significant and heat-transfer rates are similar to AM-16625 those in the non-argon atmospheres. (Author) RADIOASTRONOMICAL STUDIES AND THE IONOSPHERE OF VENUS. A. D. Danilov (Akademiia Nauk SSSR, Institut Prikladnoi Geofiziki, Moscow. USSR). (Akademiia Nauk SSSR, Doklady, vol. 162. June 1. 1965. p. 774-777. Soviet Physics - Doklady, vol. 10, Dec. 1965, p. 483-486. 17 refs. A6617900 # Translation. THE MARINER 4 OCCULTATION EXPERIMENT - SUMMARY OF [For abstract see issue 17. page 2550, Accession no. A65-277711 DATA AND REDUCTIQN METHODS. D. L. Cain, A. J. Kliore, and G. S. Levy (California Institute of Technolony. Jet Propulsion Laboratory, Pasadena, Calif. ). AS17174 # -.~ THE NATURE OF RADIO-NOISE EMISSION FROM THE SURFACE American Institute of Aeronautics and Astronautics. Space Sciences OF VENUS [0 PRIRODE RADIOSHUMOVCGO IZLUCHENLIA Meeting, 3rd. New York, N.Y., Jan. 24-26. 1966. Paper 66-148. POVERKHNOSTI VENERY 1. lop. 7 refs. V. M. Vakhnin and A. I. Lebedinskii. Members, $0.50; nonmembers, $1.00. Kosmicheskie Issledovaniia, vol. 3, Nov. -Dec. 1965, p. 917-926. Brief review of the Mariner 4 occultation experiment. which 17 refs. In Russian. used the changes in amplitude and frequency of the tracking and Discussion of a model for the radio-noise emisslon of Venus telemetry signal to yield data about the atmosphere of Mars. The which explains the high level of this emission (600 to 700°K) in experiment required the measurement of frequency to tenths of a terms of "quiet" or "glow" discharges that take place in the upper cps in a signal of 2.3 x 109 cps. This accuracy was made possible atmosphere of Venus and cause an increase in the true thermal by use of the JPL/NASA Deep Space Instrumentation Facility (DSIF), radio emission by 200 to 300°K. An explanation of the development comprising two stations at Goldstone, California and two in Aus- of atmospheric glow discharges, instead of thunderstorm phenomena tralia. The two types of data taken during the intervals of time charactenstic of the earth's atmosphere, is seen in the very slow preceding and following the occultation of the spaceflaff consisted rotation of the planet and the associated intense but hardly turbulent of the received spacecraft signal, processed through two types of atmospheric circulation. Calculations of the efficiency of Solar receiver systems which are briefly described. Methods of reduc- thermal energy ConversLon to radio noise (stepwise: first into ing the audio recorded and phase lock data are discussed, and energy of atmospheric circulation and then into electric-current associated computer programs are described. Some results of energy) are seen to support the model proposed. V.P. their application are presented. F. R. L.

59 A66- 1 8054

A6618054 with moderate to high eccentricity can cause significant changes in WATER VAPOR IN THE ATMOSPHERE OF VENUS. pericenter height for certain orientations of the satellite orbit, Murk Bottema, William Plummer. and John Strong (Johns Hopkins potentially lowering it sufficiently to drastically shorten the lifetime, University, Laboratory of Astrophysics and Physical Mbteorology, Baltimore, Md. ). or raising it and increasing the satellite's lifetime. While Martian oblateness doen not affect the pericenter height directly, it can, by Ruimtevaart, vol. 14, Dec. 1965, p. 197, 198. acting a8 a secondary effect, radically alter the character of the USAP-supported research. solar perturbation. Low inclination orbits tend to minimize these Determination of the water vapor content in the atmosphere of changes. However, the initial plane a Martian satellite can be Venus above the reflecting cloud layer using an automatic daytime of no @electedthat the solar perturbations increase the pericenter telescope with an aperture 30 cm carried aloft by a balloon to of altitude to a large extent over most, if not all, of the mission. an altitude of 26.5 km. Radiation was measured in the band at (Author) 1.13 p With a grating spectrometer of 2-A resolving power. This portion of the spectrum was scanned once every 10 sec with a set of 21 exit slits.arrayed to match 21 water absorption-line groups. AM-19072 # Based on the experimental evidence of 120 recordings, it is found INTERPRETATION OF LOW RESOLUTION SPECTRA OF MARS that water. content on Venus is the same as that produced by IN THE 2p REGION. 9. 8 x gm/Cm2 of water vapor at atmospheric pressure. The L. D. Gray (California, University, Dept. of Engineering, Los interpretation of the measured absorption requires certain assump- Angeles, Calif. ). tions about the pressures to be expected at and above the Venus American Institute of Aeronautics and Astronautics. Aerospace cloud top level and the distribution of water vapor in this region. Sciences Meeting, 3rd. New York. N.Y., Jan. 24-26, 1966, D. P. F. Paper 66-147. 12 p. 29 refs. Members, $0.50; nonmembers, $1.00. A6618055 Observation of the carbon dioxide absorption bands located at 2 &I. in the atmosphere of Marts. At a given temperature the trans- COMPOSITION OF THE CLOUDS OF VENUS. Murk Bottema, William Plummer, John Strong, and Rodolphe mission of these bands ie a function only of theproduct mp, where m is the amount of CO2 and p ii the "effective" surface pressure. Zander (Johns Hopkins University. Laboratory of Astrophysics The random Elsasser band model is used to calculate the transmis- and Physical Meteorology, Baltimore, Md. ). Ruimtevaart, vol. 14, Dec. 1965, p. 198, 199. sion of the 2-p bands both for homogeneous path lengths and for real atmospheric paths where the temperature and pressure vary con- USAF-supported research. tinuously. The calculated transmission is in excellent agreement Measurements of the reflection spectrum of the clouds in the with published laboratory measurements and with the transmission atmosphere of Venus covering the 1.7 to 3.4 )r region, with a re- Agreement with observations solving power of about 0. 08 p. using a 30-cm-aperture telescope observed for the earth's atmosphere. carried aloft by a helium balloon to an altitude of 26.2 km. The of the transmission of theMartian atmosphere is obtained using telescope wan directed toward Venus by offset nun tracking and value. of mp I 500 i 100 m-atm-mb for one "air" mass. The best automatic guiding. A coarne grating was used to produce a low- current estimates indicate the amount of CO2 in the atmosphere dinparsion spectrum; a germanium filter was used to isolate the of Mars is 60 to 85-m-atm. If the amount is 85 m-atm. the cal- first order, and the energy fell upon three adjacent indium arsenide culations described indicate an atmosphere of pure CO2 and a sur- detectors. Theobservations were extendedover a periodof 3-114 hr. face pressure of 6 mb. If m D 60 m-atm, agreement with experi- Based upon the results of a comparison between the observational mental data can be obtained for various model atmospheres covering data and the reflection spectra of liquid water, ice, and other mte- the range 42% COz, 58% Ar, with a surface pressure of 10 mb. to rials at various temperatures in the laboratory, it is concluded that 100% GOz. with a surface pressure of 4.4 mb. Thus the Martian the reflecting cloud layer of Venus is composed of particles of iurface pres8ure appear9 to be in the range of 4 to 10 mb. M.F. frozen water. D. P. F.

AM-18788 A66-19262 MEASUREMENTS OF MARS AT A 3.75 CM FROM FEBRUARY TO STABILITY OF SULFUR COMPOUNDS ON VENUS. JUNE.-. 1965. Robert F. Mueller (Chicago, University, Dept. of Geophysical W. A. Dent, M. J. Klein, and H. D. Aller (Michigan. University, Sciences, Chicago, Ill.). Radio Astronomv Observatorv, Ann Arbor, Mich. ). Icarus, vol. 4, Dec. 1965, p. 506-512. 23 refs. Astrophysical Journal, vol. 142, Nov. 15, 1965. p. 1685-1688. 9 refs NSF Grant No. GP-2062, Contract No. Nonr-1224(61). The abundances of the major sulfur compounds in the lower Discussion of a series of observations made to obtain a more atmosphere of Venus have been calculated assuming equilibrium accurate brightness -temperature measurement of Mars and to place between the atmospheric gases and the mineral phases CaSO4, an upper limit to the variation of the brightness temperature with CaSi03, SiOz. Fe304, FeS, and FeS2. Various combinations of Tlanetary phase. A possible variation of the Martian disk tempera- these phases form stable assemblages under different conditions mre with phase was investigated by computing the daily average of oxidation while certain other assemblages are excluded. By temperatures and tabulating them. These data are plotted as a func- analogy with Earth, it is expected that iron will be more abundant tion of planetocentric phase angle. M. M. than sulfur in the Venus crust, and this should result In iron compounds controlling the degree of oxidation as well as the abundances of the sulfur compounds. Maximum surface fugacities in atmo- A&6-18987 * spheres for the major sulfur species at the mean temperature of LONG LIFETIME ORBITS ABOUT MARS. 700°K and all oxidatidn conditions are as follows: P~~"lo-~, Richard L. ~011and Martin A. Krop (Lockheed Aircraft Gorp., ~~~~-1ol.6,Pso3-10-6, and PH2S-10-Z.5 with PH~Sthe least Lockheed Mis8ilei and Space Co., Aerospace Sciences Laboratory, certain of these values. A further critique of some existing views Palo Alto, Calif. 1. on the atmospheric chemistry of Venus is also presented. and it is American Inntitute of Aeronauticn and Antronautics, Aerospace concluded that these views are in contradiction with'existing observa- Science8 MeetinR, 3rd. New York, N. Y., Jan. 24-26, 1966, tional data and the theory of the interaction model. (Author) Paper 66-35. 16 p. 8 refn. Msmber8, $0. 50; nonmembern, $1.00. Atmomphsric drag. nolar gravitational perturbations, planetary oblatenenn, and other perturbations that affect the lifetime of a Mars AM-19322 orbiter iatellite are dencribed. Their influence upon realistic missio PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZXI]. trajectory ielection in analyzed for an orbiter having at least a Edited by I. K. Koval' (Akademiia Nauk Ukrainskoi SSR, Glavnaia fifty-year lifetime. Satellite lifetime estimates based on nevera1 Astronomicheskaia Obsezvatorila, Kiev, Ukrainian SSR). atmowphbric models for a wide range of pericenter heights and (Soveshchanre Raborhel Gruppy PO lssledovdnllu Atrnosfer Venery I orbital eccentricities indicate that drag effects are iignificant only Marsa, Kiev, Ukralnlan SSR. June 1964. ) for very low orbiti. Solar gravitational perturbations on orbits Kiev, Izdatel' S~VONaukova Dumka. 1965. 168 p. In Russian.

60 A66- 1 9325

CONTENTS: MARS BY THE INDICATOMETRIC METHOD [PROVERKA GIPOTEZY INTRODUCTION [WEDENIE]. p. 5. LIMONITOVOGO POKROVA NA MARSE INDIKATOMETRICHESKIM SPECTROSCOPIC STUDIES OF THE COMPOSlTION OF THE PUTEM]. T. D. Bessonwa (Leningradskii Gosudarstvennyi CYTHEREAN ATMOSPHERE [SPEKTROSKOPICHESKIE ISLE- Universitet. Leningrad, USSR). p. 105-109. 6 refs. [See DOVANIIA SOSTAVA ATMOSFERY VENERY]. V. K. Prokof'ev A66-19334 08-30] (Akademiia Nauk SSSR, Partizanskoye. Ukrainian SSR). p. 6-11. POLARIZATION INVESTIGATIONS OF THE RADIOEMISSION [See A66-19323 08-30] OF THE UPPER LAYERS AND MANTLES OF PLANETARY SUR- LUMINESCENCE OF THE NIGHT SKY OF VENUS [SVECHENIE FACE5 [WLXARIZATSIONNYE ISSLEDOVANIJA RADIOIZLUCHENlu NOCHNOGO NEBA VENERY]. N. A. Kozyrev (Akademiia Nauk VERKHNECO SLOLA I POKROVOV POVERKHNOSTI PLANET]. SSSR, Pulkovo. USSR), p. 12. 13. A. E. Basharinov, M. A. Kolosov. and A. A. Kurskaia (Akademiia SOME ASPECTS OF THE IONOSPHERIC HYFOTHESIS FOR NaukSSSR. Moscow, USSR), p. ll0, lll. RADIO EMISSION FROM VENUS [K VOPROSU OB IONOSFERNOI MULTICOLOR POLARIMETRY OF THE LIGHT OF THE GIPOTEZE RADIOIZLUCHENIIA VENERY]. A. D. Danilw and TWILIGHT AND DAYTIME SKY AT THE ZENITH [MNOGOTSYETNAIA S. P. Iatsenko (Glavnoe Upravlenie Gidrometeorologicheskoi POLIARIMETRILA SVETA SUMERECHNOGO I DNEVNOM NEBA Sluzhby, Moscow, USSR), p. 14-20. 15 refs. [See A66-19324 08-30] V ZENITE]. V. V. Avramchuk (Alcademiia Nauk Ukrainskoi SSR. EFFECT OF THE CLOUD COVER OF VENUS ON THE Kiev, Ukrainian SSR), p. ll2-120. [See A66-19335 08-13] PLANET'S RADIO EMISSION IN THE CENTIMETER AND MIL- INTENSITY -TYPE MICROHIOTOMETER DEVELOPED ON LIMETER RANGE [0 VLIIANII OBLACHNOGO POKROVA VENERY THE BASIS OF THE MF-4 [MIKROFOTOMETR INTENSNNOSTEI NA EE RADIOIZLUCHENIE V SANTIMETROVOM I MILLIMETROVOM NA BAZE MF-41. L. A. Bugaenko and K. E. Skorik (Akademiia DIAPAZONAKH VOLN]. G. M. Strelkov (Akademiia Nauk SSSR. Nauk Ukrainskoi SSR, Kiev, Ukrainian SSR). p. 121-126. [See Moscow, USSR), p. 21-46. 58 refs. [See A66-19325 08-30] A66-19336 08-14] RESULTS OF PRELIMINARY PROCESSING OF CERTAIN DETERMINATION OF THE OPTICAL PARAMETERS OF THE SPECTROGRAMS OF VENUS OBTAINED IN APRIL, 1964 MARTIAN ATMOSPHERE AND SURFACE TAKING INTO ACCOUNT [REZUL' TATY PREDVARITEL'NOI OBRABOTKI NEKOTORYKH ANISOTROPIC SCATTERING [OB OPREDELENII OPTICHESKMH SPEKTROGRAMM VENERY, POLUCHENNYKH V APRELE 1964 G. 1.- PARAMETROV ATMOSFERY I POVERKHNOSTI MARSA PRI V. V. Avramchuk and I. K. Koval' (Akademiia Nauk Ukrainskoi UCHETE ANIZOTROPII RASSEIANIIA]. A. V. MorolhmLo and SSR. Kiev, Ukrainian SSR). p. 47-51. [See A66-19326 08-30] E. G. Ianovitskii (Akademiia Nauk Ukrainskoi SSR, Kiev. OPTICAL PROPERTIES OF THE MARTIAN ATMOSPHERE Ukrainian SSR ), p. 127-131. 10 refs. [See 666-19337 08-30] ACCORDING TO THE RESULTS OF PHOTOMETRIC OBSERVA- TIONS [OPTICHESKIE SVOISTVA ATMOSFERY MARSA PO DANNYM FOTOMETRICHESKIKH NABLIUDENII]. N. P. Barabashov (Khar' kovskii Gosudarstvennyi Universitet, Kharkov, Ukrainian A66-19323 # SSR), p. 52-60. 15 refs. [See A66-19327 08-30] SPECTROSCOPIC STUDIES OF THE COMPOSITION OF THE CERTAIN REMARKS ON HYPOTHESES OF AN ABSORBING CYTHEREAN ATMOSPHERE [SPEKTROSKOPICHESKIE ISSLE- ATMOSPHERE ON MARS [NEKOTORYE ZAMECHANIIA PO DOVANIIA SOSTAVA ATMOSFERY VENERY]. VOPROSU 0 GIPOTEZAKH POGLOSHCHAIUSHCHEI ATMOSFERY V. K. Prokof'ev (Akademiia Nauk SSSR. Krymskah Aatrofizichemkaia NAMARSE]. V. V. Sharonov, p. 61-71. 28 refs. [See Obsehratoriia. Partizanskove..- Ukrainian SSR). A66-19328 08-30] (Soveshchanie Rabochei Gruppy po Issledwaniiu Atmomfer Venery i MODEL OF THE ATMOSPHERE AND SURFACE OF MARS Marsa. Kiev, Ukrainian SSR, June 1964. ) FROM THE STANDPOINT OF A PURELY SCATTERING ATMO- IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZW]. SPHERE [MODEL' ATMOSFERY 1 POVERKHNOSTI MARSA S E&ted by I. K. Koval'. TOCHKI ZRENIIA GIPOTEZY CHISTO RASSEIVAIUSHCHEI Kiev, Izdatel' stvo Naukwa Dumka. 1965. p. 6-U. In RUm8ian. ATMOSFERY]. V. V. Sharonw, p. 72-78. 13 refs. [See Discussion of a possible composition of the atmosphere of Venua A66-19329 08-30] in the light of available apectral data. Theories concerning nitrogen CERTAIN CONSIDERATIONS CONCERNING THE AEROSOL as a likely basic component are presented and observations are noted COMPONENT OF THE MARTIAN ATMOSPHERE [NEKOTORYE that give some slight evidence for the presence of oxygen and water SOOBRAZHENLLA PO POVODU AEROZOL' NO1 SOSTAVLIANSHCHEI vapor on Venus. The possible existence of traces of formaldehyde ATMOSFERY MARSA]. N. N. Sytinskaia (Leningradskii Gosu- is indicated. V.Z. darstvennyi Universitet, Leningrad, USSR), p. 79-81. [See X46-19330 08-30] AEROSOL COMPONENT OF THE ATMOSPHERE OF MARS A66-19324 * [OB AEROZOL'NOI SOSTAVWUSHCHEI ATMOSFERY MARSA]. SOME ASPECTS OF THE IONOSPHERIC HYPOTHESIS FOR RADIO E. G. Ianovitskii (Akademiia Nauk Ukrainskoi SSR. Kiev, EMISSION FROM VENUS [K VOPROSU OB IONOSFERNOI GIPOTEZE Ukrainian SSR). p. 82-90. 18 refs. [See A66-19331 08-30] RADIOIZLUCHENIIA VENERY]. COLOR OF MARS AS A RESULT OF THE OPTICAL CHAPAC- A. D. Danilov and S. P. Iatsenko (Glavnoe Upravlenie Gidrometeoro- TERISTICS OF ITS ATMOSPHERE [TSVET MARSA, KAK REZUL'TA loiicheskoi Sluehby. Institut Prikladnoi Geofiziki. Moscow. USSR). .OPTlCHESKIKH SVOISTV EGO ATMOSFERY]. N. A. Kozyrev (Akademiia Nauk SSSR, Pulkovo, USSR), p. 91, 92. CHEMICAL COMPOSITION, PRESSURE, AND TEMPERATURE OF THE ATMOSPHERE OF MARS ACCORDING TO INFRARED Edited by I. K. Kwal' . SPECTROSCOPY DATA [KHIMICHESKII SOSTAV. DAVLENIE I Kiev, Izdatel'stvo Naukova Du?nka. 1965. p. 14-20. 15 refs. TEMPERATURA ATMOSFERY MARSA PO DANNYM INFRAKRASNOI In Russian. SPEKTROSKOPII]. V. 1. Moroz (Gosudarstvennyi Astronomicheskii Discussion of Strelkov's theory of radio emission from Venus Institut. Moscow. USSR). p. 93. that holds radioactive heating of the planet's surface to be the cauae BRIEF ANALYSIS OF A PHOTOMETRIC STUDY OF THE of the high temperature of its radiation in the centimeter band. This BRIGHTNESS DISTRIBUTION ALONG THE DISK OF X4RS theory is viewed more favorably than others - e. g. I the ionospheric, [KRATKII ANALIZ FOTOMETRICHESKOGO IZUCHENIIA "greenhouse. It or neon theory (Suess) - since it does not require the RGPREDELENIIA IARKOSTI PO DISKU MARSA]. I. K. Koval' hypothesis of a strong greenhouse effect or a strong ionosphere with (Akademiia Nauk Ukrainskoi SSR, Kiev, Ukrainian SSR), p. 94-98. the attendant difficulties. v. 2. 9 refs. [See A66-19332 08-30. CHECK ON THE HYPOTHESIS OF THE LIMONITIC COVER OF BY SPECTROPHOTOMETRIC DATA [PROVERKA GIPOTEZY AM-19325 * LIMONITOVOCO POKROVA NA MARSE PO DANNYM SPEKTRO- EFFECTOFTHE CLOUDCOVEROFVENUSONTHEPLANET'S FOTO)*IETRII]. I. 1. Lebedeva (Leningradskii Gosudarstvennyi RADIO EMISSION IN THE CENTIMETER AND MILLIMETER Universitet. Leningrad, USSR). p. 99-104. 19 refs. [See RANGE [0 VLIIANII OBLACHNOGO POKROVA VENERY NA EE A66-19333 08-30] RADIOIZLUCHENIE V SANTIMETROVOM I MILLIMETROVOM CHECK ON THE HY WTHESIS OF THE LIMONITIC COVER OF DIAPAZONAKH VOLN].

61 A66- 19327

G. M. Strelkov (Akademiia Nauk SSSR, Institut Radiotekhniki i Review of the current state of the problem of applying photo- Elektroniki, Moscow, USSR). metric data to the clarification of the nature of Mars. A principle (Soveshchanie Rabochei Grupp PO Issledovaniiu Atmosfer Venery i for selecting a model of the atmosphere and surface of Mars is Marsa, Kiev, Ukrainian SSR, ',,ne 1964. )- proposed, according to which the models closest to terrestrial con- IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZIKI]. ditions are considered as most probable. From this standpoint. a Edited by I. K. Koval' . model in which the visible part of the spectrum of the atmosphere Kiev, Izdatel' stvo Naukova Dumka, 1965, p. 21-46. 58 refs. is assumed to be purely scattering, while the surface is covered In Russian. with limonitic dust is regarded as being most probable. A. B. K. Development of an atmospheric model of Venus with a chemical composition and a vertical profile of pressure and temperature based on astronomical observations at radio frequencies and in the visible and near IR spectral bands. The spectral characteristics of the AM-19330 planet's radio brightness temperature are given a thorough theo- * CERTAIN CONSIDERATIONS CONCERNING THE AEROSOL COM- retical analysis. The theoretical and experimental values of these PONENT OF THE MARTIAN ATMOSPHERE [NEKOTORYE characteristics are compared in order to verify the validity of the SOOBRAZHENIIA PO POVODU AEROZOL' NO1 SOSTAVLIARTSHCHEI model. v. z. ATMOSFERY MARSA]. N. N. Sytinskaia (Lenhgradskii Gosudarstvennyi Universitet, Astronomicheskaia Observatoriia, Leningrad, USSR). (Soveshchanie Rabochei Grupp o Issledovaniiu Atmosfer Venery i AM-19327 s MXKiev, Ukrainian SSR. ',:ne 1964. ) OPTICAL PROPERTIES OF THE MARTIAN ATMOSPHERE AC- IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZIKI]. CORDING TO THE RESULTS OF PHOTOMETRIC OBSERVATIONS Edited by I. K. Koval' . [OPTICHESKlE SVOISTVA ATMOSFERY MARSA PO DANNYM Kiev, Izdatel' stvo Naukova Dumka, 1965, p. 79-81. In Russian. FOTOMETRICHESKIKH NABLIUDENII]. Discussion of certain problems arising in connection with the N. P. Barabashov (Khar'kovskii Gosudarstvennyi Universitet, need to separate the gas and aerosol components in the brightness Astronomicheskaia Observatoriia. Kharkov. Ukrainian SSR ). of theatmospheric layer in the case of photometrically obtained data (Soveshchanie Rabochei Gruppy PO Issledovaniiu Atmosfer Venery i pertaining to the Martian atmosphere. It is pointed out that, since no Marsa, Kiev, Ukrainian SSR, June 1964. ) sufficiently reliable methods have been proposed for this separation, IN: PROBLEMS OF ASTROPHYSICS fVOPROSY ASTROFIZIKI1. it would be interesting to reverse the problem and, using the pres- Edited by I. K. Koval' . sure values determined by other methods, study the content of the Kiev, Izdatel' stvo Naukova Dumka, 1965, p. 52-60. 15 refs. suspended particles photometrically. A. B. K. In Russian. Analysis of the results of photometr'ic observations of Mars carried out on the basis of the theory of light scattering in planetary atmospheres. It is shown that the optical thickness of the Martian at- AM-19331 mosphere is most probably low and that this atmosphere possesses * AEROSOL COMPONENT OF THE ATMOSPHERE OF MARS [OB chiefly scattering properties in the visible part of the spectrum. AEROZOL' NO1 SOSTAVLIAIUSHCHEI ATMOSFERY MARSA]. The true absorption is found to increase in the short-wave part of E. C. Ianovitskii (Akademiia Nauk Ukrainskoi SSR. Glavnaia the spectrum, although the optical thickness of the atmosphere is Astronomicheskaia Observatoriia, Kiev, Ukrainian SSR). relatively small in this case too. Many areas in the maria are found (Soveshchanie Rabochei Gruppy PO Issledovaniiu Atmosfer Venery i to havea greenish tint. A. B. K. Marsa. Kiev, Ukrainian SSR, June 1964. ) IN: PROBLEMS OF ASTROPHYSlCS [VOPROSY ASTROFIZIKI]. Edited by I. K. Koval' . AM-19328 * Kiev, Izdatel'stvo Naukova Dumka, 1965, p. 82-90. 18 refs. CERTAIN REMARKS ON HYPOTHESES OF AN ABSORBING ATMO- In Russian. SPHERE ON MARS [NEKOTORYE ZAMECHANIIA PO VOPROSU 0 Explanation of the difference between the values obtained for GIPOTEZAKH POGLOSHCHAIUSHCHEI ATMOSFERY NA MARSE]. atmospheric pressure at the Martian surface obtained from photometric and polarimetric observations and those obtained by spec- V... V... Sharonov.~ ~ (Soveshchanie Rabochei Gruppy PO Issledovaniiu Atmosfer Venery i troscopic means. It is suggested that the difference arises because Marsa, Kiev, Ukrainian SSR, June 1964. ) the error due to light scattering by aerosol particles with radii IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZIKI] . r < 10-6 cm is not taken into account in photo- and polarimetric ob- Edited by I. K. Koval' . servations. The number of aerosol particles of radii on the order Kiev, Izdatel' stvo Naukova Dumka, 1965, p. 61-71. 28 refs. In of 10-6 cm in a column of the Martian atmosphere with a base of Russian. 1 cm2 is 1015 cm-2. It is shown that the saturation of the Martian Critical review of models of the atmosphere and surface of atmosphere with fine aerosol particles per unit mass of atmosphere Mars in which the atmosphere is assumed to be absorbing and not is much higher than that of the earth' s atmosphere. R.A. F. scattering, whereby the red color is ascribed to selective absorption in the atmospheric layer. The hypothesis of Carrer and the Kiesses, ascribing selective extinction to the presence of nitrous oxide in the Martian atmosphere, is said to be unacceptable in view AM-19332 * BRIEF ANALYSIS OF A PHOTOMETRIC STUDY OF THE BRIGHT- of the fact that the absorption band of this compound in the planet's NESS DISTRIBUTION ALONG THE DISK OF MARS [KRATKII spectrum is absent or very weak. Kozyrev's conception is said to ANALIZ FOTOMETRICHESKOGO IZUCHENIIA RASPREDELENIIA be contradicted by the observed brightness distribution along the IARKOSTI PO DEKU MARSA]. I. K. Koval' (Akademiia Nauk Ukrainskoi SSR, Glavnaia Astrono- micheskaia Observatoriia, Kiev, Ukrainian SSR). AM-19329 t# (Soveshchanie Rabochei Gruppy Issledovaniiu Atmosfer Venery i MODEL OF THE ATMOSPHERE AND SURFACE OF FROM PO MARS Marsa. Kiev, Ukrainian SSR. June 1964. 1 THE STANDPOINT OF A PURELY SCATTERING ATMOSPHERE IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZIKI]. [MODEL' ATMOSFERY I POVERKHNOSTI MARSA S TOCHKI Edited by I. K. Koval'. ZRENIIA GlPOTEZY CHISTO RASSEIVAIUSHCHEI ATMOSFERY]. Kiev, Izdatel' stvo Naukova Dumka, 1965, p. 94-98. 9 refs. V. V. Sharonov. In Russian. (Soveshchanie Rabochei Cruppy PO lsaledovamiu Atmosfer Venery 1 Analysis of investigations of Martian limb darkening. It is noted Marsa, Kiev. Ukrainian SSR. June 1964. ) that the great amount of accumulated photometric data is of low ac-

IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZIKII.~ ~~~~ curacy due to the observers' failure to allow for the effect of image Edited by I. K. Koval' . vibration. It is therefore difficult to use these data for a study of Kiev, Izdatel'stvo Naukova Dumka, 1965, p. 72-78. 13 refs. the variations in the aerosol component of the Martian atmosphere. In Russian. R. A. F.

62 A66-20101

A66-19333 where separation occurs between two distinct phases of the multi- CHECK ON THE HYPOTHESIS OF THE LIMONITIC COVER OF component atmosphere which have the same density but different MARS BY SPECTROPHOTOMETRIC DATA [PROVERKA GIPOTEZY compositions. The "red spot phase" would be buoyantly neutral LIMONITOVOGO POKROVA NA MARSE PO DANNYM SPEKTRO- with respect to its surroundings - a thermodynamic Cartesian diver. FOTOMETRII]. Possible hydrodynamic effects of separation between fluid phases L I. Lebedeva (Leningradskii Gosudarstvennyi Universitet. Astro- in a multicomponent gas are discussed. P.K. nomicheekaia Observatoriia, Leningrad, USSR). (Soveshchanie Rabochei Gruppy po Issledovaniiu Atmosfer Venery i Marsa, Kiev, Ukrainian SSR. June 1964. ) IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZW]. A619793 # Edited by I. K. Koval' . POSITION OF THE EQUATORIAL BOUNDARY OF ABNORMAL Kiev, Izdatel' stvo Naukova Dumka, 1965. p. 99-104. 19 refs. IONIZATION OCCURRENCE FOR VARIOUS LEVELS OF PLANE- In Russian. TARY MAGNETIC ACTIVITY [POLOZHENLE EKVATORIAL'NOI Comparison of the spectral reflecting power curve (corrected GRANITSY OBLASTI POIAVLENIIA ANOMAL'NOI IONIZATSII for atmospheric effects) for the continents in the center of the Martian V ZAVISIMOSTI OT PLANETARNOI MAGNITNOI AKTIVNOSTI]. disk with the same curves for terrestrial samples. Observations L. A. Iudovich (Akademiia Nauk SSSR, Institut Zemnogo Mag- were made at the Astronomical Observatory of the Leningrad State netizma, Ionosfery i Rasprostraneniia Radiovoln, Krasnaya Universitv.,. in the 380- to 900-mu-- ranne. The spectral reflectina Pakhra.~~~~~~, USSR\.~~~~, power curve of limonite is seen to be fairly similar to that obtained Ceomagnetizm i Aeronomiia, vol. 5. Nov. -Dec. 1965. p. 1113. lll4. for the continents of Mars. R. A. F. In Russian. Brief note on a determination of the position of the equatorial boundary of abnormally high nocturnal atmospheric ionization for various levels of planetary magnetic activity. The study was con- A66-19337 #: ducted to obtain more reliable statistical data than those available DETERMINATION OF THE OPTICAL PARAMETERS OF THE in the literature; it was based on observations of ionization along MARTIAN ATMOSPHERE AND SURFACE TAKING INTO ACCOUNT three strings of meridionally located stations in the Western and ANISOTROPIC SCATTERING [OB OPREDELENII OPTICHE%= Eastern Hemispheres and in the Antarctics, taken from Nov. 1957 PARAMETROV ATMOSFERY I POVERKHNOSTI MARSA PRI to Feb. 1958. in Nov. and Dec. 1958. and from May to Aug. 1958, UCHETE ANIZOTROPII RASSEIANIIA]. respectively. v. 2. A. V. Morozhenko and E. G. Ianovitskii (Akademiia Nauk Ukrainskoi SSR, Glavnaia Astronomicheskaia Obeervatoriia, Kiev, Ukrainian SSR). A66-20101 (Soveshchanie Rabochei Gruppy po Issledovaniiu Atmosfer Venery i SYMPOSIUM ON PLANETARY ATMOSPHERES AND SURFACES, Marsa, Kiev, Ukrainian SSR, June 1964. ) DORADO, PUERTO RICO, MAY 24-27, 1965, PROCEEDINGS. IN: PROBLEMS OF ASTROPHYSICS [VOPROSY ASTROFIZW]. Symposium sponsored by the International Scientific Radio Union. Edited by I. K. Koval' . Journal of Research, Section D - Radio Science, vol. 69D. Dec. stvo 10 refs. Kiev, Izdatel' Naukova Dumka, 1965, p. 127-131. 1965. 188 P. In Russian. Determination of the optical parameters of the Martian atmo- CONTENTS: sphere and surface from absolute photometric data both for spherical PREFACE. W. E. Cordon (Cornell-Sydney University Astronomy and elongated scattering indicatrices. A comparison of the optical Center. Arecibo. Puerto Rico), p. iii. parameters for some values of the indicatrices shows a marked increase in optical thickness and slight variations in the surface JUPITER, AS OBSERVED AT LONG RADIO WAVES. albedos for the more elongated indicatrices when the albedo of a THE DECAMETRIC RADIO EMISSIONS OF JUPITER. C. R. A. single scattering event is near unity. Tables of numerical values Ellis (Tasmania. University, Tasmania, Australia), p. 1513-1530. of the optical parameters are included. v. 2. 47 refs. [See A66-20102 09-30] RESULTS OF RECENT INVESTIGATIONS OF JUPITER'S DECAMETRIC RADIATION. T. D. Carr, S. Gulkis, A. G. Smith, J. May, G. R. Lebo. D. J. Kennedy, and H. Bollhagen (Florida, A6619457 # University. Gainesville, Fla.), p. 1530-1536. 13 refs. [See A66- MEASUREMENTS OF THE BRIGHTNESS TEMPERATURE ON THE ?nim no-an1 L"Ay* "' -"' ILLUMINATED SIDE OF VENUS AT 10.6 CM [IZMERENIIA -KO- RESULTS FROM CSIRO, SYDNEY, AUSTRALIA. 0. B. Slee STNOI TEMPERATURY OSVESHCHENNOI STORONY VENERY NA and C. S. Higgins (Commonwealth Scientific and Industrial Research VOLNE 10.6 CM]. Organization. Sydney. Australia). P. 1536. 1537. A. D. Kuz,min (Awemiia Nauk sssR, Fisicheskii Instiat, uoscow, FREQUENCY AND POLARIZATION STRUCTURE OF JUPITER'S USSR). DECAMETRIC EMISSION ON A 10-MILLISECOND SCALE. James Astronomicheskii Zhurnal. vol. 42. Nov. -Dec. 1%5. p. 1281-1286. W. Warwick and Mark A. Gordon (Colorado, University, Boulder, 19 refs. In Riasian. Colo.). p. 1537-1542. [See A66-20104 09-30] Results of measurements at 10.6 cm of the brightness tempra- ture. averaged across the planet's visible disk. of Venus approaching JUPITER, AS OBSERVED AT SHORT RADIO WAVES. its superior conjunction (k i0.84). The brightness temperature iS JUPITER, AS OBSERVED AT SHORT RADIO WAVELENGTHS. given as 5500K. and it is shown that at this frequency its values on J. A. Roberts (Commonwealth Scientific and Industrial Research both the illuminated and the dark sides of the planet are equal, Organization, Sydney, Australia), p. 1543-1552. 51 refs. [See A66- within the experimental accuracy of 5% - i.e., its phase variation 20105 09-30] does not exceed 2.5%. This result disagrees with the results Of AN INTERFEROMETRIC STUDY OF JUPITER AT 10 AND 21 other authors at 3.15 cm and challenges Troitskii'stheoryof radia- V. z. CM. G. L. Berge (California Institute of Technology, Pasadena, tion emission by the planet's surface. Calif.), p. 1552-1556. 9 refs. [See A66-20106 09-30] DEPENDENCE OF JUPITER'S DECIMETER WIATION ON THE ELECTRON DISTRIBUTION IN ITS VAN ALLEN BELTS. Ab6-19592 Kip S. Thorne (Prmceton University. Prmceton. N.J.), p. 1557- JUPITER'S GREAT RED SPOT. 1560. 9 refs. [See A66-20107 09-30] Wendell C. DeMarcus (Kentucky, University, Dept. of Physics, OBSERVATIONS OF JUPITER AT 8.6 MU. John E. Gibson Lexington, Ky. ) and Rupert Wildt (Yale University, ObserGatory. (U.S. Naval Research Laboratory, Washington, D.C. ), p. 1560. New Haven, Conn. ). SIMULTANEOUS OBSERVATIONS OF JUPITER ON THREE Nature. vol. 209. Jan. 1, 1966, p. 62. 9 refs. FREQUENCIES. I. Kazes (Cornell-Sydney University Astronomy Description of a possible explanation for the great red spot on Center. Arecibo. Puerto Rico), p 1561-1563. 16 refs. [See A66- the surface of Jupiter. It is suggested that the red spot is a region 20108 09-30]

63 A66-20111

A REPORT OF MEASUREMENTS. D. Barber (Mmistry ov OF THE MARTLAN SURFACE. Carl Sagan (Harvard University, Aviation. Great Malvern, England) and J. F. R. Gower (Mullard Smithsonian Astrophysical Observatory, Cambridge, Mass.) and Radio Astronomy Observatory, Cambridge, England), p. 1563. James B. Pollack (Smithsonian Astrophysical Observatory, Cam- bridge. Mass.), p. 1629. PASSIVE RADIO OBSERVATlONS OF VENUS, SATURN, MERCURY, RADAR SCATTERING FROM VENUS AND MERCURY AT 12.5 MARS, AND URANUS. CM. Duane 0. Muhleman (Callfornia Institute of Technology, PASSIVE RADIO OBSERVATIONS OF MERCURY, VENUS, Pasadena, Calif.), p. 1630, 1631. [See A66-20121 09-301 MARS, SATURN, AND URANUS. Alan H. Barrett (Massachusetts APPLICATION OF PLANETARY MEASUREMENTS TO PLANE- Institute of Technology. Cambridge, Mass.), p. 1565-1573. 41 refs. TARY RADIUS AND ROTATION RATE DETERMINATIONS. Irwin [See A66-20109 09-30] I. Shapiro (Massachusetts Institute of Technology, Cambridge. MARS AND VENUS AT 70-CM WAVELENGTH. H. E. Hardebeck Mass.), p. 1632, 1633. [See A66-20122 09-30] (Cornell University. Ithaca. N.Y.). p. 1573. RADAR OBSERVATIONS OF VENUS IN THE SOVIET UNION RADIO OBSERVATIONS OF MERCURY, VENUS, MARS, 1N 1964. V. A. Kotelnikov (Academy of Sclences, Moscow, USSR), SATURN, AND URANUS. Kenneth I. Kellermann (Commonwealth p. 1634-1636. [See A66-20123 09-30] Scientific and Industrial Research Organization, Sydney, Australia), RADAR OBSERVATIONS OF THE MOON. p. 1574, 1575. 10 refs. [See A66-20110 09-30] RADAR STUDIES OF THE MOON. J. V. Evans (Massachusetts THE OBSERVATlONS OF RADIO EMISSION FROM THE PLANET Institute of Technology, Lexington, Mass. ), p. 1637-1659. 69 refs. MERCURY, MARS, AND SATURN AT WAVELENGTH OF 8 MM. [See A66-20124 09-30] A. E. Salomonovich (Academy of Sciences, Moscow, USSR), p. 1576. DECAMETER-WAVE RADAR STUDIES OF THE LUNAR SUR- A SEARCH FOR THE I. 36-CM WATER-VAPOR LINE IN FACE. J. R. Davis, D. C. Rohlfs. G. A. Skaggs, and J. W. Joss VENUS. F. D. Drake (Cornell University. Ithaca, N.Y.). p. 1577. (U.S. Naval Research Laboratory, Washington, D.C.), p. 1659- RADIATION OF VENUS AT THE 13.5-MM WATER-VAPOR 1667. 10 refs. [See A66-20125 OY-30] LINE. J. E. Gibson and H. H. Corbett (U.S. Naval Research LUNAR MAPPING BY COHERENT-PULSE ANALYSIS. T. W. Laboratory, Washington, D.C. ), p. 1577-1579. [See A66-20111 Thompson (Cornell-Sydney Unlverslty Astronomy Center, Arecibo, 09-30] Puerto Rico), p. 1667-1669. [See A66-20126 09-30] OBSERVATIONS OF THE 1.35-CM WATER-VAPOR LINE IN INTERPRETATIONOFTHE ANGULARDEPENDENCEOF VENUS. W. J. Welch (California, University, Berkeley, Calif.), BACKSCATTERING FROM THE MOON AND VENUS. Petr Beckmann p. 1580. (Colorado, University, Boulder, Colo.) and W. K. Klemperer (Na- OBSERVATIONS OF MARS AT 12 5-CM WAVELENGTH n 0 ~ - .. . - - . tional Bureau of Standards, Boulder, Colo.), p. 166r-1677. 16 refs. Muhleman and T Sat0 (California Instltute of Technology, Pasadena [See A66-20127 OY-301 Calif. ), p. 1580. A NOTE ON THE RADIO REFLECTIVITY OF THE LUNAR ON THE NATURE OF THE CLOUD LAYER OF VENUS -FROM SURFACE. A Giraud (Centre National d' Etudes des T;lecommunica- RADIOMETRIC OBSERVATIONS AT MICROWAVES. A. E:Basha- tions, Issy-les-Moulmeaux. Seine, France). p. 1677-1681. 16 refs. rinov and B. G. Kutuza (Academy of Sciences, Moscow. USSR). p. [See A66-20128 OY-301 1580-1583. 11 refs. [See A66-20112 09-30] MOON DISTANCE MEASUREMENT BY LASER. A. Orszag AN ANALYSIS OFMICROWAVE OBSERVATIONS OF VENUS. (Ecole Polytechnique. Paris, France), p. 1681-1689. 12 refs. [See Carl Sagan (Harvard Unlverslty, SmithsonIan Astrophyslcal Observa- A66-20129 09-30] tory, Cambridge, Mass.) and James B. Pollack (Smithsonian hstltu SOME HIGHLIGHTS OF THE URSI SYMPOSIUM ON ELECTRO- tion. Cambridge, Mass.). p. 1583, 1584. 5 refs. [See A66-20113 MAGNETIC WAVE THEORY HELD IN DELFT, THE NETHERLANDS, 09-30] SEPTEMBER 6-11, 1965. James R. Wait (National Bureau of Standards, PASSIVE RADIO OBSERVATIONS OF THE MOON. Boulder, Colo. ), p. 1691-1693. INVESTIGATION OF THE SURFACES OF THE MOON AND INDEX TO VOLUME 6YD. p. 1695-1700. PLANETS BY THE THERMAL RADIATION. V. S. Troitsky (Gorki State University, Gorki, USSR), p. 1585-1612 95 refs. [See A66- AM-201 11 # 20114 09-30] RADIATION OF VENUS AT THE 13.5-MM WATER-VAPOR LINE. POLARIZATION OF THERMAL RADIATION OF THE MOON J. E. Gibson and H. H. Corbett (U.S. Naval Research Laboratory, AT 14.5 GC/S. P. G. Mezger (National Radio Astronomy Observato- E. 0. Hulburt Center for Space Research, Washington, D.C.). ry. Green Bank, W. Va.), p. 1612. (Symposium on Planetary Atmospheres and Surfaces, Dorado, LINEAR POLARIZATION OF LUNAR EMISSION. D. Davies R. Puerto Rico, May 24-27, 1965. Paper.) and F. F. Gardner (Commonwealth Scientific and Industrial Re- Journal of Research, Section D - Radio Science, vol. 69D. Dec. search Organization, Sydney, Australla). p. 1613. ___- 1965, p. 1577-1579. THE EFFECT OF ROUGHNESS ON THE POLARIZATION OF Investigation of the brightness variatlon of Venus between pre- THERMAL EMISSION FROM A SURFACE. T. Hagfors and J. viously observed wavelengths of 8.6 mm and 3.15 cm. with special Moriello (Massachusetts Institute of Technology, Cambridge, Mass. ), interest in the possibility that the 13.5-mm water-vapor absorption p. 1614, 1615. [See A66-20115 09-23] maximum might give evidence of water vapor in the atmosphere of MEASUREMENTS OF LUNAR RADIO BRIGHTNESS DISTRIBU- Venus. Also investigated is the existence of any variation in plane- TION AND CERTAIN PROPERTIES OF ITS SURFACE LAYER. A. tary brightness with phase of solar illumination. The first group E. Salomonovich (Academy of Sciences, Moscow, USSR), p. 1616. of measurements were on 21 occasions between Oct. 29, 1962, and Feb. 9, 1963 and the second group gave eight measurements be- RADAR OBSERVATIONS OF THE PLANETS. tween Apr. 26 and June 26, 1964. The results indicated that at a A REVIEW OF RADAR STUDIES OF PLANETARY SURFACES. wavelength of 13.5 mm the average disk brightness temperature of G. H. Pettengill (Cornell-Sydney University Astronomy Center, Venus is essentially constant at 430 to 440°K over a phase variation Arecibo, Puerto Rico), p. 1617-1623. 29 refs. [See A66-20116 of 45 to 50° each side of lower conjunction, but at greater phase 09-30] angles up to the limit of measurement just beyond dichotomy the PRELIMINARY VENUS RADAR RESULTS. Richard M. Goldstem brightness rapidly increases approximately linearly with the frac- (California Institute of Technology, Pasadena, Calif. 1, p. 1623-1625. tion of the disk illuminpted. M. F. [See A66-20117 09-30] PRELIMIiGARY MARS RADAR RESULTS. Richard M. Goldstein (California Institute of Technology, Pasadena, Calli. ), p. 1625-1627. A66-20112 # [See A66-20118 OY-30] ON THENATUREOFTHE CLOUD LAYEROFVENUS - FROM RECENT ARECIBO OBSERVATIONS OF MERCURY. G. H. RADIOMETRIC OBSERVATIONS AT MICROWAVES. Pettengill (Cornell-Sydney Universlty Astronomy Center. Areclbo, A. E. Basharinov and B. G. Kutura (Academy of Sciences, Instltute Puerto Rico). p. 1627, 1628. [See A66-20119 OY-301 for Radioengineering and Electronlcs, Moscow, USSR). RECENT ARECIBO OBSERVATIONS OF MARS AND JUPITER. (Symposium on Planetary Atmospheres and Surfaces, Dorado, R. B. Dyce (Cornell-Sydney University Astronomy Center, Areclbo, Puerto Rico. May 24-27. 1965. Paper.) Puerto Rico), p. 1628, 1629. [See A66-20120 09-30] Journal of Research, Section D - Radio Science. vol. 69D. Dec. RADIO EVIDENCE ON THE STRUCTURE AND COMPOSITION 1965, p. 1580-1583. 11 refs.

64 A66-20882

Discussion of the nature of the cloud layer of Venus while in- that, therefore, except for Mars and Venus, only brief descriptions terpreting optical observations and radio brightness temperature and tabular data are given. It is pointed out that unless a source data obtained for the nocturnal side of the planet. The hypothetical of the tabular data is designated, the values quoted are from the presence of supercooled water drops in the cloud layer of Venus Smithsonian Physical Tables. M. M. has been checked by extrapolating the 8-mm wave absorption value, obtained from phase variation of radio brightness temperatures. into millimeter and centimeter wave ranges. It has been shown A66-20289 that the extrapolated values of the radio brightness temperamre RADIO ASTRONOMY. spectrum are in satisfactory agreement with the radio brightness N. H. Dieter, J. P. Castelli. and D. W. Ushakoff (USAF. Office temperature values measured at the nocturnal side of Venus. The of Aerospace Research, Cambridge Research Laboratories. Bedford. content of water in the cloud layer is estimated to be about 0.2 to Mass. 1. 0.3 glcm2. the absorption in the layer not exceeding L5 db in the IN. HANDBOOK OF GEOPHYSICS AND SPACE ENVIRONMENTS. centimeter range and being not above 5 db in the millimeter range Edited by S. L. Valley. for a wavelength of above 3 m. M. F. New York, Mdiraw-Hill Book Co., 1965, p. 22-1 to 22-15. 16 refs. Discussion of radio astronomy, the branch of astronomy concerned with the passive reception of radiation in radio wavelrngths A66-20116 # from extraterrestrial sources. Fundamental concepts and definitions A REVIEW OF RADAR STUDIES OF PLANETARY SURFACES, are given. The effects of the earth's atmosphere discussed include G. €3. Pettengill (Cornell-Sydney University Astronomy Center, refraction. scintillation and absorption. Radio emission from the Arecibo Ionospheric Observatory, Arecibo, Puerto Rico). moon and from the planets Venus, Mars. Jupiter, Saturn, and Mer- (Symposium on Planetary Atmospheres and Surfaces. Dorado. cury is evaluated, and sources of radio emissions are reviewed. Puerto Rico, May 24-27. 1965. Paper.) It has been found that the five brightest discrete sources are Journal of Research, Section D - Radio Science, vol. 69D. Dec. Cassiopeia A. Cygnus A. Taurus A, Virgo A, and C~.II~ZUIN~A. 1965, P. 1617-1623. 29 refs. The positions and angular diameters. the flux density vs the fre- In recent years, radar has been used to study the surfaces of quency, and the spectrum of these five discrete sources are tabulated. F. the planets Mercury, Venus. Mars, and Jupiter. In the case of M. Venus. attenuation in the planetary atmosphere at short wavelengths has also been reported. For Mercury and Venus, where the diurnal rotation is difficult to establish by other means, radar has A66-20291 provided a clear-cut determination of the sidereal periods as 59 COMMUNICATIONS OF THE LUNAR AND PLANETARY LABORATO- and 247 days. respectively. Mercury is found to possess surface RY. VOLUME 3 (Numbers 52-57). conditions not unlike those on the moon. Venus appears to have a Tucson, University of Arizona Press. 1%5. 42 p. surface considerably denser and smoother than the moon, but dis- playing several localized regions of scattering enhancement. Mars CONTENTS: appears smoother than the other planets, with a marked degree of ATMOSPHERIC EXTINCTION CORRECTIONS IN THE IN- surface differentiation. Except for one brief period of observation mkD. H. L. Johnson (Arizona. University. Tucson. Ariz. ), in 1963. Jupiter appears exceedingly inefficient as a reflector of p. 67-71. [See A66-20292 09-13] decimetric radio energy. (Author) THE ABSOLUTE CALIBRATION OF THE ARIZONA PHO- TOMETRY. H. L. Johnson (Arizona, University. Tucson. Ariz. ), p. 73-77. 24 refs. [See A66-20293 09-23] A66-20181 MARINER IV - DEVELOPING THE SUENTlFIC EXPERUdENT. GleM A. Reiff (NASA, Office of Space Science and Applications, A66-2ObW* Washington, D.C.). THE PLANET MARS [LA PIANETE MARS]. Science, vol. 151. Jan. 28, 1966. p. 413-417. 13 refs. Ggrald Goy. Account of some of the experiences associated with the develop- Sciences et Industries Spatiales, vol. 2. no. 1-2, 1966. p. 69-74. ment of the scientific payload for the flight of Mariner 4 (1964 77A). In French. Steps taken to combine the scientific instruments with the other vital halysis of Mariner 4 photographs. inoluding a discussion of the elements of the spacecraft are summarized. An equipment-test superficial characteristics of the planet Mars: topography, soil matrix, a chart of the phasing of the project, and a block diagram of composition, periodically observed phenomena, atmospheric the parts-control program are included. R. A. F. phenomena. and radiation measurements. Te rre8 trial atmospheric turbulence, the small angular sire of the Martian disk (some 15" of arc i~&ametcr).~aDd the l& contrast of me Marrlai sirrace com- A66-20182 bine to make exact photographic observations of this planet extreme- MERCURY - ANOMALOUS ABSENCE FROM THE 3.4-MILLZMETER ly onerous. A technique which is based on the superposition of RADIO EMISSION OF VARIATION WITH PHASE. multiple photographic images and whichin part overcomes these Eugene E. Epstein (Aerospace Corp., El Segundo. Calif. )- difficulties is described. The periodic migration of the polar cap Science, vol. 151, Jan. 28, 1966. p. 445-447. 7 refs. from one pole to the otber and the accompanying colof changes of Contract No. AF 04(695)-669. the Martian surface are described. The presence of HzO adGOt Discussion of unusual results from some radio observations of in the Martian atmosphere and the interpretation of the photographs the planet Mercury. Radio observations of Mercury at 3.4 inm and other data obtaimd by Mariner 4 are discussed. D. P. F. from July to Oct. 1965 showed brightness temperatures of Only about 2000K. even when major fractions of the planet's illuminated hemisphere were observed. There was no significant variation with A66-20082 phase. Possible reasons for this anomaly are briefly considered. ON THE LOSS OF GASES FROM A PLANETARY ATMOSPHERE. R.A.F. P. B. Hays and V. C. Liu (Michigan, University, Dept. of Aeronautical -and Astrmautical Engineering, Ann Arbor, Mich. ). A66-20287 Planetary and Space Science, -1. 13. Doc. 1965, p. 1185-1L12. PLANETARY ENVIRONMENTS. 38 refs. Roger A. Van Tassel and John W. Salisbury (USAS. Office of Research supported by the University of Michigm and Army; Con- Aerospace Research, Cambridge Research Laboratories. Bedford, tract No. NASA-54(05). Mass. ). An analysis of the collisional transition between the lower IN: HANDBOOK OF GEOPHYSICS AND SPACE ENVIRONMENTS. atmosphere md the collisionless exosphere is carried aut based Edited by S. L. Valley. upon an integral formulation of the Bohrmnn equation. This New York, Mdiraw-Hill Book Co., 1965, p. 20-1 to 20-19. 40 refs. investigation utilises a collision model which is a combination of Speculative discussion of planetary environments. It is noted Lorentz-gas and relaxation collision models. The results of this that models which satisfy all the observations are not available and malynis indicate that intermolecular collision. act in two ways to

65 A66-2 1065 affect the atmosphere. First, 'there is a critical layer, similar to Carl Sagan (Harvard University; Smithsonian Institution, Smith- the apparent photospheric surface of the Sun, from which the ma- sonian Astrophysical Observatory, Cambridge, Mass. ) and James B. terial escaping from the planet originates. This layer is deter- Pollack (Harvard University, Harvard College Observatory, mined by collision suffered by particles moving on orbits which Cambridge, Mass. ). skim tangentially by the planet. Secondly, collisions reduce the (Annales d'Astrophysique. vol. 28, Jan. -Feb. 1965, p. 229-233.) vertical flux of material in a manner analogous to the diffusion IN: ASTRONOMICAL OBSERVATIONS FROM SPACE VEHICLES; processes which occur in the lower atmosphere. (Author) INTERNATIONAL ASTRONOMICAL UNION, SYMPOSIUM NO. 23. LIEGE, BELGIUM, AUGUST 17-20. 1964, PROCEEDINGS. [A66- 21078 10-291 Symposium supported by the International Astronomical Union and the United Nations Educatlonal, Scientific and Cultutal Organization. AM-21065 Edited by J. L. Steinberg. Paris, Centre National de la Recherche Scientifique, 1965. p. 279- SPECTROSCOPIC OBSERVATIONS OF MARS. 283; Discussion, p. 283. William 0. Davies (Illinois Institute of Technology, Research [For abstract see issue 12, page 1759. Accession no. A65-2.20981 Institute, Chicago, Ill. ). Frontier, vol. 26. Winter 1965, p. 4-9. Discussion of spectroscopic attempts to determine the composi tion of the Martian atmosphere and the pressure of the atmosphere AM-21201 at the planet's surface. The bases of the spectroscopic techniques NOTE ON THERMAL PROPERTIES OF MARS, used for these purposes are described. Current estimates of the C. Leovy (RAND Corp. ,'Santa Monica, Calif. ). composition and surface pressure of Mars' atmosphere are given. vol. 5, Jan. 1966, p. 1-6. 12 refs. The natural limitations imposed upon measurements made from the Icarus, Contract No. NASr-21(07). earth. from balloons, or from satellites of either the earthor Mars are discussed. R.A.F. Interpretation of the variation of infrared emission from the surface of Mars with local time on Mars in terms of a simplified theory of diurnal temperature variations, in which the effect of the atmosphere is included. The results suggest a very low thermal conductivity for the upper few centimeters of the Martian AM-21109 #I ground. Such low conductivities appear to be possible only If A QUANTITATIVE MEASUREMENT OF WATER-VAPOR IN THE the material composing these layers is very fine powder having ATMOSPHERE OF VENUS. a characteristic size of not more than a few microns. If a Murk Bottema, William Plummer, and John Strong (Jobns Hopkins linear relationship is assumed between convective heat transfer University. Baltimore, Md. ). and surface temperature, the appropriate constant of proportion- lAnnalcn d'Astrophysique, vol. 28, Jan. -Feb. 1965, p. 225-228. ) ality 1s on the order of cal/cm2-sec-oK. F. R. L. IN: ASTRONOMICAL OBSERVATIONS FROM SPACE VEHICLES; INTERNATIONAL ASTRONOMICAL UNION, SYMPOSIUM NO. 23, LIEGE, BELGIUM, AUGUST 17-20, 1964, PROCEEDINGS. [A66- AM-21 202 21078 10-291 PHOTOMETRIC SEARCH FOR ATMOSPHERES ON EUROPA AND Symposium supported by the International Astronomical Union and GANYMEDE. the United Nations Educational, Scientific and Cultural Organization. Alan B. Binder and Dale P. Cruikshank (Arizona, University, Edited by J. L. Steinberg. Lunar and Planetary Laboratory and Dept. of Geology, Tucson. Paris, Centre National de la Recherche Scientifique, 1965, p. 275- Ariz. ). 278. -, vol. 5, Jan. 1966, p. 7-9. Contract No. AF 19(628)-202. Grant No. NsG-161-61. [For abstract see issue 12, page 1759. Accession no. A65-220971 Results of observations of the eclipse disappearances and reappearances of JII (Europa) and JIII (Ganymede). made in continuation of earlier work, to detect possible atmospheres on these satellites revealed by excess brightness on eclipse AM-21099 ft reappearance. An observation of an eclipse reappearance of AN OBSERVATION OF JUPITER IN THE ULTRAVIOLET. JII with the Kitt Peak 36-in. telescope showed a brightness Theodore P. Stecher (NASA, Goddard Space Flight Center, Greenbelt, anomaly of 0. 03 i 0. 01 stellar magnitudes. The anomaly decayed Md. ). in 10 min. Two high-quality observations of JllI showed no F. R. L. JAnnales d'Astrophysique. vol. 28. July-Aug. 1965, p. 788-790. ) brightness anomaly greater than 0. 01 stellar magnitudes. IN: ASTRONOMICAL OBSERVATIONS FROM SPACE VEHICLES; INTERNATIONAL ASTRONOMICAL UNION, SYMPOSIUM NO. 23, LIEGE, BELGIUM, AUGUST 17-20, 1964, PROCEEDINGS. [A66- AM-21204 21078 10-291 THE GREENHOUSE EFFECT IN A GRAY PLANETARY ATMO- Symposium supported by the International Astronomical Union and SPHERE. the United Natlons Educational, Scientlflc and Cultural Organlzation. Rupert Wildt (Yale University, Observatory, New Haven, Conn. ; Edited by J. L. Steinberg. NASA, Goddard Space Flight Center, Goddard Institute for Space Paris, Centre National de la Recherche Scientifique, 1965, p. 189- Studies, New York, N. Y. ). 191; Discussion, p. 191. 13 refs. -vol. 5, Jan. 1966, p. 24-33. 6 refs. Study of a single photoelectric spectral scan of Jupiter in the UV Grant No. NGR-07-004-029. reproduced an a plot of geometric reflectivity vs wavelength. The Illustration of Hopf' s analytical solution for several values reflectivity in aanumed to be due to Rayleigh scattering by molecular of the ratio of gray absorption coefficients' for insolating and hydrogen, and a comparison ia made with three model atmospheres escaping radiation (the greenhouse parameter, n), assumed of molecular hydrogen. The beBt fit is obtained with the 10.5 h- to be constant at all depths. Three graphs are presented for atm H2 model. An upper limit to the amount of molecular hydrogen temperature distribution as a function of optical depth with a above the cloud layer of a 11 km atm is derived. The observation zero, moderate, or strong greenhouse effect for flux incident was obtained with an objective grating stellar spectrometer on board at various angles. Five graphs are presented for temperature an Aerobee rocket. M. F. as a function of loglo, for p-values of 0. 05, 0. 25. 0. 5. 0.75. and 1 at various optical depths. F. R. L.

AM-21110 # AM-2121 1 SPACECRAFT OBSERVATION OF VENUS INFRA-RED LIMB- MARINER IV OBSERVATIONS AND THE POSSIBILITY OF IRON DARKENING. OXIDES ON THE MARTIAN SURFACE.

66 A66-22458

Carl Sagan (Harvard University, Harvard College Observatory; flat-faced cylinder in the 0.3- to 2.7-p region, using a carbon- Smithsonian Institution, Smithsonian Astrophysical Observatory. coated thin-film gage for flight velocities from 20. 000 to 46,000 Cambridge, Mass.). ftlsec and mitial pressures from 0.25 to 2.0 mm Hg are described. -Icarus, vol. 5. Jan. 1%6, p. 102, 103. 10 refs. Shock stand-off distances are measured by photographic techniques, Discussion of the results produced from the flight of Mariner the intensity behind the incident shock in the 0.3- to 1.0-c region W past Mars. and their indirect bearing on the study of the is measured by photometric techniques, and the nonequilibrium compdsition of the Martian surkce. The results showed that intensity in the far UV region is measured with a tungsten photo- there was no detectable magnetic field or related radiation electric gage. Shock-front-integrated nonequilibrium and equilib- belts. and that the surface was heavily cratered. The first rium intensities, noneqdibrium relaxation distances, and time-to- reault suggests that a migration of iron to the core has not peak intensity are determined. The stagnation-point radiance re- occurred and that consequently there may be more iron on the sults are found to be higher than some current estimates. indirectly Martian surface than on the terrestrial surface. The craters giving support to the CN radical heat of formation values obtained may be attributed to asteroid impact, indicating the possibility by Knight and Rink. The integrated nonequilibrium intensity for 9% of meteoric iron on the surface. Original iron and subsequent C02 mutures obtained is 55 w/cm2-2 w ster at 25.000 ftlsec. The meteoric iron may have oxidized as a consequence of the photo- major radiating species are found to be the CN radical for C02-N2 dissociation of water vapor in the Martian atmosphere and the mixtures and the CO+ ion for 100% C02. Oscillator strengths for preferential escape of hydrogen. F. R. L. the CN red and violet systems are deduced from the measurements. v. P.

A6622264 f A&-2 1532 THE COMPUTATION OF INFRA-RED COOLlNG RATE IN PLANE- THE POSSIBLE APPLICATION OF REMOTE GEOCHEMISTRY IN TARY ATMOSPHERES. PLANETARY EXPLORATION. C. D. Rodgers and C. D. Walshav,. (Oxford, University, Clarendon A. R. Barringer (Barringer Research, Ltd., Toronto, Canada). Laboratorv. Oxford. Ennland) I. - . IN: SCIENTIFIC EXPERIMENTS FOR MANNED ORBITAL FLIGHT; Royal Meteorological Society, Quarterly Journal, vol. 92, Jan. 1966. PROCEEDINGS OF THE THIRD GODDARD MEMORIAL SYMPOGIUM, .~0. 67-92. 26 refs. WASHINGTON, D. C., MARCH 18. 19, 1965. [A66-21517 10-301 Research supported by the Meteorological Office of England. Edited by P. C. Badgley. A scheme is described for the calculation of the atmospheric Washington. D. C., American Astronautical Society (AAS Science IR radiative cooling rate which is suitable for use at all levels. and Technology Series. Volume 4). 1965. p. 303-321. 7 refs. It uses the Curtis matrix method together with the Curtis-Godson Proposal of a technique for the measurement of trace amounts approximation in a form which includes the influence of temperature of vapors in the lunar and terrestrial atmospheres as an indicator on line intensity. Doppler effect is included. Because of its sim- of biologic and geologic surface conditibns. The monatomic vapors plicity the Goody rluadom model is used for all the absorption bands of a number of metals, iodine vapor, and sulfur dioxide are oon- considered ( H20 rotation and 6.3 p, C02 15 &, O3 9.6 p) ; the use sidered, and such analytical techniques as atomic absorption and of more accurate models as they become available presents no The facility for the spectro- molecular absorption are discussed. fundamental difficulty and in any case many of the topics investigated photometric analysis of light reflected from the lunar and terrestrial are not particularly sensitive to the spectral model used. A method surfaces is described and illustrated, orbital scanning modes which of reducing the number of spectral intervals is described and its could be performed with the equipment are outlined and illustrated, accuracy demonstrated. An accurate method of dealing with diffuse and methods of carrying out feasibility studies are explained. B. B. radiation is used to test the diffuse approximation, with the result that the constant factor L 66 originally proposed by Elsasser is found to be quite adequate for most purposes. Cooling rate errors A66-21740 caused by the following factors are estimated: (1) random and systematic errors in the initial temperature and humidity profiles; THE SEARCH FOR EXTRATERRESTRIAL LIFE. (2) the size of the vertical step used in computation; (3) neglecting N. H. Horowitz (California htitute of Technology, Jet Proplsion the temperature dependence of the Curtis matrix; (4) nonlinear Laboratory, Bioscience Section, Pasadena, Calif. ). effects in forming climatological means. It is shown that the easily Science, vol. 151. Feb. 18, 1966, p. 789-792. 15 refs. computed "cooling to space"is often a good approximation. All the Examination of the Martian environment in the light of the error investigations are based on direct calculations of the cooling Mariner 4 data to determine the possibilities of the existence of profile. Some comparisons with other techniques are presented life on that planet. Owing to the low density of the atmosphere and and a number of examples of meteorological interest are used to the absence of a magnetic field the surface of Mars is subject to an illustrate the versatility of the computing scheme. (Author) almost unattenuated bombardment by cosmic rays and solar radiation. However, it would not be difficult for Martian organisms to be protected against this otherwise lethal barrage. The atmosphere ~66-22458f of Mars contains approximately 1f1000 the amount of water found in IGNITION AND COMBUSTION OF POWDERED METALS IN THE the terrestrial atmosphere so that the scarcity of water is probably ATMOSPHERES OF VENUS, EARTH, AND MARS. the most serious limiting factor for any Martianbiology. The objec- R. A. Rhein .(California Institute of Technology, Jet Propulsion tives and goals of Martian biological exploration are examined. The Laboratory, Pasadena, Calif. ). "Cullliver" culture chamber is described. D.P.F. Astronautica Acta, vol. 11, Spt. -0ct. 1965, p. 322-327. 11 refs. The ignition temperatures of a number of powdered metals have been measured in air, in a simulated Venus atmosphere (consisting, A6621773 * by volume, of 4.10% argon, 9.17% nitrogen, and the remainder car- EXPERIMENTAL MEASUREMENTS OF NONEQUILIBRIUM AND bon dioxide) and in a simulated Mars atmosphere (consisting, by EQUILIBRIUM RADIATION FROM PLANETARY ATMOSPHERES. volume, of 2.16% argon, 11.21% carbon dioxide, and the remainder G. M. Thomas and W. A. Menard (Cahfornia Institute of nitrogen). This study was conducted to show that ,the atmospheres Technology. Jet Propulsion Laboratory. Pasadena, Cahf. ). of the planets Mars and Venus could be utilized as chemical energy (AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAUTICS, sources. Typical ignition temperatures of the following powdered ENTRY TECHNOLOCY CONFERENCE, WILLIAMSBURG AND metals were observed in the simulated Mars atmosphere: lithium, WPTON. VA., OCTOBER 12-14. 1964. TECHNICAL PAPERS. 405OC; beryllium, 762OC; calcium, 163OC; boron. 1203OC; cerium, AIAA Puhhcation CP-9. p.170-185. ) 199OC; titanium, 916OC; zirconium, 614OC; thorium, 587OC; and AIAA Journal, vol. 4. Feb. 1966. p. 227-237. uranium, 16fJ°C. In the simulated Venus atmosphere, the following Investlgation of the effect of composition upon the radiation typical ignition temperatures were noted: lithium, 367OC; beryllium, from the shock-heated mixtures: 99c C02/9* N2/1% A, 30% COz/- earth ambient temperatures; magnesium, 676OC; calcium, 269OC; 70% N2. and 10% C02. An electric arc-driven shock tube was used. boron, 1000°C; aluminGm, 705OC; cerium, 147OC; titanium, 708OC; The mixtures simulate the atmospheres of Mars and Venus. Mea- zirconium. 152OC; thorium, 627OC; and uranium, 134OC. It was surements of the shock-layer radiance at the stagnation pomt of a found that, generally, the powdered metals ignited more readily in

67 A66-227 1 5

air than in the Venus atmosphere, and more readily in the Venus Verification of the hypothesis of the presence of supercooled atmosphere than in the Mars atmosphere. These ignition tempera- water droplets in the cloud layer of Venus. The values of absorption, tures were compared to those in atmospheres of pure nitrogen and obtained at a wavelength of 8 mm from measured variations of the pure carbon dioxlde. The performance of these propellants was radio brightness temperature with phases. are interpolated into the discussed, and it was concluded that boron and beryllium are the millimeter and centimeter ranges. The radio brightness tempera- preferred fuels. (Author) ture spectra thus obtained are found to be in fair agreement with the spectra measured on the planet's nocturnal side. The water content in the cloud layer is estimated at 0.1 to 0.3 g/cm2. The A66-22715 radiation absorption in the layer does not exceed 1.5 and 5 Debye in the centimeter and millimeter ranges, respectively. V.Z. A STRATEGY FOR MARS. Charles Richard Weston (Rochester, University, Dept. of Biology, Rochester, N. Y. ). AM-23504 # American Scientist. vol. 53, Dec. 1965, p. 495-507. 10 refs. SPECTROPHOTOMETRY OF METHANE ABSORPTION BANDS ON Discussion of the possibilities and nature of life on Mars and THE JOVIAN DISK IN THE NEAR INFRARED REGION (0.7 TO an evaluation of the problems involved in its detection. Martian 1.0 p) [SPEKTROFOTOMETRIIA POLOS POGLOSHCHENUA environmental conditions are discussed as a possible medium for METANA NA DISKE IUPITERA V BLIZHNEI INFRAKRASNOI the support of living organisms. The limiting effect of low temper- OBLASTI (0. 7 - 1. 0 p)]. atures. lack of water and oxygen. low atmospheric pressure. and V. G. Teifel' (Akademria Nauk Kazakhskoi SSR. Astrofizicheskii high radiation levels on life organisms is considered. It is shown Institut, Alma-Ata, Kazakh SSR). that an environment that is marginal or will not support terrestrial Astronomicheskii Zhurnal, vol. 43, Jan. -Feb. 1966, p. 154-156. organinma is not necessarily unfit for organisms which could have In Russian. evolved under the selective pressure of this alien environment. The Measurement of the intensity of the methane absorption bands problems involved in life detection experiments are analyzed. 7250 A. 8610 A t 8860 A, and 9900 A from spectrograms of various D. P. F. Jovian zones taken by an image converter tube. The absorption is slightly weaker at the planet's edge in the equatorial zone. slightly A66-22786 greater in the temperate latitudes. and decreases towqrd the DISK TEMPERATURES OF MERCURY AND MARS AT 3.4 MM. poles. The variations are far smaller than those from a conven- Eugene E. Epstein (Aerospace Gorp., El Segundo, Calif. ). tional sccant effect in a single-layer model of an absorbing atmosphere. Theories are proposed to explain these zonal variations. Astrophysical Journal, vol. 143, Feb. 1966, p. 597, 598. 6 refs. V.Z. Contract No. AF 04(695)-469. Determination of the disk temperatures of Mercury and Mars on the basis of observations made at 3.4 mm in April 1965. A66-23639 A blackbody disk temperature of 190° f40OK is obtained for LUNAR AND PLANETARY PROBES - METEOROLOGY AND COM- Mars. while in the case of Mercury the daily values of the MUNICATIONS - GEODESY AND NAVIGATION. blackbody disk temperature ranged from 130 to 320°K. the Harrie Massey (London, University. University College. Dept. of Phvsics. London. England). average value being 220 f 35OK. ~ A. B. K. (Contemporary Physics. vol. 6, Apr. 1965, p. 241-260.) IN: SPACE TRAVEL AND EXPLORATION. H. S. W. Massey (London. University. University College. Dept. A66-23414 of Physics, London, England). London. Taylor and Francis, Ltd., 1966, p. 73-92. RECENT DEVE113PMENTS IN THE THEORY OF RADIATIVE [For abstract see issue 04, page 575, Accession no. A66-133611 TRANSFER IN PLANETARY ATMOSPHERES. Zdenek Sekera (California, University, Dept. of Meteorology, Los Angeles, Calif. ). (International Association for Meteorology and Atmospheric Physics AM-23640 of the International Union of Geodesy and Geophysics, Symposium EXOBIOLOGY - MAN IN SPACE. on Theory of Radiative Transfer in Planetary Atmospheres, Harrie Massey (London, University, University College, Dept. of Leningrad, USSR, Aug. 5-12, 1964, Paper. ) Physics, London, England).- Reviews of Geophysics, vol. 4, Feb. 1966, p. 101-11L 14 refs. (Contemporary Physics, vol. 6. June 1965. p. 321-337.) Contracts No. AF 49(638)-700; No. AF 19(628)-3850. IN: SPACE TRAVEL AND EXPLORATION. Demonstration of the Chapman approach (baaed on a source H. S. W. Massey (London, University, University College, Dept. matrix and on the bolution of auxiliary equations for this matrix) of Physics, London, England). to radiative transfer problems and particularly to the derivation of London, Taylor and Francis, Ltd., 1966, p. 93-109. an equation for the inhomogeneous case of imperfect scattering. [For abstract see issue 04, page 469. Accession no. A66-138061 The integrodifferential equations for the reflection and transmission matrices for this cane are presented, and their reduction is demonstrated for the separable phase matrix in which the directional AM-23660 parameters of the incident and scattered radiation can be separated. MARS - UPPER ATMOSPHERE. It is noted that with the use of the theory of singular integral equa- S. H. Gross (Cutler-Hammer, Inc. , Airborne Instruments Laboratory tione applied to the nonlinear integral equation for X and Y function, Div., Melville, N. Y. ), W. E. McGovern (New York University, transformed into a singular form, a method has been recently School of Engineering and Science, Dept. of Meteorology and Oceanog- developed.that permits rapidly converging iteration for large optical raphy. Bronx, N. Y.), and S. I. Rasool (NASA. Goddard Space thickness. M. M. Flight Center, Goddard Institute for Space Studies. New York; New York University, School of Engineering and Science, Dept. of Mete- orology and Oceanography, Bronx, N. Y. ). AM-23503 Science. vol. 151, Mar. 11, 1966, p. 1216,1221. 9 refs. NATURE OF THE CLOUD LAYER OF VENUS - FROM RADIOMETRIC Grant No. NsG-499. OBSERVATIONS IN THE SHF RANGE [0 PRIRODE OBLACHNCGO Theoretical analysis of the thermal structure of the upper atmo- SLOIA VENERY - PO DANNYM RADIOMETRICHESKIKH NABLIU- sphere of Mars.based on spectroscopic measurements and the results DENII V SVCh-DIAPAZONE]. of the Mariner-4 occultation experiment. Based on a pure GO2 model A. E. Basharinov and B. G.Kutuza (Akademiia Nauk SSSR, Institut with a surface pressure of 5 to 10 mb. the exospheric temperature Radiotekhniki i Elektroniki, Moscow, USSR). is calculated to be 550 *150°K. The vertical temperature distribution, (Simpozium PO Radioastronomicheskim Metodam Issledovaniia which is plotted, is consistellt with the temperatures deduced from Atmosfer i Poverkhnostei Planet, Puerto Rico. May 25, 1965.) the Mariner experiment. The implications of these results for the Astronomicheskii Zhurnal, vol. 43, Jan. -Feb. 1966, p. 149-153. origin of the Martian atmosphere are considered significant. 11 refs. In Russian. R. A. F.

68 A66-24697

AM-23794 EVIDENCE OF EXTRATERRESTRIAL LEE [GBER DEN NACHWEIS EXTRATERRESTRISCHEN LEBENS]. Hans Swart. Astronomie und Raumfahrt, no. 6. 1965. p. 161-171. 10 refs. In German. Review of work currently being done to determine whether extraterrestrial life exists in the solar system. Only Mars is considered capable of supporting even lower forms of life. Various automatic systems currently being developed in the U. S. for use with the Voy- ager spacecraft are intended to soft-land on the Martian surface, gather dust samples from the Martian atmosphere. or collect samples of the Martian soil and examine them for microorganisms. The furthest developed of these systems are the "Gulliver" radioisotope experiment, the "Multivator" automatic biochemical testing apparatus. and a TV-microscope. The first launch attempt is expected to be with a Saturn-IBICentaur, not before 1%9. R. A. F.

Ab&-24697 * LANDER PAYLOAD INCREASE BY BETTER DEFINITION OF THE MARS ATMOSPHERE. Ernest J. Merz (General Electric Co., Missile adSpace Div., Philadelphia, Pa.). (American Institute of Aeronautics and Astronautics. Aerospace Sciences Meeting. 2nd. New York, N.Y., Jan. 25-27, 1965, Paper 65-22. ) Journal of Spacecraft and Rockets, voL 3, Mar. 1966. p. 359-364. 5 refs. [For abstract see issue 05, page 670. Accession no. A65-145631

69 A65-80891

A65-80869 THE ATMOSPHERE OF MARS. 1965 Richard M. Goody (Hatwsd U, Cambridge, Mass.) IN: THE ORIGIN AND EVOLUTION OF ATMOSPHERES AND OCEANS. (Conference at Goddard Institute for Space Studies, Natblul ACIUMU~~~S LC ENTRIES and Space Adminimation, New Yo&, AprU 8-9,1963, Proceedings). Edited by Peter J. Bnnurlo and A. G. W. Cameron. New Yo&, John Wileyand Sons, 11%. 1964, p. 289-298. 6 refs. Some dtfficuhies in detennining the composition, ground pressure. and saucture of the atmosphere of Mars M presented. Included ue borh A6560370 solid and inferential dam. Among the former arc poluimcuic nw~uwments ATMOSPHERE AhD EVOLUTIOK. of the total mass of the Maaiotr atmospbere and specaogxaphic meamre- Daniel L. G8ben (Jefferson Med. CoU., Dept. of physiol., PhiIadelphis). ments for oxygen and water vapor. The latter covers Mmi.rr polar ups, IN: OXYCEh IN THE AMMAL ORGAhlSM. atmospheric oxygen content, and atmospherle ninogen content. Surface @Symposium of the International union of Blochembuy and the Inter- features of Mars that could have some relevance to atmorphcrk proerrs, national Union of Physiological Sdences, London, 1963, I'mceedings.) lnscfat u therr is some kind of interchange between the surface adlcmos- Edited by Frank Dkkens and Eric Neil. phere, arc also included 0xford.Great Britain, Yergamon Fress, 1964,~.641455. 61 refs. [See A65-803551. A biosphere might possibly exist on a planet during the time atmos- its AO5-00889 phere evolved from one composed of molecular hydmgen, helium, water, THE ORIGIN AND EVOLUTION ATMOSPHERES AND methane, and ammonia into one composed of carbon dioxide and molecular OF OCEANS. nitrogen. In the beginning and ending of such a possible life-stage on a Peter J. Bancab md A. C. W. Camrron. planet, the atmosphere could be expected to contain little or no molecular Edltedby RterJ. dA.G W. Clwron (codd.Ldlnafor Spmx oxygen. The formation of water by the marriage of oxygen, the second moa abundant chemkally reactive cosmic element, to hydrogen, the predominant cosmic element, is the essential source of energy for most of the earth's biosphere. The destructive influence of this energy source on the biospbeiz is reflected in the phenomenon of oxygen toxicity.

A6560473 STAGES AND MECHANISMS OF PREBIOLOGICAL ORGANIC SYNTHESIS. J. Om (Houston U, Dept. of Chem, Ter) IN: THE ORIGINS OF PREBIOLOGICAL SYSTEMS AND OF THEIR MOLEC- ULAR MATRICES: Proceedings of a Conference Conducted at Wakuda Springs, Fla on 27-30 On 1963. Edited by Sidney W. For NewYork,Academk Rest 196S.p. 137-162. Discusaionp. 162-171. 58 refs. NASA Grant NsG-25782. Obsemations on the composition of carbon .sm atmospbereo, taterstel- lar matter, the Jovian planets, comets, and meteorires Indicate that the Syn- thesis of organic compounds in the universe is a more general process than has been thought heretofore. Prior to and during the formation of tht solar system, hut before the earth was completely formed, organk ryntheses probably Occurred in the followlng four stages for sites): carbon stax atmospheres, solar nebula, planetesimals, and protoplanets. The energyfor these syntheses was provided initially by the high temperature of Sur annospheres and then mainly by the ionizing radiation and uluaviolet light coming fmm the sun. CatalWc processes and other localized sources of energy were probably also involved in the formation of organk compounds. Astronomic and meteoNlc obsemations indicate that the conditions prevailing in the majority of cosmk bodies during the latter stages of evolution of the solar system were as follows: reducing or oxygen-tree atmosphere. aqueous en- v&onment. b& or neutral pt%, moderate temperature. and presence of a relatively hlgh concenuatinn of organk compounds. A number of general mechanisms can be pornlared to have been involved in the abiotic formanon of simple biochemiurl compounds: (a) a radical mechanism in the sgnrhesis of the aliphatk and aromatic aldehydes which are the precursors of I -amloo acids, @) a base-catalpd aldol condensation of hplealdehydes in the formation of pentoses, 2-deoxypentoses, and other monospccharldes, and (c) a base-catalyzed condensation of hydrogen cyanide and other nlrrlles. followed by other condensation reactions, in the synthesis of purines, pyrimidines, and other heterocyclic compounds.

A6560868 THE ATMOSPHERE OF VFACS. Carl Sagur (Harvard G., Cambridge, Mass.) IN: THE ORIGIN AND EVOLLTION OF ATMOSPHERES AND OCWNS. MU0891 (Conference at Goddard Institute for Space Studies, National Aeronaurier OBSERVATIONS OF WATER VAPOR ON MARS AIW VENUS. l and Space AdmmlsuatIon, New Yo& April 8-9,1963, Roceedtngr). A. Do- pbumoke de Pals, Maudon, France). Edited by Peter J. Eronuuio and A. G. W. Cameron. ik THE ORIGIN AND EVOLUTlON OF ATMOSPHERES AND OCBANS. New York, John WUey and Sons, Inc, 1964, p. 279-288. 11 refs. Eonferi?nce d coddad Inltnute for a Stud*& Nmlonrl Auo~utlcr Oata attemptlng to explaln the composition of the atmosphere of SmAdmink~nU~~~, Ncr YO* Ad8-9.1963. Venus are revlcwed. Problems vAth respect to watervapor, CO2, org.nIc Bdtad by Pew J. Brmcdo mdA. G.W. C.wroa molecules, temperature, and pressure arc Included. An explmat(on of how New Yo* John WueS. md Sons, loc, 1964. p. 257-268. (set A05-80889). the surfee stays as hot as it does is one of the key problems UI understand- De~nrol~e*meurmme~r~gpoltdrrIdc~nof~ ing the Venus environment. There is as yet no view which mtegntes all on both Venur ud Mus m prermad Obmvuwnr .M made from kt- of the obs+mnr&nal matem. loons during tliqht adfrom hlgh mountains. Dam were obtained by nuking

71 A65-80977 photome& comparlsons of the obsenratlons on Venu and Mus witb those ABS-81287 on the Sun or Moon. A flnal value of 1.5 x IO-' amsof water vapor SURVIVAL AND GROWTH OF TERRESTRIAL MICROORGANISMS IN war calculated to be about 1 X @m2, rtth a probable error of a factor AMMONIA-RICH ATMOSPHERES. of 2. ActMncs of an lnternatlonal program for photographing Venus In the S. M. Sicgel and C. Gtumarro (Unlon Cublde Res. Inst, T.rrytom. N. Y.) ulurvlolet uedelerlbed. gs,vol. 4, Apr. 1965, p. 3740. 9 refs. Contract NA Sw- 767. Varlour hacterta, and aacomyfeter were demonmated to have grom on speclmens of Euphorbla xylophylloldes and other xerophytes der 2 mOnthS A65-60977 In atmOSpbere.1 conuhlng NHs with CHI, H2.01 a+. NH3 lev& Of at lean HABITABLE PLANETS FOR MAN. 50,000 ppm fuexceeded conventlonal upper deItmlls for human toxietty. Stephen H. Dole (Rand Corp, Santa Monk+ CdK.) Ememe performance was shown by a Pmsr-adapted Penicillium brevi- NewYork, Blatdcll Publtrhlng Co, 1964,ldll+ 158'~. corn actum whtch grew slowly in 95% NH3/5% CHI. The stgnifluncc of these $5.75. o*ns for the orlgtn and current extnence of microbial Me on Jupiter Thlr book anempts to spell out the requirements of planet8 on which Is noted briefly. hunun belngs as a bbologlcal rpecier can live, and to dlrurr the ersentlll propertter mquiredof the Nus whlch provide heat UILI light. The nlne chapters Cil witb #pace and the aolu rynam, hunun rcqulnments (tcmperarure, A65-81737 lbhr, grdty, water, atmorpherlc comporlflon, mad pressun), phy&d proper- A PHYSICAL BASIS FOR LIFE DETECTION EXPERIMENTS. ties of the planets, probrblllty of occumnca of habtUble planets, J. E. Lovelock dlreutslon of the 43 stus rlth a reasonable Ilkellhood of having habhblc Nature.vol. 207,Aug. 7, 1985, p. 568-570. 19refs. planets, and changes lnecttng men in new environments. A 6-page appcndir NASA Grant NSG 199-62. contabs phystcd data on the 25 principal bodies of the rolu tynem of mass The design of an efficient and unequivocal experiment in extra-terrestrial greamrthan 1023 grams. life detectlon should take into account a deflnftlon of ltfe stated In terms favorable for Its recognition, and a desulption of the past and present envlrOn- ment of the planet to be sampled. The following experiments are suggested for the detectlon of Ilfe, specifically on Mars: (1) search for order In chemical A65-81013 structures and molecular weight distributions, also by sound and by slght; and SOirlE EARTH LIFE SEW ADAPTABLE TO MARS. (7) search for non-equilibrium, principally by differential thermal andysis and Roderick D. Htbben. gas chromatography mass spectrometry of the atmosphere, and recognition Of Avlatton Week and Space Technology, vol. 82, Apr. 12. 1965, p. 71-79. physical non-equlllbrlum such as non-random motion. A description Of past There Is evidence that cenatn plants, Insects, and primttive animal organ- and present known condttlons on Mars is Included. isms found on earth could sunrive the temperature extremes and lowaxygen environment thought to extst on Mars. There seems to be a dlrecccorrela- tion betwten the abllity of a chemical compound which acts as a plant growth accelerattng hormone and the activtty outside the llvlng plant of the compound A65-81928 as a chemical andoxidant. The chemlsay and development of preexisting THE ORIGIN OF PLANETARY ATMOSPHERES. Me forma on emh and those whlch mlght extst on netghborlng planets may A. G. W. Cameron Goddard Xnace have been rlmllar. laboratory tests showed that plants could survtve a re- \------r-- -Fllcht D Center. Insr.for Swce Studks. BeltrvUk. Md.) duced oxygen atmosphere. However, thelr chemistry was greatly changed. TRW Space Rchnology Laboktorks Leek Serks, vol. 2,1965, p. 61-70. Under thermal varlartons whtch an thought to exist on Mars, the plants had The author llsts the processes whkh may b lmponant In the formatlon vegetatlve reproductton, but no floral reproductlon was observed. Desert and regularlon of planetary atmospheres. Ihe Input processes may consist species dted but the roots produced young shoots. Meal worm Imae showed of: @)capture of gaseous maner from prlmltlve solar nebulae or solar a longer period of survival than pupae and adult invertebrates. Redear turtles wlnds, (2)result of colllslons wlth comets and meteorms; @)outgassing sunrhred but the+ redcount did nor increase, as in the case In humans, and from the Interlor; and (4)chemlcal reactlons wlth surface maner. 'Ihe loss blood volume decreased below effective circulation rcqutemcnts. In most of atmosphere may be due to: @)thermal evapotatlon; (2) sweeplng actlon cases 1% to 5% oxygen was sufftcient to support acttnry of many adult tn- of solar wlnd; (3)chemkal reactlons with sw(ace mmterlpls; and (4)rotatlOn sects. However, because anyllquid water present on Mars may have htgh InstabUity of the planet. 'Ihe authorconslders the effects of these proc- saltntty, many forms of life would be ruled out. Fungl could survlve and re- esses on the exlstlng or speculated compositlon of atmospheres whkh produce in an environment almost devoid of oxygen and water. Some lichens surround the solar planets and the moon. The author concludes that we have been found to survtve 4000 nmes the normal ultravlolet radiatlon re- have no knowledge how lmponant these varlour processes are for the cetved on euth and temperatures of -30' F. Molds and a vutety of bacteria msjorlcy of planets, nevertheless, thl8 outllne provldes a frnmework for are able to grow in pure ammonia or a mtxture of ammonia and methane. dlscusslon of varlous planetary atmospheres.

A65-81018 A65-82064 MARS. INSTRUMENTS FOR DETECTING LIFE. Robert S. Richardson and Chesley Bonestell. WUllam R. Corltss. New York, Harcoun, Brace and World, Inc., 1964, vltt+151 p. $8.50. IN: SPACE PROBES AND PLANETARY EXPZORATION. If there is extratenestrlal Me In the sola system, Mars is the only planet New York, D. Van Nostrand Co., Inc., 1965, p. 477-502. 25 refs. NASA for which we have the sltghtest evidence. In this book on Mars, there are supported research $7.50. dtscussions of the physlcal chnractertstlcs of the planet; probahlllty of life; This handbook of technlcal information on space and planetary explora- orbital characteristics and distance from Earth; time measures, seasons, tton, spacecraft deslgn, communtcatlons, guldance, and scientlftc Instruments and atmosphere on the planet; vegetative and nonvegetatlve hypotheses in space Is intended for use by engineers and others engaged in space ex- of vlstble changes; otigtn of the canals; problems and dangers of habita- ploration, ventures. Pertinent to aerospace medtcine Is Chapter 16, in which tbon; gravlratlonal amaction; and characrerlsrlcs of the Marttan satellites, are reponed techniques for the detectbn and study of Me on other planets. Phobos and Detmos. Instruments to be used for the detectlon and study include infrared and mass spectrometers, televlslon, radto Itstenlng, chromatographs, and ultraviolet spectrophotometers. Biologtcal experlments should include the determlna- ABS-81159 tion of staining propertles, reduction- oxidatton potentlals, bioluminescence IS THERE VEGETATION ON MARS 7 and opttcal rotary dlsperslon, plus rntcroscoplc observatlon and metabollsm detection by means of radlolsotopes. Llfe detectlon and study may be done by R. Smoluchowskt (Princeton C., Solid State and Materials Program, N. J.) elther remote analysls by sample analysis. Science,vol. 146, May 14, 1965, p. 946-947. 10 refs. or =snd Hlggins Fund supported research. At least some of the changes in the color of Mars at dtfferent seasons are caused by color centers produced by electromagnetic and corpuscular A65-82216 solar radiatlon in soltds on the surface. Calculated radiation flux, a1 ap- AUTOMATED LIFE DETECTION propriate energies and known temperature varlatlon. could account for Richard S. Young (NASA, Ames Res. Center, Exobiol., Dlv., Moffert FIeld, seasonal formation of color centers and bleaching if a simple trap model Calif.) is assumed. In certain Mnds Of rhyolite (S102, NaAISi308), whlch has been ______Asuonautks a$ Aeronautks, vol. 3, Oct. 1965, p. 70-78. suggested as one of the posslble constituents of the martian surface, color Posstble means for explorlng exuaterrestrlal bodles and for studylng their centers can be produced. No color centers are expected in Hmonlte, blologkal and physical evolutlon are dlscussed. Mars contlnues to offer the Fez03 . 3H20, the other likely constituent. greatest potentlal for blologlcnl actlvity and to command the most Interest

72 .

A65-82273 THE ABSORFTION WIENSITY OF THE 5, BAND OF CARBON DIOXIDE. AND THE MARTIAN co2 AB~DANCEAN% ATMOSPHERIC PRESSURE. PhUlp L. Hans and Paul R SWM (AVCO Corp, Res. and Admn. Dcselop. Dhr, Wtlmlngton. Mass.) lurur,vol. 4.Sep.1985.p.353-381. 9refr The surface pressure of the Maninn atmosphere strongly affects the des@ and payload upabilttks of Mars entry vehkles. The cumnt most widely nc- cepted dueof thb surbx pressure is 2 5 m0llbars. This value was determined by Kaplnn. Munch, and Splnrad based on thelr obsemation of CO ab- sorpaon lines neu 8700 A and on Sincon's and Kuiper's CO ohrervdnr u 2.06 microns. It is notewonhythu theirestbnatedvaiue of 25 mslibnrs is a faaor of 3 or 4 below estimates determined both by photome& and by polu- bnew technlques. A Iabomory redetermin.tton of the integrated abrorplon inteosky of the 5. band of C02 near 8700 A har been ma& wth a long- path technique andphotornultlplkr detection. This has resulted in a revision of the calibration uced by Kaplan, Munch, and Sphrad. In vkw of the Bn- ponance of the surface WSN~to curnnt mdks of Mmprober, a recllcula- tion of the pressure utilbing the new L.boNOry meaerremenu i. un*d out in this paper. The results of @e present pnalyslc give a revised dueof (31+l3) mum.for the Martian C02 abundance under the asrummn of an effectbe temperature for the Muri.n annosphere of 200' K. The suh pressure b now entmued, using this abundance value, to be (511t25) milll- bars.

1966 LC ENTRIES

A66405&'2 IIFE CN hlt.l?S. ?rancls lackson an3 Fanlck F,?oore. :ondon,Routle%e andKegan Paul, 1985, tx' 111 p. 106 refs. The author reviews the facts available at present on the conditions crlst- inn, on ?he planet mas, In order to .4ecl.k .rhether buman, animal. and plant life, as It Is 1.novm on earth, wo:M be possibl? on this planet. Ills concluslon is that some prlmlthn forms of temmlal life could ~s~rvinthe martian Bm?osphere, which has a dlfferenr comFosirioC than the atmosphere surmundtng emh. ?.e diurnal varlatlon of martian tenrperanire is more ememe than on earth, and it could k fatal to tmresulai orJanisms hut some could adapt to these rlgorous conditions. The possibiliry of the existence of manhorgan- Isms would caIl for assuming a different blochemknl system. The presence of seasonal changes of manlan surface coloring sngzgst the presence of photosynthetk plants, but it is cvidmnt that the overall mmlan srtrrace con- dklons me cot sutable for hurrnn liie support.

A6640742 SPACE AND INTELLIGENT BEINGS (KOSMOS I RAZUMNYE SUSH- CHESTVAI. F. A. TsWm (P. K. Shternberg Stare Ins. of Astronomy, MOSCOW, USSR). no. 11, Nm. 1965, p. 94-101. In Rusdsn. ?? e ph- faors are constdcred which control the RE~Ot the visibk universe. prhnrily. temperature, pretence of amosphezc emeloptng a planet and cxiaring force of gr.vZry on a planet. These fSam pc bpnportmt in the formulon of maaomolecules from whlch I& clll evolve. Essumptbn that only one out of 105-108 stars can prorCae the center af a rynm .Im- flito the sola system, creating planemy conditions suitable fa sw-8 IKe, is, according to the author, underestimation. Some m.them.tlul consklecatonr indicate a greater probahUity of the extstence of ematIIeS- trill IKe.

73 .

Subject Index

~ ~~ PLANETARY ATMOSPHERES / a continuing bibliography with indexes AUGUST 1966

ABSCWTION COEFFICIENT Typical Subject Index Listing CARBON DIOXIDE- R-BRANCH LINES OF 5 MU SUB 3 BAND FROM INTE6RAL OF ABSORPTION COEFFICIENT OF MARTIAN ATMOSPHERE 116615288

HDPF ANALYTICAL SOLUTION FOR VALUES OF RATIO OF 6RAY ABSORPTION COEFFICIENTS FOR INSOLATING AN0 ESCAPING RADIATION /GREENHOUSE PARAMETER/ ASSUME0 CONSTANT AT ALL DEPTHS. PRESENTING TEMPERATURE DISTRIBUTION GRAPHS A6621204

ACCESSION ABSORPTION SPECTRUM NUMBER LABORATORY SPECTRA FROM LEAD SULFIDE SPECTROMETER FOR TESTING PRESENCE OF MINOR CONSTITUENTS IN PLANETARY ATMOSPHERES A65-18479 A Notation of Content (NOC). rather than the title of the document. is used to Provide a more exact description of the subject matter in order to provide the LABORATORY AND PLANETARY ABSORPTION SPECTRA user with more than one approach in the search for specdic informahon. a COMPARISONS IN REGION 9700-11200 ANGSTROMS USE0 TO subiect may be listed under Several subject headings The acCeSSIOn number DETERMINE COMPOSITION AND TEMPERATURE OF JUPITER IS included to assist the user in locating the abstract in the abstract sectton ATMOSPHERE A65-21854

INFRARED SPECTROSCOPY STUDIES TO DETERMINE ABSORPTION BY CARBON DIOXIDE BETWEEN 8.000 AND A 10~0001CMIN 1 TO 1-25 MICRON REGION ABIOGENESIS U-3200 N66-22465 ATMOSPHERES CAPABLE OF PRODUCING ORGANIC COMPOUNDS DISCUSSED. STUDYING ABIOGENIC SYNTHESIS IN MARS ABSTRACT SIMULATOR A65-30683 SPACE SCIENCES BIBLIOGRAPHY WITH ABSTRACTS - ASTRONOMY. METMROL06Y. OCEANOGRAPHY. UPPER ENERGY SOURCES AND CHEMICAL REACTIONS IN ATMOSPHERE. GEOPHYSICS. SPACE PREBIOLOGICAL ORGANIC SYNTHESIS JPRS-35095 N66-23025 A65-80473 ACCELEMTIOW NUCLEIC ACID MOLECULE REPRODUCTION DISCUSSING DETERMINATION OF PLANETARY ATMOSPHERE STRUCTURE PROBABILITY OF LIFE DEVELOPMENT UNDER FAVORABLE FROM MEASURE0 ACCELERATION OF ENTRY VEHICLE ENVIRONMENTAL CIRCUMSTANCES A66-15915 NASA-TN-0-2669 N65-11118

ABLATINS MATERIAL AERoD*wIIIIC CHARACTERISTICS DENSE CARBON REINFORCED AN0 LOW DENSITY CHAR- APPROXIMATE AN0 CHARACTERISTICS METHODS TO PREDICT FORMING RESIN ABLATION MATERIALS FOR EARTH. MARS EFFECT OF GAS COMPOSITION ON FORCES AN0 STATIC AN0 VENUS ATMOSPHERE ENTRY A6515619 STABILITY OF PLANETARY ENTRY CONFIGURATIONS IN AIR AN0 ASSUMED MARTIAN ATMOSPHERES ABSORPTION AIAA PAPER 65-318 A65-29766 ABSORPTION AND PHOTOIONIZATION COEFFICIENTS OF PROPYLENE AN0 BUTENE 1 IN VACUUM ULTRAVIOLET - AERMYWMIC HEATIS PLANETARY AERONOMY HYPERSONIC AERODYNAMICS TMRWGH PLANETARY NASA-CR-18 M65-17265 ATMOSPHERES DESCRIBED BY TWO-BODY PROBLEM IN CELESTIAL MECHANICS A6523918 OBSERVED RADIATION SPECTRUM OF VENUS ATMOSPHERE WITH DECREASE IN BRIGHTNESS TEMPERATURE AEROELASTICITY EXPLAINED BY ABSORPTION IN RELATIVELY COLD EQUATIONS OF MOTION FOR ELASTIC BODIES ENTERING SURROUNDING IONOSPHERE N65-24526 PLANETARY ATMOSPHERE AT HYPERSONIC VELOCITIES N66-21667 ABSORPTION BANO I R SPECTROSCOPY OF VENUS USED TO ESTIMATE CARBON AERIHOlll DIOXIDE ABUNDANCE BY MEASUREMENT OF ABSORPTION WOPLASMATRON AS VACUUM ULTRAVIOLET LIGHT SOURCE - BANDS A65- 15691 PLANETARY AERONOMY NASA-CR-16 N65-17263 MATER VAPOR ON MARS AND VENUS. USING PHOTOMETRY OF ABSORPTION BANO WITH BALLOON MOUNTED TELESCOPE VACUUM ULTRAVIOLET LIGHT SOURCES - PLANETARY A6533299 AERONOMY NASA-CR-17 N65-17264 CARBON DIOXIDE ABSORPTION BANDS IN MARS ATMOSPHERE. TRANSMISSION, FUNCTION OF CARBON ABSORPTION AN0 PHOTOIONIZATION COEFFICIENTS OF DIOXIDE AMOUNT AND EFFECTIVE SURFACE PRESSURE PROPYLENE AN0 BUTENE 1 IN VACUUM ULTRAVIOLET - AIM PAPER 66-147 Ab6-19072 PLANETARY AERONOMY NASA-CR-18 1165-17265 IMAGE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN AERONOMICAL AND METEOROLOGICAL STUDIES OF EARTH OISK IN NEAR IR REGION A66-23504 AN0 OTHER PLANETARY ATMOSPHERES N65-24913 INTENSITY MEASUREMENTS OF METHANE ABSORPTION IN VISIBLE REGION OF JUPITERS SPECTROII PLANETARY AERONOMY - PHOTOCHEMISTRY OF PLANETARY NASA-TT-F-10062 1166-23610 ATMOSPHERE, VACUUM AN0 EXTREME ULTRAVIOLET SPECTRAL REGIONS. AN0 THEORETICAL AERONOMY

1-1 AEROSOL SUBJECT INDEX

NASA-CR-68106 N66-12248 OF PLANETS, NEBULAE, ETC, FROH UPPER ATHOSPHERE A65-28940 AEROSOL SEPARATION PROBLEHS OF GAS AN0 AEROSOL COHPONENTS PHOTOGRAPHIC OBSERVATIONS OF RAPIDLY HOVING SPOT IN BRIGHTNESS OF ATMOSPHERIC LAYER FOR PHOTOHETRIC IN JUPITkR ATMOSPHERE DATA PERTAINING TO HARS ATHOSPHERE NASA-CR-64568 N65-32025 A66-19330 ASTRONOHICAL PHOTOMETRY DIFFERENCE BETWEEN VALUES FOR ATMOSPHERIC PRESSURE BRIGHTNESS DISTRIBUTION IN HARGINAL ZONE OF HARS AT MARTIAN SURFACE WHEN OBTAINEO BY PHOTOHETRY OR USE0 TO DETERMINE ATMOSPHERIC ABSORPTION BY SPECTROSCOPY, DUE TO NONCONSIOERATION OF LIGHT Ab5-18972 SCATTERING BY AEROSOL PARTICLES A66-19331 PHOTOMETRIC DETERHINATION OF HARTIAN ATHOSPHERE AND SURFACE OPTICAL THICKNESS AND ABSORPTION AS ATHOSPHERIC REFRACTION, EXTINCTION, AN0 AEROSOL FUNCTIONS OF WAVELENGTHS Ab5-18974 EFFECTS ON ASTROPHYSICAL OBSERVATIONS INCLUDING SIGNIFICANCE OF SURFACE REFLECTANCE AN0 HIGH SURFACE PRESSURE AND CARBON DIOXIDE CONTENT OF ALTITUDE-COSHIC OUST N6b-17747 MARTIAN ATHOSPHERE, COHPARING POLARIMETRIci PHOTOHETRIC AND SPECTROSCOPIC HETHODS AIRBORNE EQUIPHENT A65-26212 BALLOON BORNE IR SPECTROSCOPY INDICATES VENUS CLOUDS CONSIST OF ICE CRYSTALS A65-14707 SEPARATION PROBLEHS OF GAS AN0 AEROSOL COHPONENTS IN BRIGHTNESS OF ATMOSPHERIC LAYER FOR PHOTOHETRIC ALBEDO DATA PERTAINING TO HARS ATHOSPHERE SPECTRAL DISTRIBUTION OF ALBEDO AND LUMINANCE AT A66-19330 CENTER OF DISK FOR DIFFUSING AND ABSORBING PLANETARY ATHOSPHERE A6b-17247 DIFFERENCE BETWEEN VALUES FOR ATMOSPHERIC PRESSURE AT HARTIAN SURFACE WHEN OBTAINEO BY PHOTOHETRY OR PLANETARY RADIATION AN0 ALBEDO EFFECTS ON THERHAL BY SPECTROSCOPY. DUE TO NONCONSIOERATION OF LIGHT BALANCE OF SPACECRAFT ORBITING HARS AN0 VENUS SCATTERING BY AEROSOL PARTICLES NASA-CR-67813 N66-10684 A66-19331

ALUMINUM OXIDE PHOTOMETRIC EXAHINATION OF BRIGHTNESS DISTRIBUTIONA66-19332 KRYPTONATE OXYGEN DETECTOR AND ALUHINUH OXIDE ALON6 DISK OF HARS HYGROHETER FOR USE AS OXYGEN SENSORS FOR PLANETARY ATHOSPHERE SPECTRAL REFLECTING POWER CURVE FOR HARTIAN DISK NASA-CR-63139 N65-25246 CENTER COMPARED WITH TERRESTRIAL EQUIVALENT A66-19333 AMBIPOLAR DIFFUSION HARTIAN IONOSPHERIC OBSERVATIONS MADE BY HARINER OPTICAL PARAHETERS OF HARS ATHOSPHERE AND SURFACE IV INTERPRETED IN TERHS OF HODEL SHOW ATMOSPHERE FROH PHDTOHETRIC DATA FOR SPHERICAL AN0 ELONGATED CONSISTS MAINLY OF CARBON OIOXIOEI LOW TEMPERATURE SCATTERING INDICATRICES 166-19337 AND NO THERHOSPHERE A66-16404 IMA6E CONVERTER TUBE SPECTROPHOTOHETRY OF ZONAL AMMONIA VARIATION OF HETHANE ABSORPTION BANDS ON A66-23504JOVIAN METHANE AN0 AMHONIA LABORATORY SPECTRA COMPARED DISK IN NEAR IR REGION WITH SPECTRA OF JUPITER, INDICATING CAUSES OF UNIOENTIFIEO ABSORPTIONS A65-35022 ASTRWOMICAL SPECTRUH MOLECULAR SPECTROSCOPY IN RELATfON TO SOLAR. APPROXIMATION METHOD PLANETARY, STELLAR, COHETARY AN0 INTERPLANETARY APPROXIMATE SOLUTION OF DIFFUSE REFLECTION AND STUDIES A65-18203 TRANSHISSION OF LIGHT BY FLAT LAYER OF PLANETARY ATHOSPHERE WITH TRUE ABSORPTION CALIBRATION OF HARTIAN SPECTRA USING LABORATORY A65-1897 5 SPECTRA OF PURE CARBON DIOXIDE AN0 IN COHBINATION WITH NITROGEN AN0 ARGON A65-18411 AR60N ARGON ABUNDANCE IN HARTIAN ATHOSPHERE DETECTOR, LABORATORY SPECTRA FROH LEAD SULFIDE SPECTROHETER USING CYLINDRICAL IONIZATION CHAMBER CONTAINING FOR TESTING PRESENCE OF HINOR CONSTITUENTS IN IRON 55 X-RAY SOURCE A65-23098 PLANETARY ATHOSPHERES A65-18419

ATHOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNATION JUPITER ATHOSPHERE. USING SPECTROPHOTOGRAPHIC POINT CONVECTIVE HEAT TRANSFER. USING ARC-HEATED OBSERVATIONS A65-33303 SHOCK TUBE SIHULATING FLIGHT VELOCITIES UP TO 34,000 FPS EARTH. BALLOON AND SATELLITE SPECTROSCOPIC AIAA PAPER 66-29 A66-17891 OBSERVATIONS OF HARS TO DETERHINE ATHOSPHERIC COHPOSITION AN0 PRESSURE AT SURFACE LEVEL ASTROOYNAH ICS A66-21065 COSMIC RESEARCH - PROBLEHS OF CELESTIAL HECHANICS AND ASTRDDYNAHICSI SOLAR CORONA RADIATION IN ASTRONOHICAL TELESCOPE SOFT X-RAY REGION, EARTH HOTIONS IN LUNAR SKY, BALLOON BORNE IR SPECTROSCOPY INDICATES VENUS LIGHT SCATTERING IN PLANETARY ATMOSPHERE CLOUDS CONSIST OF ICE CRYSTALS A65-14107 FTD-TT-64-42/ 16264 N65-24475 RADIO ASTRONOHY SKETCH NOTING SOLAR. GALACTIC AND ASTRONOHICAL OBSERVATORY COSHIC RAY OBSERVATIONS AND INSTRUMENT KITT PEAK OBSERVATORY AN0 CERRO TOLOLO DIFFICULTIES A65-15368 OBSERVATORY - INSTRUMENTATION AN0 OBSERVATIONS N65-19548 REFLECTION SPECTRUH OF CLOUDS IN VENUS ATHOSPHERE MEASURED, USING TELESCOPE MOUNTED ON RESEARCH ACTIVITIES AT HARVARO ASTRONOMICAL HELIUH BALLOON, NOTING DETAILS OF INSTRUHENT OBSERVATORY FROH 1964 THROUGH 1965 166-18055 N66-17617 ASTRONOHY ASTRONOHICAL PHOTOGRAPHY BIBLIOGRAPHY CONTAINING 275 ENTRIES ON 1924 AND 1926 OPPOSITIONS OF MARS IN ASTRONOHICAL SUBJECTS FROH ELEVEN U.S., BRITISH W. H. WRIGHT PLATES NOTING HARS OIAHETER IN IR AND SOVIET TECHNICAL PUBLICATIONS PUBLISHED IN AND UV A65-20633 1964 A65-29113

BALLOON ELEVATED / STRATOSCOPE 11/ REMOTE BIBLIOGRAPHY OF 1964 LITERATURE ON SOLAR SYSTEH CONTROLLED TELESCOPE FOR ASTRONOHICAL OBSERVATION SCIENCE A65-35373

1-2 SUBJECT 1-x

ASTRONWICAL OBSERVATIONS AND PLANETARY SHORT WAVE ABsmpTioll EFFECT ON LOW BRIGHTNESS ATMOSPHERES TENPERATURE OF RADIO EMISSIONS P-2964 165-1 5023 NASA-TT-F-9663 N6S-2 1005

SURFACE DISTURBANCES AS POSSIBLE CAUSE OF TECTONIC CONVECTIVE-RADIATIVE EQUILIBRIUM MODEL FOR MOVENENT IN JUPITER ATMOSPHERE - ASTRONOMY CONPUTING TEMPERATURE PROFILE - VERTICAL 1-439-R N66-10590 TEMPERATURE OISTRIBUTION IN MARTIAN ATMOSPHERE NASA-CR-65049 Nb5-27955 SPACE SCIENCES BIBLIOGRAPHY HIM ABSTRACTS - ASTRONOMY. METEOROLOGY. OCEANOGRAPHY. UPPER EARTH AND PLANETARY ATMOSPHERES. ISOPYCNIC LEVELS. ATMOSPHERE. GEOPHYSICS. SPACE TEMPERATURE DETERMINATION FROM DIFFUSION DATA. JPRS-35095 N66-23025 AN0 TRANSITION MODEL ATNOSPHERES NASA-CR-64008 N65-29122 ASTROPWSICS BOOK ON SOLAR SYSTEM ASTRONOMY AN0 SPACE PHYSICS DERIVATION OF ATMOSPHERIC PARAMETERS ma INCLUDING CELESTIAL MECHANICSI INTERPLANETARY GAS GREENHOUSE MODEL OF VENUS ATMOSPHERE PHYSICS. METEORITES AND PLANETARY ATMOSPHERES NASA-TM-X-53327 N65-35976 A65-17422 EMISSION AN0 ABSORPTION OF RADIANT ENERGY IN NODEL COLLECTION OF SOVIET ARTICLES ON PHYSICS OF MOON MARTIAN ATMOSPHERE COMPOSED OF 15 PERCENT CARBON AND PLANETS A65-18967 DIOXIDE AND 85 PERCENT NITRffiEN BY VOLUME A6615777 HYDROGEN MOLECULES IN ASTROPHYSICS NASA-CR-57156 N65-18918 MARTIAN IONOSPHERIC OBSERVATIONS MADE BY MARINER IV INTERPRETED IN TERMS OF MOOEL SHOW ATMOSPHERE MARTIAN ATMOSPHERE AND SURFACE CHARACTERISTICS - CONSISTS MAINLY OF CARBON DIOXIDE. LOW TEMPERATURE ASTROPHYSICS AND NO THERMOSPHERE A6616404 NASA-CR-68136 N66- 12914 PLANETARY ENVIRONMENTS IN VARIOUS MOOELS RESEARCH ACTIVITIES FROM APRIL THROUGH SEPTEMBER A6620287 1965 - PLANETARY ATMOSPHERES. IONOSPHERIC AN0 RADIO PHYSICS. PARTICLES AND FIELDS. AN0 MARS ATNOSPHERE DEFINITION IMPORTANT IN ADVANCED PLANETOLOGY LANDING VEHIUE DESIGW WITH INCREASED PAYLOAD NASA-CR-68362 N6b-12992 CAPABILITY AND REDUCED COMPLEXITY AIAI PAPER 65-22 A6624697 ATMOSPHERIC REFRACTIDN. EXTINCTION. AND AEROSOL EFFECTS ON ASTROPHYSICAL OBSERVATIONS INCLuDIN6 BEHAVIOR OF PLANETARY HAVES IN ATNOSPHERE MODEL SIGNIFICANCE OF SURFACE REFLECTANCE AND HIGH BASEO UN SPHERICAL HARMONICS ALTITUDE-COSMIC DUST 1166-11747 AFCRL-65-468 N66-10836

ATMOSPHERE PLANETARY ENVIRONMENTAL MOOELS OF VEMSI MARS. ABSENCE OF ELECTRONS IN MARS ATMOSPHERE AN0 MERCURY. JUPITER. PLUTO. NEPTUNE. AND MANUS IMPLICATIONS THEREOF AN0 SATELLITES ATMOSPHERIC COMPOSITION. NASA-CR-64870 N65-33919 TEMPERATURES. AND CIRCULATIOW N66-109% FEASIBILITY AND DESIGN OF BALLOONS FOR EXPLORATION INTERACTION OF SOLAR WIND WITH PLANETS - OF SURFACE AN0 ATMOSPHERE OF MARS PROPERTIES OF INTERPLANETARY MEDIUM A10 N65-34830 THEORETICAL MODELS OF SOLAR WIND N66-14334 ATMOSPHERE MOOEL MARS ATMOSPHERE DEFINITION IMPORTANT IN ADVANCED WMERICAL INTEtRATION OF VARIOUS PLANETARY LANDING VEHICLE DESIGW WITH INCREASED PAYLOAD CIRCULATION PATTERNS IN QUASI-GEOSTROPHIC MOOEL CAPABILITY AN0 REDUCED COMPLEXITY ATNOSPHERE INCLUDIN6 WATER VAPOR. OIAMTIC AIM PAPER 65-22 A65-14563 HEATIW. AND SURFACE FRICTION AFCRL-65-771 N66-16207 THEORETICAL MODELS OF VENUS AND MARS UPPER ATMOSPHERES. NOTING OISSOCIATION LAYERS AND CARBON CALCULATIONS FOR QUASI-GEOSTROPHIC PLANETARY MONOXIDE CONTENT A65-15454 CIRCULATION ATMOSPHERE WITH DIABETIC HEATING AND SURFACE FRICTION N66-16208 COLD ABSORBING ATMOSPHERE MODEL OF VENUS BASEO ON CENTIMETER AN0 MILLIMETER EMISSION SPECTRUM PLANETARY CIRCULATION PATTERNS FOR INTEGRATE0 THO- A65-19676 LEVEL PUASI-GEOSTROPHIC MODEL ATMOSPHERE INCLUDING WATER VAPOR N66-16209 CURRENT PICTURE OF ORI61N AND DEVELOPMENT OF PLANETARY ATMOSPHERES. BEGINNING WITH THEORY OF MOOEL FOR LOWER ATMOSPHERE OF MARS BASEO ON STELLAR EVOLUTION A65-26914 MARINER IV OCCULTATION EXPERIMENT LllSC-b-15-6542 1166-16948 CHEMICAL COMPOSITION AND TENPERATURE IN MODEL OF UPPER ATNOSPHERE 'OF MARS 1165-21 569 MARS ATMOSPHERIC NODELS BASED ON MARINER IV OCCULTATION EXPERIMENT VENUS ATMOSPHERE IN SEVERAL MODELS NOTIN6 NASA-CR-74152 N66-23493 GREENHWSE MODEL B. IONOSPHERIC MODEL. ETC A65-29998 SURFACE TEMPERATURE CALCULATIONS FOR VENUS BASED Ow THO GREENHWSE ATMOSPHERIC MDEL COMPARIYIWS ROTATIONAL. PRECESSIONAL AN0 NUTATIONAL MOTION OF NASA-TM-X-57375 N66-23614 BODY ENTERING MARS ATMOSPHERE IN VERTICAL AND OBLIQUE OIRKTIONS A65-30321 ATMOSPHERIC USOWTIOW MNl36RAPH ON RADIO EMISSION OF SUN AN0 PLANETS HISTORY OF TERRESTRIAL ATMOSPHERE AND DATA ON A6516909 CHEMICAL COMPOSITION OF VENUS ATMOSPHERE A65-33292 PHOTWETRIC OETERMINATION OF MARTIAN ATMOSPHERE AN0 SURFACE OPTICAL THICKNESS AND ABSMIPTIUN AS OUTGASSING PROCESSES ON MOON AND VENUS. USIWG FUNCTIONS OF WAVELENGTHS 1165-18974 EARTH ANALOGY M5-33298 MAUS IR SPECTRA IN 3-4 MICRON REGION ATTRIBUTE0 THEORETICAL MOOEL ATMOSPHERES OF VENUS TO TERRESTRIAL HDO MOLECULES ON BASIS OF SOLAR NASA-TN-D-2527 N65-14117 SPECTRA AND HATER VAPOR ABWDIWCES 1165-19902 VENUS ATMOSPHERE MODEL OF COLD ATMOSPHERE

1-3 ATHOSPHERIC CIRCULATION SUBJECT INDEX

I R LIHB DARKENING OF VENUS EXPLAINED IN TERHS OF 34.000 FPS THREE TYPES OF ATHOSPHERE AN0 CLOUD HOOELS AIAA PAPER 66-29 A6t- 17891 A65-34633 PROBABILITY OF PRESENCE OF NITROGEN, OXYGEN AN0 VENUS ATMOSPHERE MODEL OF COLD ATHOSPHERE WATER IN ATHOSPHERE OF VENUS. BASED ON SHORT WAVE ABSORPTION EFFECT ON LOW BRIGHTNESS SPECTROSCOPIC STUDIES A6619323 TEMPERATURE OF RADIO EHISSIONS NASA-TT-F-9663 N65-21005 SEPARATION PROBLEHS OF GAS AN0 AEROSOL COMPONENTS IN BRIGHTNESS OF ATHOSPHERIC LAYER FOR PHOTOHETRIC ATMOSPHERIC CIRCULATION DATA PERTAINING TO HARS ATHOSPHERE ATMOSPHERIC CIRCULATION ON HARS A66-19330 NASA-CR-262 N65-28631 EARTH. BALLOON AN0 SATELLITE SPECTROSCOPIC EVOLUTION OF GENERAL CIRCULATION PATTERNS IN OBSERVATIONS OF HARS TO OETERHINE ATHOSPHERIC PLANETARY ATMOSPHERES COHPOSITION AN0 PRESSURE AT SURFACE LEVELA66-21065 AFCRL-65-350 N65-30247

SPACE EXPLORATION - SPACE AROUND EARTH, EXPECTED THERHODYNAHIC EQUILIBRIUH COHPOSITION ATMOSPHERIC CIRCULATION AN0 WEATHER CONDITIONS. CALCULATED FOR ATHOSPHERES OF EARTH, VENUS. LUNAR PHOTOGRAPHYI AN0 PLANETARY STUDIES HARS. AN0 JUPITER NASA-EP-25 N65-32574 NASA-CR-69965 N66-16463

CONFERENCES ON ATHOSPHERIC PHYSICS AN0 CHEHISTRY, PLANETARY AN0 EARTH ATHOSPHERIC COHPOSI TION. ATHOSPHERIC CIRCULATION. BIOHETEOROLOGY. TEHPERATURE, AN0 ACTIVITY DATA FROH SATELLITE ENGINEERING. AN0 NEW TECHNOLOGY AN0 SOUNDING ROCKETS N66-19525 PUBL .-9 46 N65-34101 NASA-SP-98 ATMOSPHERIC CIRCULATION AROUND PLANETS OF JUPITER TEHPERATURE DISTRIBUTION. COMPOSITIONI AN0N66-19930 AN0 SATURN N66-14332 IONIZATION OF HARS ATMOSPHERE

ATHOSPHERIC CIRCULATION AN0 CLIHATOLOGY OF VENUS COHPOSITION. PRESSURE. VIOLET LAYER. STRUCTURE, AN0 MARS TEHPERATURE. CLOUDS. AN0 WINOS OF NASA-CR-7 1627 ~66-21767 VENUS ATHOSPHERES HARS AN0N66-23052

ATMOSPHERIC COHPOSITION ATMOSPHERIC DENSITY REPORTS ON HARS FROH LUNAR AN0 PLANETARY CLOSED FORH SOLUTIONS FOR INCLINATION ANGLE AN0 LABORATORY AT UNIVERSITY OF ARIZONA DENSITY OR ALTITUDE AS VELOCITY FUNCTION FOR BODY A65-18475 ENTERING PLANETARY ATHOSPHERE A65-20563

LABORATORY SPECTRA FROM LEA0 SULFIDE SPECTROHETER HARS ATHOSPHERIC MODELS BASEO ON MARINER IV FOR TESTING PRESENCE OF HINOR CONSTITUENTS IN NCULTATION EXPERIHENT PLANETARY ATHOSPHERES A65-10479 NASA-CR-74152 N66-23493

ATHOSPHERE POSTULATION BASEO ON KOZYREV ATMOSPHERIC ELECTRICITY OBSERVATION OF HYDROGEN, ENTRY TRAJECTORY ANALYSIS ATHOSPHERIC ELECTRICAL STUDIES OF OTHER PLANETS BY AND FEASIBILITY OF ATHOSPHERIC BRAKING FOR LANDING STUDIES OF ELECTROHAGNETIC RADIATION BY SUCH PAYLOAD ON HERCURY PLANETS A65-34745 AIAA PAPER 65-494 A65-29604 ATMOSPHERIC ENTRY MATER VAPOR ON MARS AN0 VENUS, USING PHOTOHETRY ORBITER INJECTED STERILIZED BALLISTIC SKIPOUT OF ABSORPTION BAND WITH BALLOON HOUNTEO TELESCOPE CAPSULE FOR IN FLIGHT HARTIAN STRATOSPHERE A65-33299 HEASUREHENTS. USING NONABLATIVE HEAT SHIELD AN0 OUTSIDE ATHOSPHERIC PROPULSION HANEUVERS COMPOSITION OF HARTIAN ATHOSPHERE. USING AIAA PAPER 65-23 A65-15944 POLARIMETRIC OBSERVATIONS A65-33301 AERODYNAMIC BRAKING TRAJECTORIES FOR HARS ORBIT JUPITER ATHOSPHERE, USING SPECTROPHOTOGRAPHIC ATTAINMENT, GIVING ENTRY CORRIDORS FOR LIFTING OBSERVATIONS A65-33303 VEHICLES AIAA PAPER 64-478 A65-28039 VENUS ATHOSPHERIC COHPOSITIONt USING BALLOON TELESCOPE OBSERVATION AN0 IHPLICATIONS FOR HOOEL SPACECRAFT DECELERATION UPON ENTRY INTO HARS ATHOSPHERE A65-33692 ORBIT BY AEROOYNAHIC BRAKING, CONSIDERING VEHICLE SHAPE AN0 VELOCITY EFFECTS ON ENTRY HEATING SURVIVAL AND GROWTH OF TERRESTRIAL HICROORGANISHS AIAA PAPER 64-419 A65-20841 IN AHHONIA-RICH ATHOSPHERES SUPPORTING POSSIBILITY OF ORIGIN AN0 EXISTENCE OF LIFE ON JUPITER DETERHINATION OF PLANETARY ATHOSPHERE STRUCTURE ~65-~1287 FROH HEASUREO ACCELERATION OF ENTRY VEHICLE NASA-TN-0-2669 N65-17110 DETERHINATION OF PLANETARY ATHOSPHERE STRUCTURE FROH HEASUREO ACCELERATION OF ENTRY VEHICLE ATHOSPHERIC BRAKING FOR TRANSFER INTO HARTIAN NASA-TN-0-2669 N65-17118 ORBIT N65-26255 NASA-TN-0-2637 COHPOSITION AN0 THERHOOYNAHIC PROPERTIES OF HARS AN0 VENUS ATMOSPHERES ANALYSIS OF EQUILIBRIUH SHOCK LAYER RADIATION FOR NASA-CR-50811 ~65-17291 HARS ATHOSPHERIC ENTRY N65-32433

RECENT DETERHINATIONS OF COHPOSITION AN0 SURFACE TRANSLATIONAL AND ROTATIONAL HOTION OF SPHERICAL PRESSURE OF MARS ATHOSPHERE BODY ENTERING HARS ATMOSPHERE - REENTRY PHYSICS NASA-CR-290 N65-33035 NASA-CR-69252 N66-15330

BIOLOGICAL SIGNIFICANCE OF HARTIAN ATHOSPHERIC ATHOSPHERIC HEATING COHPOSITIONAL ANALYSIS. AN0 LIFE DETECTION HARTIAN ATHOSPHERIC HEATING FROH SOLAR RADIATION STUDIES OF CHEMICAL FREE ENERGY IN SURFACE ABSORPTION IN UV AN0 VISIBLE BY OXYGEN AN0 OZONE HATTER AN0 IN NEAR IR BY CARBON OIOXIOE, NOTING VERTICAL NASA-CR-67354 N65-36391 DISTRIBUTION OF GASES AN0 ABSORPTION A65-23521 ATHOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNATION POINT CONVECTIVE HEAT TRANSFER, USING ARC-HEATED ATMOSWERIC IOWILATION SHOCK TUBE SIHULATING FLIGHT VELOCITIES UP TO VENUS NIGHT ATMOSPHERE INVESTIGATED BY STUDYING

1-4 SUBJECT INDEX BALLOON FLIGHT

IONOSPHERIC ELECTRON DENSITY AN0 ELECTRON ATMOSPHERIC SCATTERINS AND REFRACTION OF SWLIGHT RECOMBINATION IN NIGHT ATMOSPHERE OF EARTH INTO PLANETARY UMBRA NASA-TT-F-8244 N65-22589 P-3282 N66-20124

CALCULATIONS OF MIDDAY DAYGLOW INTENSITIES ATMOSPHERIC SHELL ARISING FROM FLUORESCENCE OF SOLAR IONIZING SATELLITE AND ROCKET OBSERVATIONS LEADING TO NEW RADIATION ASPECTS OF HETEROSPHERE STRUCTURE NOTING HEAT NASA-CR-64424 1165-31047 BALANCE. PHOTOOISSOCIATION AND GAS DIFFUSION A65-19485 POSITION DETERMINITION OF EQUATORIAL BOUNDARY OF ABNORMALLY HIGH NOCTURNAL ATMOSPHERIC IONIZATION ATMOSPHERIC TEMPERATURE FOR VARIOUS LEVELS OF PLANETARY MAGNETIC ACTIVITY ATMOSPHERIC PRESSURE ANO THIPERATUREBELOW 24 KM A66-19193 USIM SATELLITE MEASUREMENTS OF ATMOSPHERIC LIGHT REFRACTION FROM GIVEN STARS A65-34959 ATMOSPHERIC PRESSUE SPHERICAL SEMIPASSIVE PROBE FOR DENSITY/ALTITUOE MARS UPPER ATMOSPHERE THERMAL STRUCTURE FROM AN0 PRESSURE/ALTITUOE PROFILE OF PLANETARY SPECTROSCOPIC MEASUREMENTS AND MARINER IV ATMOSPHERES, NOTABLY MARS AN0 VENUS OCCULTATION EXPERIMENT A66-23660 A65-19520 COMPOSITION. PRESSURE. VIOLET LAYER, STRUCTUIE. ATMOSPHERIC PRESSURE AND TEMPERATURE BELOW 24 KM TEWPERATURE. CLOUOS. AN0 WINOS OF MARS AND USING SATELLITE MEASUREMENTS OF ATMOSPHERIC LIGHT VENUS ATMOSPHERES N66-23052 REFRACTION FROM GIVEN STARS 1165-34959 ATMOSPHERIC TURWLENCE SURFACE PRESSURE OF MARS ATMOSPHERE REDETERMINED PLANETARY BOUNOARY LAYER MODEL FOR ATIOSPHERIC FROM ABSORPTION INTENSITY OF CARBON DIOXIDE BY WIND AN0 TURBULENCE DISTRIBUTIONS LONG-PATH AN0 PHOTOMULTIPLIER DETECTION N65-22739 A65-35360 ATMOSPHERICS PLANETARY ATMOSPHERE COMPOSITION. TEMPERATURE. AND PRINCIPLES FOR DETERMINING PROPERTIES OF UNKNOWN PRESSURE OF MARS. VENUS. AN0 JUPITER PLANETARY ATMOSPHERE FROM RESPONSES OF NASA-TH-X-56223 w65-20199 REENTERING PROBE VEHICLE NASA-TM-X-56125 N66- 19491 DIFFERENCE BETWEEN VALUES FOR ATMOSPHERIC PRESSURE AT MARTIAN SURFACE WHEN OBTAINEO BY PHOTOMETRY OR ATOMIC caLIsxou BY SPECTROSCOPY. DUE TO NONCONSIOERATION OF LIGHT EXPLOSION IN RAREFIED ATMOSPHERES WHERE EXPLOSIVE SCATTERING BY AEROSOL PARTICLES PRODUCT ATOM MEAN FREE PATH IS LONGER THAN AM-19331 U(PAN0ING MATERIAL DIMENSION. ILLUSTRATING METHOD WITH CHEMICAL EXPLOSION AT 150 KM ALTITUOE EARTH. BALLOON AN0 SATELLITE SPECTROSCOPIC A65-24415 OBSERVATIONS OF MARS TO DETERMINE ATMOSPHERIC COMPOSITION AN0 PRESSURE AT SURFACE LEVEL AUROUL ACTIVITY A66-21065 JUPITER OPTICAL EMISSION AND AURORAL XTIVITY STUW PHOTOELECTRIC OBSERVATION OF ATMOSPHERIC PRESSURE AO-624895 N66-19676 ON MARS SURFACE NASA-CR-7 1312 N66-23776 B ATMOSPHERIC REFRACTION BACTERIA RADIO PATH FORMULAS FOR PLANETARY IONOSPHERES AN0 TERRESTRIAL MICROOR6ANISM SURVIVAL AN0 GROWTH ON STELLAR ATMOSPHERES FROM QUASI-CONIC EQUATION AN0 SPECIMENS OF EUPHORBIA XYLOPHYLLOIOES IN AMMONIA ELECTRON DENSITY EQUATION A65-23429 METHANE HYDROGEN-RICH ATMOSPHERES A65-23486 DIFFRACTION AN0 REFRACTION OF RADIO WAVES TO STUDY PLANETARY ATMOSPHERE A65-29491 BALLISTIC VEHICLE ORBITER INJECTED STERILIZED BALLISTIC SKIPOUT ATMOSPHERIC REFRACTION. EXTINCTION. AN0 AEROSOL CAPSULE FOR IN FLIGHT MARTIAN STRATOSPHERE EFFECTS ON ASTROPHYSICAL OBSERVATIONS IMCLUOIWG MEASUREMENTS. USING MOMABLATIVE HEAT SHIELD AN0 SIGNIFICANCE OF SURFACE REFLECTANCE AND HIGH OUTSIDE ATMOSPHERIC PROPULSION MANEUVERS ALTITUDE-COSMIC OUST N66-11147 AIAA PAPER 65-23 A65- 15944

ATWDSPHERIC SCATTERING LOW SUBSONIC OYNAMIC STABILITY DATA FOR EVALUATION OPTICAL THICKNESS. SCATTERING AN0 AEROSOL PARTICLE OF BALLISTIC DECELERATIOW VEHICLE ENTERIWG MARS CONCENTRATION OF MARS ATMOSPHERE IN UV SPECTRUM ATMOSPHERE A65-19668 NASA-CR-63117 N65-24985

VENUSIAN ATMOSPHERE STRUCTURE AN0 COMPOSITION NEAR MLLMW TOP OF CLOUD COVER. NOTING CARBON DIOXIDE VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE SCATTERING AND TEMPERATURE VARIATION WITH DEPTH INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AND OF A65-25228 STATIC EWILIBRIUM WITHIN KAPLAN ATMOSPHERE A65-19505 OUTWARD FLUX AN0 INTENSITY OF SCATTERED RADIATION FOR TOP OF RAYLEIGH ATMOSPHERE LYING ABOVE SMOOTH PAPERS PRESENTED AT SCIENTIFIC BALLOON WATER SURFACE THAT REFLECTS RADIATION ACCORDING TO SYMPOSIUM ON BALLOON DESIGN. MATERIALS. STRESS FRESNEL LAW STUDIES. INSTRUMENTATION. METEOROLOGY. LOCATING AIM PAPER 65-664 1165-35711 SYSTEM. AN0 PLANETARY EXPLORATION APPLICATIONS AFCRL-65-486 N65-34804 MODEL OF MARS ATMOSPHERE AN0 SURFACE CLOSE TO TERRESTRIAL CONOITIONS. WITH SCATTERING FEASIBILITY AN0 DESIGN OF BALLOONS FOR EXPLORATION ATMOSPHERIC SPECTRUM AN0 SURFACE COVERED WITH OF SURFACE AND ATMOSPHERE OF MARS LIMONITIC OUST A66-19329 N65-34830

OPTICAL PARAMETERS OF MARS ATMOSPHERE AND SURFACE SPECTROSCOPIC OETECTION OF WATER VAPOR IN FROM PHOTOMETRIC DATA FOR SPHERICAL'ANO ELONGATED ATMOSPHERES OF VENUS AN0 MARS USING TELESCOPE SCATTERING INOICATRICES A66-19337 CARRIED BY BALLOON N65-34835

RADIATIVE TRANSFER AN0 IMPERFECT SCATTERING IN BALLOON FLISHT PLANETARY ATMOSPHERES FROM CHAPMAN APPROACH BALLOOW BORNE IR SPECTROSCOPY INDICATES VENUS A66-23414 CLOUDS COWSIST OF ICE CRYSTALS A65-14707

1-5 BALLOOW SOUNDING SUBJECT INDEX

WATER VAPOR ON HARS AN0 VENUS, USING PHOTOHETRY BIOLOGICAL EFFECT OF ABSORPTION BAND WITH BALLOON HOUNTEO TELESCOPE EFFECTS OF SIHULATEO ANAEROBIC PLANETARY A65-33299 ENVIRONHENT ON BIOCHEHICAL ACTIVITIES OF TERRESTRIAL HICROORGANISHS VENUS ATHOSPHERIC COHPOSITION, USING BALLOON NASA-CR-79 195 N66-20131 TELESCOPE OBSERVATION AN0 IHPLICATIONS FOR HOOEL ATHOSPHERE A65-33692 BIOSIHULATION CHAHBER AN0 ELECTRICAL CIRCUIT USED TO SIHULATE BALLOON SOUNDING HARTIAN CONDITIONS FOR HICROBIOLOGICAL STRATOSPHERIC BALLOON OBSERVATIONS OF VENUSIAN INVESTIGATIONS 165-25099 CLWOS INDICATE COMPOSITION OF ICE CRYSTALS A65-28654 BLUNT BOOY FLOW FIELD AROUND SPHERICAL BLUNT BODIES IN GAS BALLOON ELEVATED / STRATOSCOPE 11/ REHOTE EQUILIBRIUH HIXTURES RESEHBLING VARIOUS CONTROLLED TELESCOPE FOR ASTRONOHICAL OBSERVATION PLANETARY ATHOSPHERES - INVERSE HETHOO OF OF PLANETS, NEBULAE, ETC, FROH UPPER ATHOSPHERE FLOW FIELD CALCULATION A65-20940 NASA-TN-0-2780 N65-22367

REFLECTION SPECTRUH OF CLOUDS IN VENUS PLANETARY ENTRY VEHICLES - LONGITUDINAL STABILITY ATHOSPHERE HEASUREO. USING TELESCOPE HOUNTEO ON CHARACTERISTICS FOR VARIOUS BLUNT-BODY HODELS HELIUH BALLOON. NOTING DETAILS OF INSTRUHENT TESTED AT HACH 6.73 IN WINO TUNNEL A66- 10055 NASA-TN-D-2785 N65-22360

BATTERY MLTLMANN EPUATION HIGH ENERGY DENSITY BATTERY FOR USE ON PLANET COLLISIONAL TRANSITION BETWEEN LOWER ATMOSPHERE VENUS AN0 COLLISIONLESS EXOSPHERE ANALYZED, USING NASA-CR-54404 N65-24338 INTEGRAL FORHULATION OF BOLTZHANN EQUATIONA66-20082 AN0 COLLISION HOOELS BEHAVIOR BEHAVIOR OF PLANETARY WAVES IN ATHOSPHERE HOOEL BOUNDARY LAYER BASED ON SPHERICAL HARHONICS PLANETARY BOUNDARY LAYER HOOEL FOR ATHOSPHERIC AFCRL-65-488 N66-10036 WINO AN0 TURBULENCE DISTRIBUTIONS N65-22739 B IBL 106RAPtlY BIBLIOGRAPHY CONTAINING 275 ENTRIES ON BOUIIOARY VALUE ASTRONOMICAL SUBJECTS FROH ELEVEN U.S. , BRITISH HODELS OF MARTIAN THERHOSPHERE WITH CONSTANTS AN0 SOVIET TECHNICAL PUBLICATIONS PUBLISHED IN AND BOUNDARY VALUES IN HYDROSTATIC AN0 HEAT-FLUX 1964 A65-29 113 EQUATIONS N65-28713

BIBLIOGRAPHY OF 1964 LITERATURE ON SOLAR SYSTEM BRAKE SCIENCE A65-35373 ATHOSPHERIC BRAKING FOR TRANSFER INTO HARTIAN ORBIT BIBLIOGRAPHY OF OOCUHENTS ON LUNAR, PLANETARY, NASA-TN-0-2037 N65-26255 AN0 SPACE ENVIRONMENTS IN RELATION TO FLIGHT HECHANICS AN0 AEROOYNAHICS OF SPACE TRAVEL BRIGMNESS NASA-CR-60469 N65- 16006 ORIGIN OF PLANETARY ATHOSPHERES - HICROWAVE BRIGHTNESS HEASUREHENTS OF VENUS N65-31367 PLANETARY ATHOSPHERE - ANNOTATED BIBLIOGRAPHY NASA-SP-7017 N65-20849 BRIGHTNESS TEMPERATURE HEASUREHENTS ON SPACE SCIENCE PROGRAH OF USA - THEORETICAL ILLUHINATEO SIDE OF VENUS AT 10.6 CH CHALLENGES ASPECTS, SUHHARY OF LAUNCHINGS FOR 1964. LIST OF TROITSKI THEORY OF PLANETARY RADIATION EHISSION RESEARCH PROJECTS AN0 AGENCIES, AN0 BIBLIOGRAPHY A66-19457 N65-29509 SUPERCOOLED WATER DROPLETS HYPOTHESIZED IN VENUS PLANETARY UPPER ATHOSPHERES - PRIORITY RATINGS FOR CLOUD LAYER. BASED ON RAOIOHETRIC OBSERVATION IN EXPERIHENTS, TYPES OF HEASUREHENTS FOR SHF RANGE A66-23503 RECOHHENOEO PROGRAH, AN0 ANNOTATED BIBLIOGRAPHY N66-14331 POLARIZATION AN0 BRIGHTNESS TEHPERATURE DISTRIBUTION HEASUREHENTS OF VENUS IN 10.6 CH SPACE SCIENCES BIBLIOGRAPHY WITH ABSTRACTS - WAVELENGTH ASTRONOHYt HETEOROLOGY. OCEANOGRAPHY, UPPER ST-RA-LPS-10334 N66-11138 ATHOSPHEREs GEOPHYSICS. SP.ACE JPRS-35095 N66-23025 PHOTOELECTRIC HEASUREHENT OF BRIGHTNESS OISTRIBUTION IN LIHB ZONE OF HARS BIOASTRONAUTICS NASA-TT-F-10010 N66-23538 PLANETARY ATHOSPHERES, LUNAR STRUCTURES, PARTICLE ENERGY SPECTRA, EXOBIOLOGY, SPACE PHYSIOLOGY, WTWE AN0 ENGINEERING SCIENCES - SPACE SCIENCES ABSORPTION AN0 PHOTOIONIZATION COEFFICIENTS OF NASA-CR-59038 N65-29433 PROPYLENE AN0 BUTENE 1 IN VACUUH ULTRAVIOLET - PLANETARY AERONOHY BIOLOGICAL PROBLEHS IN SPACE-TEXTBOOK NASA-CR-18 N65-17265 A66-00036

BIOCHEMISTRY C POSSIBLE ALTERNATIVE CHEHICAL ELEHENTS AN0 CARBON DIOXIDE COHPOUNOS SUITABLE FOR PROLONGED BIOHOLECULAR RELATION BETWEEN TOTAL ATHOSPHERIC PRESSURE AN0 EVOLUTION AN0 CHEHICAL SELECTION ON NONTERRESTRIAL CARBON DIOXIDE ABUNDANCE OF HARS TYPE PLANET A65-27090 A65-18478

BIOGENESIS HARTIAN ATHOSPHERIC HEATING FROH SOLAR RADIATION HARTIAN LIFE DEPENDS ON CHEHOGENY. BIOGENY, ABSORPTION IN UV AN0 VISIBLE BY OXYGEN AN0 OZONE COGNOGENYt SIMILARITY AN0 OISSIHILARITY TO EARTH AN0 IN NEAR IR BY CARBON DIOXIDE. NOTING VERTICAL AN0 PHYSICAL AN0 CHEHICAL ENVIRONHENT DISTRIBUTION OF GASES AN0 ABSORPTION *65-28200 A65-23521

PHYSICAL CHARACTERISTICS OF UNIVERSE AN0 VENUSIAN ATHOSPHERE STRUCTURE AN0 COHPOSITION NEAR BIOGENESIS OF EXTRATERRESTRIAL LIFE TOP OF CLOUD COVER, NOTING CARBON DIOXIDE *66-BO742 SCATTERING AN0 TEHPERATURE VARIATION WITH DEPTH

1-6 .

SWECT 1-x CLOUD SEEDIWS

A65-25228 PHYSICAL PROPERTY OF VENUS ATMOSPHERE A65-BO868 SURFACE PRESSURE AN0 CARBON DIOXIDE CONTENT OF MARTIAN ATMOSPNREt COMPARIN6 POLARIMETRIC* MARS ATMOSPHERE PROBLEMS RELATE0 TO CHEMICAL PHOTOMETRIC AND SPECTROSCOPIC METHODS COMPOSITION AN0 PHYSICAL PROPERTY 1165-26212 A65-BOB69

SURFACE PRESSURE OF MARS ATMOSPHERE REDETERMINED CHEMICAL ZVOLUTION OF TERRESTRIAL AND CYTHEREAN FROM ABSORPTION INTENSITY OF CARBON DIOXIDE BY AT )(OS PHERES A65-BOB90 LON6-PATH AND PHOTOMULTIPLIER DETECTION A65-35360 EFFECT OF UNCERTAINTIES IN ATMOSPHERIC STRUCTURE AND CHEMICAL COMPOSITION ON ENTRY INTO MARS ABSORPTION INTENSITY OF CARBON DIOXIDE BANDS AND NASA-TN-0-2584 N65-14628 MARTIAN CARBON DIOXIDE ABUNDANCE AN0 ATMOSPHERIC PRESSURE AS BASE OF DESIGN FOR MARS ENTRY VEHICLE MASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE A65-62273 FOR CHEMICAL COMPOSITION STUDY OF MARTIAN ATMOSPHERE SPECTRUMS COMPOSITION AN0 SURFACE PRESSURE. CARBON NASA-CR-71307 N66-23779 DIOXIDE ABUNDANCE* NITR06EN OIOXIOE TESTS. AN0 STRUCTURE OF ATMOSPHERE ON MARS CHEMICAL ENERGY NASA-CR-60264 N65-15223 BIOL06ICAL SIGNIFICANCE OF MARTIAN ATMOSPHERIC COMPOSITIONAL ANALYSISI AN0 LIFE OETECTION MIXTURES OF NITROGEN AN0 CARBON DIOXIDE 6ASES STUDIES OF CHEMICAL FREE ENERGY IN SURFACE HEATED BY SHOCK WAVE REFLECTION TO HIGH MATTER TEMPERATURE AT NORMAL DENSITY - VENUS NASA-CR-67354 N65-36391 ATMOSPHERE SIMULATION NASA-CR-51666 N65- 15370 CHEMICAL RPLOSIOW EXPLOSION IN RAREFIED ATMOSPHERES WHERE EXPLOSIVE THERMOOYNAMIC PROPERTIES OF 15 PERCENT CARBON PRODUCT ATOM MEAN FREE PATH IS LONGER THAN OIOXIOE-B5 PERCENT NITROGEN MIXTURE AT VARIED EXPANDING MATERIAL DIMENSIONt ILLUSTRATING METHOD TEMPERATURE AN0 PRESSURE RANGES WITH CHEMICAL EXPLOSION AT 150 KM ALTITWE STL-9990-6631-TU-000 N65-23299 A65-24615

CARBON DIOXIDE- R-BRANCH LINES OF 5 nu SUB 3 BAND U1EMICAL KINETICS FRIM INTE6RAL OF ABSORPTION COEFFICIENT OF ESTIMATE OF CHEMICAL KINETICS BEHIND NORMAL SHOCK MARTIAN ATMOSPHERE A6615286 WAVES IN CARBON DIOXIDE AN0 NITROGEN MIXTURES FOR MARTIAN ATMOSPHERIC ENTRY CARBON DIOXIOE ABSORPTION BANDS IN MARS NAS A-TN-0-3 267 N66-16940 ATMOSPHERE* TRANSMISSIONS FUNCTION OF CARBON DIOXIDE AMOUNT AN0 EFFECTIVE SURFACE PRESSURE CHEMICAL REICTIQI AIM PAPER 66-147 A66-19072 ENERGY SOURCES AND CHEMICAL REACTIONS IN PREBIOLOGICAL ORGANIC SYNTHESIS PLANETARY ATMOSPHERIC SIMULATION IN SUPERSONIC A65-80473 WIND TUNNELS WITH CARBON DIOXIDE AOOEO TO DRIED AIR WORKING FLUID CIRCULAR ORBIT NASA-CR-60792 N66- 13555 SPACE VEHICLE RECOVERY TRAJECTORIES EXTENDING FROM GIVEN INITIAL ORBIT TO ATMOSPHERE TOP ESTIMATE OF CHEMICAL KINETICS BEHIMI NORMAL SHOCK A65-19314 WAVES IN CARBON DIOXIDE AN0 NITR06EN MIXTURES FOR MARTIAN ATMOSPHERIC ENTRY CISLWM SPACE NASA-TN-0-3287 N66-169+0 RADIO AN0 RADAR ASTRONOMICAL STUDIES ON LUNAR AND PLANETARY IONOSPHERES AN0 ATMOSPHERES* AN0 SOLAR INFRARED SPECTROSCOPY STUDIES TO DETERMINE ACTIVITY ABSORPTION BY CARBOW DIOXIDE BETWEEN B*OOO AM0 NASA-CR-71090 N66-19528 10.000/CM IN 1 TO 1.25 MICRON REGION U-3200 N66-22465 CLImATmOcI ATMOSPHERIC CIRCULATION AN0 CLIMATOL06Y OF VENUS CARBON llOWOXI0E AND MARS THEORETICAL MODELS OF VENUS AN0 MARS UPPER NASA-CR-71627 1166-21767 ATMOSPHERES* NOTING DISSOCIATION LAYERS AN0 CARBON MONOXIDE CONTENT A65-15454 CLOUD COVER PHOTOMETRIC INVESTIGATION OF AUREOLE ELONGATIN6 CELESTIAL llEcwwICS VENUS HORNS AT INFERIOR CfflJUNCTION COSMIC RESEARCH - PROBLEMS OF CELESTIAL MECHANICS A65-17164 AN0 ASTROOYNAMICS~ SOLAR C.ORONA RAOIATION IN SOFT X-RAY REGION* EARTH NOTIONS IN LUNAR SKY. CLWD COVER EFFECT ON 6REENHOUSE MOOEL OF VENUS LIGHT SCATTERING IN PLANETARY ATMOSPHERE ATMOSPHERE FTD-TT-64-42/1&2$4 Nb5-24475 NASA-CR-51176 N65-14655

CELESTIAL OBSERVATION VENUS CLOUD LAYER AND BRIGHTNESS TEMPERATURE FROM SIMILARITY OF COLOR PHENOMENA ON SATURN AND RADIOMETRIC MICROWAVE OBSERVATIONS FROM NOCTURNAL JUPITER LEAOS TO SPECULATION OF SOLAR INFLUENCE SIDE OF PLANET A66-20112 A65-29288 EQUILIBRIUM TEMPERATURE OISTRIBUTIONI THERMAL POSSIBLE ATMOSPHERE DETECTION ON J-I1 AN0 EMISSION* AN0 LIMB FUNCTION COMPUTE0 FOR VENUS J-I11 SATELLITES REVEALED BY EXCESS BRIGHTNESS ON CLWO COVER MOOEL ECLIPSE REAPPEARANCE A66-21202 NASA-TM-X-55392 N66-17231

CHARGED PARTICLE CLOUD GLACIATION INTERPLANETARY GAS AN0 IONOSPHERES OF PLANET - STRATOSPHERIC BALLOON OBSERVATIONS OF VENUSIAN INVESTIGATION USING CHARGED PARTICLE TRAPS CLOUDS INDICATE COMPOSITION OF ICE CRYSTALS N65-16468 A65-28654

CHEMICAL cmrns1TIm CLOUD SEEOING CHEMICAL TRANSFORMATIONS IN OUTER SPACE DISCUSSIN6 MARS ATMOSPHERE MODEL* SOLAR WINO MECHANISM OF OCCURREWE* STATE AN0 BEHAVIOR OF ELEMENTS ON GEOMAGNETIC PULSATIONr AN0 CLOUD SEEOING IN PLANETS* MOON AN0 METEORITES A65-16981 JAPAN N66-19929

PROBLEMS REGARDING CHEMICAL COMPOSITION AND

1-7 COHERENT TRANSMISSION SUBJECT INDEX

COHERENT TRANSMISSION EFFECTS ON ASTROPHYSICAL OBSERVATIONS INCLUDING COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE SIGNIFICANCE OF SURFACE REFLECTANCE AND HIGH AN0 IONOSPHERE OF MARS INCLUDING DENSITY, ALTITUDE-COSMIC DUST N6b-17747 TEMPERATURE, SCALE HEIGHT, ETC Ab5-36328 COSMIC RADIATION COMBUSTION TEHPERATURE SOUNDING ROCKET FLIGHT TO MEASURE COSMIC RADIATION IGNITION TEMPERATURES OF POWDERED METALS IN INTENSITY AND STUQIES OF MARTIAN ATMOSPHERE AND SIMULATED ATMOSPHERES OF VENUS AND MARS SUGGEST IONOSPHERE POTENTIAL CHEMICAL ENERGY SOURCES NASA-CR-74173 Nb6-23713 Abb-22458

COMET D CLOSE APPROACH OF METEOR STREAMS AND COMETS TO DATA ACQUISITION MARS ORBIT AN0 RELATION TO BLUE CLEARING OF ENTRY VEHICLE DESIGN FOR PLANETARY EXPLORATION ATMOSPHERE A65-15342 USING NONSURVIVING NEEDLE-NOSE0 PROBE FOR DATA COLLECTION ON MARS ATMOSPHERE COMPOSITIONI COMMUNICATION SYSTEM PRESSURE AND DENSITY SCIENTIFIC RESEARCH USING INSTRUMENTS IN SPACE AIAA PAPER 65-493 Ab5-32321 VEHICLESI NOTING DIRECT OBSERVATIONS OF MOON, VENUS, MARS, GLOBAL COMMUNICATIONS, METEOROLOGY, DEEP SPACE GEODETIC AND NAVIGATION SATELLITES, ETC DEEP SPACE, SOLAR PROBE, AND OUT-OF-ECLIPTIC A66-23639 TRAJECTORIES UTILIZING LARGE PLANETARY PERTURBATIONS COMMUNICATIONS SATELLITE NASA-CR-69222 N6b-15224 SOLAR SPACE ENVIRONMENT, AND METEOROLOGICAL AND COMMUNICATIONS SATELLITES - CONFERENCE PROCEEDINGS DENSITY DISTRIBUTION NASA-CR-60132 Nb5-15488 SPHERICAL SEMIPASSIVE PROBE FOR OENSITYIALTITUDE AND PRESSURE/ALTITUDE PROFILE OF PLANETARY CONE ATMOSPHERES, NOTABLY MARS AND VENUS LAMINAR AN0 TURBULENT CONVECTIVE HEAT TRANSFER A6519520 RATES ON CONES IN PLANETARY ATMOSPHERES RAD-TM-b4-68 N65-19405 DENSITY MEASUREMENT RADIATION GAUGING METHODS FOR UNMANNED PROBE TO CONFERENCE MEASURE MARTIAN ATMOSPHERIC DENSITY DURING INSTITUTE OF ENVIRONMENTAL SCIENCES CONFERENCE ENTRY ON ENVIRONMENTAL RELATIVITY AT CHICAGO IN APRIL NASA-CR-6297 1 Nb5-24895 1965 Ab5-29982

CONFERENCE ON ORIGIN AN0 EVOLUTION OF ATMOSPHERES DETECTION AND OCEANS AT NEW YORK CITY IN APRIL 1963 PHYSICAL METHODS DESCRIPTION FOR DETECTION AN0 Ab5-33289 ANALYSIS OF TENUOUS PLANETARY ATMOSPHERIC COMPONENT GASES, ESPECIALLY WATER VAPOR SOLAR SPACE ENVIRONMENT, AN0 METEOROLOGICAL AN0 NASA-CR-70934 N6b-19901 COMMUNICATIONS SATELLITES - CONFERENCE PROCEEDINGS ENGINEERING BREADBOARD MODEL OF MICROORGANISM NASA-CR-60132 Nb5-15488 DETECTION DEVICE FOR MARS LANDING APPLICATIONS NASA-CR-74214 Nb6-23787 CONFERENCES ON ATMOSPHERIC PHYSICS AND CHEMISTRY, ATMOSPHERIC CIRCULATION* BIOMETEOROLOGY, DIFFUSE RAOIATIOK ENGINEERING, AND NEW TECHNOLOGY APPROXIMATE SOLUTION OF DIFFUSE REFLECTION AN0 PUBL.-946 Nb5-34101 TRANSMISSION OF LIGHT BY FLAT LAYER OF PLANETARY ATMOSPHERE WITH TRUE ABSORPTION PAPERS PRESENTED AT SCIENTIFIC BALLOON Ab5-18975 SYMPOSIUM ON BALLOON DESIGN, MATERIALS. STRESS STUDIES, INSTRUMENTATION, METEOROLOGYs LOCATING SYSTEM, AND PLANETARY EXPLORATION APPLICATIONS DIURNAL VARIATION AFCRL-65-486 ~65-34804 THEORY OF DIURNAL VARIATION OF MARTIAN SURFACE TEMPERATURE - GROUND AN0 ATNOSPHERE OF MARS ATMOSPHERES OF VENUS AND MARS- ASTROPHYSICS NASA-CR-63278 Nb5-26075 CONFERENCE* KIEV, UKRAINIAN SSR, JUNE 1964 Abb-19322 VARIATION OF IR EMISSION FROM MARS SURFACE WITH MARS LOCAL TIME IN TERMS OF DIURNAL TEMPERATURE PLANETARY ATMOSPHERES AND SURFACES - SYMPOSIUM, VARIATIONS, INCLUDING ATMOSPHERE EFFECT, RESULTS DORAOO. PUERTO RICO, MAY 1965 SUGGEST Low THERHOCONDUCTIVITY Ab6-2 1201 A66-20101 ORA6 CONTAMINATION SPACECRAFT DECELERATION UPON ENTRY INTO MARS MARS ENVIRONMENTAL FACTORS SUGGESTING BIOLOGICAL ORBIT BY AERODYNAMIC BRAKING, CONSIDERING VEHICLE POSSIBILITIES AND LIFE DETECTION EQUIPMENT TO SHAPE AN0 VELOCITY EFFECTS ON ENTRY HEATING PREVENT CONTAMINATION A65-82218 AIAA PAPER 64-479 Ab5-28841 CONVECTIVE HEAT TRANSFER LONG LIFETIME ORBITS ABOUT MARS AFFECTED BY LAMINAR AND TURBULENT CONVECTIVE HEAT TRANSFER ATMOSPHERIC DRAG, SOLAR GRAVITATIONAL RATES ON CONES IN PLANETARY ATMOSPHERES PERTURBATIONS, PLANETARY OBLATENESS AN0 OTHER RAD-TM-64-68 N65-19405 PERTURBATIONS AIAA PAPER 66-35 A6b- 18987 ATMOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNATION POINT CONVECTIVE HEAT TRANSFER, USING ARC-HEATED SHOCK TUBE SIMULATING FLIGHT VELOCITIES UP TO WDPLASMATRON 34,000 FPS DUOPLASMATRON AS VACUUM ULTRAVIOLET LIGHT SOURCE - AIAA PAPER 66-29 A6b-17891 PLANETARY AERONOMY NASA-CR-16 Nb5-17263 COSMIC OUST MARTIAN BLUE HAZE PROPERTIES CORRELATED WITH DYNAMIC STABILITY INTERPLANETARY DUST. METEOR SHOWERS AN0 SOLAR LOW SUBSONIC DYNAMIC STABILITY DATA FOR EVALUATION FLARES A65-26040 OF BALLISTIC DECELERATION VEHICLE ENTERING MARS ATMOSPHERE ATMOSPHERIC REFRACTION, EXTINCTION, AND AEROSOL NASA-CR-63117 Nb5-24985

1-8 SUBJECT 1-X ERROR FultTIDll

ELEMENT ABWlDMCE E LECTURES FROM TRY SPACE TECHNOLOGY EARTH LABORATOR1 ES A6S-32 62 0 MULTIOISCIPLINARY RESEARCH IN SPACE RELATE0 SCIENCE AN0 TECWOLOGY - EVOLUTION PROCESSES OF LECTURE MANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONS. ATMOSPHERE. MOON. EARTH. AN0 PLANETS BIOLOGICAL EXPLORATION OF MARS. MASERS AN0 NASA-CR-69137 N66-15068 LASERS. PLANETARY ATMOSPHERES. RELATIVITY THEORY, ELEMENT ABUNDANCE. AN0 SOLAR PARTICLES EARTH ATMOSPHERE N65-31360 MARS ATMOSPHERE PROPERTIES OISTINGUISH IT FROM EARIH ATMOSPHERE. PARTICULARLY WATER CONTENT. AWNOANCE AN0 STABILITY OF MAJOR SULFUR COMPOUNOS THERMAL FLDWS AN0 AIR MASSES CIRCULATION IN LOWER ATMOSPHERE OF VENUS CALCULATED. ASSUMIN6 A65-19853 EQUILIBRIUM BETWEEN ATMOSPHERIC GASES AND NINEML PHASES A6619262 EVOLUTION OF THE ATMOSPHERES OF THE EARTH AN0 PLANETS A65-BO370 EMISSION VENUS RADIO SPECTRUM AN0 MICROWAVE EMISSION OF CHEMICAL EVOLUTION OF TERRESTRIAL AN0 CYTHEREAN ATMOSPHERIC MOLECULAR OXYGEN ATMOSPHERES A65-BO890 MSA-CR-57309 N65-19770

EARTH AN0 PLANETARY ATMOSPHERES. ISOPYCNIC LEVELS. EMISSIOW SPECTRUM TEMPERATURE OETERMINATION FROM OIFFUSION DATA. KOLYREV HYDROGEN EMISSION LINES IN IR AN0 TRANSITION MOOEL ATMOSPHERES SPECTROGRAMS OF MERCURY NOTING CORE EMISSION NASA-CR-64008 N65-29722 A65-23491

EARTH- MARS COMPARISON OF VERTICAL TEMPERATURE EUEW DEUSITY DISTRIBUTION AN0 HEAT BALANCE IN ATMOSPHERE HIW ENERGY DENSITY BATTERY FOR USE ON PLANET NASA-CR-68992 N66-14260 VENUS NASA-CR-54404 N65-24338 PLANETARY AN0 EARTH ATMOSPHERIC COMPOSITION. TEMPERATURE. AN0 ACTIVITY DATA FROM SATELLITE EUE(L61 SOURCE AN0 SOUNDING ROCKETS ENERGY SOURCES AN0 CHENICAL REACTIONS IN NASA-SP-96 M6-19525 PREBIOLffiICAL ORGANIC SYNTHESIS EARTH MOTIffl A6560473 COSMIC RESEARCH - PROBLEMS OF CELESTIAL MECHANICS AN0 ASTRODYNAMICS. SOLAR CORONA RAOIATION IN EIEW SCECTRWI SOFT X-RAY REGION. EARTH MOTIONS IN LUNAR SKY* PLANETARY ATMOSPHERES. LUNAR STRUCTURES. PARTICLE LIGHT SCATTERING IN PLANETARY ATMOSPHERE ENERGY SPECTRA. EXOBIOLOGY. SPACE PHYSIOLOGY. FTO-TT-64-42/1&2&4 N65-2447 5 AN0 ENGINEERING SCIENCES - SPACE SCIENCES NASA-CR-59038 N6529433 ECLIPSE POSSIBLE ATMOSPHERE OETECTION ON J-I1 AN0 EWROPY J-I11 SATELLITES REVEALED BY EXCESS BRIGHTNESS ON EQUILIBRIUM THERMOOYNAMIC PROPERTIES /ENTROPY. ECLIPSE REAPPEARANCE A66-21202 ENTHALPY. PRESSURE. AN0 SOUNO SPEED/ OF THREE ELASTIC UIGINEERING MODELS OF MARTIAN ATMOSPHERE BOOY NASA-SP-3021 N65-35792 EQUATIONS OF MOTION FOR ELASTIC BODIES ENTERIWG PLANETARY ATMOSPHERE AT HYPERSONIC VELOCITIES ENVIurm(ENT SIIIIILATIOIY N66-21667 RESPONSE OF MICRWRCANISM TO SIMULATE0 MARTIAN ELECTROMAWETIC 'PROPA6ATIOW ENVIRONMENT INVESTI6ATEO. USING CULTURE ELECTROMAGNETIC PROPAGATION CHARACTERISTICS OF COLLECTIONS AN0 SOIL SAMPLES A65-30676 VENUS AND MARS DERIVE0 FROM ATMOSPHERIC DATA A66-16436 ATMOSPHERES CAPABLE OF PRODUCING OR6ANIC WMPOUNOS DISCUSSED. STUDTIN6 ABIOGENIC SYNTHESIS IN MARS ELECTROMAGNETIC RADIATION SIMULATOR A65-30683 EXPECTED OIFFRACTION EFFECTS ON ELECTROMAGNETIC RAOIATION FROM MARINER IV DUE TO MARTIAN SIMULATION OF HEAT TRANSFER ENVIRONWENTS OF SPACE ATMOSPHERE AN0 OCCULTATION A66-16039 VEHICLE ENTERING PLANETARY ATMOSPHERE WITH SUPER~RBITAL VELOCITY ELECTROMA6NETIC WAVE R64S073 N65-15600 ELECTROMAGNETIC HAVE SCATTERING IN HOMOGENEOUS PLANE-PARALLEL ATMOSPHERES - SOLAR RAOIATION PNEUMATIC SURFACE SAMPLING DEVICE FOR USE IN TRANSFER IN PLANETARY ATMOSPHERE SIMULATE0 MARS ENVIRONMENT RM-4646-PR 1166-19418 NASA-CR-70937 N66-20080

ELECTRON EFFECTS OF SIMUATEO ANAEROBIC PLAWTARY ABSENCE OF ELECTRONS IN MARS ATMOSPHERE AN0 ENVIRONMENT Ow BIOCHEMICAL ACTIVITIES OF IMPLICATIONS THEREOF TERRESTRIAL MICROORGANISMS NASA-CR-64870 N65-33919 NASA-CR-71195 N66-20131

ELECTRON DENSITY PROFILE ENVIROII((EIITM CWW GALACTIC AN0 PLANETARY RADIO ASTRONOMY - SOUNOIN6 CHAMBER AN0 ELECTRICAL CIRCUIT USE0 TO SIMULATE ROCKET LAUNCH. ORBITING TELESCOPES CARBON-OXYGEN MARTIAN CONOITIONS FOR MICROBIOLOGICAL COMPLEX PHOTOCHEMISTRY. MARS IONOSPHERE. INVESTISATIONS A65-25099 TOPSIDE ELECTRON DENSITY. AN0 NONRIGID BODIES NASA-CR-70152 N66-16597 EWVIRDMREWIAL SCIEWCE INSTITUTE OF ENVIRONMENTAL SCIENCES CONFERENCE ELECTRON INTERACTIffl ON ENVIRONMENTAL RELATIVITY AT CHICAGO IN APRIL SPECTROSCOPY OF PLANETARY ULTRAVIOLET RAOIATION - 1965 165- 29962 RAYLEIGH SCATTERING AND ELECTRON EXCITATION NASA-CR-67597 N66-15400 EWILIBRIUM EWILIBRIUM THERMOOYNAMIC PROPERTIES /ENTROPY. ELECTRON REC~INATION ENTHALPY* PRESSURE. AN0 SOUNO SPEED/ OF THREE VENUS NIGHT ATMOSPHERE INVESTIGATED BY STWYING EWINEERING MODELS OF MARTIAN ATMOSPHERE IONOSPHERIC ELECTRON DENSITY AN0 ELECTRON NASA-SP-3021 N65-35792 RECOMBINATION IN NIGHT ATMOSPHERE OF EARTH NASA-11-F-E244 N65-22589 ERROR FUNCTION ESTIMATING ERRORS IN OENSITY AN0 PRESSURE STRUCTURE OF PLANETARY ATMOSPHERE CONSTRWTEO

1-9 EVOLUTION SUBJECT INDEX

FROH HEASURED ACCELERATIONS OF ENTRY VEHICLE HARS ENVIRONHENTAL FACTORS SUGGESTING BIOLOGICAL NASA-TR-R-225 N65-29299 POSSIBILITIES AN0 LIFE DETECTION EPUIPHENT TO PREVENT CONTAHINAT ION A65-82218 EVOLUTION EVOLUTION OF THE ATHOSPHERES OF THE EARTH AND EVIDENCE FOR LIFE ON HARS - NATURE AND PLANETS A65-BO370 UNCERTAINTIES NASA-CR-58430 N65-2941 5 ORIGIN AND EVOLUTION OF PLANETARY ATHDSPHERES AND OCEANS A65-80889 HARTIAN LIFE IN LIGHT OF HARINER IV DATA ON ADVERSE ATHOSPHERIC COHPOSITIONt TEHPERATURE AND SURVIVAL AND GROWTH OF TERRESTRIAL HICRODRGANISHS RADIAT ION A66-21740 IN AHHONIA-RICH ATHOSPHERES SUPPORTING POSSIBILITY OF ORIGIN AND EXISTENCE OF LIFE ON JUPITER HARS ENVIRONHENTAL CONDITIONSt LIFE ORGANISH A65-8 1207 OETECTION, EVALUATION AND LIHITING EFFECTS A66-22715 HULTIDISCIPLINARY RESEARCH IN SPACE RELATED SCIENCE AND TECHNOLOGY - EVOLUTION PROCESSES OF SPACE TRAVEL AND EXPLORATION, BIOLOGICAL AND ATHOSPHEREs HODNt EARTHt AND PLANETS TECHNICAL DIFFICULTIES, RADIATIONt HETEOR A66-23640IHPACTt NASA-CR-69137 N66-15068 VEHICLE STERILIZATIONt ETC

EXTRATERRESTRIAL ENVIRDNHENT EXTRATERRESTRIAL LIFE IN SOLAR SYSTEH. DISCUSSING SEED GERMINATION OF COHHDN PLANT SPECIES IN EQUIPHENT FOR HARS EXPLORATION, NOTING GULLIVER RAREFIED NITROGEN ATHOSPHERES SIHULATING PROGRAHt HULTIVATOR AUTOHATIC BIOCHEHICAL TESTING EXTRATERRESTRIAL ENVIRONHENT A65-32416 APPARATUS AN0 TV HICROSCDPE A66-23794 EXTRATERRESTRIAL LIFE LIFE ON HARS - CONDITIONS, POSSIBLE TYPES OF EVIDENCE FOR LIFE ON HARS IS SEASONAL WAVE OF DRGANISHS AND THEORIES OF ADVANCED FORHS OF LIFE DARKENING AND ASSOCIATED CHANGES IN POLARIZATION A66-80582 OF DARK AREAS A65-15140 PHYSICAL CHARACTERISTICS OF UNIVERSE AND CHEHICAL TRANSFORHATIONS IN OUTER SPACE DISCUSSING BIOGENESIS OF EXTRATERRESTRIAL LIFE OCCURRENCEt STATE AND BEHAVIOR OF ELEHENTS ON A66-80742 PLANETS. HODN AND HETEDRITES A65-16981 BIOL06ICAL PROBLEHS IN SPACE-TEXTBOOK HARS NITROGEN OXIDES OBSERVED AT DIFFERENT A66-80836 WAVELENGTHSt CDHPUTING PHOTDCHEHICAL EQUILIBRIA POINT AN0 ROLE IN BLUE HAZE A65-17992 EXISTENCE AND DETECTION OF LIFE ON HARS A66-00972 AUTOHATEO BIOLOGICAL LABORATORY FOR DETECTION AND CLASSIFICATION OF LIFE ON HARS A65-19518 F FAR ULTRAVIOLET PLANETARY LIFE EFFECT ON BIOLOGICAL PRECURSOR PLANETARY AERDNOHY - PHOTOCHEHISTRY OF PLANETARY HISSIONS TO HARS ATHOSPHEREt VACUUH AND EXTREHE ULTRAVIOLET AIAA PAPER 65-249 A65-22120 SPECTRAL REGIONS, AND THEORETICAL AERDNOHY NASA-CR-68106 N66-12248 TERRESTRIAL HICROORGANISH SURVIVAL AND GROWTH ON SPECIHENS OF EUPHORBIA XYLDPHYLLDIDES IN AHHDNIA FLI6HT PATH HETHANE HYDROGEN-RICH ATHOSPHERES CLOSED FORH SOLUTIONS FOR INCLINATION ANGLE AND A65-23486 DENSITY OR ALTITUDE AS VELOCITY FUNCTION FOR BODY ENTERING PLANETARY ATHOSPHERE A65-20563 POSSIBLE WATER SOURCE BENEATH HARS SURFACE DUST AND ICE HAY CONSTITUTE POTENTIAL BIOSPHERE FLIM SIHULATION A65-26720 SIHULATED HARTIAN ENTRY CONDITIONS IN EARTH TEST PRDGRAH SHOWING REQUIREHENTS FOR LAUNCH VEHICLEt I R SPECTROSCOPY ROLE IN BIOLOGICAL EXPLORATION OF TRACKING, COST AND SCHEDULE HARS PROVIDING DATA ON ATHOSPHERIC AND SURFACE AIAA PAPER 65-219 A65-17398 PARAHETERS A65-26729 FLDY FIELD HARTIAN LIFE DEPENDS ON CHEHOGENY, BIOGENYt FLOW FIELO AROUND SPHERICAL BLUNT BODIES IN GAS COGNOGENY, SIHILARITY AND DISSIHILARITY TO EARTH EQUILIBRIUH HIXTURES RESEHBLING VARIOUS AND PHYSICAL AND CHEHICAL ENVIRONHENT PLANETARY ATHDSPHERES - INVERSE HETHOD OF A65-28200 FLOW FIELD CALCULATION NASA-TN-0-2780 ~65-22367 RESPONSE OF HICROORGANISM TO S HULATED HARTIAN ENVIRONMENT INVESTIGATED. USINE CULTURE FLUORESCENT EHISSION COLLECTIONS AND SOIL SAHPLES A65-30676 CALCULATIONS OF HIDDAY DAYGLOW INTENSITIES ARISING FRDH FLUORESCENCE OF SOLAR IONIZING HARTIAN CONDITIONS SIHULATED FROH ASTROPHYSICAL RADIAT ION DATA FOR MICRO0IOLOGICAL INVESTIGATIONS NASA-CR-64424 N65-31047 A65-30602 FLWV HISSION SOHE FORHS OF LIFE FOUND ON EARTH WHICH CAN HARS SURFACE AND ATHOSPHERE CHARACTERISTICS FRDH SURVIVE CONDITIONS THOUGHT TO EXIST ON HARS THERHAL EHISSION SPECTRUH HEASUREMENT BY A65-81013 INFRARED INTERFERDHETER ON PLANETARY FLYBY SPACECRAFl CHARACTERISTICS OF HARS AND POSSIBILITY OF NASA-TH-X-55070 N65-32114 EXISTENCE OF LIFE A65-81018 JUPITER FLYBY HISSIDNS - FUTURE STUDIES ON PLANET HARS COLOR CHANGES EXPLAINED ON BASIS OF PHYSICAL ATHDSPHERE AND HAGNETOSPHERE HODEL A65-81159 NASA-CR-69561 N66-15807

SURVIVAL AND GROWTH OF TERRESTRIAL HICROORGANISHS FRESNEL REFLECTOR IN AHHONIA-RICH ATHOSPHERES SUPPORTING POSSIBILITY OUTWARD FLUX AND INTENSITY OF SCATTERED RADIATION OF ORIGIN AND EXISTENCE OF LIFE ON JUPITER FOR TOP OF RAYLEIGH ATHOSPHERE LYING ABOVE SHOOTH

A65-81287 YATER~ SURFACE ~~ THAT REFLECTS RADIATION ACCORDING TO FRESNEL LAW PHYSICAL BASIS FOR EXTRATERRESTRIAL LIFE DETECTION AIAA PAPER 65-664 A65-35711 AND USE ON HARS A65-81737

1-10 SUBJECT Imfx

RAREFIED NITROGEN ATMOSPHERES SIMULATING G EXTRATERRESTRIAL ENVIRONMENT A65-32416

MS urn OISCHLllCE PHOTOGRAPHIC SPECTRA OF PLANETARY ATMOSPHERE GASES RAOIO NOISE EMISSION FROM VENUS SURFACE EXPLAIED OF MARS AN0 JUPITER IN TERMS OF GLOW DISCHARGE A6617174 AO-606352 N65-16776 SMVITATIOWL FIKD 6AS ANALYZER SATELLITE AN0 ROCKET OBSERVATIONS LEADING TO NEW POLAROGRAPHIC OXYGEN ANALYZER FOR OBTAINING DATA ASPECTS OF HETEROSPHERE STRUCTURE NOTIN6 HEAT ON MARS ATMOSPHERIC COMPOSITION BALANCE. PHOTODISSOCIATION AND WS DIFFUSION NASA-CR-57085 N65-18098 A65-19485

PHOTOIONIZATION MASS SPECTROMETER WITH 180 DE6 JUPITER AN0 SATURN INTERIOR TEMPERATURES FROM MAGNETIC ANALYZER AND USE AS 6AS ANALYZER EXAMINATION OF ATMOSPHERIC COMPOSITION AN0 NASA-CR-71210 N66-19636 GMVITATIO)(U MULTIPOLE MOMENT A65-33302

6AS COlPOSITIOU SMY c1s APPROXIMATE AND CHARACTERISTICS METHOOS TO PREDICT HOPF ANALYTICAL SOLUTIMI FOR 6REENHOUSE PARAMETER EFFECT OF GAS COMPOSITION ON FORCES AN0 STATIC IN GRAY PLANETARY ATMOSPHERE STABILITY OF PLANETARY ENTRY CONFIGURATIONS IN AIR NASA-TM-X-5662 1 N6622218 AND ASSWED MARTIAN ATMOSPHERES AIM PAPER 65-318 A65-29766 6REEMOUSE EFFECT YEWS ATIKISPHERE IN SEVERAL MODELS NOTIK GAS DYNAMICS GREEWHOUSE MOEL E* IONOSPHERIC MOMLt ETC SHOCK TUBE GAS DYNAMIC CHARTS SUITABLE FOR MRS A65-29998 ATMOSPHERE RAD-TH-65-23 N65-25727 THERMAL EMISSION MAPS OF JUPITER. OISCUSSING SOURCE OF NOISE FROM TRACKIN6 ERRORS AN0 645 MIXTURE PIUITOWETRIC ERRORS A6531279 THERMODYNAMIC PROPERTIES OF 15 PERCENT CARBON DIOXIOE-65 PERCENT NITROGEN MIXTURE AT VARIED CLOUO COVER EFFECT Ow GREENHOUSE MODEL OF VENUS TEMPERATURE AN0 PRESSUIE RINSES ATMOSPHERE STL-9990-6631-TU-000 N65-23299 NASA-CR-51176 N65-14655

ESTIMATE OF CHEMICAL KINETICS BEHIM NORMAL SHOCK DERIVATION OF ATMOSPHERIC PARAMETERS ma WAVES IN CARBON DIOXIDE AN0 NITROGEN MIXTIJRES GREENHOUSE MOOEL OF VENUS ATMOSPHERE FOR MARTIAN ATMOSPHERIC ENTRY NASA-TH-X-53327 N65-35976 NASA-TN-0-3287 N66-16WO HOPF ANALYTICAL SOLUTIOM FOR VALUES OF RATIO OF 6EOtHEllISTRY GRAY ABSORPTION COEFFICIENTS FOR INSOLATIN6 AN0 HISTORY OF TERRESTRIAL ATMOSPHERE AN0 DATA ON ESCAPING RADIATION /GREE"DUSE PARAMETER/ ASSUME0 CHEMICAL COMPOSITION OF VENUS ATMOSPHERE CONSTANT AT ALL DEPTHS* PRESENTIN6 TERERATURE AS-33292 OISTRIBUTION GRAPHS A66-212OI

REMOTE MEASUREMENT OF TRACE AMOUNTS OF VAPORS IN HOPF ANALYTICAL SOLUTION FOR GREENHOUSE PARAMETER LUNAR AN0 PLANETARY ATMOSPHERES AS INOICAMR OF IN GRAY PLANETARY ATMOSPHERE BIOLOGIC AND 6EOL06IC SURFACE CONDITIONS NASA-TH-X-56621 1166-22218 1166-21532 SURFACE TEMPERATURE CALCULATIONS FOR VENUS BASED ~EOLOW ON TWO GREENHOUSE ATMOSPHERIC OWL COMPARISMIS CONFERENCE ON ORIGIN AN0 EVOLUTION OF ATMOSPHERES NASA-TH-X-57375 N66-23674 AND OCEANS AT NEW YORK CITY IN APRIL 1963 A65-33289 6Rm SURVIVAL AN0 GROWTH OF TERRESTRIAL MICROOR6ANISMS GE011A6NETIC PULSATION IN AMMONIA-RICH ATMOSPHERES SUPPORTINS POSSIBILITY MARS ATMOSPHERE MODEL* SOLAR WINO MECHANISM OF OF ORIGIN AND EXISTENCE OF LIFE ON JUPITER GEOMA6NETIC PULSATION. AND CLOUO SEEDING IN A65-61267 JAPAN N66-19929 WIDUlCE AN0 CowTRaL GEOlElRICAL OPTICS VOYAGER SUBSYSTEM OESIGW STMY - 6UIDANCE AN0 JUPITER PI.r)TOELECTRIC SPECTRAL SCAN IN UV COllTROL. PROPULSION. AN0 POWER SUPPLY STUDIES REPRODUCE0 AS GEOMETRIC REFLECTIVITI VS FOR ENTRY IN MARS OR VEMJS ATMOSPHERES WAVELEN6TH. USING AEROBE€ ROCKET HAS A-CR-5 1831 N66-13407 A66-21099 WLLIYE11 P10611UI CEOPHYS ICs EXTRATERRESTRIAL LIFE IN SOLAR SYSTEM. DISCUSSING SPACE SCIENCES BIBLIOGRAPHY WITH ABSTRACTS - EWIPMENT FOR MARS EXPLORATION^ NOTIN6 SULLIVER ASTRONOMY* METEOROLOGY* OCEANOGRAPHY* UPPER PROGRAM. MULTIVATOR AUTOMATIC BIOCHEMICAL TESTIS ATMSPHERE. GEOPHYSICS. SPACE APPARATUS AND TV MICROSCOPE A6623794 JPRS-35095 1166-23025

GEOSTROPHIC WINO H NUMERICAL INTEUIATION OF VARIOUS PLANETARY MBITAlILITY CIRCULATION PATTERNS IN QUASI-GEOSTROPHIC MODEL PLANETS HABITABLE FOR MAN A6S-BO977 ATMOSPHERE INCLUDING WATER VAPOR. DIABATIC HEATING. AN0 SURFACE FRICTION SOME FORMS OF LIFE FOUND ON EARTH WHICH CAN AFCRL-65-771 N66-16207 SURVIVE CONOITIONS THOUGHT TO EXIST ON MARS 1165-81013 CALCULATIONS FOR QUASI-GEOSTROPHIC PLANETARY CIRCULATION ATMOSPHERE WITH DIABETIC HEATING AND HUTREE-F~ CMCULATIOI( SURFACE FRICTION N66-16208 COUPLED HARTREE- MCK APPROXIMATION FOR CALCULATING FREQUENCY-DEPENOENT REFRACTIVE INOEX PLANETARY CIRCULATION PATTERNS FOR INTEGRATED TWO- OF HELIUM GAS LEVEL QUASI-GEOSTROPHIC MOOEL ATMOSPHERE NASA-CR-66991 N66-14261 INCLUDING WATER VAPOR N66-16209 HUE 6ERMINATIOU MARTIAN BLUE HUE PROPERTIES CORRELATE0 WITH SEE0 GERMINATION DF COMMON PLANT SPECIES IN INTERPLANETARY OUST. METEOR SHOWERS AND SOLAR

1-11 HEAT BALANCE SUBJECT INDEX

FLARES A65-26040 CELESTIAL MECHAN ICs A65-23910

HEAT BALANCE HASS SPECTROHETER ABOARD HYPERSONIC ENTRY VEHICLE EARTH- HARS COMPARISON OF VERTICAL TEMPERATURE FOR CHEHICAL COMPOSITION STUDY OF MARTIAN DISTRIBUTION AN0 HEAT BALANCE IN ATMOSPHERE ATMOSPHERE NASA-CR-68992 N66-14280 NASA-CR-71307

HEAT SHIELO HYPERSONIC SPEED DENSE CARBON REINFORCED AN0 LOW DENSITY CHAR- EWATIONS OF HOTION FOR ELASTIC BODIES ENTERING FORMING RESIN ABLATION MATERIALS FOR EARTH1 MARS PLANETARY ATMOSPHERE AT HYPERSONIC VELOCITIES AN0 VENUS ATMOSPHERE ENTRY A65-15619 166-21667

HEAT TRANSFER HYPERVELOCITY SIMULATION OF HEAT TRANSFER ENVIRONHENTS OF SPACE HYPERVELOCITY HEAT TRANSFER STUDIES IN SIMULATED VEHICLE ENTERING PLANETARY ATHOSPHERE WITH PLANETARY ATMOSPHERES SUPERORBITAL VELOCITY NASA-CR-57500 N65-19884 R64S073 N65-15600

HYPERVELOCITY HEAT TRANSFER STUDIES IN SIMULATEO I PLANETARY ATHOSPHERES ICE FORMATION NASA-CR-57508 N65-19884 DETECTION OF WATER AND ICE CLOUDS ON VENUS P-3245 N66-13681 NUMERICAL INTEGRATION OF VARIOUS PLANETARY CIRCULATION PATTERNS IN QUASI-GEOSTROPHIC MODEL INFRARED ASTRONOMY ATHOSPHERE INCLUDING WATER VAPOR. OIABATIC BALLOON BORNE IR SPECTROSCOPY INDICATES VENUS HEATING1 AN0 SURFACE FRICTION CLOUDS CONSIST OF ICE CRYSTALS A65-14707 AFCRL-65-771 N66-16207 Ia SPECTRUH STUDY OF PLANET HERCURY FOR HELIUM ATMOSPHERIC COMPOSITION AND TEMPERATURE PROFILE PHYSICS OF PLANETARY ATMOSPHERES - VARIATION A65-15676 METHOD USED TO CALCULATE RAYLEIGH SCATTERING CROSS SECTIONS OF HELIUM AS WAVELENGTH FUNCTION VENUS IR LIMB DARKENING OBSERVATIONS BY MARINER NASA-CR-64187 N65-31052 11 A65-22098

COUPLE0 HARTREE- FOCK APPROXIMATION FOR I R SPECTRUM STUDY OF PLANET MERCURY FOR CALCULATING FREQUENCY-DEPENDENT REFRACTIVE INDEX ATMOSPHERIC COMPOSITION AN0 TEMPERATURE PROFILE OF HELIUM GAS A65-26783 NASA-CR-6099 1 N66-14281 1 R ASTRONOHY, DETECTION DEVICES AND EVALUATION OF HISTORY OBSERVATIONS OF HODN AN0 PLANETS BIOLOGICAL PROBLEMS IN SPACE-TEXTBOOK A65-30119 A66-80836 I R LIHB DARKENING OF VENUS EXPLAINED IN TERMS OF HORN THREE TYPES OF ATMOSPHERE AN0 CLOUD HOOELS PHOTOMETRY OF AUREOLE PROLONGING HORNS OF VENUS A65-34633 CRESCENT NASA-TT-F-9685 N65-339b2 I R SPECTRA OF SATURN RING AN0 GALILEAN SATELLITES OF JUPITER SHOW ABSENCE OF STRONG HUMIDITY ABSORPTION AT 8873 ANGSTROMS, INDICATING NEW UPPER FORECASTING HUMIDITY TRANSPORT IN ATMOSPHERE IN LIHIT OF METHANE ABUNDANCE A65-35505 PLANETARY-SCALE PROCESSES A65-30110 VENUS IR LIHB DARKENING OBSERVATIONS BY HYDRATION MARINER I1 A66-2 1110 I R REFLECTIVITY OF POLYHYORATEO FERRIC OXIDE HEASUREO IN CONNECTION WITH HARTIAN SURFACE INFRARED RADIATION MYORATION DETERMINATION FROM REFLECTION SPECTRA VARIATION OF IR EHISSION FROH MARS SURFACE WITH ~65-23407 MARS LOCAL TIME IN TERMS OF DIURNAL TEMPERATURE VARIATIONS, INCLUDING ATMOSPHERE EFFECT, RESULTS MY DROGEN SUGGEST LOW THERMOCONOUCTIVITY A66-21201 HYDROGEN MOLECULES IN ASTROPHYSICS NASA-CR-57156 N65- 18918 I R COOLING RATE IN PLANETARY ATMOSPHERES. NOTING CURTIS- GODSON APPROXIHATION, DOPPLER LINE MY DROST AT ICS SHAPE1 WATER VAPOR ROTATION BAND. ETC MODELS OF MARTIAN THERMOSPHERE WITH CONSTANTS A66-22264 AN0 BOUNDARY VALUES IN HYDROSTATIC AN0 HEAT-FLUX EPUATIONS N65-28713 INFRARED REFLECTIOW I R REFLECTIVITY OF POLYHYDRATED FERRIC OXIDE HYGROMETER MEASURE0 IN CONNECTION WITH MARTIAN SURFACE KRYPTONATE OXYGEN DETECTOR AN0 ALUMINUM OXIDE HYDRATION DETERMINATION FROH REFLECTION SPECTRA HYGROHETER FOR USE AS OXYGEN SENSORS FOR A65-23487 PLANETARY ATMOSPHERE NASA-CR-63139 N65-25246 INFRARED SPECTROSCOPY I R SPECTROSCOPY ROLE IN BIOLOGICAL EXPLORATION OF HYPERSONIC FLOW MARS PROVIDING DATA ON ATHDSPHERIC AN0 SURFACE ATHOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNATION PARAMETERS ~65-26729 POINT CONVECTIVE HEAT TRANSFER1 USING ARC-HEATED SHOCK TUBE SIMULATING FLIGHT VELOCITIES UP TO INFRARED SPECTROSCOPY STUDIES TO OETERHINE 34.000 FPS ABSORPTION BY CARBON DIOXIDE BETWEEN 8*000 AN0 AIAA PAPER 66-29 A66-17891 10,00O/tM IN 1 TO 1.25 MICRON REGION U-3200 N66- 2 2 465 HYPERSONIC HEAT TRANSFER SPECTRAL AND TOTAL RADIATION STUDIES OF BODIES INFRARED SPECTRUM TRAVELING AT HYPERSONIC SPEED IN SIMULATED I R SPECTROSCOPY OF VENUS USED TO ESTIHATE CARBON MARTIAN AND VENUSIAN ATMOSPHERES DIOXIDE ABUNDANCE BY MEASUREMENT OF ABSORPTION AIAA PAPER 65-116 A65- 15008 BANDS A65-15691

HYPERSONIC REENTRY I R SPECTRA OF MARS USE0 TO DETERHINE ITS HYPERSONIC AERODYNAMICS THROUGH PLANETARY ATMOSPHERIC CONSTITUENTS A65-10476 ATMOSPHERES DESCRIBED BY TWO-BODY PROBLEH IN

1-12

~ SUBJECT IlMX JUPITER /PLANET/

MARS IR SPECTRA IN 3-4 MICRON REGION ATTRIBUTED OBSERVED RADIATION SPECTRUM OF VENUS ATMOSPHERE TO TERRESTRIAL MOO MOLECULES ON BASIS OF SOLAR WITH DECREASE IN BRIGHTNESS TEMPERATURE SPECTRA AN0 WATER VAPOR ABWOAMES EXPLAINED BY ABSORPTION IN RELATIVELY COLD A65-19902 SURROUNOIHG IONOSPHERE N65-24526

INSTRUI(ENTAT1ON METHOD FOR STUDY OF PLANETARY IONOSPHERES BASE0 SPACECRAFT. MISSIONS AN0 INSTRUMENTATION FOR SPACE ON RADIO WAVE PROPAGATION BETWEEN EARTH AN0 PROBES AN0 INTERPLANETARY EXPLORATION SPACECRAFT A65-82064 NASA-CR-64460 N65-32199

PAPERS PRESENTED AT SCIENTIFIC BALLOON MULTIOISCIPLINARY STWIES ON PLANETARY ATnOSPHERES SYMPOSIUM ON BALLOON OES16Nv MATERIALS. STRESS IONOSPHERIC AN0 RAOIOPHYSICS. PARTICLES AN0 STUDIES. INSTRUMENTATIONt METEOROL06Y. LOCATINS FIELDS. AN0 PLANETS SYSTEM. AN0 PLANETARY EXPLORATION APPLICATIONS NASA-CR-70165 N66-17290 AFCRL-65-486 W5-34604 IolrosmEIIIC ELECTRON DENSITY MASS SPECTROMETER INSTRUMENTATION FOR ANALYSI S OF VENUS NIGHT ATMOSPHERE INVESTIGATED BY STWYINS MARS ATMOSPHERE IONOSPHERIC ELECTRON DENSITY AN0 ELECTRON NASA-CR-47959 N66-11743 RECOnBlNATION IN NIGHT ATMOSPHERE OF EARTH NASA-TT-F-E244 1165-225~9 INTEGRITI W INTEGRATION OF TERRESTRIAL AN0 PLANETARY IONOSPHERIC PROPIGATION ENVIRONMENT SENSING 1165-33556 MONOGRAPH ON RADIO EMISSION OF SUN AND PLANETS A65-16909 INTERFERORETER MARS SURFACE AN0 ATMOSPHERE CHARACTERISTICS FROM IRON CMlpwlD THERMAL EMISSION SPECTRUM MEASUREMENT BY MARINER IV OBSERVATIONS OF MARS SURFACE. SWWlffi INFRARED INTERFEROMETER ON PLANETARY FLYBY NO DETECTABLE MAGNETIC FIELO OR RADIATION BELTS. SPACECRAFT SUGGEST IRON ON SURFACE OXIDIZE0 FROM NASA-TM-X-55070 N65-32114 PHOTODISSOCIATION OF WATER VAPOR A6621211 TELESCOPE DESIGN FOR INTERFEROUETER SPECTROMETER FOR PLANETARY ATMOSPHERE EXPLORATION IRON OXIOE N66-14107 IR REFLECTIVITY OF POLYHYORATEO FERRIC OXIDE MEASURED IN CONNECTION WITH MARTIAN SURFACE INTERPLANETARY FL ICHT HYDRATION OETERMINATSON FROM REFLECTION SPECTRA SPACECRAFT* MISSIONS AND INSTRUnENTATION FOR SPACE A65-23487 PROBES AN0 INTERPLANETARY EXPLORATION A65-82064 ISOmOTE THERMAL EMISSION MAPS OF JUPITER. OIStUSSING ATMOSPHERIC FACTORS OF INTERPLANETARY SPACEFLIGHTS SOURCE OF NOISE FROM TRACKING ERRORS AN0 FTD-TT-65-741/1&2&4 N66-12511 PHOTOMETRIC ERRORS A65-31279

INTERPLANETARY GAS INTERPLANETARY GAS At40 IONOSPHERES OF PLANET - J INVESTIGATION USING CHARGED PARTICLE TRAPS JAPAN W5-16466 MARS ATMOSPHERE IIOOELt SOLAR WINO MECHANISM OF GEOMAGNETIC PULSATION. AN0 CLWO SEEDING IN INTERPLANETARY SPACE JAPAN N66-19929 RADIO AN0 RAOAR ASTRONOMY STUDIES OF LUNAR AN0 PLANETARY ATMOSPHERES AN0 SURFACES. AN0 RAOAR JET PROPULSION STUDIES OF SUN AN0 INTERPLANETARY MEOIUM THEORETICAL FUEL-BASE0 SPECIFIC IMPULSE LIGHT NASA-CR-57184 N65-18944 METAL-NITROGEN SYSTEM FOR RAMJET AN0 TURBOJET PROPULSION IN MARTIAN ATMOSPHERE INTERACTION OF SOLAR WINO WITH PLANETS - A65-15610 PROPERTIES OF INTERPLANETARY MEOIUM AN0 THEORETICAL MODELS OF SOLAR WINO JUPITER /PLANET/ W6-14334 THERMAL EMISSIOW OBSERVATIONS OF SHAWWS CAST ON JUPITER BY SATELLITES GANYMEOEt EUROPA AN0 10 ION SOURCE A65-16223 MASS SPECTROMETER USING HETEROENERGETIC ION SOURCE WITHOUT DEFLECTION FIELO FOR MARTIAN COWCEPTS CONCERNING JUPITER SURFACE REVISE0 ATMOSPHERE ANALYSIS FOLLOWINS TRANSFORMATIONS OBSERVED SINCE 1962 AND NASA-CR-71916 W6-23797 ESTIMATION OF ASH PARTICLES IN PLANET ATMOSPHERE A65-30238 IONIZATION TEMPERATURE DISTRIBUTION. COMPOSITION^ AN0 JUPITER AN0 SATURN INTERIOR TEMPERATURES FROM IONIZATION OF MARS ATMOSPHERE N66-19930 EXAMINATION OF ATMOSPHERIC COMWSITION AN0 SMVITATIONAL MULTIPOLE MOMENT A65-33302 IONIZATION CWBER ARGON ABUNDANCE IN MARTIAN ATMOSPHERE DETECTOR. SURVIVAL AN0 GROWTH OF TERRESTRIAL MICROORGANISMS USING CYLINDRICAL IONIZATION CHAMBER CONTAINING IN AMMONIA-RICH ATMOSPHERES SUPPORTING POSSIBILITY IRON 55 X-RAY SOURCE 1165-23096 OF ORIGIN AN0 EXISTENCE OF LIFE ON JUPITER A6581267 IONIZED 6AS RADIO PATH FORMULAS FOR PLANETARY IONOSPHERES AN0 PHOTOGRAPHIC SPECTRA OF PLANETARY ATMOSPHERE GASES STELLAR ATMOSPHERES FROM QUASI-CONIC EQUATION AN0 OF MARS AN0 JUPITER ELECTRON DENSITY EQUATION A65-23429 10-608352 N65-16776

IONIZING RAOIATIW METEOROLOGY OF PLANETS MARS. VENUS. AN0 JUPITER SOLAR IONIZING RADIATION EFFECT ON JUPITER UPPER NASA-CR-260 N65-30726 ATMOSPHERE OISSOCIATION INDICATED BY MICROWAVE SPECTRUM A65-17213 ATMOSPHERIC CIRCULATION AROUNO PLANETS OF JUPITER AN0 SATURN N66-14332 IONOSPHERE INTERPLANETARY GAS AN0 IONOSPHERES OF PLANET - JUPITER FLYBY MISSIONS - FUTURE STUDIES ON PLANET INVESTIGATION USING CHARGEO PARTICLE TRAPS ATMOSPHERE AN0 MAWETOSPHERE N65-16468 NASA-CR-69561 1166-1 5607

1-13 JUPITER ATMOSPHERE SUBJECT INDEX

JUPITER OPTICAL EMISSION AND AURORAL ACTIVITY VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN STUDY DISK IN NEAR IR REGION A6623504 AS624895 N66-19616 SURFACE DISTURBANCES AS POSSIBLE CAUSE OF TECTONIC JUPITER ATMOSPHERE MOVEMENT IN JUPITER ATMOSPHERE - ASTRONOMY SOLAR IONIZING RADIATION EFFECT ON JUPITER UPPER T-439-R N66-10590 ATMOSPHERE DISSOCIATION INDICATED BY MICROWAVE SPECTRUM A65-11213 INTENSITY MEASUREMENTS OF METHANE ABSORPTION IN VISIBLE REGION OF JUPITERS SPECTRUM MODULATION MICROWAVE RADIOMETER FOR MEASURING NASA-TT-F-10062 N66-23610 JUPITER RADIATION INTENSITY IN 700 MC RANGE A65-18553 K LABORATORY AN0 PLANETARY ABSORPTION SPECTRA KRYPTON COMPARISONS IN REGION 9100-11200 ANGSTROMS USED TO KRYPTONITE OXYGEN DETECTOR AN0 ALUMINUM OXIDE DETERMINE COMPOSITION AND TEMPERATURE OF JUPITER HYGROMETER FOR USE AS OXYGEN SENSORS FOR ATMOSPHERE A65-2 1854 PLANETARY ATMOSPHERE NASA-CR-63139 N65-25246 FINAL REDUCTION OF OBSERVATIONS OF SPORADIC OUTBURSTS IN DECAMETRIC REGION OF RADIO SPECTRUM OF JUPITER DURING 1961 AND 1962 L A65-21855 LAMINAR HEAT TRANSFM LAMINAR AND TURBULENT CONVECTIVE HEAT TRANSFER TERRESTRIAL MICROORGANISM SURVIVAL AN0 GROWTH ON RATES ON CONES IN PLANETARY ATMOSPHERES SPECIMENS OF EUPHORBIA XYLOPHYLLOIOES IN AMMONIA RAD-TM-64-68 N65-19405 METHANE HYDROGEN-RICH ATMOSPHERES A65-23486 LANDING SYSTEM VOYAGER SYSTEM DESIGN STUDY - ENTRY LANDER, AN0 CONFINEMENT OF DECAMETRIC RADIATION FROM JUPITER ORBITER SYSTEM FOR ENTRY INTO VENUS OR MARS TO NARROW BEAMS ATTRIBUTED TO BELTS OF TRAPPED ATMOSPHERES CHARGED PARTICLES SIMILAR TO VAN ALLEN BELTS NASA-CR-5 18 39 N66-13403 A65-25632 LASER LINEAR POLARIZATION, PLANETARY ROTATION OF LECTURE MANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONSI POLARIZATION, LUNAR OCCULTATION AND INTENSITY BIOLOGICAL EXPLORATION OF MARS, MASERS AN0 SPECTRUM OF JUPITER DECIMETRIC EMISSIONS LASERS. PLANETARY ATMOSPHERES, RELATIVITY A65-26042 THEORY. ELEMENT ABUNDANCE, AN0 SOLAR PARTICLES N65-31360 10 EFFECT ON SYNCHROTRON EMISSION GENERATED WITHIN RADIATION BELTS IN JUPITER ATMOSPHERE LAUNCHING A65-21015 SPACE SCIENCE PROGRAM OF USA - THEORETICAL ASPECTS. SUMMARY OF LAUNCHINGS FOR 19641 LIST OF MODULATION MICROWAVE RADIOMETER FOR MEASURING RESEARCH PROJECTS AND AGENCIES. AN0 BIBLIOGRAPHY JUPITER RADIATION INTENSITY IN 700 MC RANGE N65-2 95 09 A65-21146 LIFE DETECTOR OPTICAL THICKNESS OF JUPITER ISOTHERMAL AUTOMATED BIOLOGICAL LABORATORY FOR DETECTION ATMOSPHERE ASSUMING IT CONSISTS OF HYDROGEN, AN0 CLASSIFICATION OF LIFE ON MARS METHANE AND AMMONIA A65-30237 A65-19518

THERMAL EMISSION MAPS OF JUPITER, DISCUSSING MARTIAN LIFE DEPENDS ON CHEMOGENY, BIOGENY, SOURCE OF NOISE FROM TRACKING ERRORS AN0 COGNOGENY, SIMILARITY AN0 DISSIMILARITY TO EARTH PHOTOMETRIC ERRORS A65-31279 AN0 PHYSICAL AND CHEMICAL ENVIRONMENT A65-28200 JUPITER ATMOSPHERE, USING SPECTROPHOTOGRAPHIC OBSERVATIONS A65-33303 PHYSICAL BASIS FOR EXTRATERRESTRIAL LIFE DETECTION AN0 USE ON MARS 165-81131 METHANE AN0 AMMONIA LABORATORY SPECTRA COMPARED WITH SPECTRA OF JUPITER, INDICATING CAUSES OF SPACECRAFT, MISSIONS AN0 INSTRUMENTATION FOR SPACE UNIDENTIFIED ABSORPTIONS A65-35022 PROBES AND INTERPLANETARY EXPLORATION A65-82064 I R SPECTRA OF SATURN RING AN0 GALILEAN SATELLITES OF JUPITER SHOW ABSENCE OF STRONG MARS ENVIRONMENTAL FACTORS SUGGESTING BIOLOGICAL ABSORPTION AT 8813 ANGSTROMSw INDICATING NEW UPPER POSSIBILITIES AN0 LIFE DETECTION EQUIPMENT TO LIMIT OF METHANE ABUNDANCE A65-35585 PREVENT CONTAM INAT ION A65-82218

PHOTOGRAPHIC RECORDING OF JUPITER ATMOSPHERE BIOLOGICAL SIGNIFICANCE OF MARTIAN ATMOSPHERIC NASA-CR-50303 N65-14653 COMPOSITIONAL ANALYSIS, AN0 LIFE DETECTION STUDIES OF CHEMICAL FREE ENERGY IN SURFACE JOVIAN ATMOSPHERE AND ENVIRONMENT - COMPOSITION, MATTER STRUCTURE, AND PHOTOMETRIC PROPERTIES OF NASA-CR-67354 N65-36391 ATMOSPHERE, PERIOD OF ROTATION. MAGNETIC FIELD, AN0 JOVIAN RADIOFREQUENCY SPECTRUM AUTOMATED LIFE DETECTION ON MARTIAN ENVIRONMENT NASA-CR-63 116 N65-24983 BASE0 ON METABOLISM, REPRODUCTION AND CHEMISTRY A66-16323 PHOTOGRAPHIC OBSERVATIONS OF RAPIDLY MOVING SPOT IN JUPITER ATMOSPHERE EXISTENCE AN0 DETECTION OF LIFE ON MARS NASA-CR-64568 N65-32025 ~66-ao972

SEPARATION BETWEEN FLUID PHASES IN MULTICOMPONENT EXISTENCE AND DETECTION OF LIFE FORMS IN ATMOSPHERE AS POSSIBLE EXPLANATION OF JUPITER UNIVERSE AN0 PLANETARY SYSTEM, AN0 LIFE SUPPORT GREAT REO SPOT 166-19592 IN MANNED SPACE TRAVEL N66-19829

JUPITER PHOTOELECTRIC SPECTRAL SCAN IN UV LIFE SCIENCE REPRODUCED AS GEOMETRIC REFLECTIVITY VS POSSIBLE ALTERNATIVE CHEMICAL ELEMENTS AND WAVELENGTH, USING AEROBEE ROCKET CObIPOUNOS SUITABLE FOR PROLONGED BIOMOLECULAR A66-21099 EVOLUTION AN0 CHEMICAL SELECTION ON NONTERRESTRIAL TYPE PLANET A65-27098 IMAGE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL

1-14 SUBJECT 1-X lUUlETIC -1

NUCLEIC ACID MOLECULE REPROOUCTION DISCUSSING WAR STUDIES OF SUN AN0 INTERPLANETARY MEDIUM PROBABILITY OF LIFE DEVELOPMENT UNOER FAVORABLE NASA-CR-61194 Nb6-10609 ENVIRONMENTAL CIRCUMSTANCES A66-15915 WIO AN0 RADAR ASTRONOMICAL STUDIES ON LUNAR AND WARS ENVIRONMENTAL CONDITIONS* LIFE OR6AMISM PLANETARY IONOSPHERES AN0 ATMOSPHERES* AN0 SOLAR DETECTION. EVALUATION AN0 LIMITING EFFECTS ACT IV ITY A66-22715 NASA-CR-11090 N66- 19528 LIFE SUPPORT SYSTEM LUNAR EWVIRONHHIT EXISTENCE AND DETECTION OF LIFE FORMS IN LUNAR AN0 PLANETARY ENVIRONMENTS USE0 BY WY UNIVERSE AN0 PLANETARY SYSTEM. AND LIFE SUPPORT IIANNEO MISSION PLANNING AND DESIGN CONSIOERIW6 IN MANNED SPACE TRAVEL N6b-19629 RADIATIVE. TOPOGRAPHICAL AND ATMOSPHERIC FEATURES A65-22135 LIGHT ABSORPTION ATMOSPHERE OF MARS AS ABSORBIW. ASCRIB1116 REO BIBLIOGRAPHY OF rncunais ON LWR. PLANETARY. MLOR TO SELECTIVE ABSORPTION IN ATMDSPHERIC LAYER AN0 SPACE ENVIRONMENTS IN RELATION TO FLIIXT A66-19328 MECHANICS AND AEROOYNAMICS OF SPACE TRAVEL NASA-CRdo469 N65-16086 LIGHT SCATTERINS BRIGHTNESS DISTRIBUTION ALONG VISIBLE RADIUS OF LUIM IOMISPHERE MARS. EXAMINING ATMOSPHERIC SCATTERING RADIO AND RADAR ASTRONOMY STUDIES OF LUNAR AN0 A65-18911 PLANETARY ATMOSPHERES AND SURFACES. AND RADAR STUDIES OF SUN AND INTERPLANETARY MEOIUM OPTICAL THICKNESSI SCATTERING AN0 AEROSOL PARTICLE NASA-CR-51184 N65-18944 CONCENTRATION OF MARS ATMOSPHERE IN UV SPECTRUM A65-19668 RADIO AN0 RADAR ASTRONOIIY - LUNAR AN0 PLANETARY IONOSPHERES. ATMOSPHERES* AND SURFACES. AN0 ATMOSPHERIC PRESSURE AN0 TEMPERATURE BELOW 24 KM RADAR STUDIES OF SUN AN0 INTERPLANETARY MEOIUM USING SATELLITE MEASUREMENTS OF ATMOSPHERIC LIGHT WASA-CR-67794 166-10609 REFRACTION FROM GIVEN STARS A65-34959 LUW OBSERVATImI GRWNO SPECULAR REFLECTION MOOIFICATION OF COMMUNICATIONS OF ARIZONA LUNAR AN0 PLANETARY

LIGHT SCATTERING FROM~ PLANETARY~- ATMOSPHERE TOP LABORATORY. VOLUNE 3 A6620291 NASA-CR-57740 U65L20158 LWcI(oT0SIuPnY COSMIC RESEARCH - PROBLEMS OF CELESTIAL MECHANICS SPACE EXPLORATION - SPACE AROUND EARTH. AN0 ASTROWMAMICS~ SOLAR CORONA RAOIATION IN ATMOSPHERIC CIRCULATION AN0 WEATHER CONDITIONS* SOFT X-RAY REGION. EARTH MOTIONS IN LUNAR say. LUNAR PHOTOGRAPHY. AN0 PLANETARY STUDIES LIGHT SCATTERING IN PLANETARY ATMOSPHERE NASA-EP-25 N65-32514 FTWTT-64-42/lt2M W65-2H15 LUNM SURFACE LIGHT SCATTERING IN PLANETARY ATMOSPHERE - FORMULA COLLECTION OF SOVIET ARTICLES ON PHYSICS OF MOON FOR OETERMINING INTENSITY OF RAOIATION LEAVING AN0 PLANETS A64-18967 HOMOGENEOUS SPHERE AFTER SINGLE DIFFUSION N65-24480 BOOK ffl LUNAR AN0 PLANETARY SURFACE CONDITIONS WITH DESCRIPTIONS OF ATMOSPHERIC EFFECTS. LIFE FORMULAS FOR LIGHT PASSAGE THROUGH PLANETARY DETECTION AN0 DATA COLLECTIN6 SYSTEMS ATMOSPHERES OF FINITE OPTICAL THICKNESS* TAKING A65-26272 INTO ACCOUNT POLARIZATION A66-15415 THICKNESS OF DUST ON LUNAR FLOOR. INFRARED MARS ATMOSPHERIC OPTICAL THICKNESS AN0 SCATTERING RAOIOMETRIC TEMPERATURES OF BRIGHTER PLANETS. FROM PHOTOMETRIC OBSERVATION A66- 19321 AN0 EXTENSIVE PHOTOMETRY OF MARS AFCRL-64-926 N65-15288 OIFFERENCE BETWEEN VALUES FOR ATMOSPHERIC PRESSURE AT MARTIAN SURFACE WHEN OBTAINED BY PHOTOMETRY OR RADIO AND RADAR ASTRONOMY STUDIES OF LUNAR AND BY SPECTROSCOPY. DUE TO NONCONSIOERATION OF LIGHT PLANETARY ATMOSPHERES AND SURFACES. AND RADAR SCATTERING BY AEROSOL PARTICLES STUDIES OF SUN AND INTERPLANETARY MEDIUM A66-19331 NASA-CR-57184 N65-18944

LIGHT SCATTERING AN0 POLARIZATION IN PLANETARY PLANETARY ATMOSPHERES. LUNAR STRUCTURES. PARTICLE ATMOSPHERE ENERGY SPECTRA. EXOBIOLOGY. SPACE PHYSIOLOGY* NASA-CR-10943 N66-20017 AN0 ENGINEERIN6 SCIENCES - SPACE SCIENGES WSA-CR-59038 N6529433 ATMOSPHERIC SCATTERING AN0 REFRACTION OF SUNLIGHT INTO PLANETARY WBRA REnoTE MEASUREMENT OF TRACE AMOUITS OF VAPORS IN P-3282 N66-20124 LUNAR AN0 PLANETARY ATMOSPHERES AS INDICATOR OF BxaOGxc AND GEOLOGIC SURFACE CONOITIONS LI6HT TRIWS)IISSIffl A6621532 APPROXIMATE SOLUTION OF DIFFUSE REFLECTION AN0 TRANSMISSION OF LIGHT BY FLAT LAYER OF PLANETARY RADIO AN0 RADAR ASTRONOMY - LUNAR AN0 PLANETARY ATMOSPHERE WITH TRUE ABSORPTION IfflOSPHERESt ATMOSPHERES. AN0 SURFACES. AN0 A65-18915 RADAR STUDIES OF SUN AN0 INTERPLANETARY MEOIW NASA-CR-61194 N66-10609 LIGHTNIN6 OPTICAL DETECTION OF LIGHTNING FRON SATELLITES NASA-CR-60606 N65-17404 M MACUETIC INSTRUMENT LON6ITUDINM STABILITY PHOTOIONIZATION MASS SPECTROIIETER WITH 180 OEG PLANETARY ENTRY VEHICLES - LONGITWINAL STABILITY MAGNETIC ANALYZER AN0 USE AS GAS ANALYZER CHARACTERISTICS FOR VARIOUS BLUNT-BOOY MODELS NASA-CR-71210 N66-19636 TESTE0 AT MACH 6.13 IN WINO TUNNEL NASA-TN-0-2785 N65-22368 IUG(IET1C I(EASUREWENT MARINER IV ENCOUNTER SEQUENCE DURING APPROACH AND LUNAR ATMOSPHERE OCCULTATION OF MARS ON JULY 14 AN0 15. 1965 OUTGASSIN6 PROCESSES ON MOON AN0 VENUS* USIW 1165-36323 EARTH ANALOGY A65-33298 Iu6wElIC IUIIEWT RADIO AND RADAR ASTRONOMY - LUNAR AN0 PLANETARY X-RAY RAOIATION INTENSITY OF AURORAE POLARIS OF IONOSPHERES. ATMOSPHERES. AN0 SURFACES. AND PLANET TO OETERllIME MAGNETIC MOMENT

1-15 MAGNETICALLY TRAPPED PARTICLE SUBJECT INDEX

A65-15763 OCCULTATION OF MARS ON JULY 14 AN0 15, 1965 A65-36323 SEARCH FOR TRAPPED ELECTRONS AND MAGNETIC MOMENT AT MARS BY MARINER IV A65-36325 SEARCH FOR TRAPPED ELECTRONS AN0 MAGNETIC MOMENT AT MARS BY MARINER IV 165-36325 MAGNETICALLY TRAPPED PARTICLE CONFINEMENT OF DECAMETRIC RADIATION FROM JUPITER EXPECTEO DIFFRACTION EFFECTS ON ELECTROMAGNETIC TO NARROW BEAMS ATTRIBUTED TO BELTS OF TRAPPED RADIATION FROM MARINER IV DUE TO MARTIAN CHARGE0 PARTICLES SIMILAR TO VAN ALLEN BELTS ATMOSPHERE AN0 OCCULTATION A66-16039 A65-25632 MARTIAN IONOSPHERIC OBSERVATIONS MADE BY MARINER SEARCH FOR TRAPPED ELECTRONS AN0 MAGNETIC MOMENT IV INTERPRETEO IN TERMS OF MODEL SHOW ATMOSPHERE AT MARS BY MARINER IV A65-36325 CONSISTS MAINLY OF CARBON OIOXIOEI LOW TEMPERATURE AN0 NO THERMOSPHERE A66-16404 MAGNETOSPHERE JUPITER FLYBY MISSIONS - FUTURE STUDIES ON PLANET MARINER IV OCCULTATION EXPERIMENT ON MARTIAN ATMOSPHERE AN0 MAGNETOSPHERE ATMOSPHERE, USING AMPLITUDE AN0 FREQUENCY CHANGES NASA-CR-69561 N66-15801 OF TRACKING AN0 TELEMETRY SIGNAL AIAA PAPER 66-148 A66-17900 MANNED SPACE FLIGHT PLANETARY ATMOSPHERE OBSERVATIONS FROM SPACECRAFT INSTRUMENTATION AN0 DESIGN OF SCIENTIFIC PAYLOAD IN TWILIGHT CONDITIONS A65-31247 CARRIED BY MARINER IV A66-20181

WEIGHT AND ENERGY REPUIREMENTS OF VEHICLE SYSTEMS MODEL FOR LOWER ATMOSPHERE OF MARS BASEO ON FOR MANNED EXPLORATION OF MARS MARINER IV OCCULTATION EXPERIMENT AIAA PAPER 64-403 A65-33549 LMSC-6-75-65-62 N66-16948

PLANETARY ATMOSPHERE OBSERVATIONS FROM SPACECRAFT MARS ATMOSPHERIC MODELS BASED ON MARINER IV IN TWILIGHT CONDITIONS A65-34922 OCCULTATION EXPERIMENT NASA-CR-74152 N66-23493 PLANETARY ENVIRONMENTAL DESIGN DATA FOR FUTURE MANNED SPACE FLIGHTS TO VENUS AN0 MARS MARS /PLANET/ NASA-SP-3016 N65-23799 1924 AN0 1926 'OPPOSITIONS OF MARS IN W. H. WRIGHT PLATES NOTING MARS DIAMETER IN IR MARS ENVIRONMENTAL MEASUREMENTS IN SUPPORT OF AN0 UV A65-20633 FUTURE MANNED LANDING EXPEDITIONS NASA-CR-62872 N65-24355 WEIGHT AN0 ENERGY REPUIREMENTS OF VEHICLE SYSTEMS FOR MANNED EXPLORATION OF MARS SPACE TRAVEL AN0 EXPLORATION, BIOLOGICAL AND AIAA PAPER 64-403 A65-33549 TECHNICAL DIFFICULTIES. RADIATION, METEOR IMPACT, VEHICLE STERILIZATION* ETC A66-23640 SOME FORMS OF LIFE FOUND ON EARTH WHICH CAN SURVIVE CONDITIONS THOUGHT TO EXIST ON MARS BIOLOGICAL PROBLEMS IN SPACE-TEXTBOOK A65-81013 A66-80836 CHARACTERISTICS OF MARS AN0 POSSIBILITY OF UNMANNED SPACE MISSION TO OETERMINE MARTIAN EXISTENCE OF LIFE 165-81018 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - PHYSICAL BASIS FOR EXTRATERRESTRIAL LIFE DETECTION UNMANNED SPACECRAFT DESIGN AN0 USE ON MARS A65-81137 NASA-CR-68142 N66- 15540 OESIGN. PERFORMANCE, AN0 ENVIRONMENT PARAMETERS UNMANNED SPACE MISSION TO OETERMINE MARTIAN FOR MARS AN0 VENUS SPACE CAPSULES ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF NASA-CR-53674 N65-16498 SYSTEMS FOR MANNED SPACE MISSION TO MARS - MISSION EXPERIMENT REPUIREMENTS SPECTROPHOTOMETRIC OBSERVATIONS OF MARS NASA-CR-68741 N66-15541 N65-18512

UNMANNED SPACE MISSION TO OETERMINE MARTIAN EVIDENCE FOR LIFE ON MARS - NATURE AN0 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF UNC ERT A I NT I ES SYSTEMS FOR MANNED SPACE MISSION TO MARS - NASA-CR-58430 N65-2 947 5 SUMMARY REPORT NASA-CR-68743 N66-15542 METEOROLOGY OF PLANETS MARS, VENUS. AN0 JUPITER NASA-CR-280 N65-30726 UNMANNED SPACE MISSION TO OETERMINE MARTIAN ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF LECTURE MANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONSI SYSTEMS FOR MANNED SPACE MISSION TO MARS - BIOLOGICAL EXPLORATION OF MARS, MASERS AN0 MISSION SENSITIVITY ANALYSIS LASERS. PLANETARY ATMOSPHERES, RELATIVITY NASA-CR-68740 N66-15543 THEORY, ELEMENT ABUNDANCE, AN0 SOLAR PARTICLESN65-31360

EXISTENCE AN0 DETECTION OF LIFE FORMS IN UNIVERSE AND PLANETARY SYSTEM, AN0 LIFE SUPPORT PLANETARY METEOROLOGY - MARS AND VENUS IN MANNEO SPACE TRAVEL N66-19829 NASA-CR-64432 N65-32082

MARINER I1 SPACE PROBE MARS SURFACE AN0 ATMOSPHERE CHARACTERISTICS FROM MARINER 11 RADAR AN0 RAOIOMETRIC OBSERVATIONS OF THERMAL EMISSION SPECTRUM MEASUREMENT BY VENUS DURING 1962 CONJUNCTION - PHYSICAL DATA INFRARED INTERFEROMETER ON PLANETARY FLYBY NASA-CR-56851 N65-22203 SPACECRAFT NASA-TM-X-55070 N65-32114 MARINER II MICROWAVE RADIOMETER EXPERIMENT TO STUDY VENUS SURFACE AN0 ATMOSPHERE ANALYSIS OF EPUILIBRIUM SHOCK LAYER RADIATION FOR NASA-CR-69916 N66-16151 MARS ATMOSPHERIC ENTRY N65-32433

MARINER IV SPACE PROBE ABSENCE OF ELECTRONS IN MARS ATMOSPHERE AN0 MARS ATMOSPHERE AN0 IONOSPHERE MEASUREMENTS USING IMPLICATIONS THEREOF 2300-MC TELEMETRY SIGNAL FROM MARINER IV NASA-CR-64870 N65-33919 SPACECRAFT OCCULTAT I ON EXPER I MENTS A65-26719 FEASIBILITY AN0 DESIGN OF BALLOONS FOR EXPLORATION OF SURFACE AND ATMOSPHERE OF MARS MARINER IV ENCOUNTER SEPUENCE DURING APPROACH AN0 N65-34830

1-16 .

SUBJECT IWDU MMS ATMOSPHERE

SPECTROSCOPIC DETECTION OF WATER VAPOR IN PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE. ATMOSPHERES OF VENUS AN0 MARS USING TELESCOPE TRACKING. COST AND SCHEDULE CARRIE0 BY BALLOON N65-34835 AIAI PAPER 65-219 A65-17398

TEMPERATURE. DENSITY AND GRAVITATIONAL ESCAPE ON MARS NITROGEN OXIDES OBSERVED AT DIFFERENT MARS. MERCURY. JUPITER AN0 VENUS ATMOSPHERES WAVELENGTHS. COMPUTING PHOTOCHEMICAL EPUILIBRIA A66-15759 POINT AND ROLE IN BLUE HAZE ~65-1r992

BRIGHTNESS TEMPERATURE MEASUREMENTS OF MARS AT REPORTS ON MARS FROM LUNAR AN0 PLANETARY 3-75 CM FROM FEBRUARY TO JUNE 1965 LABORATORY AT UNIVERSITY OF ARIZONA A66-16768 A65-10475

MARINER IV PHOTOGRAPHS OF PLANET MARS NOTING IR SPECTRA OF MARS USED TO DETERMINE ITS TOPOGRAPHY. SOIL COMPOSITION. ATMOSPHERIC ATMOSPHERIC CONSTITUENTS A65-18476 PHENOMENA. POLAR CAP MIGRATION. RAOIATIW. ETC 166-20660 CALIBRATION OF MARTIAN SPECTRA USING LABORATORY SPECTRA OF PURE CARBON OIOXIDE AND IN COnBINATIW BLACK BODY DISK TEMPERATURES OF MERCURY AN0 MARS WITH NITROGEN AN0 ARGON A65-18477 FROM OBSERVATIONS AT 3.4 MM IN APRIL 1965 A66-22786 RELATION BETWEEN TOTAL ATMOSPHERIC PRESSURE AND CARBON OIOXIDE ABUNDANCE OF MARS LIFE ON MARS - CONOITIONSt POSSIBLE TYPES OF A65-18478 ORGANISMS AN0 THEORIES OF ADVANCED FORMS OF LIFE A66-60582 NITROGEN DIOXIDE CONTENT OF MARS ATMOSPHERE DERIVED FROM LABORATORY TESTS AND MICROPHOTOMETER EXISTENCE AN0 DETECTION OF LIFE ON MARS TRACES A65-16460 A66-BO972 BRIGHTNESS DISTRIBUTION ALONG VISIBLE RADIUS OF MARTIAN ATMOSPHERE AND SURFACE CHARACTERISTICS - MARS. EXAMINING ATMOSPHERIC SCATTERING ASTROPHYSICS A65-18971 NASA-CR-68136 N66- 1297 4 BRIGHTNESS DISTRIBUTION IN MARGINAL ZONE OF MARS PHENOMENON OF VOLCANIC ACTIVITY ON MARS PLANET USED TO DETERMINE ATMOSPHERIC ABSORPTION NASA-TT-F-410 N66-14051 A65-18972

MARS ATMOSPHERE MOOEL. SOLAR WINO MECHANISM OF PHOTOMETRIC DETERMINATION OF MARTIAN ATMOSPHERE GEMIAGNETIC PULSATION. AND CLOUD SEEDING IN AND SURFACE OPTICAL THICKNESS AND ABSORPTION AS JAPAN N66-19929 FUNCTIONS OF WAVELENGTHS A6516974

TEMPERATURE DISTRIBUTIONI COMPOSITION. AND OPTICAL THICKNESSI SCATTERING AND AEROSOL PARTICLE IONIZATION OF MARS ATMOSPHERE N66-19930 CWCENTRAT.ION OF MARS ATMOSPHERE IN UV SPECTRUM A6519666 AEROBEE ROCKET MEASUREMENTS OF MARS ULTRAVIOLET REFLECTIVITY - PLANETARY ATMOSPHERIC MODEL MARS ATMOSPHERE PROPERTIES DISTINGUISH IT FROM NASA-TM-X-56654 Mb6-22239 EARTH ATMOSPHERE. PARTICULARLY WATER CONTENT. THERMAL FLOWS AND AIR MASSES CIRCULATION PHOTOMETRIC AND POLARIMETRIC STUDIES OF MARS AND A65-19853 VENUS ATMOSPHERES - AEROSOLS NASA-TT-F-969B N66-23536 MARS IR SPECTRA IN 3-4 MICRON REGION ATTRIBUTED TO TERRESTRIAL HDO MOLECULES ON EASIS OF SOLAR PHOTOELECTRIC MEASUREMENT OF BRIGHTNESS SPECTRA AND WATER VAPOR ABUNDANCES DISTRIBUTION IN LIMB ZONE OF MARS A65-19902 NASA-TT-F-10018 N66-23538 ARGON ABUNDANCE IN MARTIAN ATMOSPHERE OETECTOR. MARS ATMOSPHERE USING CYLINDRICAL IONIZATION CHAMBER CONTAINING MARS ATMOSPHERE OEFINITION IMPORTANT IN ADVANCE0 IRON 55 X-RAY SOURCE A65-23096 LANDING VEHICLE DESIGN WITH INCREASED PAYLOAD CAPABILITY AND REDUCE0 COMPLEXITY MARTIAN ATMOSPHERIC HEATING FROM SOLAR RADIATION AIM PAPER 65-22 A65-14563 ABSORPTION IN UV AN0 VISIBLE BY OXYGEN AND OZONE AND IN NEAR IR BY CAREON DIOXIDEt NOTING VERTICAL CLOSE APPROACH OF METEOR STREAMS AND COMETS TO DISTRIBUTION OF GASES AND ABSORPTION MARS ORBIT AN0 RELATION TO BLUE CLEARING OF A65-23521 ATMOSPHERE A65-15342 MARS ATMOSPHERE OZONE OISTRIBUTION ANALYSIS THEORETICAL MODELS OF VENUS AND MARS UPPER INCLUDING PHOTOCHEMICAL REACTIONS AN0 DISCREPAMY ATMOSPHERESI NOTING OISSOCIATION LAYERS AND CARBON FACTORS A65-25020 MONOXIDE CONTENT A65-15454 MARTIAN BLUE HAZE PROPERTIES CORRELATED WITH THEORETICAL FUEL-BASED SPECIFIC IMPULSE LIGHT INTERPLANETARY OUST. METEOR SHOWERS AND SOLAR METAL-NITROGEN SYSTEM FOR RAMJET AN0 TURBOJET FLARES A65-26040 PROPULSION IN MARTIIN ATMOSPHERE A65-15610 SURFACE PRESSURE AND CARBON DIOXIDE CONTENT OF MARTIAN ATMOSPHERE. COMPARING POLARIMETRIC. ORBITER INJECTED STERILIZE0 BALLISTIC SKIPOUT PHOTOMETRIC AND SPECTROSCOPIC METHODS CAPSULE FOR IN FLIGHT MARTIAN STRATOSPHERE A65-26212 MEASUREMENTS. USING NONABLATIVE HEAT SHIELD AN0 OUTSIDE ATMOSPHERIC PROPULSION MANEUVERS MARS ATMOSPHERE AND IONOSPHERE MEASUREMENTS USING AIM PAPER 65-23 A65-15944 2300-MC TELEMETRY SIMAL FROM MARINER IV SPACECRAFT OCCULTATION EXPERIMENTS EARTH REENTRY SIMULATION OF PLANETARY ENTRY 165-26719 ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF MARS AN0 VENUS TYPE DISCREPANCY IN PHOTOMETRIC AND VISIBLE AIAA PAPER 65-218 A65-16606 POLARIMETRIC OETERMINATIONS OF MARS SURFACE PRESSURE ATTRIBUTED TO AEROSOL PARTICLES IN MARS ATMOSPHERIC DENSITY. TEMPERATURE. COMPOSITION MARTIAN ATMOSPHERE A65-26945 AND PRESSURE DETERMINATION FROM ENTRY RESPONSE OF SMALL PROBE A65-16989 CHEMICAL COnWSITIOW AND TEMPERATUIE IN MmEL OF UPPER ATMOSPHERE OF MARS 1165-27569 SIMULATED MARTIAN ENTRY CONOITIONS IN EARTH TEST

1-17 MARS ATMOSPHERE CON1 SUBJECT INDEX

AERODYNAMIC BRAKING TRAJECTORIES FOR MARS ORBIT COMPOSITION AN0 THERMOOYNAMIC PROPERTIES OF MARS ATTAINMENT, GIVING ENTRY CORRIDORS FOR LIFTING AN0 VENUS ATMOSPHERES VEHICLES NASA-CR-50811 N65-17291 AIAA PAPER 64-478 A65-28839 LITERATURE SURVEY ON SURFACE FEATURES. SURFACE SPACECRAFT DECELERATION UPON ENTRY INTO MARS ATMOSPHERIC CONDITIONS, BLUE HAZE, AN0 ORBIT BY AERODYNAMIC BRAKING, CONSIDERING VEHICLE ATMOSPHERIC CONSTRUCTION OF PLANET MARS SHAPE AN0 VELOCITY EFFECTS ON ENTRY HEATING NASA-TM-X-53167 N65-17995 AIAA PAPER 64-479 A65-28841 POLAROGRAPHIC OXYGEN ANALYZER FOR OBTAINING DATA OBSERVATION OF CLOUD PHENOMENA ON PLANET MARS ON MARS ATMOSPHERIC COMPOSITION A65-29289 NASA-CR-57085 N65-18098

APPROXIMATE AN0 CHARACTERISTICS METHODS TO PREDICT INSTRUMENTATION FOR ANALYSIS OF MARS ATMOSPHERE EFFECT OF GAS COMPOSITION ON FORCES AN0 STATIC AFTER SOFT LANDING STABILITY OF PLANETARY ENTRY CONFIGURATIONS IN AIR NASA-CR-62870 N65-24307 AN0 ASSUMED MARTIAN ATMOSPHERES AIAA PAPER 65-318 A65-29766 RADIATION GAUGING METHODS FOR UNMANNED PROBE TO MEASURE MARTIAN ATMOSPHERIC DENSITY DURING ROTATIONAL. PRECESSIONAL AN0 NUTATIONAL MOTION OF ENTRY BODY ENTERING MARS ATMOSPHERE IN VERTICAL AND NASA-(3-62971 N65-24895 OBLIQUE DIRECT IONS A65-30321 LOW SUBSONIC DYNAMIC STABILITY DATA FOR EVALUATION MARTIAN CONDITIONS SIMULATED FROM ASTROPHYSICAL OF BALLISTIC DECELERATION VEHICLE ENTERING MARS DATA FOR MICROBIOLOGICAL INVESTIGATIONS ATMOSPHERE 165-30682 NASA-CR-63117 N65-2498 5

ENTRY VEHICLE DESIGN FOR PLANETARY EXPLORATION SHOCK TUBE GAS DYNAMIC CHARTS SUITABLE FOR MARS USING NONSURVIVING NEEDLE-NOSE0 PROBE FOR DATA ATMOSPHERE COLLECTION ON MARS ATMOSPHERE COMPOSITION, RAD-TM-65-23 N65-25727 PRESSURE AN0 DENSITY AIAA PAPER 65-493 A65-32321 THEORY OF DIURNAL VARIATION OF MARTIAN SURFACE TEMPERATURE - GROUNO AND ATMOSPHERE OF MARS WATER VAPOR ON MARS AN0 VENUS. USING PHOTOMETRY NASA-CR-63278 N65-26075 OF ABSORPTION BAND WITH BALLOON MOUNTED TELESCOPE A65-33299 ATMOSPHERIC BRAKING FOR TRANSFER INTO MARTIAN ORB IT COMPOSITION OF MARTIAN ATMOSPHERE, USING NASA-TN-0-2837 N65-26255 POLARIMETRIC OBSERVATIONS A65-33301 CONVECTIVE-RADIATIVE EQUILIBRIUM MODEL FOR SYSTEM DESIGN OF AUTOMATED LABORATORY AN0 COMPUTING TEMPERATURE PROFILE - VERTICAL ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN . TEMPERATURE DISTRIBUTION IN MARTIAN ATMOSPHERE EXPLORATI ON A65-35112 NASA-CR-65049 N65-219 5 5

SURFACE PRESSURE OF MARS ATMOSPHERE REDETERMINED ATMOSPHERIC CIRCULATION ON MARS FROM ABSORPTION INTENSITY OF CARBON DIOXIDE BY NASA-CR-262 N65-28631 LONG-PATH AN0 PHOTOMULTIPLIER DETECTION A65-35360 MODELS OF MARTIAN THERMOSPHERE WITH CONSTANTS AN0 BOUNDARY VALUES IN HYDROSTATIC AN0 HEAT-FLUX U V REFLECTIVITY OF MARS ANALYZED FROM EQUATIONS N65-28713 SPECTROGRAMS OBTAINED ON AEROBEE ROCKET A65-35583 RECENT DETERMINATIONS OF COMPOSITION AND SURFACE PRESSURE OF MARS ATMOSPHERE MARINER IV ENCOUNTER SEQUENCE DURING APPROACH AN0 NASA-CR-298 N65-33835 OCCULTATION OF MARS ON JULY 14 AN0 15, 1965 A65-36323 EQUILIBRIUM THERMODYNAMIC PROPERTIES /ENTROPY. ENTHALPY, PRESSURE, AN0 SOUND SPEED/ OF THREE MARS ATMOSPHERE PROBLEMS RELATED TO CHEMICAL ENGINEERING MODELS OF MARTIAN ATMOSPHERE COMPOSITION AN0 PHYSICAL PROPERTY NASA-SP-3021 N65-35792

A65-80869~~ BIOLOGICAL SIGNIFICANCE OF MARTIAN ATMOSPHERIC OBSERVATIONS OF WATER VAPOR ON MARS AN0 VENUS FROM COMPOSITIONAL ANALYSIS, AN0 LIFE DETECTION BALLOONS AN0 MOUNTAINS A65-80891 STUDIES OF CHEMICAL FREE ENERGY IN SURFACE MATTER ABSORPTION INTENSITY OF CARBON DIOXIDE BANDS AN0 NASA-CR-67354 N65-36391 MARTIAN CARBON DIOXIDE ABUNDANCE AN0 ATMOSPHERIC PRESSURE AS BASE OF DESIGN FOR MARS ENTRY VEHICLE CARBON DIOXIDE- R-BRANCH LINES OF 5 MU SUB 3 BAN0 A65-82273 FROM INTEGRAL OF ABSORPTION COEFFICIENT OFA66-15288 MARTIAN ATMOSPHERE EFFECT OF UNCERTAINTIES IN ATMOSPHERIC STRUCTURE AN0 CHEMICAL COMPOSITION ON ENTRY INTO MARS EMISSION AN0 ABSORPTION OF RADIANT ENERGY IN MODEL NASA-TN-0-2584 N65-14628 MARTIAN ATMOSPHERE COMPOSED OF 15 PERCENT CARBON DIOXIDE AN0 85 PERCENT NITROGEN BY VOLUME SPECTRUMr COMPOSITION AN0 SURFACE PRESSURE. CARBON A66-15711 DIOXIDE ABUNDANCE, NITROGEN DIOXIDE TESTS, AN0 STRUCTURE OF ATMOSPHERE ON MARS EXPECTED DIFFRACTION EFFECTS ON ELECTROMAGNETIC NASA-CR-60264 N65-15223 RADIATION FROM MARINER IV DUE TO MARTIAN ATMOSPHERE AN0 OCCULTATION 166-16039 EARTH-BOUND OBSERVATIONS OF SURFACE AN0 ATMOSPHERE OF PLANET MARS N65-15491 MARTIAN IONOSPHERIC OBSERVATIONS MADE BY MARINER IV INTERPRETED IN TERMS OF MODEL SHOW ATMOSPHERE PHOTOGRAPHIC SPECTRA OF PLANETARY ATMOSPHERE GASES CONSISTS MAINLY OF CARBON DIOXIDE. LOW TEMPERATURE OF MARS AN0 JUPITER AN0 NO THERMOSPHERE A66-16404 AD-608352 N65-16776 ELECTROMAGNETIC PROPAGATION CHARACTERISTICS OF MASS SPECTROMETER INSTRUMENTATION FOR MARTIAN VENUS AN0 MARS DERIVED FROM ATMOSPHERIC DATA ATMOSPHERIC ANALYSIS A66-16436 NASA-CR-60160 w5-17216 MARINER IV OCCULTATION EXPERIMENT ON MARTIAN

1-18 SUBJECT Ilwx MARS ENVIRO(*(ENT

ATMOSPHERE. USING AMPLITUDE AN0 FREQUENCY CHANGES TRANSLATIONAL AND ROTATIONAL MOTION OF SPHERICAL OF TRACKING AN0 TELEMETRY SIGNAL Bmy ENTERING MARS ATMOSPHERE - REENTRY PHYSICS AIM PAPER 66-140 Abb-17900 NASA-CR-69252 N6b-15330

LONG LIFETIME ORBITS ABOUT MARS AFFECTED BY MODEL FOR LOWER ATMOSPHERE OF MARS BASED ON ATMOSPHERIC DRAG. SOLAR GRAVITATIONAL MARINER IV OCCULTATION EXPERIMENT PERTURBATIONS. PLANETARY OBLATENESS AND OTHER LMSC-6-75-65-62 N66- 16940 PERTURBAT IONS AIM PAPER 66-35 A66-18987 PRINCIPLES FOR DETERMINING PROPERTIES OF UNKWOYN PLANETARY ATMOSPHERE FROM RESPONSES OF CARBON DIOXIDE ABSORPTION BANDS IN MARS REENTERIN6 PROBE VEHICLE ATMOSPHERE. TRANSMISSION. FUNCTION OF CARBON MSA-TN-X-56125 N66-19497 OIOXIM AMOUNT AND EFFECTIVE SURFACE PRESSURE AIM PAPER 66-141 A66-19072 ATMSPHERIC CIRCULATION AND CLIMATOLOGY OF VENUS AND MARS ATMOSPHERES OF VENUS AND MARS- ASTROPHYSICS MSA-CR-7 1627 N66-21767 CONFERENCE. KIEV. UKRAINIAN SSRt JUNE 1964 A66-19322 COMPOSITIONI PRESSURE. VIOLET LAYER. STRUCTURE. TEMPERATURE. CLOUDS, AND WINDS OF MARS AND MARS ATMOSPHERIC OPTICAL THICKNESS AN0 SCATTERIWG VENUS ATMOSPHERES N66-23052 FROM PHOTOMETRIC OBSERVATION A66-19327 MARS ATMOSPHERIC MODELS BASED ON MARINER IV ATMOSPHERE OF MARS AS ABS0Rt)ING. ASCRIBING RED OCCULTATION EXPERIMENT COLOR TO SELECTIVE ABSORPTION IN ATMOSPHERIC LAYER MSA-CR-74152 N6623493 Ab6-19328 SOUNOING ROCKET FLIGHT TO MEASURE COSMIC RADIATION MODEL OF MARS ATMOSPHERE AN0 SURFACE CLOSE TO INTENSITY AND STUOIES OF MARTIAN ATMOSPHERE AN0 TERRESTRIAL CONOITIONSt WITH SCATTERING IONOSPHERE ATMOSPHERIC SPECTRLM AN0 SURFACE COVERED WITH UASA-GR-74173 N66-23113 LIMONITIC DUST A66-19329 MASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE SEPARATION PROBLEMS OF GAS AND AEROSOL COMPONENTS FOR CHEMICAL COMPOSITION STUDY OF MARTIAN IN BRIGHTNESS OF ATMOSPHERIC LAYER FOR PHOTOMETRIC ATMOSPHERE DATA PERTAINING TO MARS ATMOSPHERE MSA-CR-7 1307 N66-23179 A66-19330 MASS SPECTROMETER USING HETEROWERGETIC ION OIFFERENCE BETWEEN VALUES FOR ATMOSPHERIC PRESSURE SWRCE WITHOUT DEFLECTION FIELD FOR MARTIAN AT MARTIAN SURFACE MEN OBTAINED BY PHOTOnETRY OR ATMOSPHERE ANALYSIS BY SPECTROSCOPY. DUE TO NONCONSIOERATION OF LIGHT NUA-CR-719 16 N66-231 91 SCATTERING BY AEROSOL PARTICLES A66-19331 MARS HlVIROllENT EVIDENCE FOR LIFE ON MARS IS SEASONAL WAVE OF PHOTOMETRIC EXAMINATION OF BRIGHTNESS DISTRIBUTION OARKENING AN0 ASSOCIATED CHANGES IN POLARIZATION ALONG DISK OF MARS A66-19332 OF DARK AREAS A65-15140

SPECTRAL REFLECTING POWER CURVE FOR MARTIAN DISK AUTOMATED BIOLOGICAL LABORATORY FOR OETECTION CENTER COMPARED WITH TERRESTRIAL EQUIVALENT AND CLASSIFICATION OF LIFE Ow MARS A66-19333 A65-19518

OPTICAL PARAMETERS OF MARS ATMOSPHERE AN0 SURFACE PLANETARY LIFE EFFECT ON BIOLOGICAL PRECURSOR FROM PHOTOMETRIC DATA FOR SPHERICAL AND ELOWCATEO MISSIONS TO MARS SCATTERING INOICATRICES A66-19337 AIAA PAPER 65-249 A65-22120

EARTH. BALLOON AND SATELLITE SPECTROSCOPIC CHAMBER AN0 ELECTRICAL CIRCUIT USE0 TO SIMULATE OBSERVATIONS OF MARS TO DETERMINE ATMOSPHERIC MARTIAN CONDITIONS FOR MICROBIOLOGICAL COMPOSITION AND PRESSURE AT SURFACE LEVEL INVESTIGATIONS A 65-2 5 099 A66-21065 POSSIBLE WATER SWRCE BENEATH MARS SIRFACE DUST MARS UPPER ATMOSPHERE THERMAL STRUCTURE FROM AND ICE MAY CONSTITUTE POTENTIAL BIOSPHERE SPECTROSCOPIC MEASUREMENTS AN0 MARINER IV A65-26720 OCCULTATION EXPERIMENT A66-23660 I R SPECTROSCOPY ROLE IN BIOLDGICAL EXPLORATION OF EXTRATERRESTRIAL LIFE IN SOLAR SYSTEM. OISCUSSING MARS PROVIDINL DATA ON ATMOSPHERIC AND SURFACE EQUIPMENT FOR MARS EXPLORATION. NOTING GULLIVER PARAMETERS 1165-26729 PROGRAM. MULTIVATOR AUTOMATIC BIOCHEMICAL TESTING APPARATUS AND TV MICROSCOPE A66-23794 MARTIAN LIFE DEPENDS ON CHEMOGENY. BIOGENY. C06NOGENY. SIMILARITY AND DISSIMILARITY TO EARTH MARS ATMOSPHERE OEFINITION IMPORTANT IN ADVANCE0 AND PHYSICAL AN0 CHEMICAL ENVIRONMENT LANDING VEHICLE DESIGN WITH INCREASED PAYLOAD 1165-28200 CAPABILITY AND REDUCE0 COMPLEXITY AIM PAPER 65-22 Abb-24697 RESPONSE OF MICROOR6ANISM TO SIMULATED MARTIAN ENVIRONMENT INVESTIGATED. USING CULTURE PLANETARY RADIATION AND ALBEDO EFFECTS ON THERMAL COLLECTIONS AN0 SOIL SAMPLES A65-30616 BALANCE OF SPACECRAFT ORBITING MARS AND VENUS NASA-CR-67813 1166-10684 ATMOSPHERES CAPABLE OF PRODUCING ORGANIC COMPDUNDS DISCUSSED. STUDYING ABIOGENIC SYNTHESIS IN MARS PLANETARY ENVIRONMENTAL MODELS OF VENUS. MARS. SIMULATOR A65-3-03 MERCURY. JUPITER. PLUTO. NEPTUNE. AND URANUS AN0 SATELLITES ATMOSPHERIC COMPOSITION. SEARCH FOR TRAPPED ELECTRONS AND MAGNETIC MOMENT TEMPERATURES. AND CIRCULATION N66-10996 AT MARS BY MARINER IV A65-36325

MASS SPECTROMETER INSTRUMENTATION FOR ANALYSIS OF MARS COLOR CHANGES EXPLAINED ON BASIS OF PHYSICAL MARS ATMOSPHERE MODEL A65-81159 NASA-CR-67959 W6-11743 MARS ENVIRONMENTAL FACTORS SWXESTING BIOLOGICAL EARTH- MARS COMPARISON OF VERTICAL TEMPERATURE POSSIBILITIES AND LIFE DETECTION EQUIPMENT TO DISTRIBUTIOw AND HEAT BALANCE IN ATMOSPHERE PREVENT CONTAMINATION A65-8221B NASA-CR-68992 W6-14280 MARS ENVIRONMENTAL MEASUREMENTS IN SUPPORT OF

1-19 MARS PROBE SUBJECT INDEX

FUTURE MANNED LANDING EXPEDITIONS ATMOSPHERIC CONSTRUCTION OF PLANET MARS NASA-CR-62872 N65-24355 NASA-TM-X-53167 N65-17995

PROPULSION ORIENTED STUDY OF MISSION MODES FOR ATMOSPHERE' OF MARS AS ABSORBlNGr ASCRIBING REO MANNED UARS LANDING COLOR TO SELECTIVE ABSORPTION IN ATMOSPHERIC LAYER NASA-TM-X-53265 N65-28960 A66-19328

AUTOMATED LIFE DETECTION ON MARTIAN ENVIRONMENT MODEL OF MARS ATMOSPHERE AND SURFACE CLOSE TO BASED ON METABOLISM, REPRODUCTION AN0 CHEMISTRY TERRESTRIAL CONDITIONS, WITH SCATTERING A66-16323 ATMOSPHERIC SPECTRUM AND SURFACE COVERED WITH LIMONITIC DUST A66-19329 MARTIAN LIFE IN LIGHT OF MARINER IV DATA ON ADVERSE ATMOSPHERIC COMPOSITION. TEMPERATURE AN0 OPTICAL PARAMETERS OF MARS ATMOSPHERE AN0 SURFACE RAD1AT ION A66-21140 FROM PHOTOMETRIC DATA FOR SPHERICAL AN0 ELONGATED SCATTERING INOICATRICES A66-19337 MARS ENVIRONMENTAL CONDITIONS. LIFE ORGANISM DETECTION. EVALUATION AN0 LIMITING EFFECTS VARIATION OF IR EMISSION FROM MARS SURFACE WITH A66-22115 MARS LOCAL TIME IN TERMS OF DIURNAL TEMPERATURE VARIATIONS, INCLUDING ATMOSPHERE EFFECT, RESULTS UNMANNED SPACE MISSION TO DETERMINE MARTIAN SUG6EST LOW THERMOCONDUCTIVITY A66-21201 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - MARINER IV OBSERVATIONS OF MARS SURFACE. SHOWING UNMANNED SPACECRAFT DESIGN NO DETECTABLE MAGNETIC FIELD OR RADIATION BELTS. NASA-CR-68742 N66- 5540 SUGGEST IRON ON SURFACE OXIDIZED FROM PHOTODISSOCIATION OF WATER VAPOR UNMANNED SPACE MISSION TO DETERMINE MARTIAN A66-21211 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - PHOTOELECTRIC OBSERVATION OF ATMOSPHERIC PRESSURE MISSION EXPERIMENT REQUIREMENTS ON MARS SURFACE NASA-CR-68741 N66- 5541 NASA-CR-71312 N66-23176

UNMANNED SPACE UISSION TO DETERMINE MARTIAN MASER ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF LECTURE MANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONS, SYSTEMS FOR MANNED SPACE MISSION TO MARS - BIOLOGICAL EXPLORATION OF MARS, MASERS AN0 SUMMARY REPORT LASERS. PLANETARY ATMOSPHERESI RELATIVITY NASA-CR-68743 N66- 5542 THEORY. ELEMENT ABUNDANCE. AN0 SOLAR PARTICLES N65-31360 UNMANNED SPACE MISSION TO DETERMINE MARTIAN ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF MASS SPECTROMETER SYSTEMS FOR MANNED SPACE MISSION TO MARS - MASS SPECTROMETER INSTRUMENTATION FOR MARTIAN MISSION SENSITIVITY ANALYSIS ATMOSPHERIC ANALYSIS NASA-CR-68740 N66- 5543 NASA-CR-60760 N65-112 16

SYSTEMS DESIGN FOR UNMANNED SPACE MISSION TO UASS SPECTROMETER INSTRUMENTATION FOR ANALYSIS OF EVALUATE MARS ENVIRONMENT MARS ATMOSPHERE NASA-CR-69997 N66-16248 NASA-CR-61959 N66-11143

PNEUMATIC SURFACE SAMPLING DEVICE FOR USE IN PHOTOIONIZATION MASS SPECTROMETER WITH 180 OEG SIMULATED MARS ENVIRONMENT MA6NETIC ANALYZER AN0 USE AS GAS ANALYZER NASA-CR-70937 N66-20080 NASA-CR-11210 N66-19636

ENGINEERING BREADBOARD MODEL OF MICROORGANISM MASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE DETECTION DEVICE FOR MARS LANDING APPLICATIONS FOR CHEMICAL COMPOSITION STUDY OF MARTIAN NASA-CR-74214 N66-23787 ATMOSPHERE NASA-CR-71307 N66-23719 MARS PROBE COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE MASS SPECTROMETER USING HETEROENERGETIC ION AN0 IONOSPHERE OF MARS INCLUDING DENSITY, SOURCE WITHOUT DEFLECTION FIELD FOR MARTIAN TEMPERATURE, SCALE HEIGHT, ETC A65-36328 ATMOSPHERE ANALY S IS NASA-CR-71916 N66-23797 PLANETARY ENVIRONMENTAL DESIGN DATA FOR FUTURE MANNED SPACE FLIGHTS TO VENUS AND MARS MERCURY /PLANET/ NASA-SP-3016 N65-23799 I R SPECTRUM STUDY OF PLANET MERCURY FOR ATMOSPHERIC COMPOSITION AN0 TEMPERATURE PROFILE ALTERNATE MISSION PROFILES FOR MANNED MARS A65-15616 LANDING NASA-TN-0-3181 N66-14703 SURFACE TEMPERATURE DISTRIBUTION OF MERCURY BASED ON MEASUREMENTS OF MEAN DISK TEMPERATURE OVER WIDE TRAJECTORY ANALYSIS FOR MARS ATMOSPHERE PROBE - RANGE OF PHASE ANGLES A65- 22205 VOYAGER PROJECT NASA-TM-X-55376 N66-17249 KOZYREV HYDROGEN EMISSION LINES IN IR SPECTROGRAMS OF MERCURY NOTING CORE EMISSIONA6523491 MARS SPACECRAFT ABSORPTION INTENSITY OF CARBON DIOXIDE BANDS AND MARTIAN CARBON DIOXIDE ABUNDANCE AN0 ATMOSPHERIC MERCURIAN ATMOSPHERE FROM HIGH DISPERSION SPECTRAL PRESSURE AS BASE OF DESIGN FOR MARS ENTRY VEHICLE STUDY OF ABUNDANCE OF CARBON DIOXIDE. OXYGEN AN0 A65-82273 WATER Ab5-25226

MARS SURFACE I R SPECTRUM STUDY OF PLANET MERCURY FOR I R REFLECTIVITY OF POLYHYORATED FERRIC OXIDE ATMOSPHERIC COMPOSITION AN0 TEMPERATURE PROFILEA65-26783 MEASURED IN CONNECTION WITH MARTIAN SURFACE HYDRATION DETERMINATION FROM REFLECTION SPECTRA A65-23487 ATMOSPHERE POSTULATION BASED ON KOZYREV OBSERVATION OF HYDROGEN* ENTRY TRAJECTORY ANALYSIS EARTH-BOUND OBSERVATIONS OF SURFACE AN0 ATMOSPHERE AN0 FEASIBILITY OF ATMOSPHERIC BRAKING FOR LANDING OF PLANET MARS N65-15491 PAYLOAD ON MERCURY AIAA PAPER 65-494 A65-29684 LITERATURE SURVEY ON SURFACE FEATURES, SURFACE ATMOSPHERIC CONOITIONSI BLUE HAZE, AN0 ATMOSPHERE OF MERCURY, USING DIFFERENTIAL

1-20 SUBJECT INDEX

POLARIZATION EFFECT AN0 BRIGHTNESS TEMPERATURE UNIDENTIFIED ABSORPTIONS 1165-35022 MEASUREMENTS A65-33300 INTENSITY MEASUREMENTS OF METHANE ABSORPTION IN RADIO OBSERVATIONS OF MERCURY SHOW BRIGHTNESS VISIBLE REGION OF JUPITERS SPECTRUM TEMPERATURE OF ONLY 200 DEGREES K. WITH NO NASA-TT-e10062 N66-23610 SIGNIFICANT VARIATION WITH PHASE A6620 182 MXC~IOL06Y CHAMBER AN0 ELECTRICAL CIRCUIT USE0 TO SIMULATE BLACK BODY DISK TEMPERATURES OF MERCURY AND MARS MARTIAN CONOITIONS FOR MICROBIOLOGICAL FROM OBSERVATIONS AT 3.4 MM IN APRIL 1965 INVESTIGATI OMS A65-25099 A66-22786 MARTIAN CONOITIONS SIMULATED FROM ASTROPHYSICAL PLANETARY ENVIRONMENTAL MODELS OF VENUS. MARS. OATA FOR MICROBIOLOGICAL INVESTISATIONS MERCURY. JUPITER. PLUTO. NEPTUNE. AN0 URANUS A65-30682 AN0 SATELLITES ATMOSPHERIC COMPOSITION. TEMPERATURES. AN0 CIRCULATION N66-10996 MICRooI6uISSM TERRESTRIAL MICROORGANISM SURVIVAL AN0 GROWTH ON ROTATION OF PLANET MERCURY FROM RADAR OBSERVATION SPECIMENS OF EUPHORBIA XYLOPHYLLOIOES IN AMMONIA EXPLAINED BY SOLAR GRAVITATIONAL TORQUE ON TIDAL METHANE HYDROGEN-RICH ATMOSPHERES DEFORMATION AN0 EQUATORIAL PLANE ASYMMETRY A65-23486 NASA-CR-68703 N66-13573 SURVIVAL AN0 GROWTH OF TERRESTRIAL MICROORGANISMS METAL COMBUSTION IN AMMONIA-RICH ATMOSPHERES SUPPORTING POSSIBILITY THEORETICAL FUEL-BASED SPECIFIC IMPULSE LIGHT OF ORI6IN AN0 EXISTENCE OF LIFE ON JUPITER METAL-NITROGEN SYSTEM FOR RAMJET AND TURBOJET A65-81287 PROPULSION IN MARTIAN ATMOSPHERE A65-15610 EFFECTS OF SIMULATED ANAEROBIC PLANETARY ENVIRONMENT ON BIOCHEMICAL ACTIVITIES OF METEOR WST CLOUD TERRESTRIAL MICROORGANISMS CLOSE APPROACH OF METEOR STREAMS AN0 COMETS TO NASA-CR-71195 N66-20131 MARS ORBIT AND RELATION TO BLUE CLEARING OF ATMOSPHERE A65-15342 ENGINEERING BREADBOARD NOOEL OF MICROORGANISM OETECTION DEVICE FOR MARS LANOINL APPLICATIONS METEOR SHOWER NASA-CR-74214 N66-23787 MARTIAN BLUE HAZE PROPERTIES CORRELATED WITH INTERPLANETARY OUST. METEOR SHOWERS ANO SOLAR MICROUAVE FLARES A65-26MO VENUS RADIO SPECTRUM AN0 MICROWAVE EMISSION OF ATMOSPHERIC MOLECULAR OXYGEN METEOR TRAIL NASA-CR-57309 N65-19770 METEOR PHENOMENA. UPPER ATMOSPHERE WINO FIELDS FROn METEOR TRAILS. AN0 PHOTOMETRY OF A AND B MICRWAVE RADIOMETER RINGS OF SATURN MOWLATION MICROWAVE RADIOMETER FOR MEASURING AFCRL-65-33 N65-36000 JUPlTER RAOIATION INTENSITY IN 700 HC RANGE A65-18553 METEOROLOGICAL SATELLITE SOLAR SPACE ENVIRONMENTt AN0 METEOROLOGICAL AND MOWLATION MICROWAVE RADIOMETER FOR MEASURING COMMUNICATIONS SATELLITES - CONFERENCE JUPITER RADIATION INTENSITY IN 700 MC RANGE PROC E EO INGS A65-27146 NASA-CR-60132 1165-15468 MARINER I1 MICROWAVE RADIOMETER EXPERIMENT TO PLANETARY AND EARTH ATMOSPHERIC COMPOSITIONI STUDY VENUS SURFACE AND ATMOSPHERE TEMPERATURE. AND ACTIVITY OATA FROM SATELLITE NASA-CR-69916 N66-16151 AN0 SOUNDING ROCKETS NASA-SP-90 M66-19525 MICROUAVE SPECTRUM VENUS CLDUO LAYER AN0 BRIGHTNESS TEMPERATURE FROM METEOROLOGY MOIOMETRIC MICROWAVE OBSERVATIOEIS FROM NOCTURNAL AERONOMICAL AND METEOROLOGICAL STUDIES OF EARTH SIDE OF PLANET A66-20112 AND OTHER PLANETARY ATMOSPHERES M65-24913 MILLIMETER WAVE COLD ABSORBING ATMOSPHERE MODEL OF VENUS BASE0 OW METEOROLOGY OF PLANETS MARS. VENUS. AN0 JUPITER CENTIMETER AN0 MILLIMETER EMISSION SPECTRW NASA-CR-280 N65-30726 A65-19676 PLANETARY METEOROL'OGY - MARS AND VENUS MISSIoll CLANNINS NASA-CR-64432 N65-32082 SPACE ENVIROMENTAL REQUIREMENTS OF FUTUIE MISSION PLANNING CONFERENCES ON ATMOSPHERIC PHYSICS AN0 CHEMISTRY. AFSC-TOR-64-2 N65-15938 ATMOSPHERIC CIRCULATION. BIOMETEOROLOGY, ENGINEERING, AND NEW TECHNOLOGY ALTERNATE MISSION PROFILES FOR MANNED MARS PUBL.-946 N65-34101 LANDING NASA-TN-0-318 1 N64-14703 PAPERS PRESENTED AT SCIENTIFIC BALLOON SYMPOSIUM ON BALLOON DESIGN. MATERIALS. STRESS lKyKuLAR COLLISIOW STUDIES. INSTRUMENTATION. METEOROLOCY. LOCATING COLLISIOWAL TRANSITION BETWEEN LOWER ATMOSPHERE SYSTEM. AND PLANETARY EXPLORATION APPLICATIONS AN0 CMLISIONLESS EXOSPHERE ANALYZED. USING AFCRL-65-486 N65-34804 INTESRAL FORMULATION OF BOLTZMANN €&AT1 ON AN0 COLLISION MODELS A66-20882 ATMOSPHERIC CIRCULATION AN0 CLIMATOLOGY OF VENUS AN0 MARS WKfXlJLAR SPECTROSCWY NASA-CR-71627 N66-21767 WLECULAR SPECTROSCOPY IN RELATION TO SOLAR. PLANETARY. STELLAR. COMETARY AND INTERPLANETARY SPACE SCIENCES BIBLIO6RAPHY WITH ABSTRACTS - STUDIES A65-18203 ASTRONOMY. METEOROLOGY. OCEANOGRAPHY. UPPER ATMOSPHERE. GEOPHYSICS. SPACE mLKutu WEIGHT JPRS-35095 N66-23025 METHOD FOR DETERMINING TEMPERATURE-ALTITUDE PROFILES OF PLANETARY ATMOSPHERES FROM NUUBER METHANE DENSITY PROFILES OF TWO INERT GASES WITH METHANE AND AMMONIA LABORATORY SPECTRA COMPARED DIFFERENT MOLECULAR WEIGHTS WITH SPECTRA OF JUPITER. INDICATING CAUSES OF WAS A-CR-7 1862 N66-23682

1-21 MOLECULE SUBJECT INDEX

MOLECULE NORMAL SHOCK WAVE HYDROGEN MOLECULES IN ASTROPHYSICS ESTIMATE OF CHEMICAL KINETICS BEHIND NORMAL SHOCK NASA-CR-57156 N65-18918 WAVES IN CARBON DIOXIDE AND NITROGEN MIXTURES FOR MARTIAN ATMOSPHERIC ENTRY MOON NASA-TN-D-3287 N66-16940 MULTIDISCIPLINARY RESEARCH IN SPACE RELATE0 SCIENCE AN0 TECHNOLOGY - EVOLUTION PROCESSES OF WCLEIC ACIO ATMOSPHERE, MOON, EARTH. AND PLANETS NUCLEIC ACID MOLECULE REPRODUCTION DISCUSSING NASA-CR-69137 N66- 15068 PROBABILITY OF LIFE OEVELOPHENT UNDER FAVORABLE ENVIRONMENTAL CIRCUMSTANCES A66-15915 MOTION EQUATION TRANSLATIONAL AND ROTATIDNIL MOTION OF SPHERICAL NUMERICAL INTEGRATION BODY ENTERING MARS ATMOSPHERE - REENTRY PHYSICS NUMERICAL INTEGRATION OF VARIOUS PLANETARY NASA-CR-69252 N66-15338 CIRCULATION PATTERNS IN QUASI-GEOSTROPHIC MODEL ATMOSPHERE INCLUDING WATER VAPOR, OIABATIC EQUATIONS OF MOTION FOR ELASTIC BODIES ENTERING HEATING, AN0 SURFACE FRICTION PLANETARY ATMOSPHERE AT HYPERSONIC VELOCITIES AFCRL-65-771 N66-16207 N66-21667 CALCULATIONS FOR QUASI-GEOSTROPHIC PLANETARY CIRCULATION ATMOSPHERE WITH DIABETIC HEATING AND N SURFACE FRICTION N66-16208 NATURAL SATELLITE THERMAL EMISSION OBSERVATIONS OF SHADOWS CAST ON PLANETARY CIRCULATION PATTERNS FOR INTEGRATED TWO- JUPITER BY SATELLITES GANYMEDE. EUROPA AND IO LEVEL QUASI-GEOSTROPHIC MODEL ATMOSPHERE A65-18223 INCLUDING WATER VAPOR N66-16209

COLLECTION OF SOVIET ARTICLES ON PHYSICS OF MOON NUTATIONAL OSCILLATION AND PLANETS A65-18967 ROTATIONAL, PRECESSIONAL AND NUTATIONAL MOTION OF BODY ENTERING MARS ATMOSPHERE IN VERTICAL AN0 IO EFFECT ON SYNCHROTRON EMISSION GENERATED WITHIN OBLIQUE DIRECTIONS 165-30321 RADIATION BELTS IN JUPITER ATMOSPHERE A65-27015 0 PossIaLE ATMOSPHERE DETECTION ON J-11 AND OCCULTATION J-111 SATELLITES REVEALED BY EXCESS BRIGHTNESS ON BISTATIC RADAR-OCCULTATION METHOD FOR PLANETARY ECLIPSE REAPPEARANCE A66-21202 ATMOSPHERE STUDY NASA-CR-57178 N65-18946 NEAR INFRARED IMAGE CONVERTER TUBE SPECTROPHOTOHETRY OF ZONAL EXPECTED DIFFRACTION EFFECTS ON ELECTROHAGNETIC VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN RADIATION FRDH MARINER IV DUE TO MARTIAN DISK IN NEAR IR REGION A66-23504 ATMOSPHERE AND OCCULTATION A66-16039

NEPTUNE MARINER IV OCCULTATION EXPERIMENT ON MARTIAN PLANETARY ENVIRONMENTAL MODELS OF VENUS, MARS, ATMOSPHERE, USING AMPLITUDE AN0 FREQUENCY CHANGES MERCURY. JUPITER, PLUTO, NEPTUNE, AND URANUS OF TRACKING AND TELEMETRY SIGNAL AND SATELLITES ATMOSPHERIC COMPOSITION, AIAA PAPER 66-148 A66-17900 T EMPERATURES, AND CIRCULATION N66-10996 MODEL FOR LOWER ATMOSPHERE OF MARS BASED ON STRUCTURE, COMPOSITIONt ATHOSPHERE. ,AND SCIENTIFIC MARINER IV OCCULTATION EXPERIMENT OBJECTIVE SURVEYS FOR SATURN, URANUS, LMSC-6-75-65-62 N66-16948 NEPTUNE, AND PLUTO NASA-CR-70328 N66-17090 OCEANOGRAPHY CONFERENCE ON ORIGIN AND EVOLUTION OF ATMOSPHERES NIGHT IONOSPHERE AND OCEANS AT NEW YORK CITY IN APRIL 1963 VENUS NIGHT ATMOSPHERE INVESTIGATED BY STUDYING Ab5-33289 IONOSPHERIC ELECTRON DENSITY AND ELECTRON RECOMBINATION IN NIGHT ATHOSPHERE OF EARTH OCEANOGRAPHIC AN0 RELATED OBSERVATIONS FROM NASA-TT-F-8244 N65-22589 SATELLITE PHOTOGRAPHY N65-30357

NITROGEN SPACE SCIENCES BIBLIOGRAPHY WITH ABSTRACTS - MIXTURES OF NITROGEN AND CARBON DIOXIDE GASES ASTRONOMY, METEOROLOGY, OCEANOGRAPHY, UPPER HEATED BY SHOCK WAVE REFLECTION TO HIGH ATMOSPHERE, GEOPHYSICS, SPACE TEMPERATURE AT NORMAL DENSITY - VENUS JPRS-35095 N66-23025 ATMOSPHERE SIMULATION NASA-CR-51668 N65-15370 OPTICAL EMISSION JUPITER OPTICAL EMISSION AND AURORAL ACTIVITY THERMODYNAMIC PROPERTIES OF 15 PERCENT CARBON STUDY DIOXIDE-85 PERCENT NITROGEN MIXTURE AT VARIED AD-62k895 N66-19676 TEMPERATURE AND PRESSURE RANGES STL-9990-6631-TU-OD0 N65-23299 OPTICAL INSTRUMENT TELESCOPE DESIGN FOR INTERFEROMETER SPECTROMETER NITROGEN OXIDE FOR PLANETARY ATHOSPHERE EXPLORATION MARS NITROGEN OXIDES OBSERVE0 AT DIFFERENT N66-14107 WAVELENGTHS. COMPUTING PHOTOCHEMICAL EQUILIBRIA POINT AND ROLE IN BLUE HAZE A65-17992 OPTICAL MEASUREMENT OPTICAL PARAMETERS OF MARS ATHOSPHERE AND SURFACE NITROGEN DIOXIDE CONTENT OF MARS ATMOSPHERE FROH PHOTOMETRIC DATA FOR SPHERICAL AND ELONGATED DERIVED FROM LABORATORY TESTS AND MICROPHOTOMETER SCATTERING INDICATRICES A66-19337 TRACES 165-18480 OPTICAL POLARIZATION SEE0 GERMINATION OF COMMON PLANT SPECIES IN LIGHT SCATTERING AND POLARIZATION IN PLANETARY RAREFIED NITROGEN ATMOSPHERES SIHULATING ATMOSPHERE EXTRATERRESTRIAL ENVIRONMENT A65-32416 NASA-CR-70943 N66-20077

NDNEPUILIERIUM RADIATION OPTICAL PRDPERTV EQUILIBRIUM AND NONEQUILIBRIUH STAGNATION POINT BRIGHTNESS DISTRIBUTIDN ALONG VISIBLE RADIUS OF SHOCK LAYER RADIATION IN SIHULATED PLANETARY MARS. EXAMINING ATMOSPHERIC SCATTERING ATMOSPHERES OF VARYING COMPOSITION A65-18971 A66-21773

1-22 SUOJECT INDEX PHOTO1WI LIT1 ON

OPTICAL RERECTIVITI P APPROXIRATE SOLUTION OF DIFFUSE REFLECTION AN0 TRANSRISSION OF LIGHT BY FLAT LAYER OF PLANETARY ?ARTICLE DIFFUSIQl ATROSPHERE WITH TRUE ABSORPTION PHOTOMETRIC INVEST16ATION OF AUREOLE ELONGATING A65-18975 VENUS HORNS AT INFERIOR CONJUNCTION A65-17164 REFLECTION SPECTRUR OF CLOUDS IN VENUS CUTICLE FLUX ATROSPHERE MEASUREO. USING TELESCOPE MOUNTED ON RESEARCH ACTIVITIES FROR APRIL THROUGH SEPTEMBER HELIUR BALLOON. NOTING DETAILS OF INSTRURENT 1965 - PLANETARY ATROSPHERES. IONOSPHERIC AN0 A66-18055 RADIO PHYSICS. PARTICLES AN0 FIELDS. UIO PLANETOLOGY OPTICAL SENSOU NASA-CR-68362 N66-12992 OPTICAL OETECTION OF LIGHTNING FROM SATELLITES NASA-CR-60806 N65-17404 PAYLOAD WSS RATIO RARS ATHOSPHERE DEFINITION IMPORTANT IN AOVANCEO OPTICAL THlCKNESS LANOIW VEHICLE DESIGN WITH INCREASED PAYLOAD PHOTORETRIC OETERRINATION OF RARTIAN ATROSPHERE CAPABILITY AN0 REOUCEO COMPLEXITY AN0 SURFACE OPTICAL THICKNESS AN0 ABSORPTION AS AIAI PAPER 65-22 1165-14563 FUNCTIONS OF WAVELENGTHS A65-18974 RMS ATROSPHERE DEFINITION IRPORTANT IN AOVANCEO OPTICAL THICKNESS. SCATTERIN6 AN0 AEROSOL PARTICLE LANDING VEHICLE OESI6N WITH INCREASE0 PAYLOAD CONCENTRATION OF RARS ATMOSPHERE IN UV SPECTRUM CAPABILITY AN0 REOUCEO CORPLEXITY A65-19668 AlAA PAPER 65-22 A6624697 CHOTOCHHIICAL REACTIm OPTICAL THICKNESS OF JUPITER ISOTHERMAL NITROGEN OXIDES OBSERVED AT DIFFERENT ATROSPHERE ASSURING IT CONSISTS HYDROGENr HARS OF UAVELEN6THS CORWT IN6 PHOTOCHERICAL EPUILIBRIA RETHANE AN0 AMRONIA A65-30237 . POINT AN0 ROLE IN BLUE HAZE 1165-17992 ORBITAL TRANSFER MARS ATMOSPHERE OZONE OISTRIBUTION ANALYSIS ATNOSPHERIC BRAKING FOR TRANSFER INTO RARTIAN ORBIT INCLUDIN6 PHOTOCHEMICAL REACTIONS AN0 DISCREPANCY FACTORS A6525020 NASA-TN-0-2837 N65-26255 PtiDTOcIKMISTRY OR6ANIC CMlPOUlD PLANETARY AERONOMY - PHOTOCHEIIISTRY OF PLANETARY ATNOSPHERES CAPABLE OF PRODUCING ORGANIC COMPOUNOS ATMOSPHEREI VACUUR AN0 EXTREME ULTRAVIOLET DISCUSSED. STUDYING ABIOGENIC SYNTHESIS IN NARS SPECTRAL REGIONS. AND THEORETICAL AERONOMY S IWL AT OR A65-30683 NASA-CR-68 106 N66-12248 OR6ANIC MATERIAL GALACTIC AN0 PLANETARY RADIO ASTRONOMY - SOUNOIN6 ENERGY SOURCES AN0 CHEMICAL REACTIONS IN ROCKET LAUNCH. ORBITIN6 TELESCOPE. CARBOWOXY6EN PREBIOLOGICAL ORGANIC SYNTHESIS COMPLEX PHOTOCHEMISTRY. MARS IONOSPHERE. A6580473 TOPSIDE ELECTRON OENSITY. AN0 NONRIGID BODIES NASA-CR-70152 N66-16597 ORI61N ORIGIN AN0 EVOLUTION OF PLANETARY ATROSPHERES ANU PHOTODISSOCIATION OCEANS A65-80889 SATELLITE AN0 ROCKET OBSERVATIONS LEADING TO NEW ASPECTS OF HETEROSPHERE STRUCTURE NOTING HEAT PROCESSES OF ORIGIN OF PLANETARY ATROSPHERES BALANCE. PHOTOOISSOCIATION AN0 6AS OIFFUSION 1165-61928 A65-19485

ORIGIN OF PLANETARY ATMOSPHERES - RICROYAVE PIKITOELECTRIC mOTOllRRY BRI6HTNESS REASURERENTS OF VENUS BRIGHTNESS OISTRIBUTION IN MAR6INAL LONE OF MARS Nb5-31367 USE0 TO DETERMINE ATMOSPHERIC ABSORPTION A65-18972

OXYGEN PHOTOELECTRIC IIEASUREMENT OF BRIGHTNESS VENUS RADIO SPECTRUR AN0 RICROYAVE ERISSION OF OISTRIBUTION IN LIMB ZONE OF RARS ATROSPHERIC ROLECULAR OXYGEN NASA-TT-F1001B N66-2 3 53 8 NASA-CR-57309 1165-19770 PHOTOELECTRIC OBSERVATION OF ATMOSPHERIC PRESSURE ON MARS SURFACE OXY6EN MTECTDR NASA-CR-7 1312 N66-23776 POLAR06RAPHIC OXYSEN ANALYZER FOR OBTAININ6 OATA ON RARS ATMOSPHERIC COMPOSITION Pnmo61um IWTERPRETATIW NASA-CR-57085 1165-18098 1924 AN0 1926 OPPOSITIONS OF MARS IN W. H. WRIGHT PLATES NOT1116 MARS OIAHETER IN IR KRYPTONATE OXYGEN DETECTOR AN0 ALURINUR OXIDE AN0 uv A65-20633 HYGROMETER FOR USE AS OXYGEN SENSORS FOR PLANETARY ATMOSPHERE MINER IV PHOTOGRAPHS OF PLANET MARS NOTING NASA-CR-63139 N65-25246 TOPOGRAWYI SOIL COMPOSITIONI ATROSPHERIC PHENORENA. POLAR CAP RIGRATION. RAOIATION. ETC 1166-20660 OXYGEN SENSOR KRYPTONATE OXYGEN DETECTOR AN0 ALURINUR OXIDE PHOTOG(UPH1C MEASUIEMWT HYGROMETER FOR USE AS OXYGEN SENSORS FOR PHOTORETRIC EXAHINATION OF BRIGHTNESS OISTRIBUTION PLANETARY ATROSPHERE MOW6 DISK OF MARS A66-19332 NASA-CR-63139 N65-252kb PHOTOGRAPHIC RECORDING PHOTOGRAPHIC RECORDING OF JUPITER ATmSPHERE OZONE NASA-CR-50303 N65-14653 RARTIAN ATROSPHERIC HEATING FROM SOLAR RAOIATION ABSORPTION IN UV'ANO VISIBLE BY OXYGEN AN0 OZONE ?HOTOIONIZATION AND IN NEAR IR BY CARBON OIOXIOE. NOTING VERTICAL ABSORPTION AN0 PHOTOIONIZATION COEFFICIENTS OF OISTRIBUTION OF GASES AN0 ABSORPTION PROPYLENE AN0 BUTENE 1 IN VACUUM ULTRAVIOLET - A65-23521 PLANETARY AERONORY NASA-CR-18 N65-17265 MARS ATROSPHERE OZONE OISTRIBUTION ANALYSIS INCLUDING PHOTOCHERICAL REACTIONS AN0 DISCREPANCY PHOTOIONIZATION RASS SPECTRORETER WITH 180 DE6 FACT ORs A65-25020 HAGWETIC ANALYZER AN0 USE AS GAS ANALYZER

1-23 PHOTOHETRY SUBJECT INDEX

NASA-CR-7 1210 Nbb-19636 SURFACE FRICTION Nbb-16208

PHOTOHETRY PLANETARY .CIRCULATION PATTERNS FOR INTEGRATED TWO- WATER VAPOR ON MARS AN0 VENUS, USING PHOTOMETRY LEVEL QUASI-GEOSTROPHIC MDOEC ATMOSPHERE OF ABSORPTION BAND WITH BALLOON MOUNTED TELESCOPE INCLUDING WATER VAPOR Nb6-16209 Ab5-33299 PLANETARY CONSTITUTION THICKNESS OF OUST ON LUNAR FLOOR, INFRARED JUPITER AND SATURN INTERIOR TEMPERATUIES FROM RADIOMETRIC TEMPERATURES OF BRIGHTER PLANETS, EXAMINATION OF ATMOSPHERIC COMPOSITION AN0 AND EXTENSIVE PHOTOMETRY OF MARS GRAVITATIONAL MULTIPOLE MOMENT Ab5-33302 AFCRL-64-926 Nb5-15288 I R SPECTRA OF SATURN RING AN0 GALILEAN PHOTOMETRIC OBSERVATIONS OF STARS IN OCCULTATION SATELLITES OF JUPITER SHOW ABSENCE OF STRONG AN0 PLANETARY ATMOSPHERIC EXPLORATION FROM ABSORPTION AT 8873 ANGSTROMS, INDICATING NEW UPPER ARTIFICIAL SATELLITE IN ORBIT LIMIT OF METHANE ABUNDANCE Ab5-35585 NASA-TT-F-8219 Nb5-22579 PLANETARY DISK JOVIAN ATMOSPHERE AND ENVIRONMENT - COMPOSITION. DEGREE OF POLARIZATION OVER CYTHEREANiEREAN DISK FOUND STRUCTURE. AN0 PHOTOMETRIC PROPERTIES OF TO INCREASE WITH DISTANCEISTANCE-FROM FROM CENTER OF PLANET ATMOSPHERE. PERIOD OF ROTATION, MAGNETIC FIELD. Ab5-25694 AND JOVIAN RADIOFREQUENCY SPECTRUM NASA-CR-63116 Nb5-24983 PLANETARY ENTRY SPECTRAL AND TOTAL RADIATION STUDIES OF BODIES PHOTOMETRY OF AUREOLE PROLONGING HORNS OF VENUS TRAVELING AT HYPERSONIC SPEED IN SIMULATED CRESCENT MARTIAN AN0 VENUSIAN ATMOSPHERES NASA-TT-F-9685 Nb5-33962 AIAA PAPER 65-116 Ab5-15008

METEOR PHENOMENA, UPPER ATMOSPHERE WIND FIELDS DENSE CARBON REINFORCED AND LOW DENSITY CHAR- FROM METEOR TRAILS, AND PHOTOMETRY OF A AN0 B FORMING RESIN ABLATION MATERIALS FOR RINGS OF SATURN AND VENUS ATMOSPHERE ENTRY EARTH,A 65- 15MARS6 19 AFCRL-65-33 Nb5-36000 EARTH REENTRY SIMULATION OF PLANETARY ENTRY PHYSICAL PROPERTY ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF PROBLEMS REGARDING CHEMICAL COMPOSITION AND MARS AND VENUS TYPE PHYSICAL PROPERTY OF VENUS ATMOSPHERE AIAA PAPER 65-218 Ab5-16606 Ab5-80868 MARS ATMOSPHERIC OENSITY, TEMPERATURE, COMPOSITION MARS ATMOSPHERE PROBLEMS RELATED TO CHEMICAL AND PRESSURE DETERMINATION FROM ENTRY RESPONSE OF COMPOSITION AND PHYSICAL PROPERTY SHALL PROBE Ab5-16989 165-80869 SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST PHYSICAL METHODS DESCRIPTION FOR DETECTION AN0 PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE. ANALYSIS OF TENUOUS PLANETARY ATMOSPHERIC TRACKING, COST AN0 SCHEDULE Ab5-17398 COMPONENT GASES, ESPECIALLY WATER VAPOR AIAA PAPER 65-219 NASA-CR-70934 Nbb-19901 VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE PHYSICAL SCIENCE INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AN0 OF RECENT SPACE RESEARCH IN PHYSICAL SCIENCES - STATIC EQUILIBRIUM WITHIN KAPLAN ATMOSPHERE LITERATURE SUMMARY AN0 DISCUSSION Ab5-19505 NASA-TM-X-51903 Nb5-29458 CLOSED FORM SOLUTIONS FOR INCLINATION ANGLE AN0 PHYSIOLOGICAL RESPONSE DENSITY OR ALTITUDE AS VELOCITY FUNCTION FOR BODY PLANETARY LIFE EFFECT ON BIOLOGICAL PRECURSOR ENTERING PLANETARY ATMOSPHERE Ab5-20563 MISSIONS TO MARS AIAA PAPER 65-249 Ab5-22120 AERODYNAMIC BRAKING TRAJECTORIES FOR MARS ORBIT ATTAINMENT, GIVING ENTRY CORRIDORS FOR LIFTING PLANET VEHICLES PLANETS AND SATELLITES IN SOLAR SYSTEM AIAA PAPER 64-478 Ab5-28839 NASA-TT-F-77 Nb5-14613 SPACECRAFT DECELERATION UPON ENTRY INTO MARS THICKNESS OF DUST ON LUNAR FLOOR, INFRARED ORBIT BY AERODYNAMIC BRAKING, CONSIDERING VEHICLE RADIOMETRIC TEMPERATURES OF BRIGHTER PLANETS. SHAPE AN0 VELOCITY EFFECTS ON ENTRY HEATING AND EXTENSIVE PHOTOMETRY OF MARS AIAA PAPER 64-479 Ab5-2 884 1 AFCRL-64-926 N65-15288 APPROXIMATE AN0 CHARACTERISTICS METHODS TO PREDICT INTERACTION OF SOLAR WIND WITH PLANETS - EFFECT OF GAS COMPOSITION ON FORCES AN0 STATIC PROPERTIES OF INTERPLANETARY MEDIUM AND STABILITY OF PLANETARY ENTRY CONFIGURATIONS IN AIR THEORETICAL MODELS OF SOLAR WINO AND ASSUMED MARTIAN ATMOSPHERES Ab5-29766 Nbb-14334 AIAA PAPER 65-318

MULTIDISCIPLINARY RESEARCH IN SPACE RELATED ROTATIONAL. PRECESSIONAL AN0 NUTATIONAL MOTION OF SCIENCE AND TECHNOLOGY - EVOLUTION PROCESSES OF BODY ENTERING MARS ATMOSPHERE IN VERTICALAb5-30321 AN0 ATMOSPHERE, MOON, EARTH, AND PLANETS OBLIQUE DIRECTIONS NASA-CR-69137 Nbb-15068 PLANETARY ENTRY VEHICLES - LONGITUDINAL STABILITY MULTIDISCIPLINARY STUDIES ON PLANETARY ATMOSPHERES CHARACTERISTICS FOR VARIOUS BLUNT-BODY MODELS IONOSPHERIC AN0 RADIOPHYSICS, PARTICLES AND TESTED AT MACH 6.73 IN WIND TUNNEL Nb5-22368 FIELDS, AN0 PLANETS NASA-TN-0-2785 NASA-CR-10165 Nbb-17290 PLANETARY ENVIRONMENT PLANETARY CIRCULATIONS PROJECT LUNAR AN0 PLANETARY ENVIRONMENTS USE0 BY NASA NUMERICAL INTEGRATION OF VARIOUS PLANETARY MANNED MISSION PLANNING AND DESIGN CONSIDERING CIRCULATION PATTERNS IN QUASI-GEOSTROPHIC MODEL RADIATIVE, TOPOGRAPHICAL AND ATMOSPHERIC AFEATURES 65-22 135 ATMOSPHERE INCLUDING WATER VAPOR, DIABATIC HEATING. AN0 SURFACE FRICTION AFCRL-65-771 Nbb-16207 SOLAR WINO PROTON VELOCITY. TEMPERATURE AND OENSITY DETERMINED WHEN MARINER I1 WAS NEAR CALCULATIONS FOR QUASI-GEOSTROPHIC PLANETARY VENUS Ab5-22598 CIRCULATION ATMOSPHERE WITH DIABETIC HEATING AND

1-24 SUBJECT INDEX ?LmT&RY MOIATIDll

POSSIBLE ALTERNATIVE CHEMICAL ELEMENTS AN0 ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN COMPOUNOS SUITABLE FOR PROLONGED BIOMOLECULAR EXPLORATION A6535112 EVOLUTION AND CHEMICAL SELECTION ON NONTERRESTRIAL TYPE PLANET 1165-27096 LECTURE MANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONS. BIOLO6ICAL EXPLORATION OF MARS. MASERS AND PLANETS HABITABLE FOR MAN A65-80977 LASERS. PLANETARY ATMOSPHERES. RELATIVITY THEORY. ELEMENT ABUNDANCE. AND SOLAR PARTICLES BIBLIOGRAPHY OF DOCUMENTS ON LUNAR. PLANETARY. N65-31360 AND SPACE ENVIRONMENTS IN RELATION TO FLIGHT MECHANICS AND AERODYNAMICS OF SPACE TRAVEL SPACE EXPLORATION - SPACE AROUND EARTH. NASA-CR-60469 N65-16086 ATMOSPHERIC CIRCULATION AN0 WEATHER COMOITIONS. LUNAR PHOTOGRAPHY. AND PLANETARY STUDIES PLANETARY ENVIRONMENTAL DESIGN DATA FOR FUTURE NASA-EP-25 ~ei-325r4 MANNED SPACE FLIGHTS TO VENUS AND MARS NASA-SP-3016 ~65-23799 PAPERS PRESENTED AT SCIENTIFIC BALLOON SYMPOSIUM ON BALLOON DESIGN. MATERIALS. STRESS HIGH ENERGY DENSITY BATTERY FOR USE ON PLANET STUDIES. INSTRUMENTATION. METEOROLOGY. LOCATING VENUS SYSTEM.-ANO PLANETARY EXPLORATION APPLICATIONS NASA-CR-54404 N65-24338 AFCRL-65-466 N65-34804

INTEGRATION OF TERRESTRIAL AND PLANETARY FEASIBILITY AN0 OESI6N OF BALLOONS FOR EXPLORATION ENVIRONMENT SENSING N65-33556 OF SURFACE AND ATMOSPHERE OF MARS N65-34830 SPACE ENVIRONMENT - DATA ON ELECTROMAGNETIC AN0 PARTICULATE RAOIATIONI METEOROID FLUX. AN0 COMMUNICATIONS OF ARIZONA LUNAR AN0 PLANETARY STRUCTURE. AN0 COMPOSITION OF PLANETARY LABORATORY. VOLUME 3 116620291 ATMOSPHERE - SOLAR SYSTEM SPACE ENVIRONMENT NASA-CR-294 W5-34244 SCIENTIFIC RESEARCH USING INSTRUIIEMTS IN SPACE VEHICLES. NOTING DIRECT OBSERVATIONS DF MOON. NUCLEIC ACID MOLECULE REPRODUCTION DISCUSSING VENUS. MARS* 6LOBM COMMUNICATIONS~METEOROL06Yr PROBABILITY OF LIFE DEVELOPMENT UNDER FAVORABLE GEODETIC AND NAVIGATION SATELLITES. EX ENVIRONMENTAL CIRCUMSTANCES A66-15915 A66-23639

PLANETARY ENVIRONMENTS IN VARIOUS MOOELS EXTRATERRESTRIAL LIFE IN SOLAR SYSTEM. DISCUSSING A66-20287 EQUIPMENT FOR MARS EXPLORATION. NOTING 6ULLIVER PROGRAM. MULTIVATOR AUTOMATIC BIOCHEMICAL TESTING SPACE TRAVEL AN0 EXPLORATIONI BIOLOGICAL AN0 APPARATUS AND TV MICROSCOPE A66-237% TECHNICAL OIFFICULTIES. RADIATION. METEOR IMPACT. VEHICLE STERILIZATION. ETC A66-23640 TELESCOPE OESIW FOR INTERFERMIETER SPECTROMETER FOR PLANETARY ATMOSPHERE EXPLORATION PLANETARY ENVIRONMENTAL MODELS OF VENUS. MARS. N66-14107 MERCURY. JUPITER. PLUTO. NEPTUNE. AND URANUS AN0 SATELLITES ATMOSPHERIC COMPOSITION^ PLANETMY 6RAVITATlOU TEMPERATURES. AND CIRCULATION 1166-10996 TEMPERATURE. DENSITY AND GRAVITATIONAL ESCAPE ON MARS. MERCURY* JUPITER AND VENUS ATMOSPHERES EFFECTS OF SIMULATED ANAEROBIC PLANETARY A6615759 ENVIRONMENT ON BIOCHEMICAL ACTIVITIES OF TERRESTRIAL MICROORGANISMS CLAUl3MY LIIOIIK NASA-CR-71195 W6-20131 MARS ATMOSPHERE OEFINITION IMPORTANT IN AOVANCEO LANDING VEHICLE DESIGN WITH INCREASED PAYLOAD PLANETARY EVOLUTION CAPABILITY AN0 REDUCED COMPLEXITY PLANETARY ATMOSPHERES ORIGIN DUE TO OUTGASSING OR AIM PAPER 65-22 A65-145b3 CAPTURE FROM PRIMITIVE SOLAR NEBULA OR SOLAR WINO AND ATMOSPHERIC LOSSES DUE TO REVERSE PROCESSES MARS ATMOSPHERE DEFINITION IMPORTANT IN AOVANCEO A65-32627 LANDING VEHICLE DESI6N WITH INCREASED PAYLOAD CAPABILITY AN0 REWCED COMPLEXITY PLANETARY EXPLORATION AIM PAPER 65-22 A66-24697 ORBITER INJECTEO STERILIZED BALLISTIC SKIPOUT CAPSULE FOR IN FLIGHT MARTIAN STRATOSPHERE ALTERNATE MISSION PROFILES FOR MANNED MARS MEASUREMENTS. USING NONABLATIVE HEAT SHIELD AND LANOING OUTSIDE ATMOSPHERIC PROPULSION MANEUVERS NASA-TN-0-3181 W6-14703 AIM PAPER 65-23 A65-15944 PLANElUY IUG(IETIC FIELD I R SPECTROSCOPY ROLE IN BIOLOGICAL EXPLORATION OF SEARCH FOR TRAPPED ELECTRONS AN0 MA6NETIC MOMENT MARS PROVIDING DATA ON ATMOSPHERIC AND SURFACE AT MARS BY MARIMER IV A65-36325 PARAMETERS A65-26729 JOVIAN ATMOSPHERE AN0 ENVIROIIMEEIT - CO(lP0SITIffl. BALLOON ELEVATE0 I STRATOSCOPE 11/ REMOTE STRUCTURE. AN0 PHOTOMETRIC PROPERTIES OF CONTROLLED TELESCOPE FOR ASTRONOMICAL OBSERVATION ATMOSPHERE. PERIOD OF ROTATION. MAGNETIC FIELO. OF PLANETS. NEBULAE. ETC. FROM UPPER ATMOSPHERE AN0 JOVIAN RADIOFREWENCY SPECTRUI A65-28940 NASA-CR-63116 165-24983

ATMOSPHERE POSTULATION BASE0 ON KOZYREV POSITION DETERMINATION OF EQUATORIAL BOUNDARY OF OBSERVATION OF HYDROGEN. ENTRY TRAJECTORY ANALYSIS ABNORMALLY HIGH NOCTURNAL ATMOSPHERIC IONIZATION AN0 FEASIBILITY OF ATMOSPHERIC BRAKING FOR LANDING FOR VARIOUS LEVELS OF PLANETARY MAGNETIC ACTIVITY PAYLOAD ON MERCURY ~66-19r93 AIM PAPER 65-494 A65-29684 PLuKfARY MOTION ENTRY VEHICLE DESIGN FOR PLANETARY EXPLORATION TELESCOPIC OBSERVATIONS OF VENUS INDICATE FOUR- USING NONSURVIVING NEEDLE-NOSED PROBE FOR DATA DAY RETROGRADE ROTATION PERIOD BASED ON UV COLLECTION ON MARS ATMOSPHERE COMPOSITION. PHOTOGRAPHS ~65-zr550 PRESSURE AN0 DENSITY AIM PAPER 65-493 A65-32321 CLAlETARY MDIATIW HOMOGRAPH ON RADIO EMISSION OF SUN AN0 PLANETS WEIGHT AN0 ENERGY REQUIREMENTS OF VEHICLE SYSTEMS A65-16909 FOR MANNED EXPLORATION OF MARS AIM PAPER 64-403 A65-33549 MOWLATION MICROWAVE RADIOMETER FOR MEASUIING JUPITER RADIATION INTENSITY IN roo m RANSE SYSTEM DESIGN OF AUTOMATE0 LABORATORY AND A65-18553

1-25 PLANETARY SURFACE SUBJECT INDEX

FINAL REDUCTION OF OBSERVATIONS OF SPORADIC ILLUMINAT ION PHASE A66-20111 OUTBURSTS IN DECAMETRIC REGION OF RADIO SPECTRUM OF JUPITER DURING 1961 AN0 1962 RADIO OBSERVATION OF PLANETARY AN0 STELLAR A65-218 5 5 EMISSION AND EFFECTS OF TERRESTRIAL ATMOSPHERE A66-20289 BRIGHTNESS TEMPERATURE OF RADIO EMISSION FROM VENUS A65-24803 EQUILIBRIUM AN0 NONEQUILIBRIUV STAGNATION POINT SHOCK LAYER RADIATION IN SIMULATED PLANETARY CONFINEMENT OF DECAMETRIC RADIATION FROM JUPITER ATMOSPHERES OF VARYING COMPOSITION TO NARROW BEAMS ATTRIBUTED TO BELTS OF TRAPPED A66-21773 CHARGED PARTICLES SIMILAR TO VAN ALLEN BELTS A65-25632 PLANETARY RADIATION AN0 ALBEDO EFFECTS ON THERMAL BALANCE OF SPACECRAFT ORBITING MARS AN0 VENUS LINEAR POLARIZATIONI PLANETARY ROTATION OF NASA-CR-67813 N66-10684 POLARIZATION, LUNAR OCCULTATION AN0 INTENSITY SPECTRUM OF JUPITER OECIMETRIC EMISSIONS RADIO ASTRONOMY - PASSIVE RECEPTION OF RADIATION A65-26042 IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL SOURCES SUCH AS MOON/LUNAR THERMAL EMISSION, AND MODULATION MICROWAVE RADIOMETER FOR MEASURING PLANETARY RADIO EMISSION N66-10998 JUPITER RADIATION INTENSITY IN 700 MC RANGE A65-27146 PLANETARY SURFACE PHOTOMETRIC DETERMINATION OF MARTIAN ATMOSPHERE OBSERVATIONS CONCERNING ORIGIN OF VENUS RADIO AND SURFACE OPTICAL THICKNESS AN0 ABSORPTION AS EMISSION AN0 ABOUT IONOSPHERE SURROUNDING PLANET FUNCTIONS OF WAVELENGTHS A~S-1~974 A65-27771 BOOK ON LUNAR AN0 PLANETARY SURFACE CONDITIONS I R ASTRONOMY, DETECTION DEVICES AN0 EVALUATION OF UITH DESCRIPTIONS OF ATMOSPHERIC EFFECTS, LIFE OBSERVATIONS OF MOON AND PLANETS DETECTION AN0 DATA COLLECTING SYSTEMS A65-30119 A65-26272

THERMAL EMISSION MAPS OF JUPITER, DISCUSSING CONCEPTS CONCERNING JUPITER SURFACE REVISED SOURCE OF NOISE FROM TRACKING ERRORS AN0 FOLLOWING TRANSFORMATIONS OBSERVED SINCE 1962 AN0 PHOTOMETRIC ERRORS A65-31279 ESTIMATION OF ASH PARTICLES IN PLANET ATMOSPHERE A65-30238 METHANE AN0 AMMONIA LABORATORY SPECTRA COMPARED WITH SPECTRA OF JUPITER, INDICATING CAUSES OF RAOIO AND RADAR ASTRONOMY STUDIES OF LUNAR AND UNIDENTIFIED ABSORPTIONS A65-35022 PLANETARY ATMOSPHERES AN0 SURFACES, AND RADAR STUDIES OF SUN AN0 INTERPLANETARY MEDIUM VENUS ATMOSPHERE BRIGHTNESS-TEMPERATURE MAPPING OF NASA-CR-57184 ~65-le944 8-14 MICRON RADIATION BEFORE 1964 CONJUNCTION A65-35025 BISTATIC RADAR METHODS USE0 TO STUDY PLANETARY IONOSPHERES AND SURFACES N65-24310 DIFFERENTIAL POLARIZATION AN0 DISTRIBUTION OF NASA-CR-62823 RAOIOEMISSION OF DIFFERENT PARTS OF VISIBLE DISK OF VENUS MEASURED BY INTERFEROMETER MARS SURFACE AN0 ATMOSPHERE CHARACTERISTICS FROM A65-35268 THERMAL EMISSION SPECTRUM MEASUREMENT By INFRARED INTERFEROMETER ON PLANETARY FLYBY SURFACE PRESSURE OF MARS ATMOSPHERE REDETERMINED SPACECRAFT N65-32114 FROM ABSORPTION INTENSITY OF CARBON DIOXIDE BY NASA-TM-X-55070 LONG-PATH AN0 PHOTOMULTIPLIER DETECTION A65-35360 PLANETARY ATMOSPHERES AN0 SURFACES - SYMPOSIUM. DORAOO. PUERTO RICOS MAY 1965 U V REFLECTIVITY OF MARS ANALYZED FROM A66-20101 SPECTROGRAMS OBTAINED ON AEROBEE ROCKET ~65-35583 RADAR OBSERVATIONS OF MERCURY. VENUSi MARS AN0 JUPITER SURFACES A6620116 ANALYSIS OF EQUILIBRIUM SHOCK LAYER RADIATION FOR MARS ATMOSPHERIC ENTRY N65-32433 SURFACE DISTURBANCES AS POSSIBLE CAUSE OF TECTONIC MOVEMENT IN JUPITER ATMOSPHERE - ASTRONOMY EMISSION AN0 ABSORPTION OF RADIANT ENERGY IN MODEL T-439-R N66-10590 MARTIAN ATMOSPHERE COMPOSED OF 15 PERCENT CARBON DIOXIDE AN0 85 PERCENT NITROGEN BY VOLUME RADIO AN0 RADAR ASTRONOMY - LUNAR AN0 PLANETARY A66- 15117 IONOSPHERES, ATMOSPHERES, AN0 SURFACES, AN0 RADAR STUDIES OF SUN AN0 INTERPLANETARY MEDIUMN66- 10609 ELECTROMAGNETIC PROPAGATION CHARACTERISTICS OF NASA-CR-67794 VENUS AND MARS DERIVED FROM ATMOSPHERIC DATA A66-16436 MARINER I1 MICROWAVE RADIOMETER EXPERIMENT TO STUDY VENUS SURFACE AND ATMOSPHERE OBSERVATIONS CONCERNING ORIGIN OF VENUS RADIO NASA-CR-69916 N66-16151 EMISSION AN0 ABOUT IONOSPHERE SURROUNDING PLANET A66-16625 PNEUMATIC SURFACE SAMPLING DEVICE FOR USE IN SIMULATED MARS ENVIRONMENT RADIO NOISE EMISSION FROM VENUS SURFACE EXPLAINED NASA-CR-70937 N66-20080 IN TERMS OF GLOW DISCHARGE A66-17174 PLANETARY TEMPERATURE STRELKOV THEORY OF RADIO EMISSION FROM VENUS SURFACE TEMPERATURE DISTRIBUTION OF MERCURY BASE0 ATTRIBUTES HIGH TEMPERATURE RADIATION TO ON MEASUREMENTS OF MEAN DISK TEMPERATUIE OVERA65-22205 WIDE RADIOACTIVE HEATING OF PLANETARY SURFACE RANGE OF PHASE ANGLES A66-19324 JUPITER AN0 SATURN INTERIOR TEMPERATURES FROM ATMOSPHERIC COMPOSITION OF VENUS AN0 EFFECT ON EXAMINATION OF ATMOSPHERIC COMPOSITION AN0A65-33302 RADIO EMISSION IN VISIBLE AND NEAR IR SPECTRAL GRAVITATIONAL MULTIPOLE MOMENT BANDS A66-19325 DIFFERENTIAL POLARIZATION AN0 DISTRIBUTION OF MARS ATMOSPHERIC OPTICAL THICKNESS AN0 SCATTERING RADIOEMISSION OF DIFFERENT PARTS OF VISIBLE DISK FROM PHOTOMETRIC OBSERVATION A66-19327 OF VENUS MEASURED By INTERFEROMETER A6535268

VENUS RADIATION AT 13.5 MM WATER VAPOR LINE AND PLANETARY BRIGHTNESS VARIATION WITH SOLAR RADIO EMISSION OF SATURN ON WAVELENGTH OF e MM

1-26 SUBJECT 1-X RADAR OBSRIVATIOU

COMPARE0 WITH VALUES OBTAINED AT OTHER WAVELEWTHS POLARIZATIONI LUNAR OCCULTATION AND INTENSITY A65-35841 SPECTRUM OF JUPITER OECIMETRIC EMISSIONS A65-26042 PLANETARY ATMOSPHERE COMPOSITION. TEMPERATURE. AN0 PRESSURE OF MARS. VENUS. AN0 JUPITER DIFFERENTIAL POLARIZATION AN0 DISTRIBUTION OF NASA-TM-X-56223 N65-20799 RIOlOEMISSION OF DIFFERENT PARTS OF VISIBLE 01% OF VENUS MEASURE0 BY INTERFEROMETER BRIGHTNESS TEMPERATURE MEASUREMENTS OF MARS AT A65-35268 3.75 CM FROM FEBRUARY TO JUNE 1965 A66-18788 PoLAm6MPHY POLAROGRAPHIC OXYGEN ANALYZER FOR OBTAINIMG DATA BRIGHTNESS TEMPERATURE MEASUREMENTS ON 011 MARS ATMOSPHERIC COMPOSITION ILLUMINATED SIDE OF VENUS AT 10-6 CM CHALLEWES NASA-CR-57085 Nb5-18098 TROITSKI THEORY OF PLANETARY RADIATION EMISSION A66-19457 MlOElED METAL IGWITION TEMPERATURES of POWDERED METALS IN VENUS RADIATION AT 13.5 MM MATER VAPOR LINE AND SIMULATED ATMOSPHERES OF VENUS AND MARS SU;GEST PLANETARY BRIGHTNESS VARIATION WITH SOLAR POTENTIAL CHEMICAL ENERGY SOURCES ILLUMINATION PHASE A66-20111 A66-22458

VENUS CLOUD LAYER AN0 BRIGHTNESS TEMPERATURE FROn PWER SERIES RADIOMETRIC MICROWAVE OBSERVATIONS FROM NOCTURNAL CLOSE0 FORM SOLUTIONS FOR INCLINATION AN6LE AND SIDE OF PLANET A66-20112 DENSITY OR ALTITUDE AS VELXITY FUNCTION FOR BODY ENTERING PLANETARY ATMOSPHERE 1165-20563 RADIO OBSERVATIONS OF MERCURY SHOW BRIGHTNESS TEMPERATURE OF ONLY 200 DEGREES K. WITH NO MYER SUPcL* SIGNIFICANT VARIATION WITH PHASE VOYAGER SUBSYSTEM DESIGN STUDY - GUIOIWCE AN0 M6-20182 CONTROL. PROPULSION. AND POWER SUPPLY STUDIES FOR ENTRY IN MARS OR VENUS ATMOSPHERES BLACK BODY DISK TEMPERATURES OF MERCURY AND MARS NASA-CR-51837 166-13407 FROM OBSERVATIONS AT 3.4 MM IN APRIL 1965 A6622786 PROCELLANT UlMWSTIOW THEORETICAL FUEL-BASE0 SPECIFIC IMPULSE LIGHT PLANT /BIOL/ METAL-NITROGEN SYSTEM FOR RAMJET AN0 TURBOJET SEE0 GERMINATION OF COMMON PLANT SPECIES IN PROPULSION IN MARTIAN ATMOSPHERE RAREFIED NITROGEN ATMOSPHERES SIMULATING A65-15610 EXTRATERRESTRIAL ENVIRONMENT A65-32416 PROPULSION PLUTO IPLANET/ PRDPULSIOW ORIENTED STUDY OF MISSION MJOES FOR PLANETARY ENVIRONMENTAL MODELS OF VENUS. MARS+ MANNED MARS LANDING MERCURY. JUPITER. PLUTO. NEPTUNE. AND URANUS NASA-TM-X-53265 N65-28960 AN0 SATELLITES ATMOSPHERIC CfflPOSITION. TEMPERATURES. AN0 CIRCULATION N66-10996 VOYAGER SUBSYSTEM DESIGN STUDY - GUIDANCE AN0 CONTROL. PROPULSION. AND POWER SUPPLY STUDIES STRUCTURE. COMPOSITION. ATMOSPHERE. AN0 SCIENTIFIC FOR ENTRY IN MARS OR VENUS ATMOSPHERES OBJECTIVE SURVEYS FOR SATURN. URANUS. NAS A-CR-5 1837 1166-13407 NEPTUNE. AN0 PLUTO NASA-CR-70328 N66-17090 rn0m-E ABSORPTION AND PHOTOIONIZATION COEFFICIENTS OF PNEUMATIC EQUIPI(HIT PROPYLENE AND BUTENE 1 IN VACUUM ULTRAVIOLET - PNEUMATIC SURFACE SAMPLIIIG DEVICE FOR USE IN PLANETARY AERONOMY SIMULATED MARS ENVIRONMENT NASA-CR-18 1165-17265 NASA-CR-70937 N6620080

POLARIMETRY R SURFACE PRESSURE AND CARBON DIOXIDE CONTENT OF RADAR ASTROWOIY MARTIAN ATMOSPHERE. COMPARING POLARIMETRIC. RADIO AN0 RADAR ASTRONOMY STUDIES OF LUNAR AND PHOTOMETRIC AN0 SPECTROSCOPIC METHODS PLANETARY ATMOSPHERES AN0 SURFACES. AN0 RADAR A65-26212 STUDIES OF SUN AND INTERPLANETARY MEDIUM NASA-CR-57 184 1165-18944 POLAR IZAT ION CHARACTER I STICS DEGREE OF POLARIZATION OVER CYTHEREAN DISK FOUND RADIO AND RADAR ASTRONOMY - LWAR AND PLANETARY TO INCREASE WITH DISTANCE FROM CENTER OF PLANET IONOSWERESs ATMOSPHERES. AND SURFACES. AND A65-25694 RADAR STUDIES OF SUN AN0 INTERPLANETARY MEDIUM NAS A-CR-67794 N66-10609 ATMOSPHERE OF MERCURY. USING DIFFERENTIAL POLARIZATION EFFECT AN0 BRIGHTNESS TEMPERATURE RADIO AN0 RADAR ASTRONOMICAL STUDIES OW LUNAR AND MEASUREMENTS A65-33300 PLANETARY IONOSPHERES AND ATMOSPHERES. AND SOLAR ACTIVITY COMPOSITION OF MARTIAN ATMOSPHERE. USIW NASA-CR-71090 N66-19528 POLARIMETRIC OBSERVATIONS A65-33301 RADU MEASURUIENT POLARIZATION AN0 BRIGHTNESS TEMPERATURE TWO-FREQUENCY BISTATIC RADAR-OCCULTATION TECHNIQUE OISTRIBUTION MEASUREMENTS OF VENUS IN 10.6 CM TO INVESTIGATE PLANETARY ATMOSPHERES WAVELENGTH A65-31267 STdA-LPS-10334 N66-11138 RADAR OBSERVATIOW POLARIZED Lf6HT BISTATIC RADAR-OCCULTATION METHOD FOR PLANETARY DISCREPANCY IN PHOTOMETRIC AND VISIBLE ATMOSPHERE STUDY POLARIMETRIC OETERHINATIDNS OF MARS SURFACE NASA-CR-57178 N65-lBW6 PRESSURE ATTRIBUTE0 TO AEROSOL PARTICLES IN MARTIAN ATMOSPHERE A65-26945 MARINER I1 RADAR AND RADIOMETRIC OBSERVATIONS OF VENUS DURING 1962 CONJUNCTION - PHYSICAL OATA FORMULAS FOR LIGHT PASSAGE THROUGH PLANETARY NASA-CR-56851 N65-22203 ATMOSPHERES OF FINITE OPTICAL THICKNESS. TAKIN6 INTO ACCOUNT POLARIZATION A66-15415 BISTATIC RADAR METHODS USED TO STUDY PLANETARY IONOSPHERES AND SURFACES PMARIZEO MDIATIOW NASA-CR-62823 N65-24310 LINEAR POLARIZATION. PLANETARY ROTATION OF

1-27 RADIATION ABSORPTION SUBJECT INDEX

RADAR OBSERVATIONS OF MERCURY, VENUS. MARS AN0 A65-16909 JUPITER SURFACES A66-20116 RADIO PATH FORMULAS FOR PLANETARY IONOSPHERES AN0 ROTATION OF PLANET MERCURY FROM RADAR OBSERVATION STELLAR ATMOSPHERES FROM QUASI-CONIC EQUATION AN0 EXPLAINED BY SOLAR GRAVITATIONAL TORQUE ON TIDAL ELECTRON DENSITY EQUATION A65-23429 DEFORMATION AN0 EQUATORIAL PLANE ASYMMETRY NASA-CR-68703 N66-13573 RADIO ASTRONOMICAL OBSERVATIONS OF VENUS WITH HIGH RESOLVING POWER RAD1AT ION ABSORPT ION NRL-TRANS-936 N65-17990 EMISSION AN0 ABSORPTION OF RADIANT ENERGY IN MODEL MARTIAN ATMOSPHERE COMPOSED OF 15 PERCENT CARBON ANALYTICAL RELATIONS CONNECTING BRIGHT TEMPERATURE DIOXIDE AN0 85 PERCENT NITROGEN BY VOLUME OF RADIO EMISSION OF VENUS COVERED BY ABSORBING A66-15777 ATMOSPHERE WITH PHYSICAL PARAMETERS N65-2 722 6 RADIATION BELT CONFINEMENT OF DECAMETRIC RADIATION FROM JUPITER ATMOSPHERIC COMPOSITION OF VENUS AN0 EFFECT ON TO NARROW BEAMS ATTRIBUTED TO BELTS OF TRAPPED RADIO EMISSION IN VISIBLE AN0 NEAR IR SPECTRAL CHARGED PARTICLES SIMILAR TO VAN ALLEN BELTS BANDS A66-19325 A65-25632 PLANETARY ATMOSPHERES AN0 SURFACES - SYMPOSI UMt RADIATION COOLING OORAOO, PUERTO RICO, MAY 1965 I R COOLING RATE IN PLANETARY ATMOSPHERES, NOTING A66-20101 CURTIS- GODSON APPROXIMATION. DOPPLER LINE SHAPE. WATER VAPOR ROTATION BAND, ETC RADIO OBSERVATIONS OF MERCURY SHOW BRIGHTNESS A66-22264 TEMPERATURE OF ONLY 200 DEGREES K. WITH NO SIGNIFICANT VARIATION WITH PHASE RADIATION DETECTOR A66-20182 I R ASTRONOMY, DETECTION DEVICES AN0 EVALUATION OF OBSERVATIONS OF MOON AN0 PLANETS RADIO OBSERVATION OF PLANETARY AN0 STELLAR 165-301 19 EMISSION AND EFFECTS OF TERRESTRIAL ATMOSPHERE A66-20289 RADIATION EMISSION RADIO ASTRONOMY - PASSIVE RECEPTION OF RADIATION RADIO AN0 RADAR ASTRONOMY - LUNAR AN0 PLANETARY IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL IONOSPHERES, ATMOSPHERES, AN0 SURFACES. AN0 SOURCES SUCH AS MOON/LUNAR THERMAL EMISSION, AN0 RADAR STUDIES OF SUN AN0 INTERPLANETARY MEDIUM PLANETARY RADIO EMISSION N66-10998 NASA-CR-67794 N66-10609 RADIATION INTENSITY RADIO ASTRONOMY - PASSIVE RECEPTION OF RADIATION X-RAY RADIATION INTENSITY OF AURORAE POLARIS OF IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL PLANET TO DETERMINE MAGNETIC MOMENT SOURCES SUCH AS MOON/LUNAR THERMAL EMISSION. AND A65-15763 PLANETARY RADIO EMISSION N66-10998

MODULATION MICROWAVE RADIOMETER FOR MEASURING GALACTIC AN0 PLANETARY RADIO ASTRONOMY - SOUNDING JUPITER RADIATION INTENSITY IN 100 MC RANGE ROCKET LAUNCH, ORBITING TELESCOPE, CARBON-OXYGEN A65- 18553 COMPLEX PHOTOCHEMISTRY, MARS IONOSPHERE. TOPSIDE ELECTRON DENSITY, AN0 NONRIGID BODIES MODULATION MICROWAVE RADIOMETER FOR MEASURING NASA-CR-70 152 N66-16597 JUPITER RADIATION INTENSITY IN 700 MC RANGE A65-27146 RAOIO AN0 RADAR ASTRONOMICAL STUDIES ON LUNAR AN0 PLANETARY IONOSPHERES AN0 ATMOSPHERES, AN0 SOLAR LIGHT SCATTERING IN PLANETARY ATMOSPHERE - FORMULA ACTIVITY FOR DETERMINING INTENSITY OF RADIATION LEAVING NASA-CR-71090 N66-19520 HOMOGENEOUS SPHERE AFTER SINGLE DIFFUSION N65-24480 JUPITER OPTICAL EMISSION AND AURORAL ACTIVITY STUDY CALCULATIONS OF MIDDAY DAYGLOW INTENSITIES AD-624895 N66- 19676 ARISING FROM FLUORESCENCE OF SOLAR IONIZING RAD1AT ION RADIO BURST NASA-CR-64424 N65-31047 FINAL REDUCTION OF OBSERVATIONS OF SPORADIC OUTBURSTS IN DECAMETRIC REGION OF RADIO SPECTRUM RADIATION MEASUREMENT OF JUPITER DURING 1961 AN0 1962 RADIATION GAUGING METHODS FOR UNMANNED PROBE TO A65-21855 MEASURE MARTIAN ATMOSPHERIC DENSITY DURING ENTRY RAOIO EMISSION NASA-CR-62971 N65-24895 COLD ABSORBING ATMOSPHERE MODEL OF VENUS BASED ON CENTIMETER AN0 MILLIMETER EMISSION SPECTRUM RADIATION SPECTRUM A65-19676 OBSERVED RADIATION SPECTRUM OF VENUS ATMOSPHERE WITH DECREASE IN BRIGHTNESS TEMPERATURE BRIGHTNESS TEMPERATURE OF RADIO EMISSION FROM EXPLAINED BY ABSORPTION IN RELATIVELY COLD VENUS A65-24803 SURROUNDING IONOSPHERE N65-2 452 6 LINEAR POLARIZATION, PLANETARY ROTATION OF RADIATION TRANSFER POLARIZATION, LUNAR OCCULTATION AN0 INTENSITY RADIATIVE TRANSFER AN0 IMPERFECT SCATTERING IN SPECTRUM OF JUPITER OECIMETRIC EMISSIONS PLANETARY ATMOSPHERES FROM CHAPMAN APPROACH A65-26042 A66-23414 OBSERVATIONS CONCERNING'ORIGIN OF VENUS RADIO RADIATIVE HEAT TRANSFER EMISSION AN0 ABOUT IONOSPHERE SURROUNDING PLANET EQUILIBRIUM AN0 NONEQUILIBRIUM STAGNATION POINT A65-27771 SHOCK LAYER RADIATION IN SIMULATED PLANETARY ATMOSPHERES OF VARYING COMPOSITION DIFFERENTIAL POLARIZATION AN0 DISTRIBUTION OF A66-21113 RADIOEMISSION OF DIFFERENT PARTS OF VISIBLE DISK OF VENUS MEASURE0 BY INTERFEROMETER RADIO ASTRONOMY A65-35268 RADIO ASTRONOMY SKETCH NOTING SOLAR, GALACTIC AN0 COSMIC RAY OBSERVATIONS AN0 INSTRUMENT RADIO EMISSION OF SATURN ON WAVELENGTH OF 8 MM DIFFICULTIES A65-15368 COMPARED WITH VALUES OBTAINED AT OTHER WAVELENGTHS A65-35841 MONOGRAPH ON RADIO EMISSION OF SUN AN0 PLANETS

1-28 SUBJECT INDEX wILIw6 DEVICE

OBSERVATIONS CONCERNING ORIGIN OF VENUS RADIO SPECTROSCOPY OF PLANETARY ULTRAVIOLET RADIATION - EMISSION AND ABWT IONOSPHERE SURROLMOING PLANET RAYLEIGH SCATTERIN6 AND ELECTRON EXCITATION A66-16625 NASA-CR-67597 N66-15400 RADIO NOISE IKMERY ZOlE RADIO NOISE EMISSION FROM VENUS SURFACE EXPLAINED SPACE VEHICLE RECOVERY TRAJECTORIES EMENDIN6 FROM IN TERMS OF GLOW DISCHARGE A66-17174 GIVEN INITIAL ORBIT TO ATMOSPHERE TOP A65-19314 RADIO OBSERVATION SURFACE TEMPERATURE OISTRIBUTION OF MERCURY BASED REENTRY MllOITIOl ON MEASUREMENTS OF MEAN 01% TEMPERATURE OVER WIDE EMTH REENTRY SIlluLATION OF PLANETARY ENTRY RANGE OF PHASE AN6LES A65-22205 ENVIROWMENT WITH EXWNENTIAL ATMOSPHERES OF MARS AN0 VENUS TYPE RADIO PROPAGATION AIAA PAPER 65-218 A65-16606 RADIO PATH MRMULAS FOR PLANETARY IONOSPHERES AND STELLAR ATMOSPHERES FROM QUASI-CONIC EQUATION AND REEUTRY WSICS ELECTRON DENSITY EQUATION Ab5-23429 TRANSLATIONAL AN0 ROTATIONAL MOTION OF SPHERICAL BODY ENTERING MARS ATMOSPHERE - REENTRY PHYSICS DIFFRACTION AN0 REFRACTION OF RADIO WAVES TO STWY WJA-CR-69252 ~6b-is33a PLANETARY ATMOSPHERE A65-29491 REWRY SliII3.D RADIO SOURCE DENSE CARBON REINFORCED AN0 LOW DENSITY CHAR- RADIO ASTRONOMY - PASSIVE RECEPTION OF RADIATION FOR111116 RESIN ABLATION MATERIALS FOR EARTH. MARS IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL AND VENUS ATMOSPHERE ENTRY A6515619 SOURCES SUCH AS M00N1LlWAR THERMAL EMISSION. AND PLANETARY RADIO EMISSION N66-10998 REEUTRY VEHICLE ESTIMATING ERRORS IN DENSITY AND PRESSURE RADIO SPECTRIM STRUCTURE OF PLANETARY ATMOSPHERE CONSTRUCTEO VEWS RADIO SPECTRUM AND MICROWAVE EMISSION OF FROM MEASURED ACCELERATIONS OF ENTRY VEHICLE ATMOSPHERIC MOLECULAR OXYGEN NASA-TR-R-225 N65-29299 NASA-CR-57309 N65-19770 PRINCIPLES FOR DETERMINING PROPERTIES OF UNKNOWN RADIO TRANSHISSION PLANETARY ATMOSPHERE FROM RESPONSES OF COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE REENTERING PROBE VEHICLE AND IONOSPHERE OF MARS INCLUDING DENSITY. NASA-TM-X-56125 N6b-19497 TEMPERATURE. SCALE HEIGHTS ETC A65-36328 REFLECTIOl COEFFICIB(T RADIO WAVE JUPITER PHOTOELECTRIC SPECTRAL SCAN IN UV METHOD FOR STUDY OF PLANETARY IONOSPHERES BASE0 REPROWCED AS GEOMETRIC REFLECTIVITY VS ON RADIO WAVE PROPAGATION BETWEEN EARTH AND WAVELENGTH. USING AEROBEE ROtKET SPACECRAFT A66-21099 NASA-CR-64460 N65-32199 REFRACTIVE IWEX RADIOMETRY COUPLE0 HARTREE- FOCK APPROXIMATION FOR THICKNESS OF OUST ON LUNAR FLOOR. INFRARED CALCULATING FREQUENCY-DEPENDENT REFRACTIVE INOEX RAOIOIIETRIC TEMPERATURES OF BRISHTER PLANETS. OF HELIUN GAS AND EXTENSIVE PHOTOMETRY OF MARS NASA-CR-66991 N66-14281 AFCRL-64-926 N65-15288 UELATIVIlV T-Y METHODS FOR OBTAINING TEMPERATURE PROFILE OF LECTURE MANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONS. PLANETARY ATMOSPHERE FROM REMOTE RAOIOIIETRIC BIOLOGICAL EXPLORATIMI OF MARS. MASERS AND MEASUREMENTS LASERS. PLANETARY ATMOSPHERES. RELATIVITY NASA-TN-0-2940 N65-30733 THEORY. ELEMENT ABUNDANCES AND SOLAR PARTICLES N65-31360 VENUS CLOUD LAYER AND BRIGHTNESS TEMPERATURE FROM RADIOMETRIC MICROWAVE OBSERVATIONS FROM NOCTURNAL RESUICH PROJECT SIDE OF PLANET A66-20112 SPACE SCIENCE PROGRAM OF USA - THEORETICAL ASPECTS. SUMMARY OF LAUNCHINGS FOR 1964. LIST OF RADIOPHYSICS RESEARCH PROJECTS AND AGENCIESS AND 8IBL106RAPHY MULTIDISCIPLINARY STUDIES ON PLANETARY ATMOSPHERES N65-29509 IONOSPHERIC AND RAOIOPHYSICS~PARTICLES AN0 FIELDS. AND PLANETS RESEARCH ACTIVITIES AT HARVARO ASTRONOMICAL NASA-CR-70165 N66-17290 OBSERVATORY FROn 1964 THROUGH 1965 N66-17617 RAMJET ENGINE THEORETICAL FUEL-BASE0 SPECIFIC IMPULSE LIGHT Rot- S0UIQ)INC METAL-NITROGEN SYSTEM FOR RAMJET AND TURBOJET AERONOIIICAL AND RETMROLOGICAL STWIES OF EARTH PROPULSION IN MARTIAN ATMOSPHERE AND OTHER PLANETARY ATMOSPHERES A65-15610 N65-24913

RARE 6AS ROTATIWG SPHERE METHOD FOR DETERMINING TEMPERATURE-ALTITUOE ROTATIONAL. PRECESSIONAL AN0 NUTATIONAL MOTION OF PROFILES OF PLANETARY ATMOSPHERES FROM NUMBER EDDY ENTERING MARS ATMOSPHERE IN VERTICAL AN0 DENSITY PROFILES OF TWO INERT GASES WITH OBLIQUE OIRECTIONS A6530321 0 IFFERENT MOLECULAR NE I6HTS NASA-CR-71862 N66-23682 ROTATION ROTATION OF PLANET MERCURY FROM RAOAR OBSERVATION RAYLEI6H EQUATION EXPLAINED BY SOLAR GRAVITATIONAL TORQUE ON TIDAL PHYSICS OF PLANETARY ATMOSPHERES - VARIATIOW DEFORMATION AN0 EQUATORIAL PLANE ASYMMETRY METHOD USED TO CALCULATE RAYLEIGH SCATTERING NASA-CR-68703 N66- 13573 CROSS SECTIONS OF HELIUM AS WAVELENGTH FUNCTION NASA-CR-64187 N65-31052 S RAYLEIGH SCATTERIN6 SIJIPLIWG DEVICE OUTWARD FLUX AND INTENSITY OF SCATTERED RADIATIW PWEUMATIC SURFACE SANPLING DEVICE FOR US€ IN FOR TOP OF RAYLE.IGH ATMOSPHERE LYING ABOVE SMOOTH SIMULATE0 MARS ENVIRONMENT WATER SURFACE THAT REFLECTS RADIATION ACCORDIWG TO NASA-CR-70937 N66-20080 FRESNEL LAW AIM PAPER 65-664 A65-35711

1-29 SATELLITE SUBJECT INDEX

SATELLITE SCATTERIMG CROSS SECTION PLANETS AN0 SATELLITES IN SOLAR SYSTEM PHYSICS OF PLANETARY ATMOSPHERES - VARIATION NASA-TT-F-77 N65-14673 METHOD USED TO CALCULATE RAYLEIGH SCATTERING CROSS SECTIONS OF HELIUM AS WAVELENGTH FUNCTION OPTICAL DETECTION OF LIGHTNING FROM SATELLITES NASA-CR-64187 N65-31052 NASA-CR-60806 N65-17404 SENSING SATELLITE INSTRUMENTATION INTEGRATION OF TERRESTRIAL AN0 PLANETARY SCIENTIFIC RESEARCH USING INSTRUMENTS IN SPACE ENVIRONMENT SENSING N65-33556 VEHICLES, NOTING DIRECT OBSERVATIONS OF MOON, VENUS, MARS, GLOBAL COMMUNICATIONS* METEOROLOGYI SHADOW GEODETIC AND NAVIGATION SATELLITES, ETC THERMAL EMISSION OBSERVATIONS OF SHADOWS CAST ON A66-23639 JUPITER BY SATELLITES GANYMEDE, EUROPA AN0 IO A65-18223 SATELLITE MEASUREMENT ATMOSPHERIC PRESSURE AND TEMPERATURE BELOW 24 KM SHOCK HEATING USING SATELLITE MEASUREMENTS OF ATMOSPHERIC LIGHT SPECTRAL AND TOTAL RADIATION STUDIES OF BODIES REFRACTION FROM GIVEN STARS 165-34959 TRAVELING AT HYPERSONIC SPEED IN SIMULATED MARTIAN AND VENUSIAN ATMOSPHERES PHOTOMETRIC OBSERVATIONS OF STARS IN OCCULTATION AIAA PAPER 65-116 A65-15008 AND PLANETARY ATMOSPHERIC EXPLORATION FROM ARTIFICIAL SATELLITE IN ORBIT SHOCK LAYER NASA-TT-F-8219 N65-22 579 ANALYSIS OF EPUILI8RIUM SHOCK LAYER RADIATION FOR MARS ATMOSPHERIC ENTRY N65-32433 SATELLITE OBSERVATION SATELLITE AN0 ROCKET OBSERVATIONS LEADING TO NEW EPUILIBRIUM AN0 NONEPUILIBRIUH STAGNATION POINT ASPECTS OF HETEROSPHERE STRUCTURE NOTING HEAT SHOCK LAYER RADIATION IN SIMULATED PLANETARY BALANCE. PHOTODISSOCIATION AN0 GAS DIFFUSION ATMOSPHERES OF VARYING COMPOSITION 165-19485 ~66-21773

VENUS IR LIMB DARKENING OBSERVATIONS BY MARINER SHOCK TUNNEL I1 A65-22098 SHOCK TUBE GAS DYNAMIC CHARTS SUITABLE FOR MARS ATMOSPHERE VENUS IR LIMB DARKENING OBSERVATIONS BY RAD-TM-65-23 N65-25127 MARINER I1 1166-21110 ATMOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNATION MARINER IV OBSERVATIONS OF MARS SURFACE, SHOWING POINT CONVECTIVE HEAT TRANSFER, USING ARC-HEATED NO DETECTABLE MAGNETIC FIELD OR RADIATION BELTS, SHOCK TUBE SIMULATING FLIGHT VELOCITIES UP TO SUGGEST IRON ON SURFACE OXIDIZED FROM 34,000 FPS ~66-17a9i PHOTOOISSOClATION OF WATER VAPOR AIAA PAPER 66-29 A66-2 1211 SHOCK WAVE SCIENTIFIC RESEARCH USING INSTRUMENTS IN SPACE NORMAL SHOCK WAVE AND STAGNATION POINT SOLUTIONS VEHICLES, NOTING DIRECT OBSERVATIONS OF MOON. FOR FOUR VENUSIAN ATMOSPHERIC AN0 CHEMICAL VENUS, WARS. GLOBAL COMMUNICATIONS* METEOROLOGY, MODELS GEODETIC AND NAVIGATION SATELLITES. ETC R64S065 N65- 135 19 A66-23639 MIXTURES OF NITROGEN AN0 CARBON OIOXIOE GASES SATELLITE ORBIT HEATED BY SHOCK WAVE REFLECTION TO HIGH LONG LIFETIME ORBITS ABOUT MARS AFFECTED BY TEMPERATURE AT NORMAL DENSITY - VENUS ATMOSPHERIC DRAG. SOLAR GRAVITATIONAL ATMOSPHERE S IMUL AT ION PERTURBATIONS, PLANETARY OBLATENESS AN0 OTHER NASA-CR-51668 N65-15370 PERTURBAT IONS AIAA PAPER 66-35 A66-18987 SHOCK YAVE PROPAGATION EXPLOSION IN RAREFIED ATMOSPHERES WHERE EXPLOSIVE SATELLITE PHOTOGRAPHY PRODUCT ATOM MEAN FREE PATH IS LONGER THAN OCEANOGRAPHIC AN0 RELATED OBSERVATIONS FROM EXPANDING MATERIAL DIMENSION, ILLUSTRATING METHOD SATELLITE PHOTOGRAPHY N65-30357 WITH CHEMICAL EXPLOSION AT 150 KM ALTITUDE A65-24615 SATURN /PLANET/ SIMILARITY OF COLOR PHENOMENA ON SATURN AN0 SILICON COMPOUND JUPITER LEADS TO SPECULATION OF SOLAR INFLUENCE POSSIBLE ALTERNATIVE CHEMICAL ELEMENTS AN0 A65-29288 COMPOUNDS SUITABLE FOR PROLONGEO BIOMOLECULAR EVOLUTION AN0 CHEMICAL SELECTION ON NONTERRESTRIAL JUPITER AN0 SATURN INTERIOR TEMPERATURES FROM TYPE PLANET A65-27098 EXAMINATION OF ATMOSPHERIC COMPOSITION AN0 GRAVITATIONAL MULTI POLE MOMENT A6 5 - 33 30 2 SIMULATION MIXTURES OF NITROGEN AN0 CARBON DIOXIDE GASES I R SPECTRA OF SATURN RING AN0 GALILEAN HEATED BY SHOCK WAVE REFLECTION TO HIGH SATELLITES OF JUPITER SHOW ABSENCE OF STRONG TEMPERATURE AT NORMAL DENSITY - VENUS ABSORPTION AT 8873 ANGSTROMS. INDICATING NEW UPPER ATMOSPHERE SIMULATION LIMIT OF WETHANE ABUNDANCE 165-35585 NASA-CR-51668 N65-15370

RADIO EMISSION OF SATURN ON WAVELENGTH OF 8 MM PLANETARY ATMOSPHERIC SIMULATION IN SUPERSONIC COMPARED WITH VALUES OBTAINED AT OTHER WAVELENGTHS WIND TUNNELS WITH CARBON OIOXIOE ADDED TO DRIED A65-35841 AIR WORKING FLUID NASA-CR-68792 N66- 13555 METEOR PHENOMENA, UPPER ATMOSPHERE WINO FIELDS FROM METEOR TRAILS, AN0 PHOTOMETRY OF A AN0 B SOFT LANDING RINGS OF SATURN INSTRUMENTATION FOR ANALYSIS OF MARS ATMOSPHERE AFCRL-65-33 N65-36000 AFTER SOFT LANDING NASA-CR-62870 N65-24307 ATMOSPHERIC CIRCULATION AROUND PLANETS OF JUPITER AND SATURN N66-14332 SOLAR ACTIVITY RADIO AN0 RADAR ASTRONOMICAL STUDIES ON LUNAR AND STRUCTURE, COMPOSITION^ ATMOSPHERE, AND SCIENTIFIC PLANETARY IONOSPHERES AND ATMOSPHERES, AND SOLAR OBJECTIVE SURVEYS FOR SATURN* URANUS, ACTIVITY NEPTUNE, AND PLUTO NASA-CR-71090 N66-19528 NASA-CR-70328 N66- 17090

1-30 SUBJECT 1- SPACE EXPLORATION

SOLAR ENERGY SPACE ENVIRONMENT - DATA ON ELECTROMA6NETIC AND MARTIAN ATMOSPHERIC HEATING FROM SOLAR RADIATION PARTICULATE RADIATION. METEOROID FLUX. AN0 ABSORPTION IN UV AN0 VISIBLE BY OXYGEN AND OZONE STRUCTURE. AND COMPOSITION OF PLANETARY AN0 IN NEAR IR BY CARBON DIOXIDE. NOTIN6 VERTICAL ~TMOSPHERE - Sam SYSTEM SPACE ENVIRONMENT OISTRIBUTION OF GASES AN0 ABSORPTION NASA-CR-294 N65-34244 A65-23521 EXTRATERRESTRIAL LIFE IN SOLAR SYSTEM, DISCUSSING TEMPERATURE. DENSITY AN0 GRAVITATIONAL ESCAPE ON EQUIPMENT FOR MARS EXPLORATION. NOTIWG WLLIVER MARS. MERCURY. JUPITER AND VENUS ATMOSPHERES PROGRAM. MULTIVATOR AUTOMATIC BIOCHEMICAL TESTING A66-15759 APPARATUS AND TV MICROSCOPE A6623794

SOLAR GRAVITATIONAL EFFECT SOLAU YIND ROTATION OF PLANET MERCURY FROM RADAR OBSERVATION SOLAR WINO PROTON VELOCITY, TEMPERATURE AND EXPLAINED BY SOLAR GRAVITATIONAL TORQUE ON TIDAL DENSITY OETERMINEO WHEN MARINER I1 WAS NEAR DEFORMATION AN0 EQUATORIAL PLANE ASYMMETRY VEWS A65-22598 NASA-CR-68703 N66-1357 3 PLANETARY ATMOSPHERES ORICIN DUE TO OUTGASSING OR SOLAR PROBE CAPTURE FROM PRIMITIVE SOLAR NEBULA OR SOLAR YIND DEEP SPACE. SOLAR PROBE. AN0 OUT-OFECLIPTIC AN0 ATMOSPHERIC LOSSES DUE TO REVERSE PROCESSES TRAJECTORIES UTILIZING LARGE PLANETARY A65-32627 PERT UR BAT ION S NASA-CR-69222 N66-15224 INTERACTION OF SOLAR WINO WITH PLANETS - PROPERTIES OF INTERPLANETARY MEDIUM AND SOLAR PROTON THEORETICAL MODELS OF SOLAR WIND SOLAR WIND PROTON VELOClTYt TEMPERATURE AN0 N66-14334 DENSITY DETERMINED WHEN MARINER I1 WAS NEAR VENUS A65-22598 SOLID ?ROPELLUIT ICWITION I6NITION TEMPERATURES OF POWDERED METALS IN SOLAR RADIATION SIMULATED ATMOSPHERES OF VENUS AND MARS SWEST SOLAR IONIZIN6 RADIATION EFFECT ON JUPITER UPPER POTENTIAL CHEMICAL ENERGY SOURCES ATMOSPHERE OISSOCIATION INOICATEO BY MICROWAVE A6622456 SPECTRUM A65-17213 S0UY)INC ROCKET ABSOLUTE INTENSITY MEASUREMENTS IN EXTREME UV AND PLANETARY AN0 EARTH ATMOSPHERIC COMPOSITION* SOFT X-RAY REGIONS OF SOLAR SPECTRUM TEMPERATURE. AN0 ACTIVITY DATA FROM SATELLITE A65-32654 &NO SOUNDING ROCKETS NASA-SP-96 N66-19525 SOLAR SPACE ENVIRONMENT. AND METEOROLWICAL AN0 COMMUNICATIONS SATELLITES - CONFEREKE SWNOING ROCKET FLIGHT TO MEASURE COSMIC RADIATION PROCEEDINGS INTENSITY AN0 STUDIES OF MARTIAN ATMOSPHERE AND NASA-CR-60132 N65-15466 IONOSPHERE USA-CR-74173 Nb6-23713 CALCULATIONS OF MIODAY DAYGLOW INTENSITIES ARISING FROM FLUORESCENCE OF SOLAR IONIZING SPACE CAPSULE RADIATION ORBITER INJECTED STERILIZED BALLISTIC SKIPOUT NASA-CR-64424 N65-31047 CAPSULE FOR IN FLIGHT MARTIAN STRATOSPHERE MEASUREMENTS. USING MOMABLATIVE HEAT SHIELD AND LECTURE MANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONSI OUTSIDE ATMOSPHERIC PROPULSION MANEUVERS BIOLOGICAL EXPLORATION OF MARS. MASERS AN0 AIAA PAPER 65-23 A65-15944 LASERS, PLANETARY ATMOSPHERES. RELATIVITY THEORY+ ELEMENT ABUNOANCEt AND SOLAR PARTICLES DESIGN. PERFORMANCE. AN0 ENVIRONMENT PARAMETERS N65-31360 FOR MARS AND VENUS SPACE CAPSULES NASA-CR-53674 W65-16498 HOPF ANALYTICAL SOLUTION FOR VALUES OF RATIO OF GRAY ABSORPTION COEFFICIENTS FOR INSOLATIN6 AND SPACE HlvIRDwllHn ESCAPING RADIATION /GREENHOUSE PARAMETER/ ASSUME0 SOLAR SPACE ENVIRONMENT^ AND METEOROLOGICAL AND CONSTANT AT ALL DEPTHS. PRESENTING TEMPERATURE COMMUNICATIONS SATELLITES - CONFERENCE OISTRIBUTION GRAPHS A66-21204 PROCEEDINGS NAS A-UI-60 132 N65-15468 ELECTROMA6NETIC WAVE SCATTERING IN HOMOGENEOUS PLANE-PARALLEL ATMOSPHERES - SOLAR RADIATION SPACE ENVIRONIIENTAL REQUIREMENTS OF FUTURE TRANSFER IN PLANETARY ATMOSPHERE MISSION PLANNING RM-4646-PR N66-19416 AFSC-TOR-64-2 N65-15938

SOLAR RADIO HAVE BlBLI06RAPHY OF WCUWENTS ON LUNAR. PLANETARY. HOWGRAPH ON RID10 EMISSION OF SUN AND PLANETS AND SPACE ENVIRONMENTS IN RELATION TO FLIGHT A65-16909 MECHANICS AN0 AERODYNAMICS OF SPACE TRAVEL NASA-CR-60469 N65-16086 SOLAR SYSTEM CHEMICAL TRANSFORMATIONS IN OUTER SPACE OISCUSSIK SPACE ENVIRONMmT - DATA ON ELECTROMAGNETIC AND OCCURRENCE. STATE AN0 BEHAVIOR OF ELEMENTS ON PARTICULATE RADIATION. METEOR010 FLUX. AN0 PLANETS. MOON AN0 METEORITES A65-1698 1 STRUCTURE. AN0 COMPOSITION OF PLANETARY ATMOSPHERE - SOLAR SYSTEM SPACE ENVIRONMENT BOOK ON SOLAR SYSTEM ASTRONOMY AND SPACE PHYSICS NASA-CR-294 N65-34244 INCLUDING CELESTIAL MECHANICS. INTERPLANETARY GAS PHYSICS. METEORITES AND PLANETARY ATMOSPHERES BIOLOGICAL PROBLEMS IN SPACE-TEXTBOOK A65-17422 1166-60636

BIBLIOGRAPHY CONTAINING 275 ENTRIES ON EXPECTEO THERMODYNAMIC EQUILIBRIUM COMPOSITION ASTRONOMICAL SUBJECTS FROM ELEVEN U-S- BRITISH CALCULATE0 FOR ATMOSPHERES OF EARTH. VENUSs AND SOVIET TECHNICAL PUBLICATIONS PUBLISHED IN MARS. AN0 JUPITER 1964 A65-29113 NASA-CR-69965 N66-16463

BItKIOGRAPHY OF 1964 LITERATURE ON SOLAR SYSTEM SPACE ExPLoRITI(*I SCIENCE A65-35373 SPACE EXPLORATION - SPACE AROUND EARTH. ATMOSPHERIC CIRCULATION AN0 WEATHER CONOITIONSv PLANETS AN0 SATELLITES IN SOLAR SYSTEM LUNAR PHOTOGRAPHYr AN0 PLANETARY STUDIES NASA-11-F-77 N65-14613 NASA-EP-25 N65-32514

1-31 SPACE MISSION SUBJECT INDEX

SCIENTIFIC RESEARCH USING INSTRUMENTS IN SPACE SPACE SCIENCES BIBLIOGRAPHY WITH ABSTRACTS - VEHICLES, NOTING DIRECT OBSERVATIONS OF MOON* ASTRONOMY, METEOROLOGY. OCEANOGRAPHY. UPPER VENUS, MARS, GLOBAL COMMUNICATIONS, METEOROLOGY, ATMOSPHERE. GEOPHYSICSI SPACE GEODETIC AND NAVIGATION SATELLITES, ETC JPRS-35095 N66-23025 A66-23639 SPACE TRAJECTORY PROGRAM SPACE TRAVEL AND EXPLORATION, BIOLOGICAL AND DEEP SPACE. SOLAR PROBE, AND OUT-OF-ECLIPTIC TECHNICAL DIFFICULTIES, RADIATION, METEOR IMPACT, TRAJECTORIES UTILIZING LARGE PLANETARY VEHICLE STERILIZATION. ETC A66-23640 PERTURBATIONS NASA-CR-69222 N66-15224 SPACE MISSION PROPULSION ORIENTED STUDY OF MISSION MODES FOR SPACE VEHICLE MANNED MARS LANDING SIMULATION OF HEAT TRANSFER ENVIRONMENTS OF SPACE NASA-TM-X-53265 N65-28960 VEHICLE ENTERING PLANETARY ATMOSPHERE WITH SUPERDRBXTAL VELOCITY UNMANNED SPACE MISSION TO DETERMINE MARTIAN R64SD73 N65-15600 ENVIRONMENTAL FACTORS INFLUENCING OESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - SPACECRAFT COMMUNICATIONS SYSTEM UNMANNED SPACECRAFT DESIGN UARS ATMOSPHERE AND IONOSPHERE MEASUREMENTS USING NASA-CR-60lk2 N66- 15540 2300-MC TELEMETRY SIGNAL FROM MARINER IV SPACECRAFT OCCULTATION EXPERIMENTS UNMANNED SPACE MISSION TO DETERMINE MARTIAN A65-26719 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - SPACECRAFT OESIGN MISSION EXPERIMENT REQUIREMENTS MARS ATMOSPHERC DEFINITION IMPORTANT IN ADVANCED NASA-CR-60741 N66-15541 LANDING VEHICLE DESIGN WITH INCREASED PAYLOAD CAPABILITY AND REDUCED COMPLEXITY UNMANNED SPACE MISSION TO DETERMINE MARTIAN AIAA PAPER 65-22 A65-14563 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - ENTRY VEHICLE DESIGN FOR PLANETARY EXPLORATION SUMMARY REPORT USING NDNSURVIVING NEEDLE-NOSED PROBE FOR DATA NASA-CR-60743 N66-15542 COLLECTION ON MARS ATMOSPHERE COMPOSITIONt PRESSURE AND DENSITY UNMANNED SPACE MISSION TO DETERMINE MARTIAN AIAA PAPER 65-493 A65-32321 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - SYSTEM DESIGN OF AUTOMATED LABORATORY AND MISSION SENSITIVITY ANALYSIS ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN NASA-CR-68740 N66-15543 EXPLORATION A65-35112

SYSTEMS OESIGN FOR UNMANNED SPACE MISSION TO SPACECRAFT, MISSIONS AN0 INSTRUMENTATION FOR SPACE EVALUATE MARS ENVIRONMENT PROBES AN0 INTERPLANETARY EXPLORATION NASA-CR-69997 N66-16248 A65-82064

SPACE PROBE INSTRUMENTATION AND DESIGN OF SCIENTIFIC PAYLOAD SPHERICAL SEMIPASSIVE PROBE FOR DENSITY/ALTITUDE CARRIED BY MARINER IV A66-2 018 1 AND PRESSURE/ALTITUDE PROFILE OF PLANETARY ATMOSPHERES, NOTABLY MARS AND VENUS MARS ATMOSPHERE DEFINITION IMPORTANT IN ADVANCED A65-19520 LANDING VEHICLE DESIGN WITH INCREASED PAYLOAD CAPABILITY AND REDUCED COMPLEXITY SPACE SCIENCE AIAA PAPER 65-22 A66-24697 CHEMICAL TRANSFORMATIONS IN OUTER SPACE DISCUSSING OCCURRENCE, STATE AND BEHAVIOR OF ELEMENTS ON UNMANNED SPACE MISSION TO DETERMINE MARTIAN PLANETS, MOON AND METEORITES A65-16981 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - BOOK ON SOLAR SYSTEM ASTRONOMY AND SPACE PHYSICS UNMANNED SPACECRAFT DESIGN N66-15540 INCLUDING CELESTIAL MECHANICS, INTERPLANETARY GAS NASA-CR-68742 PHYSICS, METEORITES AN0 PLANETARY ATMOSPHERES 165-17422 UNMANNED SPACE MISSION TO DETERMINE MARTIAN ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF LECTURES FROM TRW SPACE TECHNOLOGY SYSTEMS FOR MANNED SPACE MISSION TO MARS - LABORATORIES A65-32620 MISSION EXPERIMENT REQUIREMENTS NASA-CR-68741 N66-15541 BIBLIOGRAPHY OF 1964 LITERATURE ON SOLAR SYSTEM SCIENCE A65-35373 UNMANNED SPACE MISSION TO DETERMINE MARTIAN ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF UNITED STATES SPACE SCIENCE PROGRAM SYSTEMS FOR MANNED SPACE MISSION TO MARS - N65-24908 SUMMARY REPORT NASA-CR-68743 N66-15542 AERONOMICAL AND METEOROLOGICAL STUDIES OF EARTH AND OTHER PLANETARY ATMOSPHERES UNMANNED SPACE UISSION TO DETERMINE MARTIAN N65-24913 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - UNITED STATES SPACE SCIENCE REPORTS - CONDENSED MISSION SENSITIVITY ANALYSIS CDMP ILATIDN N65-28716 NASA-CR-68740 N66-15543

PLANETARY ATMOSPHERES, LUNAR STRUCTURES, PARTICLE SPACECRAFT IWSTRUMENTATION ENERGY SPECTRA, EXOBIOLOGY. SPACE PHYSIOLOGY, INSTRUMENTATION AN0 DESIGN OF SCIENTIFIC PAYLOAD AND ENGINEERING SCIENCES - SPACE SCIENCES CARRIED BY MARINER IV A66-20181 NASA-CR-59038 N65-29433 SPACECRAFT LANDING RECENT SPACE RESEARCH IN PHYSICAL SCIENCES - ATMOSPHERE POSTULATION BASE0 ON KOZYREV LITERATURE SUMMARY AND DISCUSSION OBSERVATION OF HYDROGEN. ENTRY TRAJECTORY ANALYSIS NASA-TM-X-51903 N65-29458 AN0 FEASIBILITY OF ATMOSPHERIC BRAKING FOR LANDING PAYLOAD ON MERCURY SPACE SCIENCE PROGRAM OF USA - THEORETICAL AIAA PAPER 65-494 A65-29684 ASPECTS, SUMMARY OF LAUNCHINGS FOR 1964. LIST OF RESEARCH PROJECTS AND AGENCIES, AND BIBLIOGRAPHY EMlSSION AND ABSORPTION OF RADIANT ENERGY IN MODEL N65-29509 MARTIAN ATMOSPHERE COMPOSED OF 15 PERCENT CARBON DIOXIDE AND 85 PERCENT NITROGEN BY VOLUME

1-32 SUBJECT IWEX SUIFACE WESSUE

A66-15777 WISA-CR-57740 ~65-zors8

SPACECRAFT RECOVERY SPHERE SPACE VEHICLE RECOVERY TRAJECTORIES EXTENDING FROM TRANSLATIONAL AN0 ROTATIONAL MOTION OF SPHERICAL GIVEN INITIAL ORBIT TO ATMOSPHERE TOP BODY ENTERING MARS ATMOSPHERE - REENTRY PHYSICS A65-19314 MASA-CR-69252 N66-15338

SPECIFIC IllPULSE SPHRICAL HMMONICS THEORETICAL FUEL-BASED SPECIFIC IMPULSE LIGHT BEHAVIOR OF PLANETARY WAVES IN ATMOSPHERE MODEL METAL-NITROGEN SYSTEM FOR RAMJET AND TURBOJET BASED ON SPHERICAL HARMONICS PROPULSION IN MARTIAN ATMOSPHERE AFCRL-65-488 N66-10836 A65-15610 STA6WlTIOW WIWT SPECTRAL ANALYSIS NORMAL SHOCK WAVE AND STAGNATION POINT SOLUTIONS SPECTRAL AND TOTAL RADIATION STUDIES OF BODIES FOR FOUR VENUSIAN ATMOSPHERIC AN0 CHEMICAL TRAVELING AT HYPERSONIC SPEED IN SIMULATED MODELS MARTIAN AN0 VENUSIAN ATMOSPHERES R64S065 1165-13519 AIAA PAPER 65-116 A65-15008 ATMOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNATION CALIBRATION OF MARTIAN SPECTRA USING LABORATORY POINT COUVECTIVE HEAT TRANSFER, USING ARC-HEATED SPECTRA OF PURE CARBON OIOXIOE AND IN COMBINATION SHOCK TUBE SIMULATING FLIGHT VELOCITIES UP TO WITH NITROGEN AN0 ARGON A65-18477 34.000 FPS AIAA PAPER 66-29 ~66-17891 METHANE AND AMMONIA LABORATORY SPECTRA COMPAREO WITH SPECTRA OF JUPITER. INOICATING CAUSES OF STELLAR ATMOSPHERE UNIDENTIFIED ABSORPTIONS A65-35022 POSSIBLE ATMOSPHERE DETECTION ON J-I1 AND J-I11 SATELLITES REVEALED BY EXCESS BRIGHTNESS ON SPECTRAL BAND ECLIPSE REAPPEARANCE A66-21202 INFRARED SPECTROSCOPY STMIES TO DETERMINE ABSORPTION BY CARBON DIOXIDE BETWEEN 8.000 AN0 STELLAR EvauTmu 10s000/CM IN 1 TO 1.25 MICRON REGION CURRENT PICTURE OF ORIGIN AND DEVELOPMENT OF U-3200 N66-22465 PLANETARY ATMOSPHERES. BEGINNING WITH THEORY OF STELLAR EVOLUTION A6526914 SPECTRAL LINE SPECTRAL OISTRIBUTION OF ALBEDO AN0 LUMINANCE AT STELLAR OCCULTATIOW CENTER OF DISK FOR DIFFUSING AND ABSORBING PHOTOMETRIC OBSERVATIONS OF STARS IN OCCULTATION PLANETARY ATMOSPHERE A66-17247 AN0 PLANETARY ATMOSPHERIC EXPLORATION FROM ARTIFICIAL SATELLITE IN ORBIT SPECTRAL REFLECTAWE NASA-TT-F-8219 N65-22579 SPECTRAL REFLECTING POWER CURVE FOR MARTIAN DISK CENTER COMPARED WITH TERRESTRIAL EPUIVALENT STRATOSCOPE I1 TELESCOPE A66-19333 BALLOON ELEVATED / STRATOSCOPE II/ REMOTE CONTRMLEO TELESCOPE FOR ASTRONOMICAL OBSERVATION SPECTROSRAPHY OF PLANETS. NEBULAE. ETCs FROM UPPER ATMOSPHERE INTENSITY MEASUREMENTS OF METHANE ABSORPTION IN A65-28940 VISIBLE REGION OF JUPITERS SPECTRUM NASA-TT-F-10062 N66-23610 STRESS ANMYSIS PAPERS PRESENTED AT SCIENTIFIC BALLOON SPECTROMETER SWPOSIUM ON BALLOON DESIGN, MATERIALS. STRESS TELESCOPE DESIGN FOR INTERFEROMETER SPECTROMETER STUDIES. INSTRUMENTATION^ METEOROLOGY. LOCATIWG FOR PLANETARY ATMOSPHERE EXPLORATION SYSTEM. AN0 PLANETARY EXPLORATION APPLICATIONS N66-14107 AFCRL-65-486 1165-34804

SPECTROPHOTOMETRY SUBSOWIC SPEED SPECTROPHOTOMETRIC OBSERVATIONS OF MARS LOW SUBSONIC DYNAMIC STABILITY DATA FOR EVALUATION N65-18512 OF BALLISTIC DECELERATION VEHICLE ENTERING MARS ATMOSPHERE SPECTRAL REFLECTING POWER CURVE FOR MARTIIN DISK NASA-CR-63117 W5-24985 CENTER COMPARED WITH TERRESTRIAL EPUIVALENT A6619333 SULFUR CrnWWID ABUNOANCE AN0 STABILITY OF MAJOR SULFUR COMPOUNDS SPECTROSCOPY IN LOVER ATMOSPHERE OF VENUS CALCULATED. ASSUMING MERCURIAN ATMOSPHERE FROM HIGH DISPERSION SPECTRAL EWILIBRIUM BETYEEN ATMOSPHERIC GASES AND MINERAL STUDY OF ABUNOANCE OF CARBON DIOXIDE. OXYGEN AN0 PHASES A6619262 WATER A65-25226 SUll SURFACE PRESSURE AN0 CARBON DIOXIDE CONTENT OF RADIO AN0 RADAR ASTRONOMY STUDIES OF LUNAR AN0 MARTIAN ATMOSPHERE* COMPARING POLARIMETRIC. PLANETARY ATMOSPHERES AND SURFACES. AN0 RADAR PHOTOMETRIC AND SPECTROSCOPIC METHODS STUDIES OF SUN AN0 INTERPLANETARY MEDIUM A65-26212 NASA-CR-57184 N65-18944

SPECTROSCOPIC DETECTION OF WATER VAPOR IN SUrrICHT ATMOSPHERES OF VENUS AN0 MARS USING TELESCOPE ATMOSPHERIC SCATTERING AN0 REFRACTION OF SUNLIGHT CARRIED BY BALLOON N65-34835 INTO PLANETARY UMBRA P-3282 N66-20124 SPECTRUM PHOTOGRAPHIC SPECTRA OF PLANETARY ATMOSPHERE GASES SUPEUSONIC MIND TVHlEL OF MARS AN0 JUPITER PLANETARY ATMOSPHERIC SIMULATION IN SUPERSONIC AD-608352 ~65-16776 WINO TUNNELS WITH CARBON OIOXIOE AOOEO TO ORIED AIR WORKING FLUID SPECULAR REFLECTION NASA-CR-68792 N66-13555 WTWARO FLUX AND INTENSITY OF SCATTERED RADIATION FOR TOP OF RAYLEIGH ATMOSPHERE LYING ABOVE SMOOTH SURFACE WATER SURFACE THAT REFLECTS RADIATION ACCORDING TO MARTIAN ATMOSPHERE AN0 SURFACE CHARACTERISTICS - FRESNEL LAW ASTROPHYSICS AIM PAPER 65-664 A65-35711 NISA-CR-68136 ~66-12974

GRWNO SPECULAR REFLECTION MOOIFICATIOM OF SURFACE PRESSURE LIGHT SCATTERING FROM PLANETARY ATMOSPHERE TOP SURFACE PRESSURE AN0 CARBON DIOXIDE COWTENT OF

1-33 SURFACE TEHPERATURE SUBJECT INDEX

- HARTIAN ATHOSPHERE, COHPARING POLARIHETRIC, USA-CR-63278 N65-26075 PHDTOHETRIC AN0 SPECTROSCOPIC HETHODS A65-26212 TEMERATUIIE DISTRIBUTION CONVECTIVE-RADIATIVE EQUILIBRIUH HODEL FOR DISCREPANCY IN PHOTOHETRIC AND VISIBLE COHPUTING TEMPERATURE PROFILE - VERTICAL POLARIHETRIC DETERHINATIONS OF HARS SURFACE TEHPERATURE DISTRIBUTION IN HARTIAN ATHOSPHERE PRESSURE ATTRIBUTED TO AEROSOL PARTICLES IN NASA-CR-65049 ~65-2r 955 HARTIAN ATHOSPHERE A65-26945 HDPF ANALYTICAL SOLUTION FOR VALUES OF RATIO OF SPECTRUH, COHPOSITION AND SURFACE PRESSURE, CARBON 6RAY ABSORPTION COEFFICIENTS FOR INSOLATING AND DIOXIDE ABUNDANCE, NITROGEN DIOXIDE TESTS, AN0 ESCAPING RADIATION /GREENHOUSE PARAHETERI ASSUHEO STRUCTURE OF ATHOSPHERE ON HARS CONSTANT AT ALL DEPTHS, PRESENTING TEMPERATURE NASA-CR-60264 N65-15223 DISTRIBUTION GRAPHS A66-21204

PLANETARY ATHDSPHERE COHPOSITION. TEHPERATURE. AND POLARIZATION AND BRIGHTNESS TEHPERATURE PRESSURE bF HARS, VENUS, AND JUPITER DISTRIBUTION HEASUREHENTS OF VENUS IN 10-6 CH NASA-TM-X-56223 N65-20799 WAVELENGTH ST-RA-LPS-10334 N66-11138 RECENT DETERHINATIONS OF COHPOSITION AND SURFACE PRESSURE OF HARS ATHOSPHERE EARTH- HARS COHPARISON OF VERTICAL TEHPERATURE NASA-CR-298 N65-33835 DISTRIBUTION AND HEAT BALANCE IN ATHOSPHERE NASA-CR-68992 N66-14280 CARBON DIOXIDE ABSORPTION BANDS IN HARS ATHOSPHERE, TRANSHISSIONI FUNCTION OF CARBON EQUILIBRIUH TEHPERATURE DISTRIBUTION, THERHAL DIOXIDE AHOUNT AND EFFECTIVE SURFACE PRESSURE EHISSION, AND LIHB FUNCTION COHPUTEO FOR VENUS AIAA PAPER 66-147 A66- 19012 CLOUD COVER HODEL NASA-TH-X-55392 N66-17231 SURFACE TEMPERATURE SURFACE TEHPERATURE DISTRIBUTION OF HERCURY BASEO TEHPERATURE DISTRIBUTION. COHPOSITION, AND ON HEASUREHENTS OF HEAN DISK TEHPERATURE OVER YIDE IONIZATION OF HARS ATHOSPHERE N66-19930 RANGE OF PHASE ANGLES A65-22205 TEMPERATURE EFFECT THEORY OF DIURNAL VARIATION OF HARTIAN SURFACE TEHPERATURE. ‘DENSITY AN0 GRAVITATIONAL ESCAPE ON TEHPERATURE - GROUND AN0 ATHOSPHERE OF HARS HARS, HERCURYt JUPITER AND VENUS ATHOSPHERES NASA-CR-63278 ~65-26075 A66- 15159

SURFACE TEHPERATURE CALCULATIONS FOR VENUS BASEO TEHPERATURE GRADIENT ON TWO GREENHOUSE ATHOSPHERIC HODEL COHPARISONS HARS ATHOSPHERIC HOOELS BASEO ON HARINER IV NASA-TH-X-57375 ~66-23674 OCCULTATION EXPERIHENT NASA-CR-74152 N66-23493 SURVIVAL SURVIVAL AND GROYTH OF TERRESTRIAL HICROORGANISHS TEMPERATURE MEASUREMENT IN AHHONIA-RICH ATHOSPHERES SUPPORTING POSSIBILITY BRIGHTNESS TEHPERATURE HEASUREHENTS OF HARS AT OF ORIGIN AND EXISTENCE OF LIFE ON JUPITER 3.15 CH FROH FEBRUARY TO JUNE 1965 A65-81287 A6618788

SYNCHROTRON RADIATION POLARIZATION AND BRIGHTNESS TEHPERATURE IO EFFECT ON SYNCHROTRON EMISSION GENERATED WITHIN DISTRIBUTION HEASUREHENTS OF VENUS IN 10.6 CH RADIATION BELTS IN JUPITER ATHOSPHERE YAVELENGTH A65-21015 ST-RA-LPS-10334 N66-11138

SYSTEHS DESIGN TEMPERATURE PROFILE SYSTEH DESIGN OF AUTOHATED LABORATORY AN0 CONVECTIVE-RADIATIVE EQUILIBRIUH HOOEL FOR ASSOCIATE0 ENTRY VEHICLE FOR UNHANNEO HARTIAN COHPUTING TEHPERATURE PROFILE - VERTICAL EXPLORATION A65-35112 TEHPERATURE DISTRIBUTION IN HARTIAN ATHOSPHERE NASA-CR-65049 ~65-27955 VOYAGER SYSTEH DESIGN STUDY - ENTRY LANDER, AN0 ORBITER SYSTEH FOR ENTRY INTO VENUS OR HARS HETHOOS FOR OBTAINING TEHPERATURE PROFILE OF ATHOSPHER ES PLANETARY ATHOSPHERE FROH REHOTE RADIOHETRIC NASA-CR-51839 N66-13403 HEASUREHENT S NASA-TN-0-2940 N65-30133 VOYAGER SUBSYSTEH DESIGN STUDY - GUIDANCE AN0 CONTROL, PROPULSION, AN0 POWER SUPPLY STUDIES HETHOO FOR DETERHINING TEHPERATURE-ALTITUDE FOR ENTRY IN HARS OR VENUS ATHOSPHERES PROFILES OF PLANETARY ATHOSPHERES FROH NUHBER NASA-CR-5 1831 N66-13407 DENSITY PROFILES OF TWO INERT GASES WITH DIFFERENT HOLECULAR WEIGHTS SYSTEHS DESIGN FOR UNHANNED SPACE HISSION TO NASA-CR-7 1862 N66-23602 EVALUATE HARS ENVIRDNHENT NASA-CR-69997 N66-16248 TEST PR06RU SIHULATED HARTIAN ENTRY CONOITIONS IN EARTH TEST PRDGRAH SHOYING REQUIREHENTS FOR LAUNCH VEHICLE, T TRACKING, COST AND SCHEDULE TECTONIC MOVEMENT AIAA PAPER 65-219 SURFACE DISTURBANCES AS POSSIBLE CAUSE OF TECTONIC HOVEHENT IN JUPITER ATHOSPHERE - ASTRONOHY THERMAL EMISSION 1-439-R N66-10590 THERHAL EHISSION OBSERVATIONS OF SHADOWS CAST ON JUPITER BY SATELLITES GANYHEOE, EUROPA AN0 IO TELESCOPE A65-18223 SPECTROSCOPIC DETECTION OF YATER VAPOR IN ATHOSPHERES OF VENUS AN0 HARS USING TELESCOPE OPTICAL THICKNESS OF JUPITER ISOTHERHAL CARRIED BY BALLOON N65-34835 ATHOSPHERE ASSUHING IT CONSISTS OF HYDROGEN. HETHANE AN0 AHHONIA A65-30231 TELESCOPE DESIGN FOR INTERFEROHETER SPECTROHETER FOR PLANETARY ATHOSPHERE EXPLORATION THERHAL EHISSION HAPS OF JUPITER, DISCUSSING ~66-14107 SOURCE OF NOISE FROH TRACKING ERRORS AND PHOTOHETRIC ERRORS ~65-31279 TEHPEMTURE DIFFERENCE THEORY OF DIURNAL VARIATION OF HARTIAN SURFACE HARS SURFACE AND ATHOSPHERE CHARACTERISTICS FROH TEHPERATURE - GROUND AN0 ATHOSPHERE OF HARS THERHAL EHISSION SPECTRUH HEASUREHENT BY

1-34 SUBJECT INDEX

INFRARED INTERFEROMETER ON PLANETARY FLYBY TyILIulT SPACECRAFT PLANETARY ATMOSPHERE OBSERVATIONS FROM SPACECRAFT NASA-TM-X-55070 W5-32 114 IN TWILIGHT CMlDlTIONS A6531247

EauILI8Riw TEMPERATURE DISTRIBUTION. THERMAL TYO-WDV PmMM EMISSION. AND LIMB FUNCTION COMPUTED FOR VENUS HYPERSONIC AERM)YNMICS THROUGH PLANETARY CLOUD COVER MODEL ATMOSPHERES OES~RIBED BY TWO-BODY PROBLEM IN NASA-TM-X-55392 1166-17231 CELESTIAL MECHMICS A6S-23918

THERMAL ENVIRONMENT PLANETARY RADIATION AND ALBEDO EFFECTS ON THERMAL U BALANCE OF SPACECRAFT ORBIT1116 MARS AND VENUS ULTMVIUET REFLECTION NASA-CR-67813 W6-10684 U V REFLECTIVITY OF MARS ANALYZED FRDW SPECTROGRAMS DBTAINEO ON AERDBEE ROCKET THERMAL RADIO tillISSION A65-35583 VENUS ATMOSPHERE MODEL OF COLD ATMOSPHERE SHORT WAVE ABSORPTION EFFECT ON LOW BRIGHTNESS ULTMVI MET SPECTILOIIIOTO)IElRY TEMPERATURE OF RADIO EMISSIONS ABSOLUTE INTENSITY MEASUIHIENTS IN EXTREME UV AND NASA-TT-F-9663 M5-21005 YYT X-RAY REGIONS OF SOLAR SPECTRUM A65-32654 RADIO NOISE EMISSION FROM VENUS SURFACE EXPLAINED IN TERMS OF GLOW DISCHARGE A6617174 ULTRAVIOLET SPEtTROSCWY TELESCOPIC OBSERVATIONS OF VENUS INDICATE FOUR- RAOIO ASTRONOMY - PASSIVE RECEPTION OF RADIATION DAY RETR06RADE ROTATION PERIOD BASED ON UV IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL PHOTOGRAPHS 1165-27550 SOURCES SUCH AS MOON/LUNAR THERMAL EMISSION. AND PLANETARY RADIO EMISSION 166-10998 SPECTROSCOPY OF PLANETARY ULTRAVIOLET RADIATION - RAYLE16H SCATTERING AND ELECTRON EXCITATION THERNOCONWtTIVITY NASA-CR-67597 N66-15400 VARIATION OF IR EMISSION FROM MARS SURFACE WITH MARS LOCAL TIME IN TERMS OF OIURNAL TEMPERATURE AEROBEE ROCKET MEASUREMENTS OF MARS UTRAVIDLET VARIATIONS. INCLUDING ATMOSPHERE EFFECT. RESULTS REFLECTIVITY - PLANETARY ATMOSPHERIC MIDEL SUSEST LOW THERM0CONDU;TIVITY A66-21201 NASA-TM-X-56654 N66-22239

THERMODYN~~)~IC MUILXBIIIU~ ULTMVIUET S?ECTRUM EXPECTED THERMODYNAMIC EQUILIBRIUM COMPOSITION OPTICAL THICKNESS. SCATTER1116 AND AEROSOL PARTICLE CALCULATED FOR ATMOSPHERES OF EARTH. VEMIS. CONCENTRATION OF MARS ATMOSPHERE IN UV SPECTRUM MARS. AND JUPITER A65-19668 NASA-CR-69965 N66-16463 JUPITER PHOTOELECTRIC SPECTRAL SCAN IN UV THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES REPRDWCEO AS GEOMETRIC REFLECTIVITY VS NASA-CR-69829 N66-21229 YAVELEIIGTH. USING AEROBEE ROCKET A66-21099 THERMWYNAMIC PUDPWTY COMPOSITION AND THERMODYNAMIC PROPERTIES OF MARS PLANETARY AERONOMY - PHOTOCHEMISTRY OF PLANETARY AND VENUS ATMOSPHERES ATMOSPHERE. VAWlM AND EXTREME ULTRAVIOLET NASA-CR-50811 1165-17291 SPECTRAL RE61ONS. AND THEORETICAL AERONOMY NASA-CR-68 106 N66-12248 THERMOOYNAMIC PROPERTIES OF 15 PERCENT CARBON OIOXIDE-85 PERCENT NITROGEN MIXTURE AT VARIED unm TEMPERATURE AND PRESSURE RANGES ATMOSPHERIC SCATTERING AND REFRACTION OF SUWLIGHT STL-9990-6631-TU-DO0 N65-23299 INTO PLANETARY UMBRA P-3282 W6-20124 EauILmRIum THERMODYNAMIC PROPERTIES /ENTROPY. ENTHALPY. PRESSURE. AND SOUND SPEED/ OF THREE UEEITAIllTl ENGINEERING MODELS OF MARTIAN ATMOSPHERE EVIDENCE FOR LIFE ON MARS - NATURE A10 NASA-SP-3021 W5-35792 WERTAINTIES MSA-CR-58430 N6S-2 947 5 THWI(OSPHERE MODELS OF MARTIIN THERMOSPHERE WITH CONSTANTS UlUmED SPltEUIAFT AND BOUNDARY VALUES IN HYDROSTATIC AND HEAT-FLUX SYSTEM DESI6N OF AUTOMATED LABORATDRY AND EQUATIONS N65-28713 ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORATION A65-35112 TRAJECTORY ANALYSIS TRAJECTORY ANALYSIS FOR MARS ATMOSPHERE PROBE - UlOUNNED SPACE MISSION TO DETERMINE MARTIAN VOYAGER PROJECT ENVIRONMENTAL FACTORS INFLUCNCING DESIGN OF NASA-TM-X-55376 N66-17249 SYSTEMS FOR MMED SPACE MISSION TO MARS - UNMA"f3 SPACECRAFT DESIGN TRWLCTORY cwmm NASA-CR-68742 N66-15540 SPACE VEHICLE RECOVERY TRAJECTORIES EXTENDIN6 FROM GIVEN INITIAL ORBIT TO ATMOSPHERE TOP UNMANNED SPACE MISSION TO DETERMINE NARTIAN A65-19314 ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - AERODYNAMIC BRAKING TRAJECTORIES FOR MARS ORBIT MISSION EXPERIMENT REQUIREMENTS . ATTAINMENT. GIVING ENTRY CORRIDORS FOR LIFTING NASA-CR-68741 N66-15541 VEHICLES AIM PAPER 64-478 M5-28839 UWANNED SPACE MISSION TO DETERMINE MARTIAN ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF TRANSLATXWL IY)TION SYSTEMS FOR MANNED SPACE MISSION TO MARS - TRANSLATIONAL AND ROTATIONAL MOTION OF SPHERICAL SUMMARY REPORT BODY ENTERING MARS ATMOSPHERE - REENTRY PHYSICS NASA-CR-68743 N66-15542 NASA-CR-69252 NU-15338 UWnANNEO SPACE MISSION TO DETERMINE MARTIAN TURBULEWT HEAT TRANSFER EWIRONMENTAL FACTORS INFLUENCING DESIGN OF LAMINAR AND TURBULHlT CONVECTIVE HEAT TRANSFER SYSTEMS FOR MANNED SPACE MISSION TO MARS - * RATES ON CONES IN PLANETARY ATMOSPHERES MISSION SENSITIVITY ANALYSIS RAD-TM-64-68 N65-19405 NASA-CR-68740 N66-15543 SYSTEMS DESIGN FOR UNMANNED SPACE MISSION TO

1-35 UPPER ATMOSPHERE SUBJECT INDEX

EVALUATE MARS ENVIRONMENT NASA-CR-54404 N65-24338 NASA-CR-69997 N66- 16248 ANALYTICAL RELATIONS CONNECTING BRIGHT TEMPERATURE UPPER ATMOSPHERE OF RADIO EMISSION OF VENUS COVERED BY ABSORBING BALLOON ELEVATED / STRATOSCOPE II I REMOTE ATMOSPHERE WITH PHYSICAL PARAMETERS CONTROLLED TELESCOPE FOR ASTRONOMICAL OBSERVATION N65-27226 OF PLANETS. NEBULAE. ETC, FROM UPPER ATMOSPHERE A65-28940 METEOROLOGY OF PLANETS MARS, VENUS, AN0 JUPITER NASA-CR-280 N65-30726 METEOR PHENOMENA, UPPER ATMOSPHERE WIND FIELDS FROM METEOR TRAILS, AN0 PHOTOHETRY OF A AND B ORIGIN OF PLANETARY ATMOSPHERES - MICROWAVE RINGS OF SATURN BRIGHTNESS MEASUREMENTS OF VENUS AFCRL-65-33 N65-36000 N65-31367

PLANETARY UPPER ATMOSPHERES - PRIORITY RATINGS FOR PLANETARY METEOROLOGY - MARS AN0 VENUS N65-32082 EXPERIMENTS. TYPES OF MEASUREMENTS FOR NASA-CR-64432 RECOMMENDED PROGRAM, AND ANNOTATED BIBLIOGRAPHY N66-14331 PHOTOMETRY OF AUREOLE PROLONGING HORNS OF VENUS CRESCENT SPACE SCIENCES BIBLIOGRAPHY WITH ABSTRACTS - NASA-TT-F-9685 N65-33962 ASTRONOMY, METEOROLOGY. OCEANOGRAPHY, UPPER ATMOSPHEREI GEOPHYSICS, SPACE SPECTROSCOPIC DETECTION OF WATER VAPOR IN JPRS-35095 N66-23025 ATMOSPHERES OF VENUS AN0 MARS USING TELESCOPE CARRIED BY BALLOON ~65-34835 URANUS PLANETARY ENVIRONMENTAL MOOELS OF VENUS. MARS, RADIO NOISE EMISSION FROM VENUS SURFACE EXPLAINED MERCURY, JUPITER, PLUTO, NEPTUNE. AN0 URANUS IN TERMS OF GLOW DISCHARGE A66-17174 AN0 SATELLITES ATMOSPHERIC COMPOSITION. TEMPERATURES, AND CIRCULATION N66-10996 BRIGHTNESS TEMPERATURE MEASUREMENTS ON ILLUMINATED SIDE OF VENUS AT 10.6 CM CHALLENGES STRUCTURE, COMPOSITION* ATMOSPHERE, AND SCIENTIFIC TROITSKI THEORY OF PLANETARY RADIATION EMISSION OBJECTIVE SURVEYS FOR SATURN. URANUS. A66-19457 NEPTUNE, AN0 PLUTO NASA-CR-70328 N66-11090 VENUS RADIATION AT 13.5 MM WATER VAPOR LINE AND PLANETARY BRIGHTNESS VARIATION WITH SOLAR V ILLUMINATION PHASE A66-20111 VACUUM ULTRAVIOLET DETECTION OF WATER AND ICE CLOUDS ON OUOPLASMATRON AS VACUUM ULTRAVIOLET LIGHT SOURCE - P-3245 VENUSN66-13681 PLANETARY AERONOMY NASA-CR-16 N65-17263 PHOTOMETRIC AND POLARIMETRIC STUDIES OF MARS AN0 VENUS ATMOSPHERES - AEROSOLS N66-23536 VACUUM ULTRAVIOLET LIGHT SOURCES - PLANETARY NASA-TT-F-9898 AERONOMY NASA-CR-17 N65-17264 SURFACE TEMPERATURE CALCULATIONS FOR VENUS BASED ON TWO GREENHOUSE ATMOSPHERIC MODEL COMPARISONSN66-23674 ABSORPTION AND PHOTOIONIZATION COEFFICIENTS OF NASA-TM-X-57315 PROPYLENE AN0 BUTENE 1 IN VACUUM ULTRAVIOLET - PLANETARY AERONOMY VENUS ATMOSPHERE NASA-CR-18 N65-17265 BALLOON BORNE IR SPECTROSCOPY INDICATES VENUS CLOUDS CONSIST OF ICE CRYSTALS A65-14707 PLANETARY AERONOMY - PHOTOCHEMISTRY OF PLANETARY ATMOSPHERE, VACUUM AN0 EXTREME ULTRAVIOLET THEORETICAL MODELS OF VENUS AND MARS UPPER SPECTRAL REGIONS, AN0 THEORETICAL AERONOMY ATMOSPHERES, NOTING DISSOCIATION LAYERS AN0 CARBON NASA-CR-68106 N66- 12248 MONOXIDE CONTENT A65-15454

VARIATION METHOD I R SPECTROSCOPY OF VENUS USED TO ESTIMATE CARBON PHYSICS OF PLANETARY ATMOSPHERES - VARIATION DIOXIDE ABUNDANCE BY MEASUREMENT OF ABSORPTION METHOD USE0 TO CALCULATE RAYLEIGH SCATTERING BANDS A65-15691 CROSS SECTIONS OF HELIUM AS WAVELENGTH FUNCTION NASA-CR-64187 N65-31052 EARTH REENTRY SIMULATION OF PLANETARY ENTRY ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF VELOCITY PROFILE MARS AND VENUS TYPE CLOSED FORM SOLUTIONS FOR INCLINATION ANGLE AND AIAA PAPER 65-218 165-1 6606 DENSITY OR ALTITUDE AS VELOCITY FUNCTION FOR BODY ENTERING PLANETARY ATMOSPHERE Ab5-20563 PHOTOMETRIC INVESTIGATION OF AUREOLE ELONGATING VENUS HORNS AT INFERIOR CONJUNCTION VENUS 165-17164 BRIGHTNESS TEMPERATURE OF RADIO EMISSION FROM VENUS A65-24803 UPPER LIMIT TO MOLECULAR OXYGEN CONTENT OF VENUS ATMOSPHERE OBTAINED WITH DOPPLER SHIFT TECHNIQUEA65-17189 TELESCOPIC OBSERVATIONS OF VENUS INDICATE FDUR- AND CURVE-OF-GROWTH ANALYSIS DAY RETROGRADE ROTATION PERIOD BASED ON UV PHOTOGRAPHS A65-27550 VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AN0 OF RADIO ASTRONOMICAL OBSERVATIONS OF VENUS WITH STATIC EQUILIBRIUM WITHIN KAPLAN ATMOSPHEREA65-19505 HIGH RESOLVING POWER NRL-TRANS-936 N65-17990 COLD ABSORBING ATMOSPHERE MODEL OF VENUS BASED ON VENUS RAD10 SPECTRUM AND MICROWAVE EMISSION OF CENTIMETER AN0 MILLIMETER EMISSION SPECTRUM ATMOSPHERIC MOLECULAR OXYGEN A65-19676 NASA-CR-57309 N65-19110 DATA RECORDING. DATA REDUCTION AND INTERPRETATION MARINER 11 RADAR AN0 RADIOMETRIC OBSERVATIONS OF OF INFORMATION ON WATER CONTENT OF VENUS VENUS WRING 1962 CONJUNCTION - PHYSICAL DATA ATMOSPHERE GATHERED BY BALLOON-BORNE INSTRUMENTS NASA-CR-56851 N65-22203 A65-22097

HIGH ENERGY DENSITY BATTERY FOR USE ON PLANET VENUS 1R LIMB DARKENING OBSERVATIONS BY A65-22MARINER 098 VENUS I1

1-36 SUBJECT IWEX VENUS ATWISPHERE

VENUSIAN ATMOSPHERE STRUCTURE AN0 COMPOSITION NEAR WAS A-TT-F8 244 1165-22589 TOP OF CLOUD COVER. NOTING CARBON OIOXIOE SCATTERING AND TEMPERATURE VARIATION WITH DEPTH OBSERVE0 RADIAl ON SPECTRUM OF VENUS ATMOSPHERE 1165-25228 WITH DECREASE I BRIGHTNESS TEMPERATURE EXPLAINED BY AS DRPTIOM IN RELATIVELY CCHO DEGREE OF POLARIZATION OVER CYTHEREAN DISK FOUNO SURROUNDING IONOSPHERE N65-24526 TO INCREASE WITH DISTANCE FROM CENTER OF PLANET A65-25694 ANALYTICAL RELATIONS CONNECTING BRIGHT TEMPERATURE OF RADIO EMISSION OF VENUS COVERED BY ABSORBING OBSERVATIONS CONCERNING ORIGIN OF VENUS RAOIO ATMOSPHERE WITH PHYSICAL PARAMETERS EMISSION AN0 ABOUT IONOSPHERE SURROUNDING PLANET N65-27226 ~65-2r771 DETECTION OF WATER VAPOR IN ATMOSPHERE OF VENUS STRATOSPHERIC BALLOON OBSERVATIONS OF VENUSIAN FTD-TT-65-296/1C2 N65-30746 CLOUOS INDICATE COMPOSITION OF ICE CRYSTALS A65-28654 DERIVATION OF ATMOSPHERIC PARAMETERS FOR GREENHOUSE MOOEL OF VENUS ATMOSPHERE VENUS ATMOSPHERE IN SEVERAL MODELS NOTING NASA-TH-X-53327 N65-35976 GREENHOUSE MODEL 8. IONOSPHERIC MODEL. ETC Ab5-29998 ELECTROMAGNETIC PROPAGATIOW CHARACTERISTICS OF

~ VENUS AN0 MARS DERIVE0 FROM ATMOSPHERIC OATA HISTORY OF TERRESTRIAL ATMOSPHERE AN0 DATA ON A6616436 CHEMICAL COMPOSITION OF VENUS ATMOSPHERE A65-33292 OBSERVATIONS CONCERNING ORICIN OF VENUS RADIO EMISSION AND AEOUT IONOSPHERE SURROUNDING PLANET OUTGASSING PROCESSES ON MOON AND VENUS. USING A6616625 EARTH ANALOGY A65-33298 WATER VAPOR CONTENT IN VENUS ATMOSPHERE ABOVE WATER VAPOR ON MARS AN0 VENUS. USING PHOTOMETRY REFLECTING CLOUD LAYER DETERMINED. USING AUTOMATIC OF ABSORPTION BAN0 WITH BALLOON MOUNTED TELESCOPE DAYTIME TELESCOPE AN0 6RATIN6 SPECTRORETER A65-33299 Ab618054

VENUS ATMOSPHERIC COMPOSITION. USING BALLOON REFLECTION SPECTRUM OF CLOUDS IN VENUS TELESCOPE OBSERVATION AND IMPLICATI ONS FOR MOOEL ATMOSPHERE MEASURED. USINC TELESCOPE WJUWTED ON ATMOSPHERE A65-33692 HELIUM BALLOON. NOTING DETAILS OF INSTRUMENT Ab61BO5S I R LIMB OARKENING OF VENUS EXPLAINEO IN TERMS OF THREE TYPES OF ATMOSPHERE AN0 CLOUD MODELS ABUNDANCE AN0 STABILITY OF MAJOR SULFUR CMlPWWDS A65-34633 IN LONER ATMOSPHERE OF VENUS CALCULATED. ASSWIN6 EQUILIBRIUM BETWEEN ATMOSPHERIC GASES AND MINERAL VENUS ATMOSPHERE BRIGHTNESS-TEMPERATURE MAPPING OF PHASES Ab619262 8-14 MICRON RADIATION BEFORE 1964 CONJUNCTION A65-35025 ATMOSPHERES OF VENUS AN0 MARS- ASTROPHYSICS CONFERENCE. KIEV. UKRAINIAN SSR. JUNE 1964 OIFFERENTIAL POLARIZATION AN0 DISTRIBUTION OF Ab619322 RADIOEMISSION OF DIFFERENT PARTS OF VISIBLE DISK OF VENUS MEASURED BY INTERFEROMETER PROBABILITY OF PRESENCE OF NITROCEN. OXYGEN AN0 A65-35268 WATER IN ATMOSPHERE OF VENUS. BASED ON SPECTROSCOPIC STUDIES Ab619323 PROBLEMS REGARDING CHEMICAL COMPOSITION ANO PHYSICAL PROPERTY OF VENUS ATMOSPHERE STRELKOV THEORY OF RADIO EMISSION FROM VENUS A6 5-6 0 868 ATTRIBUTES HIGH TEMPERATURE RAOIATION TO RAOIOACTIVE HEATING OF PLANETARY SURFACE CHEMICAL EVOLUTION OF TERRESTRIAL AND CYTHEREAN Ab619324 AT MOSPHERES A65-80890 ATMOSPHERIC COMPOSITION OF VENUS AN0 EFFECT Ow OBSERVATIONS OF WATER VAPOR ON MARS AN0 VENUS FROM RADIO EnIssIm IN VISIBLE AND NEAR IR SPECTRAL BALLOONS AN0 MOUNTAINS A65-BOB91 BANDS A6619325

NORMAL SHOCK WAVE AND STAGNATION POINT SOLUTIONS VENUS CLOUD LAYER AND BRIGHTNESS TEMPERATURE FROM FOR FOUR VENUSIAN ATMOSPHERIC AND CHEMICAL RADIOMETRIC MICROWAVE OBSERVATIOWS FROM NOCTURNAL MODELS SIDE OF PLANET A6b-20112 R64SD65 N65-13519 DATA RECORDING. DATA REDUCTION AND INTERPRETATION THEORETICAL MOOEL ATMOSPHERES OF VENUS OF INFORMATION ON WATER CONTENT of VENUS NASA-TN-0-2527 N65-14117 ATMOSPHERE GATHERED BY BALLMW)-WJRNE INSTRUMENTS Ab621109 CLWO COVER EFFECT ON GREENHOUSE MOOEL OF VENUS ATMOSPHERE VENUS IR LIMB OARKENING OBSERVATIONS BY NASA-CR-51116 Nb5-14655 MARINER I1 A6621110

MIXTURES OF NITROGEN AN0 CARBON OIOXIOE GASES SUPERCOOLED WATER DROPLETS HYPOTHESIZED IN VENUS HEATED BY SHOCK WAVE REFLECTION TO HI6H CLOUD LAYER. BASE0 Ow RADIOMETRIC OBSERVATION IN TEMPERATURE AT NORMAL DENSITY - VENUS SHF RANGE A6623503 ATMOSPHERE SIMULATION NASA-CR-51668 N65-15370 PLANETARY RADIATION AND AmEm EFFECTS ON THERMAL BALANCE OF SPACECRAFT ORBITING MARS AN9 VENUS COMPOSITION AN0 THERMODYNAMIC PROPERTIES OF MARS NASA-CR-676 13 N66-10684 AND VENUS ATMOSPHERES NASA-CR-5081I W5-17291 PLANETARY ENVIRONMENTAL MODELS OF VENUS. Was. MERCURY. JUPITER. PLUTO. NEPTUNE. AN0 URANUS VENUS ATMOSPHERE MOOEL OF COLD ATMOSPHERE AN0 SATELLITES ATMOSPHERIC COMPOSITION. SHORT WAVE ABSORPTION EFFECT ON LOW BRIGHTNESS TEMPERATURES. UID CIRCULATION N6610996 TEMPERATURE OF RAOIO EMISSIONS NASA-Ti-F-9663 N65-21005 POLARIZATION AN0 BRIGHTNESS TEMPERATURE

DISTRIBUTION MEASUREMENTS~ OF VENUS IN 10.6 CM VENUS NIGHT ATMOSPHERE INVESTIGATED BY STUOYIW WAVREUGTH IONOSPHERIC ELECTRON DENSITY AN0 ELECTRON ST-RA-LPS-10334 N66-11138 RECOMBINATION IN NIGHT ATMOSPHERE OF EARTH

1-37 VEWS PROBE SUBJECT INDEX

MARINER I1 MICROWAVE RADIOMETER EXPERIMENT TO SPECTRA AN0 WATER VAPOR ABUNOANCES STUDY VENUS SURFACE AN0 ATMOSPHERE A65-19902 NASA-CR-69916 N66-16151 DATA RECORDING, DATA REDUCTION AN0 INTERPRETATION EPUILIBRIUM TEMPERATURE DISTRIBUTION, THERMAL OF INFORMATION ON WATER CONTENT OF VENUS EMISSIONI AN0 LIMB FUNCTION COMPUTED FOR VENUS ATMOSPHERE GATHERED BY BALLOON-BORNE INSTRUMENTS CLWO COVER MODEL A65-22091 NASA-TM-X-55392 N66-17231 WATER VAPOR ON MARS AN0 VENUS, USING PHOTOMETRY ATMOSPHERIC CIRCULATION AN0 CLIMATOLOGY OF VENUS OF ABSORPTION BAND WITH BALLOON MOUNTED TELESCOPE AN0 MARS A65-33299 NASA-CR-71627 ~66-2ir67 VENUS ATMOSPHERIC COMPOSITION, USING BALLOON COMPOSITION. PRESSURE, VIOLET LAYER. STRUCTURE, TELESCOPE OBSERVATION AN0 IMPLICATIONS FORA65-33692 MODEL TEMPERATURE, CLOUOSI AN0 YINOS OF MARS AN0 ATMOSPHERE VENUS ATMOSPHERES N66-23052 DETECTION OF WATER VAPOR IN ATMOSPHERE OF VENUS VENUS PROBE FTO-TT-65-296/ lh2 N65-30746 VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AN0 OF SPECTROSCOPIC DETECTION OF WATER VAPOR IN STATIC EPUILIBRIUM WITHIN KAPLAN ATMOSPHERE ATMOSPHERES OF VENUS AN0 MARS USING TELESCOPE 1165-19505 CARRIED BY BALLOON N65-34835

SOLAR WINO PROTON VELOCITY. TEMPERATURE AN0 WATER VAPOR CONTENT IN VENUS ATMOSPHERE ABOVE DENSITY DETERMINED WHEN MARINER I1 WAS NEAR REFLECTING CLOUD LAYER DETERMINED, USING AUTOMATIC VENUS A65-22598 DAYTIME TELESCOPE AN0 GRATING SPECTROMETER A66-18054 DESIGN. PERFORMANCEI AN0 ENVIRONMENT PARAMETERS FOR MARS AN0 VENUS SPACE CAPSULES VENUS RADIATION AT 13.5 MM WATER VAPOR LINE AN0 NASA-CR-53674 N65-1b49B PLANETARY BRIGHTNESS VARIATION WITH SOLAR ILLUMINATION PHASE 166-20111 PLANETARY ENVIRONMENTAL DESIGN DATA FOR FUTURE MANNED SPACE FLIGHTS TO VENUS AN0 MARS DATA RECORDING. DATA REDUCTION AN0 INTERPRETATION NASA-SP-3016 N65-23799 OF INFORMATION ON WATER CONTENT OF VENUS ATMOSPHERE GATHERED BY BALLOON-BORNE INSTRUMENTS166-2 1109 VERTICAL DISTRIBUTION CONVECTIVE-RADIATIVE EPUILIBRIUM MODEL FOR COMPUTING TEMPERATURE PROFILE - VERTICAL DETECTION OF WATER AN0 ICE CLOUDS ON VENUS TEMPERATURE DISTRIBUTION IN MARTIAN ATMOSPHERE P-3245 N66-13681 NASA-CR-65049 N65-21955 NUMERICAL INTEGRATION OF VARIOUS PLANETARY VIRIAL THEOREM CIRCULATION PATTERNS IN PUASI-GEOSTROPHIC MODEL EXPLOSION IN RAREFIED ATMOSPHERES WHERE EXPLOSIVE ATMOSPHERE INCLUDING WATER VAPOR, OIABATIC PRODUCT ATOM MEAN FREE PATH IS LONGER THAN HEATING, AND SURFACE FRICTION EXPANDING MATERIAL DIMENSION, ILLUSTRATING METHDD AFCRL-65-77 1 N6b-16201 WITH CHEMICAL EXPLOSION AT 150 KM ALTITUDE A65-24615 PLANETARY CIRCULATION PATTERNS FOR INTEGRATED TWO- LEVEL PUASI-GEOSTROPHIC MODEL ATMOSPHERE N66-16209 VISIBLE SPECTRUM INCLUDING WATER VAPOR BRIGHTNESS DISTRIBUTION ALONG VISIBLE RADIUS OF MARS. EXAMINING ATMOSPHERIC SCATTERING PHYSICAL METHODS DESCRIPTION FOR DETECTION AN0 A65-18911 ANALYSIS OF TENUWS PLANETARY ATMOSPHERIC COMPONENT GASES, ESPECIALLY WATER VAPOR INTENSITY MEASUREMENTS OF METHANE ABSORPTION IN NASA-CR-70934 N66-19901 VISIBLE REGION OF JUPITERS SPECTRUM NASA-TT-F-10012 N66-23610 WAVE BEHAVIOR OF PLANETARY WAVES IN ATMOSPHERE MODEL VOLCANICS BASED ON SPHERICAL HARMONICS PHENOMENON OF VOLCANIC ACTIVITY ON MARS PLANET AFCRL-65-488 N66-10836 NASA-TT-F-410 N66-14057 YAVE DIFFRACTION VOYAGER PROJECT EXPECTED DIFFRACTION EFFECTS ON ELECTROMAGNETIC VOYAGER SYSTEM DESIGN STUDY - ENTRY LANDER, AN0 RADIATION FROM MARINER IV DUE TO MARTIAN ORBITER SYSTEM FOR ENTRY .INTO VENUS OR MARS ATMOSPHERE AN0 OCCULTATION A66-16039 ATMOSPHERES NASA-CRZ51839 N66-13403 YAVE SCATTERING ELECTROMAGNETIC WAVE SCATTERING IN HOMOGENEOUS VOYAGER SUBSYSTEM DESIGN STUDY - GUIDANCE AN0 PLANE-PARALLEL ATMOSPHERES - SOLAR RADIATION CONTROL, PROPULSIONi AN0 POWER SUPPLY STUDIES TRANSFER IN PLANETARY ATMOSPHERE FOR ENTRY IN MARS OR VENUS ATMOSPHERES RM-4846-PR N66-1941 B NASA-CR-51837 . .-NU-^ - - --uni .- . YEATHER CONDtTION TRAJECTORY ANALYSIS FOR MARS ATMOSPHERE PROBE - SPACE EXPLORATION - SPACE AROUND EARTH*

VOVAGER PROJECT ATMOSPHERIC. __ ~ ._ CIRCULATION. AN0 WEATHER CONDITIONS, NASA-TM-X-55376 N66-11249 LUNAR PHOTOGRAPHY, AN0 PLANETARY STUDIES NASA-EP-25 N65- 32574

W YEATHER FORECASTIN6 WATER CONTENT FORECASTING HUMIDITY TRANSPORT IN ATMOSPHERE IN POSSIBLE WATER SOURCE BENEATH MARS SURFACE DUST PLANETARY-SCALE PROCESSES A65-30110 AN0 ICE MAY CONSTITUTE POTENTIAL BIOSPHERE A65-26120 YEIW ANALYSIS WEIGHT AN0 ENERGY REPUIREMENTS OF VEHICLE SYSTEMS OBSERVATIONS OF WATER VAPOR ON MARS AND VENUS FROM FOR MANNED EXPLORATION OF MARS BALLOONS AN0 MOUNTAINS A65-BOB91 AIAA PAPER 64-403 A65-33549

WATER VAPOR MIND MARS IR SPECTRA IN 3-4 MICRON REGION ATTRIBUTED ETEOR PHENOMENA, UPPER ATMOSPHERE WINO FIELDS TO TERRESTRIAL HDO MOLECULES ON BASIS OF SOLAR FROM METEOR TRAILS, AN0 PHOTOMETRY OF A AND B

1-38 SUBJECT IlDEX

R1N6S OF SATUlN AFCRL-65-33 N65-36000

YIWD PROFILE PLANETARY BOUNDARY LAYER MOLBEL FOR ATMOSPHERIC WIND AND TURBULENCE DISTRIBUTIONS N65-22739 X X-RAY X-RAY RADIATION INTENSITY OF AURORAE POLARIS OF PLANET TO DETERMINE HAWETIC MOMENT A65-15763

X-RAY SPECTRIMETRY ABSOLUTE INTENSITY MEASUREMENTS IN EXTREME UV AND SOFT X-RAY REGIONS OF SOLAR SPECTRUM A65-32154

1-39 Personal Author Index

PLANETARY ATMOSPHERES / a continuing bibliography with indexes AUGUST 1966

WIN1 CONVECTIVE HEAT TRANSFER. USING ARC-HEATED SHOCK TUBE SIMULATING FLIGHT VELOCITIES UP TO Typical Personal Author index Listing 34.000 FPS AIAA PAPER 66-29 A6617891

MILET* H. E- ATMOSPHERE OF MARS BASED ON EPUILIBRIUM THERMODYNAMIC PROPERTIES /ENTROPY. MARINER IV OCCULTATION EXPERIMENT ENTHALPY* PRESSURE. AND SOW0 SPEED/ OF THREE LMSC-6-75-65-62 ENGINEERING MODELS OF MARTIAN ATMOSPHERE II NASA-SP-3021 N65-35792 0ARABASHM* N. Pa MARS ATMOSPHERIC OPTICAL THICKNESS AND SCATTERING FROM PHOTOMETRIC OBSERVATION A6619327

MRR€TT* Ao H- A Notation of Content (NOCI. rather than the title of the document. is used to provide a more exaci dexription of the wbpct matter The accesson number VENUS RADIO SPECTRUM AN0 MICROWAVE EMISSION OF ATMOSPHERIC MOLECULAR OXYGEN IS included to assist user in locating abstract in the abstract section the the NASA-CR-57309 N65-19770

MRRING€R* A- R- REMOTE MEASUREMENT OF TRACE AMOUNTS OF VAPORS IN LWAR AND PLANETARY ATMOSPHERES AS INDICATOR OF A BIOLOGIC AND 6EOL06IC SURFACE CONDITIONS ABRAMOYITZ* J. A66-2 1532 PHYSICAL METHODS DESCRIPTION FOR OETECTICM AND ANALYSIS OF TENUOUS PLANETARY ATMOSPHERIC EARTH. C. A. COMPONENT GASES. ESPECIALLY WATER VAPOR SPECTROSCOPY Of PLANETARY ULTRAVIOLET RAOIATION - NASA-CR-70934 N66-19901 RAYLEIGH SCATTERINS AN0 ELECTRON EXCITATION NASA-CR-67597 N66-15400 ADAMSs E. HYPERSONIC AERODYNAMICS THROUGH PLANETARY BMTKD. F- ATMOSPHERES DESCRIBED BY TWO-BODY PROBLEM IN EQUILIBRIUM TEMPERATURE OISTRIBUTIDN. THERMAL CELESTIAL MECHANICS 165-23916 EMISSION. AND LIMB FUNCTION COMPUTED FOR VENUS CLOUD COVER MODEL ALLERs H. 0- NASA-TM-X-55392 N66-17231 BRIGHTNESS TEMPERATURE MEASUREMENTS OF MARS AT 3.75 CM FROM FEBRUARY TO JUNE 1965 BASHARINW* A- E- A6618788 VENUS CLOUD LAYER AND BRIGHTNESS TEMPERATWE FROM RADIOMETRIC MICROWAVE OBSERVATIONS FROM NOCTURNAL ANDERSONs A- 0- SIDE OF PLANET A6620112 MODEL FOR LOWER ATMOSPHERE OF MARS BASED ON MARINER IV OCCULTATION EXPERIMENT SUPERCOOLED WATER DROPLETS HYPOTHESIZED IN VENUS LMSC-6-75-65-62 N66-16940 CLOUD LAYER. BASED Ow RADIOMETRIC OBSERVATION IN SHF RANGE A6623503 ANDERSONs C. E- SYSTEM DESIGN OF AUTOMATED LABORATORY AND BASU. Bo ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN MARTIAN BLUE HAZE PROPERTIES CORRELATED WITH EXPLORATION A65-35112 INTERPLANETARY DUST* METEOR SHOWERS AND SOLAR FLARES A65-26040 ANDERSON* H- R- MARINER IV ENCOUNTER SEQUENCE OURIN6 APPROACH AND BERWQT. P. To OCCULTATION OF MARS ON JULY 14 AN0 15. 1965 PLANETARY ENTRY VEHICLES - LONGITUDINAL STABILITY A65-36323 CHARACTERISTICS FOR VARIOUS BLUNT-BODY MODELS TESTED AT MACH 6-73 IN WINO TUNNEL ANDERSON. W. 6. NASA-TN-0-2785 N65-22368 HIGH ENERGY DENSITY BATTERY FOR USE ON PLANET VENUS BERNSTEIW* Y. NASL-CR-54404 1165-24338 ARGON ABUNDANCE IN MARTIAN ATMO.SPHERE OETECTOR. USING CYLINDRICAL IONIZATION CHAMBER CONTAINING APPLEBY. J. F. IRON 55 X-RAY SOURCE A6523098 PLANETARY BOUNDARY LAYER MODEL FOR ATMOSPHERIC WINO AN0 TURBULENCE OISTRIBUTIONS BEUF. F. 6- N65-22739 SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST PROGRAM SHOWING REPUIREMENTS FOR LAUNCH VEHICLE. ARWOLOs J. 0. TRACKINGs COST AND SCHEDULE SPECTRAL AN0 TOTAL RADIATION STUDIES OF BODIES AIAA PAPER 65-219 A65-17398 TRAVELING AT HYPERSONIC SPEED IN SIMULATED MARTIAN AND VENUSIAN ATMOSPHERES SYSTEM DESIGN OF AUTOMATED LABORATORY AND AIM PAPER 65-116 A65-15008 ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORATIDN A65-35112

B BINOR. A- B. BABINUUX~T. L. POSSIBLE ATMOSPHERE DETECTION ON J-I1 AND ATMOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNAT.ICM J-I11 SATELLITES REVEALED BY EXCESS BRIGHTNESS ON

1-41 .

BLAVET. H- PERSONAL AUTHOR INDEX

ECLIPSE REAPPEARANCE A66-21202 N65-31360

BLAVET. H- BUCKENDNU. 0. E- BALLOON ELEVATED / STRATOSCOPE 11/ REHOTE ENGINEERING BREADBOARD MODEL OF HICROORGANISH CONTROLLED TELESCOPE FOR ASTRDNDHICAL OBSERVATION DETECTION'DEVICE FOR HARS LANDING APPLICATIONS OF PLANETS, NEBULAE. ETC. FROH UPPER ATMOSPHERE NASA-CR-74214 N6b-23707 A65-28940 W6AYENKD. L- A. BOESEt R- Y. CARBON DIOXIDE- R-BRANCH LINES' OF 5 HU SUB 3 BAND . BRIGHTNESS DISTRIBUTION IN MARGINAL ZONE OF MARS FROM INTEGRAL OF ABSORPTION COEFFICIENT OF USED TO DETERMINE ATMOSPHERIC ABSORPTION HARTIAN ATMOSPHERE A66-15288 A65- 18972

BOLLHAGENS H. PHOTOELECTRIC HEASUREMENT OF BRIGHTNESS FINAL REDUCTION OF OBSERVATIONS OF SPORADIC DISTRIBUTION IN LIMB ZONE OF HARS OUTBURSTS IN OECAHETRIC REGION OF RADIO SPECTRUM NASA-TT-F-10010 N66-23538 OF JUPITER DURING 1961 AND 1962 A65-21855 WIAIENKO. 0- I- BONESTELL. C. BRIGHTNESS DISTRIBUTION IN MARGINAL ZONE OF MARS CHARACTERISTICS OF HARS AND POSSIBILITY OF USED TO DETERHINE ATHOSPHERIC ABSORPTION EXISTENCE OF LIFE A65-81018 A65-10972

BOOBAR. H. 6. PHOTOELECTRIC MEASUREMENT OF BRIGHTNESS SYSTEMS DESIGN FOR UNMANNED SPACE HISSION TO DISTRIBUTION IN LIMB ZONE OF HARS EVALUATE HARS ENVIRONHENT NASA-TT-F-10018 N66-23538 NASA-CR-69997 N66-16248 BURCH. 0- E. BORISWA. Fa INFRARED SPECTROSCOPY STUDIES TO DETERMINE ATHOSPHERIC FACTORS OF INTERPLANETARY SPACEFLIGHTS ABSORPTION BY CARBON DIOXIDE BETWEEN 8.000 AND FTO-TT-65-741/1&2h4 N66- 1251 1 lD.OOO/CM IN 1 TO 1-25 MICRON REGION U-3200 N66-22465 BDRTNER. Ha H. HASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE BURLEI. R- R- FOR CHEMICAL COHPOSITION STUDY OF HARTIAN ALTERNATE MISSION PROFILES FOR HANNED HARS ATHOSPHERE LAND ING NASA-CR-71307 N66-23779 NASA-TN-0-3181 N66-14703

BDSYORTHt Fa NORMAL SHOCK WAVE AND STAGNATION POINT SOLUTIONS C FOR FOUR VENUSIAN ATMOSPHERIC AND CHEHICAL CAFARD. C- HODELS PLANETARY RADIATION AND ALBEDO EFFECTS ON THERHAL R64SD65 N65-13519 BALANCE OF SPACECRAFT ORBITING MARS AND VENUS NASA-CR-67813 N66-10684 BOTTEMA. M. DATA RECORDING. DATA REDUCTION AND INTERPRETATION CAIN. 0- L. OF INFORHATION ON WATER CONTENT OF VENUS HARS ATHDSPHERE AND IONOSPHERE HEASUREHENTS USING ATHOSPHERE GATHERED BY BALLOON-BORNE INSTRUMENTS 2300-MC TELEMETRY SIGNAL FROH HARINER IV A65-22091 SPACECRAFT OCCULTAT ION EXPERIMENTS A65-26719 VENUS ATMOSPHERIC COMPOSITION^ USING BALLOON TELESCOPE OBSERVATION AND IHPLICATIONS FOR HODEL COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE ATHOSPHERE A65-33692 AND IONOSPHERE OF HARS INCLUDING DENSITY. TEMPERATURE. SCALE HEIGHT, ETC A65-36328 WATER VAPOR CONTENT IN VENUS ATMOSPHERE ABOVE REFLECTING CLOUD LAYER DETERMINED. USING AUTDHATIC HARINER IV OCCULTATION EXPERIMENT ON HARTIAN DAYTIME TELESCOPE AND GRATING SPECTROMETER ATHOSPHERE. USING AHPLITUDE AND FREQUENCY CHANGES A66-18054 OF TRACKING AND TELEMETRY SIGNAL AIAA PAPER 66-148 1166-17900 REFLECTION SPECTRUH OF CLOUDS IN VENUS ATMOSPHERE MEASURED. USING TELESCOPE HOUNTED ON CAMERON. A- 6- Y. HELIUH BALLOON, NOTING DETAILS OF INSTRUHENT PLANETARY ATHOSPHERES ORIGIN DUE TO OUTGASSING OR A66-18055 CAPTURE FROH PRIHITIVE SOLAR NEBULA OR SOLAR HIND AND ATMOSPHERIC LOSSES DUE TO REVERSE PROCESSES DATA RECORDING. DATA REDUCTION AND INTERPRETATION A65-32627 OF INFORHATION ON WATER CONTENT OF VENUS ATMOSPHERE GATHERED BY BALLOON-BORNE INSTRUMENTS ORIGIN AND EVOLUTION OF PLANETARY ATNOSPHERES AN0 A66-21109 OCEANS A65-80889

BDYER. CH. PROCESSES OF ORIGIN OF PLANETARY ATMOSPHERES TELESCOPIC OBSERVATIONS OF VENUS INDICATE FDUR- A65-0192 8 DAY RETROGRADE ROTATION PERIOD BASE0 ON UV PHOTOGRAPHS A65-27550 RECENT SPACE RESEARCH IN PHYSICAL SCIENCES - LITERATURE SUMMARY AN0 DISCUSSION BRANCAZIO. P. J- NASA-TM-X-51903 N65-29458 ORIGIN AND EVOLUTION OF PLANETARY ATMOSPHERES AND OCEANS *65-80809 ORIGIN OF PLANETARY ATMOSPHERES - MICROWAVE BRIGHTNESS IIEASUREHENTS OF VENUS BRANOT. J- C. N65-31367 BOOK ON SOLAR SYSTEM ASTRDNDHY AND SPACE PHYSICS INCLUOING CELESTIAL MECHANICS, INTERPLANETARY GAS CANN. H- Y- P- PHYSICS. METEORITES AND PLANETARY ATMOSPHERES RECENT DETERHINATIONS OF COHPOSITION AND SURFACE

~~ A65- 17~ 42 2 PRESSURE OF HARS ATHOSPHERE NASA-CR-298 N65-33835 BRANI6ANs 1. L. LECTURE HANUSCRIPTS ON HIGH ALTITUDE EXPLOSIONS. JUPITER FLYBY MISSIONS - FUTURE STUDIES ON PLANET BIOLOGICAL EXPLORATION OF HARS, MASERS AND ATMOSPHERE AND MAGNETOSPHERE LASERS, PLANETARY ATHOSPHERESI RELATIVITY NASA-CR-69561 N66-15807 THEORYI ELEMENT ABUNDANCEI AND SOLAR PARTICLES

1-42 CAM. To D. DEFORMATION AND EWATORIAL PLANE ASYMMETRY FINAL REDUCTION OF OBSERVATIONS OF SPORADIC NASA-CR-68703 N66-13573 OUTBURSTS IN DECAMETRIC REGION OF RADIO SPECTRUM OF JUPITER DURING 1961 AND 1962 CO”h Bo J. A65-21855 METHODS FOR OBTAINING TEMPERATURE PROFILE OF PLANETARY ATMOSPHERE FROM REMOTE RADIOMETRIC CASTEUI. J. P. MEASUREMENTS RADIO OBSERVATION OF PLANETARY AND STELLAR NASA-TN-D-2940 N65-30733 EMISSION AND EFFECTS OF TERRESTRIAL ATMOSPHERE A66-20289 COOK. A- F. METEOR PHENOMENA. UPPER ATMOSPHERE WIlo FIELDS RADIO ASTRWOMY - PASSIVE RECEPTION OF RADIATION FROM METEOR TRAILS. AND PHOTOMETRY OF A AND B IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL RIIIGS OF SATURN SOURCES SUCH AS MOOW/LUNAR THERMAL EMISSION. AND AFCRL-65-33 N65-36000 PLANETARY RADIO EMISSION N66-10996 coar. c. CHAMBERLAIN. J. Y- NORMAL SHOCK WAVE AN0 STAGNATION POINT SOLUTIONS VENUSIAN ATMOSPHERE STRUCTURE AND COMPOSITION NEAR FOR FOUR VEWSIAN ATMOSPHERIC AND CHEMICAL TOP OF CLOUD COVER. NOTIW CARBON DIOXIDE MDELS SCATTERING AND TEMPERATURE VARIATION WITH DEPTH R64SM5 N65-13519 A65-25220 COIBElT. H- H. SURFACE PRESSURE AND CARBON DIOXIDE CONTENT OF VENUS RADIATION AT 13.5 MM WATER VAPOR LINE AND MARTIAN ATMOSPHERE. COHPARIN6 POLARIMETRIC. PLANETARY BRIGHTNESS VARIATION WITH SOLAR PHOTOMETRIC AND SPECTROSCOPIC METHODS ILLUMINATION PHASE A6620111 M5-26212 tMLISS. Y. R. CHEMICAL COMPOSITION AND TEMPERATURE IN MODEL OF SPACECRAFT. MISSIONS AND INSTRUMENTATION FOR SPACE UPPER ATMOSPHERE OF MARS A65-27569 PROBES AND INTERPLANETARY EXPLORATION A65-82064 MOMLS OF MARTIAN THERMOSPHERE WITH CONSTANTS AN0 BOUNDARY VALUES IN HYDROSTATIC AND HEAT-FLUX CrnTmIGHT. E. I(. EQUATIONS 1165-28713 SPACE EXPLORATION - SPACE AROUND EARTH. ATMOSPHERIC CIRCULATION AN0 WEATHER CONDITIONS. PLANETARY UPPER ATMOSPHERES - PRIORITY RATINGS FOR LUNAR PHOTOGRAPHY. AND PLANETARY STUDIES EXPERIMENTS. TYPES OF MEASUREMENTS FOR NASA-EP-25 N65- 32 574 RECOMMENDED PR06RAM. AND ANNOTATED BIBLIOsRAPHY N66-14331 CRlJIKSMMt. D- Po LABORATORY SPECTRA FROM LEAD SULFIDE SPECTROMETER C“. Yo Y. FOR TESTING PRESENCE OF MINOR CONSTITUENTS IN PHYSICS OF PLANETARY ATMOSPHERES - VARIATION PLANETARY ATMOSPHERES A65-18479 METHOD USE0 TO CALCULATE RAYLEICW SCATTERIMS CROSS SECTIONS OF HELIUM AS WAVELEN6TH FUWTIDN rnssIBLE ATMOSPHERE DETECTION ON J-11 AND NASA-CR-64187 1165-31052 J-I11 SATELLITES REVEALED BY EXCESS BRIGHTNESS ON ECLIPSE REAPPEIRANCE A66-2 1202 CHANEY. La MARS SURFACE AND ATMOSPHERE CHARACTERISTICS FROM SPECTRUM* COMPOSITIOW AND SURFACE PRESSURE. CARBON THERMAL EMISSION SPECTRUM MEASUREMENT BY DIOXIDE ABUNDANCE. NITROGEN DIOXIDE TESTS. AND INFRARED INTERFEROMETER ON PLANETARY FLYBY STRUCTURE OF ATMOSPHERE ON MARS SPACECRAFT WASA-CR-60 264 N65-15223 NASA-TM-X-55070 N65-32114 CUBLEI. H- D- CHRISTENSEU. 0. EXPECTED DIFFRACTION EFFECTS W ELECTROMAGNETIC BIBLIOGAAPHY OF DOCUMENTS ON LUNAR. PLANETARY. RADIATION FROM MARINER IV DUE TO MARTIAN AND SPACE ENVIRONMENTS IN RELATION TO FLIGHT ATMOSPHERE AN0 OCCULTATION A66-16039 MECHANICS AND AERODYNAMICS OF SPACE TRAVEL NASA-CR-60469 N65-16086 D SPACE ENVIRONMENT - DATA ON ELECTROMA6NETIC AND DAL6UM. A- PARTICULATE RADIATION. METEOROID FLUX. AND CALCULATIONS OF MIDDAY DAY6LOW INTENSITIES STRUCTURE. AND COMPOSITION OF PLANETARY ARISIMS FROM FLUORESCENCE OF SOLAR IONIZING ATMOSPHERE - SOLAR SYSTEM SPACE ENVIRONMENT RADIATIOII NASA-CR-294 N65-34244 NASA-CR-64424 1165-31M7 CHVOJMVA. E. PHYSICS OF PLANETARY ATMOSPHERES - VARIATION RADIO PATH FORMULAS ma PLANETARY IONOSPHERES AND METHOD USED TO CALCULATE RAYLEICH SCATTERIW STELLAR ATMOSPHERES FROM QUASI-CONIC EQUATION AND CROSS SECTIWS OF HELIUM AS WAVELEWTH FWCTION ELECTRON DENSITY EQUATION A6523429 NASA-CR-64187 N65-31052

CITRON. S. J. COUPLE0 HARTREE- FOCK APPROXIMATION FOR CLOSED FORM SOLUTIONS FOR INCLINATION AWGLE AND CALCULATING FREQUENCY-DEPENDENT REFRACTIVE INDEX DENSITY OR ALTITUDE AS VELOCITY FUNCTION FOR BODY OF HELIUM GAS ENTERING PLANETARY ATMOSPHERE A65-20563 NASA-CR-6B991 1166-14281

CLARK. B. 6. MLLWS. A. DIFFERENTIAL POLARIZATION AND DISTRIBUTION OF WATER VAPOR ON MARS AND VENUS. USING PHOTOMETRY RADIOEMISSION OF DIFFERENT PARTS OF VISIBLE DISK OF ABSORPTION BAND WITH BALLOON MOUNTED TELESCOPE OF VENUS MEASURED BY INTERFEROMETER A65-33299 A65-35268 DANILOV. A. 0- COLEUAN. Po J-. JRo OBSERVATIONS CONCERNING ORIGIN OF VEWS RADIO INTERACTIOII OF SOLAR WIND WITH PLANETS - EMISSION AND ABOUT IONOSPHERE SURROUNDING PLANET PROPERTIES OF INTERPLANETARY MEDIUM AND A6527771 THEORETICAL MODELS OF SOLAR WIND N66-14334 OBSERVATIONS CO)lCERNING ORIGIN OF VENUS RAOID EMISSION AND ABOUT IOWOSPHERE SURROUNDING PLANET COLOIIOO. 6. A6616625 ROTATION OF PLANET MERCURY FROM RADAR OBSERVATION EXPLAINED BY SOLAR GRAVITATIONAL TORQUE ON TIDAL STRELKOV THEORY OF RADIO EMISSIOW FROM VENUS

1-43 DAVIES, W- 0. PERSONAL AUTHOR INDEX

ATTRIBUTES HIGH TEMPERATURE RADIATION TO RADIATION BELTS IN JUPITER ATMOSPHERE RADIOACTIVE HEATING OF PLANETARY SURFACE A65-27015 A66-19324 DICKERMAN* P. J. VENUS NIGHT ATMOSPHERE INVESTIGATED BY STUDYING STRUCTUR6, COMPOSITIONt ATMOSPHERE. AN0 SCIENTIFIC IONOSPHERIC ELECTRON DENSITY AND ELECTRON OBJECTIVE SURVEYS FOR SATURN. URANUS, RECOMBINATION IN NIGHT ATMOSPHERE OF EARTH NEPTUNE, AN0 PLUTO NASA-TT-F-8244 ~65-22589 NASA-CR-70328 N66-17090

DAVIES. W. 0. DIDYCHENKD. YE- I. EARTH, BALLOON AND SATELLITE SPECTROSCOPIC SPECTROPHOTOMETRIC OBSERVATIONS OF MARS OBSERVATIONS OF MARS TO DETERMINE ATMOSPHERIC N65-18512 COMPOSITION AND PRESSURE AT SURFACE LEVEL 166-21065 DIETER. N- Ha RADIO OBSERVATION OF PLANETARY AND STELLAR RECENT OETERMINATIONS OF COMPOSITION AND SURFACE EMISSION AN0 EFFECTS OF TERRESTRIAL ATMOSPHERE PRESSURE OF MARS ATMOSPHERE A66-20289 NASA-CR-298 N65-3383 5 RADIO ASTRONOMY - PASSIVE RECEPTION OF RADIATION DAVIS, M. H. IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL FEASIBILITY AND DESIGN OF BALLOONS FOR EXPLORATION SOURCES SUCH AS MOON/LUNAR THERMAL EMISSION, AN0 OF SURFACE AND ATMOSPHERE OF MARS PLANETARY RADIO EMISSION ~661099a N65-34830 DOLE. S. H. DAYHDFF, M. 0- PLANETS HABITABLE FOR MAN A65-80977 EXPECTED THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATED FOR ATMOSPHERES OF EARTH, VENUS, DOLLFUS, A- MARS. AND JUPITER PHOTOMETRIC INVESTIGATION OF AUREOLE ELONGATING NASA-CR-69965 N66-16463 VENUS HORNS AT INFERIOR CONJUNCTION 16s-17164 THERHODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES NASA-CR-69829 N66-21229 OBSERVATIONS OF WATER VAPOR ON MARS AN0 VENUS FROM BALLOONS AND MOUNTAINS A65-80891 DE VAUCOULEURSr G. COMPOSITIDNt PRESSURE, VIOLET LAYER, STRUCTURE, PHOTOMETRY OF AUREOLE PROLONGING HORNS OF VENUS TEMPERATURE, CLOUDS. AND WINDS OF MARS AN0 CRESCENT VENUS ATMOSPHERES N66-23052 NASA-TT-F-9685 N65-33962 DEIRMENDJIAN* 0- DETECTION OF WATER AND ICE CLOUDS ON VENUS SPECTROSCOPIC DETECTION OF WATER VAPOR IN ATMOSPHERES OF VENUS AND MARS USING TELESCOPE P-3245 N66-13681 CARRIE0 BY BALLOON N6 5- 3483 5 DEMARCUS, W. C. SEPARATION BETWEEN FLUID PHASES IN MULTICOMPONENT DORDN. E- ATMOSPHERE AS POSSIBLE EXPLANATION OF JUPITER PLANETARY CIRCULATION PATTERNS FOR INTEGRATED TWO- GREAT RED SPOT A66-19592 LEVEL PUASI-GEOSTROPHIC MODEL ATMOSPHERE INCLUDING WATER VAPOR N66- 16209 DENNIS. A. 5. OPTICAL DETECTION OF LIGHTNING FROM SATELLITES DRAKE. F. 0. NASA-CR-60806 ~65-17404 MARS ATMOSPHERE AND IONOSPHERE MEASUREMENTS USING 2300-MC TELEMETRY SIGNAL FROM MARINER IV DENT. W. A- SPACECRAFT OCCULTATION EXPERIMENTS BRIGHTNESS TEMPERATURE MEASUREMENTS OF MARS AT ~65-26719 3.75 CM FROM FEBRUARY TO JUNE 1965 A66-18788 COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE AND IONOSPHERE OF MARS INCLUDING DENSITY, DERGARABEOIAN, P. TEMPERATURE, SCALE HEIGHT, ETC ~65-3632a UNMANNED SPACE MISSION TO DETERMINE MARTIAN ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF DRESSLER. K- SYSTEMS FOR MANNED SPACE MISSION TO MARS - HYDROGEN MOLECULES IN ASTROPHYSICS UNMANNED SPACECRAFT DESIGN NASA-CR-57156 N65-18918 NASA-CR-60742 N66- 15540 UNMANNED SPACE MISSION TO DETERMINE MARTIAN t ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF UK. R- V. SYSTEMS FOR MANNED SPACE MISSION TO MARS - EXPECTED THERMODYNAMIC EQUILIBRIUM COMPOSITION MISSION EXPERIMENT REQUIREMENTS CALCULATED FOR ATMOSPHERES OF EARTH, VENUS. NASA-CR-60741 N66-15541 MARS, AND JUPITER NASA-CR-69965 N66-16463 UNMANNED SPACE MISSION TO DETERMINE MARTIAN ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES SYSTEMS FOR MANNED SPACE MISSION TO MARS - NASA-CR-69829 N66-21229 SUMMARY REPORT NASA-CR-60743 N66-15542 EG6LESTON. J. M. LUNAR AN0 PLANETARY ENVIRONMENTS USE0 BY NASA UNMANNED SPACE MISSION TO DETERMINE MARTIAN MANNED MISSION PLANNING AN0 DESIGN CONSIDERING ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF RADIATIVE, TOPOGRAPHICAL AND ATMOSPHERIC FEATURES SYSTEMS FOR MANNED SPACE MISSION TO MARS - A 6 5-22 135 MISSION SENSITIVITY ANALYSIS NASA-CR-60740 N66-15543 EHRLICH. R- RESPONSE OF MICROORGANISM TO SIMULATED MARTIAN DIACONIS, N. S. ENV IRONMENT INVESTIGATED. USING CULTURE SIMULATION OF HEAT TRANSFER ENVIRONMENTS OF SPACE COLLECTIONS AND SOIL SAMPLES ~65-30676 VEHICLE ENTERING PLANETARY ATMOSPHERE WITH SUPERORBITAL VELOCITY EISENBERS. J- 0- R 645 073 N65-15600 ALTERNATE MISSION PROFILES FOR MANNED MARS LANDING DICKEL, J. R. NASA-TN-0-3181 N66- 14703 10 EFFECT ON SYNCHROTRON EMISSION GENERATED WITHIN . PERSONAL AuTwyl INOEX FJELOBO. C.

EKSINBR. D. HEATED BY SHOCK WAVE REFLECTION TO HIGH MARS ATMOSPHERE PROPERTIES DISTINGUISH IT FROM TEMPERATURE AT NORMAL OENSITY - VENUS EARTH ATMOSPHERE. PARTICULARLY WATER CONTENT. ATMOSPHERE SIMULATION THERMAL FLOWS AND AIR MASSES CIRCULATION NASA-CR-51668 N65-15370 A65-19853 FAIRCHILO. II. K- EPSTEIN. E, E. PLANETARY RADIATION AN0 ALBEW EFFECTS ON THERMAL RADIO OBSERVATIONS OF MERCURY SHOW BRIGHTNESS BALANCE OF SPACECRAFT ORBITING MARS AND VENUS TEMPERATURE OF ONLY 200 DEGREES Kr WITH NO NASA-CR-678 13 Nb6-10684 SIGNIFICANT VARIATION WITH PHASE A6b-20182 FEITIS. P, H. ROTATIONAL. PRECESSIONAL AN0 NUTATIONAL MOTION OF BLACK BODY DISK TEMPERATURES OF MERCURY AN0 MARS BODY ENTERING MARS ATMOSPHERE IN VERTICAL AND FROM OBSERVATIONS AT 3.4 MM IN APRIL 1965 OBLIQUE DIRECTIONS A65-30321 A66-22786 TRANSLATIONAL AND ROTATIONAL MOTION OF SPHERICAL ERSWWICH. A. 1. BOOY ENTERING MARS ATMOSPHERE - REENTRY PHYSICS X-RAY RADIATION INTENSITY OF AURORAE POLARIS OF NASA-CR-69252 N6b-15338 PLANET TO DETERMINE MAGNETIC MOMENT A65-15163 FESE*I[OI. V. 6. ATMOSPHERIC REFRACTION. EXTINCTION. AND AEROSOL ESHLEMAN. V. R. EFFECTS ON ASTROPHYSICAL OBSERVATIONS INCLUDING MARS ATMOSPHERE AND IONOSPHERE MEASUREMENTS USING SIGNIFICANCE OF SURFACE REFLECTANCE AND HIGH 2300-MC TELEMETRY SIGNAL FROM MARINER IV ALTITUDE-COSMIC WST N66-17747 SPACECRAFT OCCULTATION EXPERIMENTS A65-26719 FIELD. 6. 8. MERCURIAN ATMOSPHERE FROM HIGH DISPERSION SPECTRAL DIFFRACTION AND REFRACTION OF RADIO WAVES TO STUOY STUDY OF ABUNDANCE OF CARBON DIOXIDE. OXYCEN AND PLANETARY ATMOSPHERE A65-29491 WATER A65-25226 THO-FREQUENCY BISTATIC RADAR-OCCULTATION TECHNIQUE TO INVESTIGATE PLANETARY ATMOSPHERES ATMOSPHERE OF MERCURY. USING DIFFERENTIAL A65-31267 POLARIZATION EFFECT AN0 BRIGHTNESS TEMPERATURE MEASUREMENTS A6533300 COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE AND IONOSPHERE OF MARS INCLUOING DENSITY. HYDROGEN MOLECULES IN ASTROPHYSICS TEMPERATURE. SCALE HEIGHT. ETC A65-36328 NASA-CR-57156 N65-18918

RADIO AND RADAR ASTRONOMY STUDIES OF LUNAR AND FI)IU(. T- Y. PLANETARY ATMOSPHERES AN0 SURFACES. AND RADAR AERODYNAMIC BRAKING TRAJECTORIES FOR MARS ORBIT STUDIES OF SUN AND INTERPLANETARY MEDIUM ATTAINHENTI GIVING ENTRY CORRIDORS FOR LIFTING NASA-CR-57184 N65-18944 VEHICLES AIAA PAPER 64-478 A65-28839 BISTATIC RADAR-OCCULTATION METHOD FOR PLANETARY ATMOSPHERE STUDY FIRSOFF. V. A. NASA-CR-57178 N65-18946 POSSIBLE ALTERNATIVE CHEMICAL ELEMENTS AND COMPOUNDS SUITABLE FOR PROLONGED BIOUOLECULAR METHOO FOR STUDY OF PLANETARY IONOSPHERES BASED EVOLUTIOW AND CHEMICAL SELECTION ON NONTERRESTRIAL ON RADIO WAVE PROPAGATION BETWEEN EARTH AND TVPE PLANET A65-27098 SPACECRAFT NASA-CR-64460 N65-32199 FISCIWW. F- F. ATMOSPHERIC PRESSURE AND TEMPERATURE BELOW 24 KM RADIO AN0 RADAR ASTRONOMY - LUNAR AND PLANETARY USING SATELLITE MEASUREMENTS OF ATMOSPHERIC LIGHT IONOSPHERESt ATMOSPHERES* AND SURFACES. AND REFRACTION FROM GIVEN STARS A6534959 RADAR STUDIES OF SUN AND INTERPLANETARY MEDIUM NASA-CR-61795 N66-1-09 FJELDBO. 6- MARS ATMOSPHERE AND IONOSPHERE MEASUREMENTS USING RADIO AND RADAR ASTRONOMICAL STUOIES ON LUNAR AND 2300-HC TRMETRY SIGNAL FROM MARINER IV PLANETARY IONOSPHERES AN0 ATMOSPHERES. AN0 SOLAR SPACECRAFT OCCULTATION EXPERIMENTS ACTIVITY A6526719 NASA-CR-7 1090 N66-19528 DIFFRACTION AND REFRACTION OF RADIO WAVES TO STWY MARS ATMOSPHERIC MOOELS BASED ON MARINER IV PLAIIETARY ATMOSPHERE A65-29491 OCCULTATION EXPERIMENT NASA-CR-74152 N66-23493 TWO-FREQUENCY BISTATIC RADAR-OCCULTATION TECHNIQUE TO INVESTIGATE PLANETARY ATMOSPHERES EVANS. 0. c. U V REFLECTIVITY OF MARS ANALYZE0 FROM SPECTROGRAMS OBTAINED ON AEROBEE ROCKET COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE A65-35583 AN0 IONOSPHERE OF MARS INCLUDING DENSITY. TEMPERATURE. SCALE HEIGHT. ETC A65-36328 AEROBEE ROCKET MEASUREMENTS OF MARS ULTRAVIOLET REFLECTIVITY - PLANETARY ATMOSPHERIC MODEL BISTATIC RAOAR-OCCULTATION METHOO FOR PLANETARY NASA-TM-X-56654 N66-22239 ATMOSPHERE STUDY NISI-CR-57178 . N65-18946 EVANS. 0- E- LUNAR AN0 PLANETARY ENVIRONMENTS USE0 BY NASA BISTATIC RADAR METHODS USED TO STUDY PLANETARY MANNED MISSION PLANNING AND DESIGN CONSIOERING IOWOSPHERES AND SURFACES RAOIATIVE* TOPOGRAPHICAL AN0 ATMOSPHERIC FEATURES NASA-Ut-62823 N65-24310 A6522135 METHOD FOR STUDY OF PLANETARY IONOSPHERES BASED PLANETARY ENVIRONMENTAL DESICN DATA FOR FUTURE ON RADIO WAVE PROPA6ATION BETHEEN EARTH AN0 MANNED SPACE FLIGHTS TO VENUS AN0 MARS SPACECRAFT NASA-SP-3016 N65-23799 NASA-CR-64460 N65-32199

MARS ATMOSPHERIC MODELS BASE0 ON MARINER IV F OCCULTATION EXPERIMENT FAIRBAIRN* A. NASA-CR-74152 N66-23493 MIXTURES OF NITROGEN AN0 CARBON DIDXIDE GASES

I45 PERSONAL AUTHOR INDEX

FJELDBO* W. C. GILBERT. L- MARS ATMOSPHERIC MODELS BASED ON MARINER IV NORMAL SHOCK WAVE AND STAGNATION POINT SOLUTIONS OCCULTATION EXPERIMENT FOR FOUR VENUSIAN ATMOSPHERIC AN0 CHEMICAL NASA-CR-74152 N66-23493 MODELS R6 4 5 D6 5 N65-13519 F06AROLI. R. P. MASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE EILLESPIE. R. W. FOR CHEMICAL COMPOSITION STUDY OF MARTIAN INTEGRATION OF TERRESTRIAL AND PLANETARY ATMO SPHER E ENVIRONMENT SENSING N65-33556 NASA-CR-71307 N66-23779 6IUMRRO. C- FOLEY. R. T. TERRESTRIAL MICROORGANISM SURVIVAL AND GROWTH ON POLAROGRAPHIC OXYGEN ANALYZER FOR OBTAINING DATA SPECIMENS OF EUPHORBIA XYLOPHYLLOIOES IN AMMONIA ON MARS ATMOSPHERIC COMPOSITION METHANE HYDROGEN-RICH ATMOSPHERES NASA-CR-57085 N65-18098 A65-23486

FOX. N- SEE0 GERMINATION OF COMMON PLANT SPECIES IN PLANETARY ATMOSPHERIC SIMULATION IN SUPERSONIC RAREFIED NITROGEN ATMOSPHERES SIMULATING WINO TUNNELS WITH CARBON DIOXIDE ADDED TO DRIED EXTRATERRESTRIAL ENVIRONMENT A65-32416 AIR WORKING FLUID NASA-CR-68792 N66-13555 SURVIVAL AN0 GROWTH OF TERRESTRIAL MICROORGANISMS IN AMMONIA-RICH ATMOSPHERES SUPPORTING POSSIBILITY FRANCIS. C. E- OF ORIGIN AN0 EXISTENCE OF LIFE ON JUPITER ELECTROMAGNETIC PROPAGATION CHARACTERISTICS OF A65-81287 VENUS AND MARS DERIVE0 FROM ATMOSPHERIC DATA A66-16436 6MO. T. OUTGASSING PROCESSES ON MOON AND VENUS, USING FRANK. L- A. EARTH ANALOGY A65-33290 ABSENCE OF ELECTRONS IN MARS ATMOSPHERE AN0 IMPLICATIONS THEREOF GOLOSTEIN. HI W. NASA-CR-64870 N65-33919 MASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLL FOR CHEMICAL’COMPOSITION STUDY OF MARTIAN FRASER. R. S. ATMOSPHERE OUTWARD FLUX AN0 INTENSITY OF SCATTERED RADIATION NASA-CR-71307 ~66-23779 FOR TOP OF RAYLEIGH ATMOSPHERE LYING ABOVE SMOOTH WATER SURFACE THAT REFLECTS RADIATION ACCORDING TO 600OY. RI H- FRESNEL LAW COMPOSITION OF MARTIAN ATMOSPHERE, USING AIAA PAPER 65-664 A65-35111 POLARIMETRIC OBSERVATIONS 165-33301

GROUND SPECULAR REFLECTION MODIFICATION OF MARS ATMOSPHERE PROBLEMS RELATED TO CHEMICAL LIGHT SCATTERING FROM PLANETARY ATMOSPHERE TOP COMPOSITION AN0 PHYSICAL PROPERTY NASA-CR-57740 N65-20758 A65-00869

LIGHT SCATTERING AND POLARIZATION IN PLANETARY PLANETARY UPPER ATMOSPHERES - PRIORITY RATINGS FOR ATMOSPHERE EXPERIMENTS, TYPES OF MEASUREMENTS FOR NASA-CR-70943 ~6-20077 RECOMMENDED PROGRAM, AN0 ANNOTATED BIBLIOGRAPHY N66-14331 FRIEQHAN. H. L- MASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE 60Y. 6. FOR CHEMICAL COMPOSITION STUDY OF MARTIAN MARINER IV PHOTOGRAPHS OF PLANET MARS NOTING ATMOSPHERE TOPOGRAPHY. SOIL COMPOSITION, ATMOSPHERIC NASA-CR-71307 N66-2 3119 PHENOMENA. POLAR CAP MIGRATIONI RADIATION, ETC A66-20660

G 6RAYs L- 0. 6A6EN-TORN. V. A. CARBON DIOXIDE ABSORPTION BANDS IN MARS DEGREE OF POLARIZATION OVER CYTHEREAN DISK FOUNO ATMOSPHEREI TRANSMISSION, FUNCTION OF CARBON TO INCREASE WITH DISTANCE FROM CENTER OF PLANET DIOXIDE AMOUNT AN0 EFFECTIVE SURFACE PRESSURE A65-25694 AIAA PAPER 66-147 A66-19072

GARAZW, V. 1. GREENFIELD. S. M. OPTICAL THICKNESS, SCATTERING AN0 AEROSOL PARTICLE FEASIBILITY AN0 DESIGN OF BALLOONS FOR EXPLORATION CONCENTRATION OF MARS ATMOSPHERE IN UV SPECTRUM OF SURFACE AN0 ATMOSPHERE OF MARS A65-19668 N65-34830

GARRIOTTI 0. K- 6REENSPANs J- A. TWO-FREPUENCY BISTATIC RADAR-OCCULTATION TECHNIQUE RECENT DETERMINATIONS OF COMPOSITION AN0 SURFACE TO INVESTIGATE PLANETARY ATMOSPHERES PRESSURE OF MARS ATMOSPHERE A65-31267 NASA-CR-298 N65-33835

METHOD FOR STUDY OF PLANETARY IONOSPHERES BASED 6RIN6AUZ. K. I- ON RADIO HAVE PROPAGATION BETWEEN EARTH AND INTERPLANETARY GAS AND IONOSPHERES OF PLANET - SPACECRAFT INVESTIGATION USING CHARGED PARTICLE TRAPS NASA-CR-64460 N65-32199 N65-16468

GEORGIEV. S. GROSS. F- R- DENSE CARBON REINFORCED AND LOW DENSITY CHAR- VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE FORMING RESIN ABLATION MATERIALS FOR EARTH, MARS INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AND OF AND VENUS ATMOSPHERE ENTRY A65-15619 STATIC EPUILIBRIUM WITHIN KAPLAN ATMOSPHERE A65-19505 GIBSON. J. E. VENUS RADIATION AT 13.5 MM WATER VAPOR LINE AND GROSS. 5. HI PLANETARY BRIGHTNESS VARIATION WITH SOLAR MARS UPPER ATMOSPHERE THERMAL STRUCTURE FROM ILLUMINATION PHASE A66-20111 SPECTROSCOPIC MEASUREMENTS AN0 MARINER IV OCCULTATION EXPERIMENT A66-23660 GILBERT. 0. L. EVOLUTION OF THE ATMOSPHERES OF THE EARTH AND 6RUNOTNERs H- J- PLANElS A65-80370 PNEUMATIC SURFACE SAMPLING DEVICE FOR USE IN SIMULATED MARS ENVIRONMENT

1-46 NASA-CR-70937 N66-20080 IRON 55 X-RAY SOURCE A65-23098

GIUSZUYNSKI. J.. 5. WRYLEWICZ+ E. J. SIWLATION OF HEAT TRANSFER ENVIRONMENTS OF SPACE RESPONSE OF MIQIOORWISM TO SIMULATE0 MARTIAN VEHICLE EWERIN6 PLANETARY ATMOSPHERE WITH ENVIRDNMENT INVESTIGATED* USING CULTURE SUPERORBITAL VELOCITY COLLECTIONS AN! SOIL SAMPLES A65-30676 R64SS1173 N65- 15600 -. n. w. HYPERVELOCITY Hk4T TRANSFER STUDIES IN SIMULATED NEI6HT AND ENERGY REPUIREMENTS OF VEHICLE SYSTEMS PLANETARY ATMafPHERES FOR “ME0 EXPLORATION OF MARS NASA-CR37508 N65-19864 AIU PAPER 64-403 A65-33549

GRIVNAK. Do A. HAYS. c. e. IWFnARFb SiYCTROSCOPY STUDIES TO DETERMINE COLLISIoI(U. TRNtSITIOW BETWEEN LONER ATWSf‘iiERE ABSORPTION BY CARBON OIOXIOE BETWEEN 8.000 AMI AND COLLISIONLESS EXOSPHERE ANALYZED* USING 10~000/CM IN 1 TO 1-25 MICRON REGION INTEGRAL FORMULATION OF BOLTZMA“ EPUITION AMI U-3200 .- . N66-22465 COLLISION MODELS A6620882 HERON, a. H SHOCK TUBE 6AS DYNAMIC CHARTS SUITABLE FOR MARS HADDOCK. F. T, ATMOSPHERE GALACTIC AN0 PLANETARY RADIO ASTRONOMY - SOUNOIN6 RAD-TM-65-23 N65-25727 ROCKET LAUNCH. ORBITING TELESCOPE* CARBON-OXYGEN COWLEX PHOTOCHEMISTRYr MARS 1OWOSPHERE. HL1UBEs. 5. TOPSIDE ELECTRON DENSITY* AND NONRIGID BODIES MmEcuLm SPECTROSCOPY IN RELATION TO SOLAR. NASA-CR-70152 N66-16597 PLANETARY. STELLAR. COMETARY AN0 INTERPLANETARY STUDIES 165-18203 SWNOING ROCKET FLIGHT TO MEASURE COSMIC RADIATION INTENSITY AN0 STUDIES OF MARTIAN ATMOSPHERE AMI HLIUOE. I-F. K- IONOSPHERE MASS SPECTROMETER INSTRUMENTATION FOR MARTIAN NASA-CR-74173 1166-23713 ATMOSPHERIC ANALYSIS NASA-CR-60760 N65-172 16 HAS€& C. A. RESPONSE OF MICROORGANISM TO SIMULATE0 MARTIAN MASS SPECTROMETER USING HETEROENERSETIC ION ENVIRONMENT INVESTIGATEDI USING CULTURE SWRCE WITHOUT OEFLECTIaJ FIELD FOR MARTIAN COLLECTIONS AND SOIL SAMPLES A65-30676 ATMOSPHERE ANALYSIS NASA-CR-71916 N66-23797 HALPERT. 6. POLAROGRAPHIC OXYGEN*ANALYZER FOR OBTAINING DATA nmm. R. 0. ON MARS ATMOSPHERIC COMPOSITION SOME FORMS OF LIFE FOUND ON EARTH WHICH CAN NASA-CR-57085 N65-18098 SURVIVE CWOITIONS THOUGHT TO EXIST ON MARS A65-81013 HANEL. R. A. MARS SURFACE AND ATMOSPHERE CHARACTERISTICS FROM nmE. R. THERMAL EMISSION SPECTR~~MEASUREM~T BY ATMOSPHERIC CIRCULATION AROUND PLANETS OF JUPITER INFRARED INTERFEROMETER ON PLANETARY FLYBY AND SATURN N66-14332 SPACECRAFT NASA-TM-X-55070 N65-32114 HILLS. n. K. ABSENCE OF ELECTRONS IN MARS ATMOSPHERE AM0 EQUILIBRIUM TEMPERATURE DISTRIBUTIONv THERMAL IMPLICATIONS THEREOF EMISSION. AN0 LIMB FUNCTION COMPUTED FOR VENUS NASA-CR-64870 N65-33919 CLOUD COVER MODEL NASA-TM-X-55392 116617231 n1Ls-n. E. TELESCOPE DESIW FOR INTERFEROMETER SPECTROMETER HANET. 6. II. FOR PLANETARY ATMOSPHERE EXPLORATION SPACECRAFT DECELERATION UPON ENTRY INTO MARS N6614107 ORBIT BY AEROOYNAMIC BRAKING. CONSIDERING VEHICLE SHAPE AN0 VELOCITY EFFECTS ON ENTRY HEATIK HINTERECCER~ n. E. AIAA PAPER 64-479 A65-28841 ABSOLUTE INTENSITY MEASUREMENTS IN EXTREME UV AND SOFT X-RAY REGIONS OF SOLAR SPECTRUM “ST. P- L. A65-32654 MARS NITROGEN OXIDES OBSERVE0 AT DIFFERENT WAVELENGTHS. COMPUTIN6 PHOTOCHEMICAL EQUILIBRIA HIfCHtaX. 0. R- POINT AND ROLE IN BLUE HAZE A65-17992 BIOLOGICAL SIGIIIFICANCE OF MARTIAN ATMOSPHERIC COMPOSITIONAL ANALYSISI AND LIFE DETECTION SURFACE PRESSURE Ok MARS ATMOSPHERE REDETERMINED STUDIES OF CHEMICAL FREE ENERGY IN SURFACE FROM ABSORPTION INTENSITY OF CARBON OIOXIDE BY MATTER LONG-PATH AND PHOTOMULTIPLIER DETECTION NASA-CR-67354 N65-36391 A65-35360 HOD6E. P. w. ABSORPTION INTENSITY OF CARBON OIOXIOE BANDS AN0 BOOK ON SOLAR SYSTEM ASTRONOMY ANDSPMX PHYSICS MARTIAN CARBON DIOXIOE ABUNOAIICE AND ATMOSPHERIC INCLUDING CELESTIAL MECHANICS. INTERPLANETARY GAS PRESSURE AS BASE OF OESIGII FOR MARS ENTRY VEHICLE PHYSICS. METEORITES ANO PLANETARY -ATMOSPHERES A65-82273 165-17422

HAMIS. n. J. KOZYREV HYDROGEN EMISSION LINES IN IR PLANETARY RADIATION AN0 ALBEDO EFFECTS ON THERMAL SPECTROGRAMS OF MERCURY NOTING tea€ EMISSION BALANCE OF SPACECRAFT ORBITIN6 MARS AND VENUS 165-23491 NASA-CR-67813 N66-10684 MRCURIAN ATMOSPHERE FROM HIGH OISPERSION SPECTRAL HIMIS* JI W. STUDY OF ABUNDANCE OF CARBON DIOXIDE. OXYGEN AND LUNAR AND PLANETARY ENVIRfflMENTS USE0 BY NASA WATER 1165-25226 MAMNEO MISSION PLANNING AND OESISN CfflSIOERIN6 RAOIATIVE. TOPOGRAPHICAL AN0 ATMOSPHERIC FEATURES HOEWIG. 5. A. A65-22 135 PHYSICAL METHODS OESCRIPTION FOR DETECTION AN0 ANALYSIS OF TENUOUS PLANETARY ATMOSPHERIC HARRISON. F. 0. COMPONENT GASES. ESPECIALLY WATER VAPOR ARGON ABUNDANCE IN MARTIAN ATMOSPHERE DETECTOR* NASA-CR-70934 N66-19901 USING CYLINDRICAL IONIZATION CHAMBER CONTAININ6

1-47 HDSAN. J. Sa, JR. PERSONAL AUTHOR INDEX

HDSAN. J. 5.. JR. APPROXIMATE SOLUTION OF DIFFUSE REFLECTION AND MARTIAN ATMOSPHERIC HEATING FROM SOLAR RADIATION TRANSMISSION OF LIGHT BY FLAT LAYER OF PLANETARY ABSORPTION IN UV AND VISIBLE BY OXYGEN AN0 OZONE ATMOSPHERE WITH TRUE ABSORPTION AND IN NEAR IR BY CARBON DIOXIDE, NOTING VERTICAL Ab5-10975 DISTRIBUTION OF GASES AND ABSORPTION Ab5-23521 OPTICAL THICKNESS, SCATTERING AN0 AEROSOL PARTICLE CONCENTRATION OF MARS ATMOSPHERE IN UV SPECTRUM HOLLAND, H. 0- Ab5-19668 HISTORY OF TERRESTRIAL ATMOSPHERE AN0 DATA ON CHEMICAL COMPOSITION OF VENUS ATMOSPHERE DIFFERENCE BETWEEN VALUES FOR ATMOSPHERIC PRESSURE Ab5-33292 AT MARTIAN SURFACE WHEN OBTAINED BY PHOTOMETRY OR BY SPECTROSCOPY, DUE TO NONCONSIOERATION OF LIGHT CHEMICAL EVOLUTION OF TERRESTRIAL AN0 CYTHEREAN SCATTERING BY AEROSOL PARTICLES Abb-19331 ATMOSPHERES Ab5-80090

HOLMAN. F. S. OPTICAL PARAMETERS OF MARS ATMOSPHERE AN0 SURFACE SPHERICAL SEMIPASSIVE PROBE FOR DENSITY/ALTITUOE FROM PHOTOMETRIC DATA FOR SPHERICAL AND ELONGATED AND PRESSURE/ALTITUOE PROFILE OF PLANETARY SCATTERING INOICATRICES A 66- 19337 ATMOSPHERES, NOTABLY MARS AN0 VENUS Ab5-19520 IATSENKD. S. P. STRELKOV THEORY OF RADIO EMISSION FROM VENUS HOLMES-SIEDLE, A- 6- ATTRIBUTES HIGH TEMPERATURE RADIATION TO EXISTENCE AN0 DETECTION OF LIFE FORMS IN RADIOACTIVE HEATING OF PLANETARY SURFACE UNIVERSE AN0 PLANETARY SYSTEM, AN0 LIFE SUPPORT Abb-19324 IN MANNED SPACE TRAVEL Nbb-19829 INN. E. C. Y. HOLZER, R. E. CARBON DIOXIDE- R-BRANCH LINES OF 5 MU SUB 3 BAND ATMOSPHERIC ELECTRICAL STUDIES OF OTHER PLANETS BY FROM INTEGRAL OF ABSORPTION COEFFICIENT OFAb 6- 15200 STUDIES OF ELECTROMAGNETIC RADIATION BY SUCH MARTIAN ATMOSPHERE PLANETS Ab5-34745 INWYE, M- HDRDWITZ, Ne Ha FLOW FIELD AROUND SPHERICAL BLUNT BODIES IN GAS MARTIAN LIFE IN LIGHT OF MARINER IV DATA ON EQUILIBRIUM MIXTURES RESEMBLING VARIOUS ADVERSE ATMOSPHERIC COMPOSITIONI TEMPERATURE AND PLANETARY ATMOSPHERES - INVERSE METHOD OF RAD1AT ION Abb-21740 FLOW FIELD CALCULATION NASA-TN-0-2780 Nb5-22367 EXISTENCE AN0 DETECTION OF LIFE ON MARS Abb-80972 ISAACS. J- 0- OCEANOGRAPHIC AN0 RELATED OBSERVATIONS FROM HORTDN. T. E. SATELLITE PHOTOGRAPHY Nb5-30357 ATMOSPHERIC ARGON EFFECT ON HYPERSONIC STAGNATION POINT CONVECTIVE HEAT TRANSFER, USING ARC-HEATED IUDOVICH. L. A. SHOCK TUBE SIMULATING FLIGHT VELOCITIES UP TO POSITION DETERMINATION OF EPUATORIAL BOUNDARY OF 34,000 FPS ABNORMALLY HIGH NOCTURNAL ATMOSPHERIC IONIZATION AIAA PAPER 66-29 Abb-17891 FOR VARIOUS LEVELS OF PLANETARY MAGNETIC ACTIVITY Abb-19793 HOUSE, F. 6. ATMOSPHERIC CIRCULATION AN0 CLIMATOLOGY OF VENUS AN0 MARS J NASA-CR-71627 Nbb-21767 JACKSON. F- LIFE ON MARS - CONOITIONSI POSSIBLE TYPES OF HOVIS. W. A.r JR- ORGANISMS AN0 THEORIES OF ADVANCED FORMS OF LIFE I R REFLECTIVITY OF POLYHYORATED FERRIC OXIDE Abb-80582 MEASURED IN CONNECTION WITH MARTIAN SURFACE HYDRATION DETERMINATION FROM REFLECTION SPECTRA JASTRDY. R. Ab5-23487 CURRENT PICTURE OF ORIGIN AN0 DEVELOPMENT OF PLANETARY ATMOSPHERES. BEGINNING WITH THEORY OF HUNTEN. D. M. STELLAR EVOLUTION Ab5-26914 SURFACE PRESSURE AND CARBON DIOXIDE CONTENT OF MARTIAN ATMOSPHERE, COMPARING POLARIMETRIC, TEMPERATURE, DENSITY AN0 GRAVITATIONAL ESCAPE ON PHOTOMETRIC AN0 SPECTROSCOPIC METHODS MARS. MERCURY, JUPITER AND VENUS ATMOSPHERES Ab5-26212 Abb-15759

HUSS, A. PLANETARY ATMOSPHERE COMPOSITION, TEMPERATURE, AN0 EVOLUTION OF GENERAL CIRCULATION PATTERNS IN PRESSURE OF MARS, VENUS, AND JUPITER PLANETARY ATMOSPHERES NASA-TM-X-56223 Nb5-20799 AFCRL-65-350 Nb5-30247 RECENT SPACE RESEARCH IN PHYSICAL SCIENCES - NUMERICAL INTEGRATION OF VARIOUS PLANETARY LITERATURE SUMMARY AN0 DISCUSSION CIRCULATION PATTERNS IN QUASI-GEOSTROPHIC MODEL NASA-TM-X-51903 Nb5- 29456 ATMOSPHERE INCLUDING WATER VAPOR, DIABATIC HEATING, AND SURFACE FRICTION JENISCH. Y-t JR. AFCRL-65-771 Nbb-16207 BIBLIOGRAPHY OF DOCUMENTS ON LUNAR. PLANETARY. AND SPACE ENVIRONMENTS IN RELATION TO FLIGHT CALCULATIONS FOR PUASI-GEOSTROPHIC PLANETARY MECHANICS AN0 AERODYNAMICS OF SPACE TRAVEL CIRCULATION ATMOSPHERE WITH DIABETIC HEATING AND NASA-CR-60469 Nb5- 16086 SURFACE FRICTION Nb6- 16208 JOHNSON. F- S. PLANETARY CIRCULATION PATTERNS FOR INTEGRATED TWO- MARTIAN IONOSPHERIC OBSERVATIONS MADE BY MARINER LEVEL QUASI-GEOSTROPHIC MODEL ATMOSPHERE IV INTERPRETED IN TERMS OF MODEL SHOW ATMOSPHERE INCLUDING YATER VAPOR Nbb-16209 CONSISTS MAINLY OF CARBON DIOXIDE, LOU TEMPERATURE AN0 NO THERMOSPHERE 666- 16404

I JONES. 0- E- IANDVITSKIIs E. G- MARINER I1 MICROWAVE RADIOMETER EXPERIMENT TO PHOTOMETRIC DETERMINATION OF MARTIAN ATMOSPHERE STUDY VENUS SURFACE AN0 ATMOSPHERE AND SURFACE OPTICAL THICKNESS AN0 ABSORPTION AS NASA-CR-69916 Nbb- 16 151 FUNCTIONS OF WAVELENGTHS Ab5-18974

1-48 . PERSONAL AUTHOR 1II)EX UII?M. 6. P.

JORGWSW. L. H. COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE APPROXIMATE AND CHARACTERISTICS METHODS TO PREDICT AN0 IONOSPHERE OF MARS INCLUDING DENSITY. EFFECT OF GAS COMPOSITION 011 FORCES AND STATIC TEMPERATURE. SCALE HEIGHT. ETC A65-36328 STABILITY OF PLANETARY ENTRY CONFIGURATIONS IN AIR AND ASSUME0 MARTIAN ATMOSPHERES MARINER IV OCCULTATION EXPERIMENT ON MARTIAN AIM PAPER 65-318 A65-29766 ATMOSPHERE. USING AMPLITUDE AND FREPUENCY CHANGES OF TRACKING AND TELEMETRY SIGNAL K AIAA PAPER 66-148 A6617900 KAMIYMA. n. KOESIEI. n. TEMPERATUIE DISTRIBUTIONS COMPOSITION+ AND PLANETARY ATMOSPHERIC SIMULATION IN SUPERSONIC IONIZATION OF MARS ATMOSPHERE N66-19930 WIMD TUWELS WITH CARBON DIOXIDE ADDED TO DRIED AIR WORKING FLUID KAPLIII. L. 0. NASA-CR-68792 N66-13555 MARINER I1 RADAR AN0 RAOIOMETRIC OBSERVATIONS OF VENUS WRING 1962 CONJUNCTION - PHYSICAL DATA KOIKSIIOFF. N- M- NASA-CR-56851 N65-22203 LINEAR WLARIZATIONt PLANETARY ROTATIOW OF POLARIZATION. LUNAR OCCULTATION AM0 INTENSITY KAPPRAFF. J- SPECTRUM OF JUPITER DECIMETRIC EMISSIONS ALTERNATE MISSION PROFILES FOR MANNED MARS A65-21042 LANDING NASA-TN-0-3161 N66-14703 KOWDILlrTIEV. I. I- CHAMBER AN0 ELECTRICAL CIRCUIT USED TO SIMULATE KATTHIFELD. 6. N- MARTIAN CONDITIONS FOR MICROBIOLOGICAL PHENOMENON OF VOLCANIC ACTIVITY ON MARS PLANET INVESTIMTIONS A65-25099 NASA-TT-F-410 N66-14057 NARTIAN CDNOITIONS SIMULATED FROM ASTROPHYSICAL KATZt 6. 0. DATA FOR MICROBIOLOGICAL INVESTIGATIONS SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST A65-30682 PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE. TRACKING. COST AN0 SCHEDULE KORNt A- 0.. JR. AIM PAPER 65-219 A65-17398 PAPERS PRESWTEO AT SCIENTIFIC BALLOON SYMPOSIW ON BALLOON DESIGN. MATERIALS. STRESS KELLERMANN. K. 1- STUDIES. INSTRUIIENTATION~METEOROLOGY. LOCATING SURFACE TEMPERATURE DISTRIBUTION OF MERCURY BASED SYSTEM. AND PLANETARY EXPLORATION APPLICATIONS ON MEASUREMENTS OF MEAN DISK TEMPERATURE OVER WIDE lrFCRL-65-466 N65-34804 RANGE OF PHASE ANIXES A65-22205 KOUKKOT. 0- V. KENNET. Ha RADIO ASTRONWICAL OBSERVATIONS OF VENUS WITH ORBITER INJECTED STERILIZED BALLISTIC SKIPOUT HIGH RESOLVING POWER CAPSULE FOR IN FLIGHT MARTIAN STRATOSPHERE MLL-TRANS-936 N65-17990 MEASUREMENTS. USING NONABLATIVE HEAT WIELD AND OUTSIDE ATMOSPHERIC PROPULSION MANEUVERS KOVU. 11 K- AIM PAPER 65-23 A65-15944 BRIGHTNESS DISTRIBUTION ALONG VISIBLE RADIUS OF MARS, EXAMINING ATMOSPHERIC SCATTERIWG EARTH REENTRY SIMULATION OF PLANETARY ENTRY A65-18971 ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF MARS AN0 VENUS TYPE BRIGHTNESS DISTRIBUTION IN MARGINAL ZONE OF MARS AIM PAPER 65-216 A65-16606 USED TO DETERMINE ATMOSPHERIC ABSORPTION ~65-189r2 SPHERICAL SEMIPASSIVE PROBE FOR DENSITY/ALTITUDE AND PRESSURE/ALTITUDE PROFILE OF PLANETARY PHOTOMETRIC EXAMINATION OF BRIGHTNESS OISTRIBUTION ATMOSPHERES. NOTABLY MARS AND VENUS ALONG DISK OF MARS A6619332 A65-19520 SPECTROPHOTOMETRIC OBSERVATIONS OF MARS KERN- R, J. N65-18512 SIMULATED MARTIAN ENTRY CDNOITIDNS IM EARTH TEST PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE. PHOTOMETRIC AND POLARIMETRIC STUDIES ff MARS AND TRACKING. COST ANO SCHEDULE VEMUS ATMOSPHERES - AEROSOLS AIM PAPER 65-219 A65-17398 NASkTT-F-989B N66-23536

KH*IKIN. 5, E. PHOTOELECTRIC MEASUREMENT OF BRIGHTNESS RADIO ASTRONOMICAL OBSERVATIONS OF VENUS WITH DISTRIBUTION IN LIMB ZONE OF MARS HIGH RESOLVING POWER NASA-TT-F1001B N66-23538 NRL-TRANS-936 N65-17990 KRASE. Y. H. KHIZHNIAKOV. 1. P. MARS ENVIRONMENTAL MEASUREMENTS IN SUPPORT OF OPTICAL THICKNESS OF JUPITER ISOTHERMAL FUTURE HAMMED LANDING EXPEDITIONS ATMOSPHERE ASSUMING IT CONSISTS OF HYDROGEN. NASA-CR-62872 1365-24355 METHANE AND AMMONIA A65-30237 KRAUS. 6. L- KLARK. 6. 0. PLANETARY ENVIRONMENTAL DESIGN DATA FOR FUTUIE POLARIZATION AND BRIGHTNESS TEMPERATURE MANNED SPACE FLIGHTS TO VENUS AND MARS DISTRIBUTION MEASUREMENTS OF VENUS IN 10.6 CM NASA-SP-3016 N65-23799 WAVELENGTH ST-RA-LPS-10334 N66- 11 136 KRIIIIGIS. 5. M- ABSENCE OF ELECTRONS IN MARS ATMOSPHERE AND KLEIN. M. J. IMPLICATIONS THEREOF BRIGHTNESS TEMPERATURE MEASUREMENTS OF MARS AT NASA-CR-64670 N65-33919 3-75 CM FROM FEBRUARY TO JUNE 1965 1166-16768 WW. MI A- Low6 LIFETIME ORBITS AWT MARS AFFECTED BY KLIORE. A- J. ATMOSPHERIC DRAG. SOLAR GRAVITATIONAL MARS ATMOSPHERE AND IONOSPHERE MEASUREMENTS USING PERTURBATIONS. PLANETARY OBLATENESS Am OTHER 2300-MC TELEMETRY SIGNAL FROM MARINER IV PERTURBATIONS SPNECRAFT OCCULTATION EXPERIMENTS AIAA PAPER 66-35 A66- 16987 A65-26719 KUICER. 5- P- IR SPECTRA OF MARS USE0 TO DETERMINE ITS

1-49 KUTUZA. 8. 6- PERSONAL AUTHOR INDEX

ATMOSPHERIC CONSTITUENTS A65-18 47 6 LANMDIS. Y- E. EQUATIONS OF HOTION FOR ELASTIC BODIES ENTERING CALIBRATION OF MARTIAN SPECTRA USING LABORATORY PLANETARY ATMOSPHERE AT HYPERSONIC VELOCITIES SPECTRA OF PURE CARBON DIOXIDE AND IN COHBINATION N66-21667 WITH NITROGEN AND ARGON A65- 18 47 7 LASCODY. 0. N. LABORATORY SPECTRA FROH LEAD SULFIDE SPECTROHETER WEIGHT AND ENERGY REQUIREMENTS OF VEHICLE SYSTEHS FOR TESTING PRESENCE OF MINOR COINSTITUENTS IN FOR HANNEO EXPLORATION OF HARS PLANETARY ATMOSPHERES A65-18479 AIAA PAPER 64-403 A65-33549

SPECTRUM. COMPOSITION AN0 SURFACE PRESSURE. CARBON LATTERELL. R. DIOXIDE ABUNDANCE, NITROGEN DIOXIDE TESTS, AND SEE0 GERHINATION OF COMMON PLANT SPECIES IN STRUCTURE OF ATMOSPHERE ON HARS RAREFIED NITROGEN ATHOSPHERES SIMULATING NASA-CR-60264 N65-15223 EXTRATERRESTRIAL ENVIRONMENT A65-32416

PHOTOGRAPHIC SPECTRA OF PLANETARY ATMOSPHERE GASES LEEEOEVAr 1- I. OF MARS AN0 JUPITER SPECTRAL REFLECTING POWER CURVE FOR HARTIAN DISK Ab608352 N65-16776 CENTER CDHPARED WITH TERRESTRIAL EQUIVALENT A6619333 KUTUZA. 8. 6. RADIO EMISSION OF SATURN ON WAVELENGTH OF 8 HM LEEEOINSKII~A- I- COHPARED WITH VALUES OBTAINED AT OTHER WAVELENGTHS RADIO NOISE EMISSION FROH VENUS SURFACE EXPLAINED A65-35841 IN TERMS OF GLOW DISCHARGE A6617 174

VENUS CLOUD LAYER AND BRIGHTNESS TEMPERATURE FROM LEEO. 6. R- RADIOHETRIC MICROWAVE OBSERVATIONS FROM NOCTURNAL FINAL REDUCTION OF OBSERVATIONS OF SPORADIC SIDE OF PLANET A66- 20 112 OUTBURSTS IN DECAMETRIC REGION OF RADIO SPECTRUH OF JUPITER DURING 1961 AND 1962 SUPERCOOLED WATER DROPLETS HYPOTHESIZED IN VENUS A6521855 CLWO LAYERt BASED ON RADIOMETRIC OBSERVATION IN SHF RANGE A66-23503 LECUYER. J - CHEHICAL COMPOSITION AN0 TEMPERATURE IN MOOEL OF KUZMIN* A. 0. UPPER ATMOSPHERE OF MARS A65-27569 COLD ABSORBING ATMOSPHERE HODEL OF VENUS BASE0 ON CENTIHETER AND HILLIMETER EMISSION SPECTRUM HODELS OF HARTIAN THERHOSPHERE WITH CONSTANTS A65-19676 AN0 BOUNDARY VALUES IN HYDROSTATIC AN0 HEAT-FLUX EQUATIONS N65-28713 BRIGHTNESS TEMPERATURE OF RADIO EHISSION FROM VENUS . A65-24803 LEDEREER6. J- MARTIAN LIFE DEPENDS ON CHEHOGENY. BIOGENYt DIFFERENTIAL POLARIZATION AND DISTRIBUTION OF COGNOGENY, SIMILARITY AN0 OISSIMILARITY TO EARTH RAOIOEHISSION OF DIFFERENT PARTS OF VISIBLE DISK AND PHYSICAL AND CHEMICAL ENVIRONMENT OF VENUS MEASURED BY INTERFEROHETER A65-28200 A65-35268 LEMEER6r E. BRIGHTNESS TEHPERATURE HEASUREHENTS ON ENGINEERING BREADBOARD HODEL OF MICROORGANISM ILLUMINATED SIDE OF VENUS AT 10.6 CM CHALLENGES DETECTION DEVICE FOR MARS LANDING APPLICATIONS TROITSKI THEORY OF PLANETARY RADIATION EMISSION NASA-CR-742 14 N66-23787 A66-19457 LENOELE. J. VENUS ATMOSPHERE HODEL OF COLD ATHOSPHERE SPECTRAL DISTRIBUTION OF ALBEDO AN0 LUHINANCE AT SHORT WAVE ABSORPTION EFFECT ON LOW BRIGHTNESS CENTER OF DISK FOR DIFFUSING AND ABSORBING TEHPERATURE OF RADIO EHISSIONS PLANETARY ATMOSPHERE A66-17247 NASA-TT-F-9663 N65-21005 LEOVY. c. OBSERVED RADIATION SPECTRUM OF VENUS ATMOSPHERE VARIATION OF IR EMISSION FROM MARS SURFACE WITH WITH DECREASE IN BRIGHTNESS TEMPERATURE MARS LOCAL TIME IN TERHS OF DIURNAL TEMPERATURE EXPLAINED BY ABSORPTION IN RELATIVELY COLD VARIATIONSs INCLUDING ATHOSPHERE EFFECT. RESULTS SURROUNDING IONOSPHERE N65-24526 SUGGEST LOW THERMOCONOUCTIVITY A66-21201 ANALYTICAL RELATIONS CONNECTING BRIGHT TEMPERATURE THEORY OF DIURNAL VARIATION OF MARTIAN SURFACE OF RADIO EHISSION OF VENUS COVERED BY ABSORBING TEMPERATURE - GROUND AN0 ATHOSPHERE OF MARS ATMOSPHERE WITH PHYSICAL PARAMETERS NASA-CR-63278 N65-26075 N65-27226 EARTH- MARS COMPARISON OF VERTICAL TEMPERATURE POLARIZATION AND BRIGHTNESS TEMPERATURE DISTRIBUTION AND HEAT BALANCE IN ATHOSPHERE DISTRIBUTION MEASUREHENTS OF VENUS IN 10.6 CM NASA-CR-68992 N66-14280 WAVELENGTH ST-RA-LPS-10334 N66-11138 LEVIN. 6- M- ENTRY VEHICLE DESIGN FOR PLANETARY EXPLORA,TION USING NONSURVIVING NEEDLE-NOSED PROBE FOR DATA KVIZDVAI J. COLLECTION ON HARS ATHOSPHERE COMPOSITIDNI CLOSE APPROACH OF METEOR STREAMS AND COHETS TO PRESSURE AND DENSITY MARS ORBIT AND RELATION TO BLUE CLEARING OF AIAA PAPER 65-493 A65- 32 32 1 ATHOSPHERE A65- 15342 LEVINEr P- DENSE CARBON REINFORCED AND LOW DENSITY CHAR- L FORMING RESIN ABLATION MATERIALS FOR EARTHS MARS LA6RDNEr A. H. AND VENUS ATMOSPHERE ENTRY A65-15619 EXPECTED DIFFRACTION EFFECTS ON ELECTROHAGNETIC RADIATION FROH MARINER IV DUE TO M4RTIAN LEVY. 6- S. ATMOSPHERE AND OCCULTATION A66-16039 HARS ATMOSPHERE AND IONOSPHERE MEASUREHENTS USING 2300-MC TELEHETRY SIGNAL FROM MARINER IV LANOSTRDHr W. 6. SPACECRAFT OCCULTATION EXPERIHENTS SYSTEMS DESIGN FOR UNMANNED SPACE HISSION TO A65-26719 EVALUATE HARS ENVIRONHENT NASA-CR-69997 N66-16248 COHERENT RADIO TRANSMISSION TO PROBE ATMOSPHERE AND IONOSPHERE OF HARS INCLUDING DENSITY, TEHPERATUREI SCALE HEIGHTt ETC A65-36328

1-50 PERSONAL AUTHOR INOEX ((c KENLIE. 1. I..

MARINER IV OCCULTATION EXPERIMENT ON MARTIAN ATMOSPHERIC CIRCULATION AND CLIMATOLOGY OF VENUS ATMOSPHERE. USING AMPLITUDE AND FREQUENCY CHANGES AND MARS OF TRACKING AND TELEMETRY SIGNAL NASA-CR-71627 ~66-21767 AIM PAPER 66-148 A66- 17900 IUII(US. c. LEVY. J. WEIGHT AND ENERGY REQUIREMENTS OF VEHICLE SYSTEMS FINAL REDUCTION OF OBSERVATIONS OF SPORADIC FOR MANNED EXPLORATION OF MARS OUTBURSTS IN OECAMETRIC REGION OF RADIO SPECTRUM AIAA PAPER 64-3 A6533549 OF JUPITER DURING 1961 AND 1962 A65-21855 IURtlIh F. F. MARS ATMOSPHERE OZONE DISTRIBUTION ANALYSIS LICHTI31STEIN. J. H. INCLUDING PHOTOCHWICAL RUCTIONS AM0 DISCREPAWCY ATMOSPHERIC BRAKING FOR TRANSFER INTO MARTIAN FACTORS A65-25020 ORBIT NASA-TN-0-2837 N65-26255 ABSORPTION AND PHOTOIONIZATIW COEFFICIENTS OF PROPYLENE AND BUTENE 1 IN VACUUM ULTRAVIOLET - LIEBL. H. J. PLANETARY AH10110nY WOPLASMATRON AS VACUUM ULTRAVIOLET LIGHT SOURCE - NASA-CR-18 N65-17265 PLANETARY AERONOIIY NASA-CR-16 165-17263 PLANETARY AERONOMY - PHOTOCHEMISTRY OF PLANETARY ATMOSPHERE. VACUUM AND EXTREME ULTRAVIOLET LIWI(. F. SPECTRAL REGIONS. AND THEORETICAL AERONOMY PHOTOMETRIC OBSERVATIONS OF STARS IN OCCULTATION NASA-CR-68106 N66-12248 AN0 PLANETARY ATMOSPHERIC EXPLORATION FROM ARTIFICIAL SATELLITE IN ORBIT IUIYULL. JI V. NASA-TT-F-8219 ~65-22579 NITROGEN DIOXIDE CONTENT OF MARS ATMOSPHERE DERIVED FROM LABORATORY TESTS AND MICROPHDTOllETER LIPPIWCOTT. E. R. TRACES A6518480 EXPECTED THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATED FOR ATMOSPHERES OF EARTH. VENUS. SPECTRUM. COMPOSITION AND SURFACE PRESSURE. CARBON MARS. AN0 JUPITER DIOXIDE ABUNDAHtE. NITROGEN DIOXIDE TESTS. AND NASA-CR-69965 N66- 1646 3 STRUCTURE OF ATMOSPHERE ON MARS NASA-CR-60264 N65-15223 THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES NASA-CR-69829 N66-21229 I(U1E. J- E. LOW SUBSONIC DYNAMIC STABILITY DATA FOR EVALUATION LIU. v. c. OF BALLISTIC DECELERATION VEHICLE ENTERING MARS COLLISIONAL TRANSITION BETWEEN LOWER ATMOSPHERE ATMOSPHERE AND COLLISIWLESS EXOSPHERE ANALYZEO. USING NASA-CR-631 17 116524985 INTEGRAL FORMULATION OF BOLTZMANN EQUATIOW AND COLLISION MODELS A66-20882 WSSEI. H- SCIENTIFIC RESEARCH USING INSTRUMENTS IN SPACE LOSOV!3CII. 8. IA- VEHICLES. NOTING DIRECT OBSERVATIONS OF MOON. RADIO EMISSION OF SATURN ON WAVELENGTH OF 8 MM VENUS. MARS. GLOBAL COMMUNICATIONS. METMROLDGYi COMPARED WITH VALUES OBTAINED AT OTHER WAVELENGTHS 6EODETIC AND NAVI6ATION SATELLITES. ETC A65-35841 A6623639

LOVELOCK. J- E- SPACE TRAVEL AND EXPLORATION. BIOLOGICAL AND PHYSICAL BASIS FOR EXTRATERRESTRIAL LIFE DETECTION TECHNICAL DIFFICULTIES. RADIATIfflr METEOR IMPACT. AN0 USE ON MARS A65-81737 VEHICLE STERILIZATION. ETC A6623640

BIOLOGICAL SIGNIFICANCE OF MARTIAN ATMOSPHERIC WUICE. E. COMPOSITIONAL ANALYSIS. AND LIFE DETECTION PHOTOMETRIC INVESTIGATION OF AUREOLE ELONGATING STUDIES OF CHEMICAL FREE ENERGY IN SURFACE VENUS HORNS AT INFERIOR CONJUNCTION MATTER A65-171M NASA-CR-67354 N65-36391 PHOTOMETRY OF AUREOLE PROLONGING HORNS OF VENUS CRESCENT LUIDBlf. R. Y. NASA-TT-F-9685 N65-33962 ALTERNATE MISSION PROFILES FOR MANNED MARS LANOIN6 IUV. J- NASA-TN-0-3181 N66-14703 FINAL REDUCTION OF OBSERVATIONS OF SPORADIC OUTBURSTS IN DECAMETRIC RE6IW OF RADIO SPECTRW OF JUPITER DURING 1961 AND 1962 LURIE. R. M, A6521855 DENSE CARBON REINFORCED AN0 LOW DENSITY CHAR- FORMING RESIN ABLATION MATERIALS FOR EARTH. MARS W: CAY. 8- K- AND VENUS ATMOSPHERE ENTRY A65- 15619 ATMOSPHERES CAPABLE OF PRODUCING ORGANIC COMPOUNDS DISCUSSED. STUDYING ABIOGENIC SYNTHESIS IN MARS SIMULATOR A65-30683 LION. F. J. SPACECRAFT DECELERATION UPON ENTRY INTO MARS W CUOSKY. R- E- ORBIT BY AERODYNAMIC BRAKING. CONSIOERING VEHICLE METEOR PHENOMENA. UPPER ATMOSPHERE YIWD FIELDS SHAPE AN0 VELOCITY EFFECTS ON ENTRY HEATING FROM METEOR TRAILS. AND PHOTOMETRY OF A AN0 B AIM PAPER 64-479 A65-28841 RINGS OF SATURN AFCRL-65-33 N65-36000 M IC; ELUOI. n. I). AND TEMPERATURE IN MODEL OF MARIANO. J. F. CHEMICAL COMPOSITION UPPER ATMOSPHERE MARS A65-27569 CLOUD COVER EFFECT ON GREENHOUSE MODEL OF VENUS OF ATMO SPHER E MODELS OF MARTIAN THERMOSPHERE WITH CONSTANTS NASA-CR-51176 N65-14655 AWJ BOUNDARY VALUES IN HYDROSTATIC AND HEAT-FLUX EQUATIONS N65-28713 CONVECTIVE-RADIATIVE EauiLiaRIun MODEL FOR COMPUTING TEMPERATURE PROFILE - VERTICAL CALCULATIONS OF MIDDAY DAYGLOW INTENSITIES TEMPERATURE DISTRIBUTION IN MARTIAN ATMOSPHERE ARISIN6 FROM FLUORESCENCE OF SOLAR IONIZING NASA-CR-65049 N65-27955 RAD1AT1 ON WAS A-CR-6442 4 1165-31047 METEOROLOGY OF PLANETS MARS. VENUS, AND JUPITER iu KENLIE. I. L. NASA-CR-280 ~65-30726 EFFECT OF UNCERTAINTIES IN ATMOSPHERIC STRUCTURE

1-51 MC WELLIS, J- PERSONAL AUTHOR INDEX .

AN0 CHEMICAL COMPOSITION ON ENTRY INTO MARS PROFILES OF PLANETARY ATMOSPHERES FROM NUMBER NASA-TN-0-2584 N65-14628 DENSITY PROFILES OF TWO INERT GASES WITH DIFFERENT MOLECULAR WEIGHTS ESTIMATE OF CHEMICAL KINETICS BEHIND NORMAL SHOCK NASA-CR-71862 N66-23682 WAVES IN CARBON OIOXIOE AN0 NITROGEN MIXTURES FOR MARTIAN ATMOSPHERIC ENTRY mu. I. L. NASA-TN-0-3287 N66-16940 LONG LIFETIME ORBITS ABOUT MARS AFFECTED BY ATMOSPHERIC DRAG. SOLAR GRAVITATIONAL MC NELLIS, J- PERTURBATIONS, PLANETARY OBLATENESS AN0 OTHER TRAJECTORY ANALYSIS FOR MARS ATMOSPHERE PROBE - PERTURBATIONS VOYAGER PROJECT AIAA PAPER 66-35 A66-18987 NASA-TM-X-55376 N66-17249 MOORE.__ ~- P. SIMILARITY OF COLOR PHENOMENA ON SATURN AND MCGOVERN, W- E- JUPITER LEADS TO SPECULATION OF SOLAR INFLUENCE MARS UPPER ATMOSPHERE THERMAL STRUCTURE FROM A65-29288 SPECTROSCOPIC MEASUREMENTS AN0 MARINER IV OCCULTATION EXPERIMENT 666-23660 OBSERVATION OF CLOUD PHENOMENA ON PLANET MARS A65-29289

MCNALLY, 0. LIFE ON MARS - CONDITIONS, POSSIBLE TYPES OF CONFINEMENT OF DECAMETRIC RADIATION FROM JUPITER ORGANISMS AN0 THEORIES OF ADVANCED FORMS OF LIFE TO NARROW BEAMS ATTRIBUTED TO BELTS OF TRAPPED A6680582 CHARGED PARTICLES SIMILAR TO VAN ALLEN BELTS A65-25632 MOORE. R- C- ATMOSPHERIC SCATTERING AN0 REFRACTION OF SUNLIGHT HEIR. 1- C. INTO PLANETARY UMBRA N66-20124 CLOSED FORM SOLUTIONS FOR INCLINATION ANGLE AN0 P-3282 DENSITY OR ALTITUDE AS VELOCITY FUNCTION FOR BODY ENTERING PLANETARY ATMOSPHERE A65-20563 MOROL. V. 1. 1 R SPECTRUM STUDY OF PLANET MERCURY FOR ATMOSPHERIC'COMPOSITION AN0 TEMPERATURE PROFILE MENARD. Y. A- A65-15676 EQUILIBRIUM AN0 NONEQUILIBRIUM STAGNATION POINT SHOCK LAYER RADIATION IN SIMULATED PLANETARY I R SPECTROSCOPY OF VENUS USEO TO ESTIMATE CARBON ATMOSPHERES OF VARYING COMPOSITION DIOXIDE ABUNDANCE BY MEASUREMENT OF ABSORPTION ~66-21773 BANDS A65-15691 I R SPECTRUM STUDY OF PLANET MERCURY FOR MENZELI 0. Ha ATMOSPHERIC COMPOSITION AN0 TEMPERATURE PROFILEA65-26783 RESEARCH ACTIVITIES AT HARVARO ASTRONOMICAL OBSERVATORY FROM 1964 THROUGH 1965 NU-17617 IIOROZHENKO~ A. V. BRIGHTNESS DISTRIBUTION IN MARGINAL ZONE OF MARS MERZ, E. J. USEO TO DETERMINE ATMOSPHERIC ABSORPTION MARS ATMOSPHERE DEFINITION IMPORTANT IN ADVANCED A65-18972 LANDING VEHICLE DESIGN WITH INCREASED PAYLOAD CAPABILITY AN0 REDUCED COMPLEXITY PHOTOMETRIC DETERMINATION OF MARTIAN ATMOSPHERE AIAA PAPER 65-22 A65- 1456 3 AN0 SURFACE OPTICAL THICKNESS AN0 ABSORPTIONA65-18974 AS FUNCTIONS OF WAVELENGTHS MARS ATMOSPHERE DEFINITION IMPORTANT IN ADVANCED LANDING VEHICLE DESIGN WITH INCREASED PAYLOAD OPTICAL PARAMETERS OF MARS ATMOSPHERE AN0 SURFACE CAPABILITY AN0 REDUCED COMPLEXITY FROM PHOTOMETRIC DATA FOR SPHERICAL AN0 ELONGATED166-19337 AIAA PAPER 65-22 A66-24697 SCATTERING INOICATRICES

MILLER, B. A. SPECTROPHOTOMETRIC OBSERVATIONS OF MARS ALTERNATE MISSION PROFILES FOR MANNED MARS N6 5- 18512 LANDING NASA-TN-0-3181 N66-14703 PHOTOELECTRIC MEASUREMENT OF BRIGHTNESS DISTRIBUTION IN LIMB ZONE OF MARS MILLER. J. H. NASA-TT-F-10018 N66-23538 CARBON DIOXIDE- R-BRANCH LINES OF 5 MU SUB 3 BAND FROM INTEGRAL OF ABSORPTION COEFFICIENT OF MOULIN. L- MARTIAN ATMOSPHERE A66- 15288 SPACE VEHICLE RECOVERY TRAJECTORIES EXTENDING FROM GIVEN INITIAL ORBIT TO ATMOSPHERE TOP MININr I. N. A65-19314 FORMULAS FOR LIGHT PASSAGE THROUGH PLANETARY ATMOSPHERES OF FINITE OPTICAL THICKNESS, TAKING MUELLER. K. H. INTO ACCOUNT POLARIZATION A66-15415 THEORETICAL FUEL-BASE0 SPECIFIC IMPULSE LIGHT METAL-NITROGEN SYSTEM FOR RAMJET AN0 TURBOJET LIGHT SCATTERING IN PLANETARY ATMOSPHERE - FORMULA PROPULSION IN MARTIAN ATMOSPHERE FOR DETERMINING INTENSITY OF RADIATION LEAVING A65-15610 HOMOGENEOUS SPHERE AFTER SINGLE DIFFUSION N65-24480 MUELLER. R- F. ABUNDANCE AND STABILITY OF MAJOR SULFUR COMPOUNDS MINOVITCHI M. A- IN LOWER ATMOSPHERE OF VENUS CALCULATED, ASSUMING DEEP SPACE, SOLAR PROBE, AN0 OUT-OF-ECLIPTIC EQUILIBRIUM BETWEEN ATMOSPHERIC GASES AN0 MINERAL TRAJECTORIES UTILIZING LARGE PLANETARY PHASES A66-19262 PERTURBATIONS NASA-CR-69222 N66-15224 MJLLIKIN. 1. Y- ELECTROMAGNETIC WAVE SCATTERING IN HOMOGENEOUS MINZNERI R. A. PLANE-PARALLEL ATMOSPHERES - SOLAR RAdIATION EARTH AN0 PLANETARY ATMOSPHERES. ISOPYCNIC LEVELS. TRANSFER IN PLANETARY ATMOSPHERE TEMPERATURE DETERMINATION FROM DIFFUSION DATA, RH-4846-PR N66-19418 AN0 TRANSITION MODEL ATMOSPHERES NASA-CR-64008 N65-29722 MJRRAV. 8. c. I R ASTRONOMY, DETECTION DEVICES AN0 EVALUATION OF METHOD FOR DETERMINING TEMPERATURE-ALTITUDE OBSERVATIONS OF MOON AN0 PLANETS A65-30119

1-52 . PERSONAL AUTHOR INDEX PARUER-JQIES. n. A.

VENUS ATMOSPHERE BRIGHTNESS-TEMPERATURE MAPPIN6 OF UEMY. 80 1. 6-14 MICRON RADIATION BEFORE 1964 CONJUNCTION MARS IR SPECTRA IN 3-4 MICRON REGION ATTRIBUTED A65-35025 TO TERRESTRIAL HW MOLECULES 011 BASIS OF SOLAR SPECTRA AN0 WATER VAPOR ABUIDANCES MUSAELIANs SH. A- 165- 19902 FORECASTING HUMIDITY TRANSPORT IN ATMOSPHERE IN PLANETARY-SCALE PROCESSES A65-30110 DISCREPANCY IN PHOTOMETRIC AN0 VISIBLE POLARIMETRIC DETERMINATIONS OF MARS SURFACE MY€& H. 6. PRESSURE ATTRIBUTED TO AEROSOL PARTICLES IN EMISSION AND ABSORPTION OF RADIANT ENERGY IN MODEL MARTIAN ATMOSPHERE A65-26945 MARTIAN ATMOSPHERE conmsEo OF 15 PERCENT CARBON OIOXIOE AN0 85 PERCENT NITROGEN BY VOLUME OIOs J- A66-15771 ENERGY SOURCES AN0 CHEMICAL REACTIONS IN PREBIOLOSICAL ORGANIC SYNTHESIS N ~6s-ao473 NAW(OV. A- P. OMEN. R. Bo OPTICAL THICKNESS OF JUPITER ISOTHERMAL VENUS ATMOSPHERE IN SEVERAL MODELS NOTING ATMOSPHERE ASSUMING IT CONSISTS OF HYDROGEN. GREENHOUSE MOOEL BI IONOSPHERIC MOOEL. ETC METHANE AN0 AMMONIA A65-30237 A65-29998

NEUSEBIUERI M. THEORETICAL MOOEL ATMOSPHERES OF VENUS SOLAR WINO PROTON VELOCITY. TEMPERATURE AND NASA-TN-0-2527 N65-14117 DENSITY DETERMINE0 YHEN MARINER I1 WAS NEAR VENUS A65-22598 LITERATURE SURVEY ON SURFACE FEATURES. SURFACE ATMOSPHERIC CONOITIONSt BLUE HAZE. AN0 NEUMANM. 1. Y. ATMOSPHERIC CONSTRUCTION OF PLANET MARS AUTOMATED BIOLOGICAL LABORATORY FOR OETECTION NASA-TM-X-53167 N65-17995 AN0 CLASSIFICATION OF LIFE ON MARS A65-39518 OERIVATIOW OF ATMOSPHERIC PARAMETERS FOR SREEWIIMISE MOOEL OF VENUS ATMOSPHERE PLANETARY LIFE EFFECT ON BIOLOGICAL PRECURSOR NASA-TM-X-53327 N65-35976 MISSIONS TO MARS AIM PAPER 65-249 A65-22120 SURFACE TEMPERATURE CALCULATIONS FOR VENUS BASE0 MI TWO GREENHOUSE ATMOSPHERIC MOEL COMPARISONS NICOLET. M- NASA-TK-X-57375 N66-23674 SATELLITE AN0 ROCKET OBSERVATIONS LEADING TO NEW ASPECTS OF HETEROSPHERE STRUCTURE NOTING HEAT OYHI. 1. BALANCE. PHOTODISSOCIATION AN0 GAS DIFFUSION L~BORATORY ANO PLANETARY ABSORPTION SPECTRA A65-19485 COMPARISWS IN REGIW 9700-11200 ANGSTROMS USED TO DETERMINE COMPOSITION AND TEMPERATURE OF JUPITER 0 ATMOSPHERE A65-21854 OCfflNELs E- METHANE AN0 MMONIA LABORATORY SPECTRA COMPARED BIBLIOGRAPHY CONTAININS 275 ENTRIES ON WITH SPECTRA OF JUPITERs INOICATING CAUSES OF ASTRONOMICAL SUBJECTS FROM ELEVEN U.S.. BRITISH UNIOENTIFIEO ABSORPTIONS 1165-35022 AN0 SOVIET TECHNICAL PUBLICATIONS PUBLISHED IN 1964 A65-29113 I R SPECTRA OF SATURN RING AN0 GALILEAN SATELLITES OF JUPITER SHOW ABSENCE OF STRONG BIBLIOGRAPHY OF 1964 LITERATURE ON SOLAR SYSTEM ABSORPTIOU AT 8873 ANGSTROMS. INOICATINS NEW UPPER SCIENCE 1165-35373 LIMIT OF METHANE ABUNDANCE A65-35585

OSULIGHER. J. J. MI. 1. c. SEARCH FOR TRAPPED ELECTRONS AN0 MSNETIC MOMENT CALIBRATION OF MARTIAN SPECTRA USING LABORATORY AT MARS BY MARINER IV 1165-36325 SPECTRA OF PURE CARBON OIOXIOE AN0 IN COWBINATION WITH NITROGEN AN0 ARSON A65-18477 OHMSTEDEs We 0. PLANETARY BOUNDARY LAYER MODEL FOR ATMOSPHERIC RELATION BETWEEN TOTAL ATMOSPHERIC PRESSURE AND YIND AN0 TURBULENCE OISTRIBUTIONS CARBON DIOXIDE AWNOANCE OF MARS N65-22739 A65-18478

OHRENBERSER. J. 1. SPECTRUM. COMPOSITION AN0 SURFACE PRESSURE. CARBON EMISSION AN0 ABSORPTION OF RADIANT ENERGY IN MODEL OIOXIOE AWNOANCE. NITROGEN OIOXIOE TESTS. AN0 MARTIAN ATMOSPH€RE COMPOSE0 OF 15 PERCENT CARBOU STRUCTURE OF ATMOSPHERE ON MARS OIOXIOE AN0 85 PERCENT NITROGEN BY VOLUME NASA-CR-60264 N65-15223 A66-15777 RECENT DETERMINATIONS OF COMPOSITION AN0 SURFACE THERMOOYNAMIC PROPERTIES OF 15 PERCENT CARBON PRESSURE OF MARS ATMOSPHERE DIOXIDE-85 PERCENT NITROGEN MIXTURE AT VARIED NASA-CR-29B N65-33835 TEMPERATURE AND PRESSURE RANSES STL-9990-6631-TU-000 N65-23299 JUPITER FLYBY MISSIONS - FUTURE STUDIES ON PLANET ATMOSPHERE AN0 MAGNETOSPHERE OHRIN6. 6. WSA-CR-69561 N66-15807 CLOUD COVER EFFECT ON GREENHOUSE MODEL OF VENUS ATMOSPHERE NASA-CR-51176 165-14655 P PALM. A- CONVECTIVE-RADIATIVE EQUILIBRIUM MOOEL FOR HMTIAN BLUE HUE PROPERTIES CORRELATED WITH COMPUTING TEMPERATURE PROFILE - VERTICAL INTERPLANETARY OUST. METEOR SHOWERS AND SOLAR TEMPERATURE OISTRIBUTION IN MARTIAN ATMOSPHERE FLARES A65-2 6040 NASA-CR-65049 N65-27955 PMIYSKII. YU- N. METEOROLOGY OF PLANETS MARS. VENUS. ANO JUPITER RADIO ASTRONOWICAL OBSERVATIONS OF VENUS WITH NASA-CR-280 N65-30726 HIGH RESOLVING POWER NRL-TRANS-936 N65-17990 ATMOSPHERIC CIRCULATION AN0 CLIMATOLOGY OF VENUS AN0 MARS PMKER-JOIIES. ti. A. NASA-CR-71627 N66-21767 HISH ENERSY DENSITY BATTERY FOR USE ON PLANET VENUS

1-53 PATTY. R. R- PERSONAL AUTHOR INDEX

NASA-CR-54404 N65-24338 PHOTOIONIZATION HASS SPECTROHETER WITH 180 OEG HAGNETIC ANALYZER AN0 USE AS GAS ANALYZER PATTY. R. R. NASA-CR-71210 N66-1963b INFRARED SPECTROSCOPY STUOIES TO DETERHINE ABSORPTION BY CARBON DIOXIDE BETWEEN 8.000 AN0 HASS SPECTROMETER USING HETkROENERGETIC ION 10,000/CH IN 1 TO 1.25 HICRON REGION SOURCE WITHOUT DEFLECTION FIELD FOR HARTIAN U-3200 N66-22465 ATMOSPHERE ANALYSIS NASA-CR-71916 N66-23797 PEEBLESS P. J- E. JUPITER AN0 SATURN INTERIOR TEHPERATURES FROH PRAWAKARA~ C. EXAHINATION OF ATHOSPHERIC COHPOSITION AN0 HARTIAN ATMOSPHERIC HEATING FROM SOLAR RADIATION GRAVITATIONAL HULTIPOLE HOHENT A65-33302 ABSORPTION IN UV AND VISIBLE BY OXYGEN AN0 OZONE AN0 IN NEAR IR BY CARBON DIOXIDE, NOTING VERTICAL PETERSON, L. R. OISTRIBUTION OF GASES AN0 ABSORPTION HETHOO FOR OETERHINING TEHPERATURE-ALTITUDE A65-2352 1 PROFILES OF PLANETARY ATHOSPHERES FROH NUHBER DENSITY PROFILES OF TWO INERT GASES WITH PRIBOTEVA, N. V. DIFFERENT HOLECULAR WEIGHTS INTENSITY HEASUREHENTS OF HETHANE ABSORPTION IN NASA-CR-71862 N66-23682 VISIBLE REGION OF JUPITERS SPECTRUM NASA-TT-F-10062 N66-23610 PETERSON. V. Lo DETERHINATION OF PLANETARY ATHOSPHERE STRUCTURE PROKOFEV. V. K. FROH HEASUREO ACCELERATION OF ENTRY VEHICLE PROBABILITY OF PRESENCE OF NITROGEN, OXYGEN AND NASA-TN-0-2669 N65-17118 WATER IN ATHOSPHERE OF VENUS. BASE0 ON SPECTROSCOPIC STUOIES A66-19323 ESTIHATING ERRORS IN DENSITY AN0 PRESSURE STRUCTURE OF PLANETARY ATMOSPHERE CONSTRUCTED FROH MEASURED ACCELERATIONS OF ENTRY VEHICLE R NASA-TR-R-225 Nb5-29299 RAKDS. K- 0. PHOTOELECTRIC OBSERVATION OF ATHOSPHERIC PRESSURE PETTENSILL, 6- ti. ON MARS SURFACE RADAR OBSERVATIONS OF HERCURY, VENUS, HARS AN0 NASA-CR-11312 N66-23776 JUPITER SURFACES Ab6-20116 RANFTL. J. W. PITTS, 0. E. INSTRUHENTATION FOR ANALYSIS OF HARS ATHOSPHERE PLANETARY ENVIRONHENTAL DESIGN DATA FOR FUTURE AFTER SOFT LANDING HAWED SPACE FLIGHTS TO VENUS AND HARS NASA-CR-62870 N65-24301 NASA-SP-3016 N65-23799 RADIATION GAUGING HETHOOS FOR UNHANNEO PROBE TO PLACE, T. M. HEASURE MARTIAN ATHOSPHERIC DENSITY DURING HIGH ENERGY DENSITY BATTERY FOR USE ON PLANET ENTRY N65-24895 VENUS NASA-CR-62971 NASA-CR-54404 Nb5-24338

RASWL. S.-~ I.~~ PLUMMER. W. TEHPERATURE, DENSITY AND GRAVITATIONAL ESCAPE ON DATA RECORDING, DATA REDUCTION AN0 INTERPRETATION HARS, HERCURY. JUPITER AN0 VENUS ATMOSPHERES OF INFORHATION ON WATER CONTENT OF VENUS A66- 151 59 ATHOSPHERE GATHERED BY BALLOON-BORNE INSTRUHENTS A65-22091 HARS UPPER ATHOSPHERE THERHAL STRUCTURE FROH SPECTROSCOPIC HEASUREHENTS AN0 HARINER IV VENUS ATMOSPHERIC COHPOSITIONI USING BALLOON OCCULTATION EXPERIHENT A66-23660 TELESCOPE OBSERVATION AN0 IHPLICATIONS FOR HODEL ATHOSPHERE A65-33692 PLANETARY ATHOSPHERE COHPOSITION. TEHPERATURE, AN0 PRESSURE OF HARS, VENUS, AN0 JUPITER WATER VAPOR CONTENT IN VENUS ATHOSPHERE ABOVE NASA-TH-X-56223 N65-20799 REFLECTING CLOUD LAYER OETERHINEO. USING AUTOHATIC OAYTIHE TELESCOPE AN0 GRATING SPECTROHETER REA. 0. 6. A66-18054 EVIDENCE FOR LIFE ON HARS IS SEASONAL WAVE OF DARKENING AN0 ASSOCIATED CHANGES IN POLARIZATION REFLECTION SPECTRUH OF CLOUDS IN VENUS OF DARK AREAS A65-15140 ATHOSPHERE HEASUREO. USING TELESCOPE HOUNTED ON HELIUH BALLOON, NOTING DETAILS OF INSTRUHENT HARS IR SPECTRA IN 3-4 HICRON REGION ATTRIBUTED A66-18055 TO TERRESTRIAL HOO HOLECULES ON BASIS OF SOLAR SPECTRA AN0 WATER VAPOR ABUNDANCES DATA RECORDING, DATA REDUCTION AN0 INTERPRETATION A65-19902 OF INFORMATION ON WATER CONTENT OF VENUS ATHOSPHERE GATHERED BY BALLOON-BORNE INSTRUHENTS I R SPECTROSCOPY ROLE IN BIOLOGICAL EXPLORATION OF A66-21109 HARS PROVIDING DATA ON ATMOSPHERIC AN0 SURFACE PARAHETERS A65-26729 POLLACK. J. 0. VENUS IR LIHB DARKENING OBSERVATIONS BY HARINER OISCREPANCY IN PHOTOHETRIC AN0 VISIBLE 11 A65-22098 POLARIHETRIC DETERHINATIONS OF HARS SURFACE PRESSURE ATTRIBUTED TO AEROSOL PARTICLES IN I R LIHB DARKENING OF VENUS EXPLAINED IN TERHS OF MARTIAN ATHOSPHERE A65-26945 THREE TYPES OF ATHOSPHERE AN0 CLOUD HODELS A65-34633 EVIDENCE FOR LIFE ON HARS - NATURE AN0 UNCERTAINTIES VENUS IR LIHB DARKENING OBSERVATIONS BY NASA-CR-58430 N65-29415 HARINER I1 A66-21110 HARTIAN ATHOSPHERE AN0 SURFACE CHARACTERISTICS - PONIIAMPERUMAr C- ASTROPHYSICS ATHOSPHERES CAPABLE OF PRODUCING ORGANIC COMPOUNDS NASA-CR-68 136 N66-12974 OISCUSSEO, STUDYING ABIOGENIC SYNTHESIS IN HARS S IHULATOR A65-30683 REES. Lo W- PNEUHATIC SURFACE SAHPLING DEVICE FOR USE IN POSCHENRIEDER* Y. Pa SIHULATED MARS ENVIRONHENT HASS SPECTROHETER INSTRUHENTATION FOR HARTIAN NASA-CR-70937 N66-20080 ATMOSPHERIC ANALYSIS NASA-CR-60760 N65- 17216

1-54 PERSONAL AUTHOR IWX SEIFF. A-

REESE. D- E.. JR- S MARS ATMOSPHERIC DENSITY. TEMPERATURE. COMPOSITION AND PRESSURE DETERMINATION FROM ENTRY RESPONSE OF SMALL PROBE A65-16989 S16UI. C. WSNITROGEN OXIDES OBSERVED AT DIFFERENT PRINCIPLES FOR DETERMINING PROPERTIES OF IMKNDWN WAVELENGTHSI COMPUTING PHOTOCHEMICAL EQUILIBRIA PLANETARY ATMOSPHERE FROM RESPONSES OF POINT AWD RrnE IN BLUE HAZE A65-11992 REENTERING PROBE VEHICLE NASA-TI+-X-56125 N66-19497 VEMJS IR LIMB DARKENING OBSERVATIDWS BY HARINER I1 A65-22096 REESEI E- Jo PHOTOGRAPHIC OBSERVATIDWS OF RAPIDLY MOVING SPOT 1 R LlMB DARKENIN6 OF VENUS EXPLAINED IN TERMS OF IN JUPITER ATMOSPHERE THREE TYPES OF ATMOSPHERE AN0 CLOUD HOOELS NASA-CR-64568 W5-32025 A65-34633

REIFF. 6. A- PROBLEMS REGARDING CHEMICAL COIIWSITIIM AND INSTRUMENTATION AN0 DESIGN OF SCIENTIFIC PAYLOAD PHYSICAL PROPERTY OF VENUS ATMOSPHERE CARRIED BY MARINER IV A66-20181 A65-BO868

REIS. V- H- VENUS IR LIMB OARKENING OBSERVATIONS BY SPECTRAL AN0 TOTAL RADIATION STUDIES OF BODIES WINER 11 A6621110 TRAVELING AT HYPERSONIC SPEED IN SIMULATED MARTIAN AN0 VENUSIAN ATMOSPHERES MARINER IV OBSERVATIONS OF MARS SIRFACE. SHOWIN6 AIM PAPER 65-116 A65-15008 MI OETECTABLE MA6NETIC FIELD OR RADIATION BELTS. SU66EST IRON ON SURFACE OXIDIZED FROM RHEIN. Ro A- PHOTODISSOCIATION OF WATER VAPOR IGNITION TEMPERATURES OF POWOEREO METALS IN A6621211 SIMULATED ATMOSPHERES OF VENUS AND MARS SUGGEST POTENTIAL CHEMICAL ENERGY SOURCES THERMOOYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES A6622458 NASA-CR-69829 N6621229

RICE. Fo 0. SUISmY. J. Y. CHEMICAL TRANSFORMATIONS IN OUTER SPACE DISCUSSIN6 PLANETARY ENVIRONMENTS IN VARIOUS MODELS OCCURRENCE. STATE AN0 BEHAVIOR OF ELEMENTS ON A6620287 PLANETS. MOON AN0 METEWITES *45-16981 PLANETARY ENVIRONMENTAL MODELS OF VENUS. MARS. RIUURDSDllr E. Ho MERCURY. JUPITER, PLUTO, NEPTWEt AND URANUS UPPER LIMIT TO MOLECULAR OXYGEN CONTENT OF VENUS *LD SATELLITES ATMOSPHERIC COMWSITIOW. ATMOSPHERE OBTAINEO WITH DOPPLER SHIFT TECHNIQUE TEMPERATURES. AND CIRCULATION N6610996 AN0 CURVE-OF--GROWTH ANALYSIS A65-17189 SUaOl#IVItn. A- YE- RICHARDSOHI R- S- RADIO EMISSION OF SATURN ON WAVELENSTH OF 8 Iv1 CHARACTERISTICS OF MARS AN0 POSSIBILITY OF COMPARED WITH VALUES OBTAINEO AT OTHER NAVELEWGTHS EXISTENCE OF LIFE A65-81018 A65-35841

RIED. La. JR. DFTECTION OF WATER VAPOR IN ATMOSPHERE OF VENUS EN6INEERING BREADBOARD MODEL OF MICROORGANISM FTD-TT-65-296/ 1C2 W5-30746 OETECTION DEVICE FOR MARS LANDING APPLICATIONS NASA-CR-74214 N66-23787 SA". J- A- R- ROBERT. A- WOPLASMATRON AS VACWM ULTRAVIOLET LIGHT SOURCE - BEHAVIOR OF PLANETARY WAVES IN ATMOSPHERE MODEL PLANETARY AERONOMY BASEO ON SPHERICAL HARMONICS NASA-CR-16 N65-17263 AFCRL-65-468 1166-10836 VACUUM ULTRAVIOLET L16HT SOURCES - PLANETARY ROBERTS. J. A- AERONOMY LINEAR POLARIZATION. PLANETARY ROTATION OF NASA-CR-17 N65-17264 POLARIZATION. LUNAR OtCULTATION AN0 INTENSITY SPECTRUW OF JUPITER DECIMETRIC EMISSIONS ABSORPTION AN0 PHOTOIOMIZATIOW COEFFICIENTS OF A65-21042 PROPYLENE AND BUTENE 1 IN VACUUM ULTRAVIOLET - PLANETARY AEROEIDMY ROD6ERS. C. D. NASA-CR-18 1165-17265 I R COOLIW RATE IN PLANETARY ATMOSPHERES. NOTIN6 CURTIS- 600SON APPROXIMATION. DOPPLER LINE SUIERMUM. 6- 0- SHAPE. MATER VAPOR ROTATION BAND. ETC HETHO0 FOR OETHIMINIWG TEMPERATURE-ALTITUDE A66-22264 PROFILES OF PLANETARY ATMOSPHERES FROn NUMBER OENSITY PROFILES OF TWO INERT 6ASES WITH ROTH. 6. II. DIFFERENT MOLECULAR WEI6HTS ATMOSPHERE POSTULATION BASEO ON KOZYREV NASA-CR-71862 N66-23682 OBSERVATION OF HYOROGEN. ENTRY TRAJECTORY ANALYSIS AN0 FEASIBILITY OF ATMOSPHERIC BRAKIN6 FOR LANOING SCALA. 5. PAYLOAD ON MERCURY -MAL SHOCK WAVE AN0 STAGNATION POINT SOLUTIONS AIM PAPER 65-494 A65-29684 FOR FWR VENUSIAN ATMOSPHERIC AND CHEMICAL I(06ELS RDZENBER6. 6- V. R64S065 N65-13519 PLANETARY ATMOSPHERE OBSERVATIONS FROM SPACECRAFT IN TWILIGHT CONOITIONS A65-31247 SCHILLING 6- Fo ASTRONOMICAL OBSERVATIONS AN0 PLANETARY PLANETARY ATMOSPHERE OBSERVATIONS FROM SPACECRAFT ATMOSPHERES IN TWILIGHT CONDITIONS A65-34922 P-2964 N65- 15023

RLHIBA. 0- N. ATMOSPHERIC SCATTERINS AN0 REFRACTION OF SUIILIGHT MODULATION MICROWAVE RAOIOMETER FOR MEASURIN6 INTO PLANETARY UMBRA JUPITER RADIATION INTENSITY IN 700 Ilt RANGE P-3282 N6620124 A65-10553 SIEIFF. A- MODULATION MICROWAVE RAOIOWETER FOR MASURIIIG MARS ATMOSPHERIC OENSITY. TEMPERATURE. COIlPOSITION JUPITER RAOIATION INTENSITY IN 700 Ilt RAN6E AN0 PRESSURE DETERMINATION FROM ENTRY RESPONSE OF A65-27146 SHALL PROBE Ab5-16989

1-55 SEKERA. 2. PERSONAL AUTHOR INDEX

PRINCIPLES FOR DETERHINING PROPERTIES OF UNKNOWN SINTON. Y- M. PLANETARY ATHOSPHERE FROH RESPONSES OF MARS IR SPECTRA IN 3-4 HICRON REGION ATTRIBUTED REENTERING PROBE VEHICLE TO TERRESTRIAL no0 HOLECULES ON BASIS OF SOLAR NASA-TM-X-56125 N66-19497 SPECTRA AN0 WATER VAPOR ABUNDANCES A65-19902 SEKERA. Z. RADIATIVE TRANSFER AN0 IHPERFECT SCATTERING IN THICKNESS OF OUST ON LUNAR FLOOR. INFRARED PLANETARY ATMOSPHERES FROH CHAPMAN APPROACH RADIOHETRIC TEHPERATURES OF BRIGHTER PLANETS, A66-23414 AN0 EXTENSIVE PHOTOMETRY OF HARS AFCRL-64-926 N65- 15288 SHAPIRO. 1. 1- ROTATION OF PLANET MERCURY FROH RADAR OBSERVATION SIX. N- Fer JR. EXPLAINED BY SOLAR GRAVITATIONAL TORQUE ON TIDAL FINAL REDUCTION OF OBSERVATIONS OF SPORADIC DEFORMATION AND EQUATORIAL PLANE ASYMHETRY OUTBURSTS IN DECAMETRIC REGION OF RAOIO SPECTRUH NASA-CR-68703 N66-13573 OF JUPITER WRING 1961 AN0 1962 A65-21855 SHARANOV. V. V. ATHOSPHERE OF MARS AS ABSORBING. ASCRIBING REO SLATER. A- E. COLOR TO SELECTIVE ABSORPTION IN ATHOSPHERIC LAYER NUCLEIC ACID MOLECULE REPRODUCTION DISCUSSING A66-19328 PROBABILITY OF LIFE DEVELOPMENT UNDER FAVORABLE ENVIRONMENTAL CIRCUHSTANCES A66-15915 SHARDANAND MARS ATMOSPHERE OZONE OISTRIBUTION ANALYSIS SLOBODENIUK. G. I- INCLUDING PHOTOCHEHICAL REACTIONS AN0 DISCREPANCY HODULATION HICROWAVE RADIOMETER FOR HEASURING FACTORS Ab5-25020 JUPITER RADIATION INTENSITY IN 700 MC RANGE A65-18553 SHARONOVs V. V. HOOEL OF MARS ATHOSPHERE AN0 SURFACE CLOSE TO MOOULATION HICROWAVE RADIOMETER FOR MEASURING TERRESTRIAL CONDITIONSs WITH SCATTERING JUPITER RADIATION INTENSITY IN 700 HC RANGE ATMOSPHERIC SPECTRUM AN0 SURFACE COVERED WITH A65-27 146 LIHONITIC OUST A66-19329 SMITH. A. 6- PLANETS AND SATELLITES IN SOLAR SYSTEH FINAL REDUCTION OF OBSERVATIONS OF SPORADIC NASA-TT-F-77 N65-14673 OUTBURSTS IN DECAHETRIC REGION OF RADIO SPECTRUM OF JUPITER DURING 1961 AND 1962 SHAY. H. S. Ab5-21855 ATMOSPHERE POSTULATION BASED ON KOZYREV OBSERVATION OF HYDROGEN. ENTRY TRAJECTORY ANALYSIS SMITH. 8- A- AND FEASIBILITY OF ATHOSPHERIC BRAKING FOR LANDING PHOTOGRAPHIC RECORDING OF JUPITER ATMOSPHERE PAYLOAD ON MERCURY NASA-CR-50303 N65-14653 AIAA PAPER 65-494 A65-29684 PHOTOGRAPHIC OBSERVATIONS OF RAPIOLY MOVING SPOT SHIBANDVs A. IN JUPITER ATHOSPHERE ATHOSPHERIC FACTORS OF INTERPLANETARY SPACEFLIGHTS NASA-CR-6k568 N65-32025 FTLkTT-65-741/1&2&4 N66-12511 SMITH. F. L.. I11 snIMIzu. n. TWO-FREQUENCY BISTATIC RADAR-OCCULTATION TECHNIQUE THEORETICAL MODELS OF VENUS AND HARS UPPER TO INVESTIGATE PLANETARY ATMOSPHERES ATHOSPHERES, NOTING OISSOCIATION LAYERS AN0 CARBON A65-31267 MONOXIDE CONTENT Ab5-15454 METHOD FOR STUDY OF PLANETARY IONOSPHERES BASE0 SOLAR IONIZING RADIATION EFFECT ON JUPITER UPPER ON RADIO WAVE PROPAGATION BETWEEN EARTH AN0 ATMOSPHERE DISSOCIATION INDICATE0 BY MICROWAVE SPACECRAFT SPEC TRUM 165-17213 NASA-CR-64460 N65-32199

SHLOSIN6ER. A. P. SMITH. H. J. PLANETARY RADIATION AN0 ALBEDO EFFECTS ON THERHAL JUPITER OPTICAL EMISSION AN0 AURORAL ACTIVITY BALANCE OF SPACECRAFT ORBITING MARS AND VENUS STUDY NASA-CR-67813 N66-10684 Ao-62489 5 N66-19676

SHOVLIN. M. D. SMOLUCHOYSKI~R. ALTERNATE-MISSION PROFILES FOR HANNED HARS MARS COLOR CHANGES EXPLAINED ON BASIS OF PHYSICAL LANDING MODEL A65-81159 NASA-TN-0-3181 N66-14703 SWIDEU. C. Y. SIEGEL. S. II. SOLAR WIND PROTON VELOCITY, TEMPERATURE AND TERRESTRIAL MICROORGANISM SURVIVAL AN0 GROWTH ON DENSITY OETERHINEO WHEN MARINER I1 WAS NEARA65-22598 SPECIHENS OF EUPHORBIA xYLoPnYLLoIoEs IN AMMONIA VENUS METHANE HYDROGEN-RICH ATMOSPHERES A65-23486 sownEv. v. v. LIGHT SCATTERING IN PLANETARY ATHOSPHERE - FORMULA SEE0 GERMINATION OF COMHON PLANT SPECIES IN FOR DETERMINING INTENSITY OF RADIATION LEAVING RAREFIED NITROGEN ATHOSPHERES SIMULATING HOHOGENEOUS SPHERE AFTER SINGLE DIFFUSION EXTRATERRESTRIAL ENVIRONMENT A65-32416 N65-24480

SURVIVAL AND GROWTH OF TERRESTRIAL HICROORGANISMS SOHN. 1. L- IN AHHONIA-RICH ATHOSPHERES SUPPORTING POSSIBILITY UNHANNED SPACE MISSION TO DETERHINE HARTIAN OF ORIGIN AND EXISTENCE OF LIFE ON JUPITER ENVIRONHENTAL FACTORS INFLUENCING DESIGN OF A65-81287 SYSTEHS FOR MANNED SPACE MISSION TO MARS - UNHANNEO SPACECRAFT DESIGN SIMONS. R. E. NAS A-CR-687 42 N66-15540 HASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE FOR CHEMICAL COMPOSITION STUDY OF HARTIAN UNHANNED SPACE HISSION TO DETERHINE HARTIAN ATHOSPHERE ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF NASA-CR-71307 N66-23779 SYSTEMS FOR HANNEO SPACE HISSION TO HARS - MISSION EXPERIHENT REQUIREHENTS SIMPSON. J. A. NASA-CR-68741 N66-15541 SEARCH FOR TRAPPED ELECTRONS AND MAGNETIC HOMENT AT MARS BY HARINER IV A65-36325 UNHANNEO SPACE MISSION TO DETERMINE HARTIAN

1-56 PERSONAL AUTHOR INDEX TIIIOFEEVA. 6. M.

ENVIRONMENTAL FACTORS INFLUENCING DESIGN OF STUART. 6- Y. SYSTEMS FOR MANNED SPACE MISSION TO MARS - EXPLOSION IN RAREFIED ATMOSPHERES WHERE EXPLOSIVE SUMMARY REPORT PRODUCT ATOM MEAN FREE PATH IS LONGER THAN NASA-CR-68743 N66-15H2 EXPAND1116 MATERIAL DIMENSIONI ILLUSTRATING METHOD WITH CHEMICAL EXPLOSION AT 150 KH ALTITUDE UNMANNED SPACE MISSION TO DETERMINE MARTIAN A65-24615 ENVIRONMENTAL FACTORS INFLUENCINS DESIGN OF SYSTEMS FOR MANNED SPACE MISSION TO MARS - SUMASKY. WI J. MISSION SENSITIVITY ANALYSIS HIGH ENER6Y DENSITY BATTERY FOR USE ON PLANET NASA-CR-68740 -15543 VENUS NASA-CR-54404 N65-24338 SOMERVILLE. Yo B. HYDROGEN MOLECULES IN ASTROPHYSICS SWAN. P. a. NASA-CR-57156 N65-18918 SURFACE PRESSURE OF MARS ATMOSPHERE REDETERMINED FROM ABSORPTION INTENSITY OF CARBON DIOXIDE BY SONES. P. LOW6-PATH AND PHOTOMULTIPLIER DETECTION LAMINAR AND TURBULENT CONVECTIVE HEAT TRANSFER 1165-35360 RATES ON CONES IN PLANETARY ATMOSPHERES RAD-TM-64-66 N65-19405 ABSORPTION INTENSITY OF CARBON DIOXIDE BANDS AND MARTIAN CARBON DIOXIOE ABUNDANCE AND ATMOSPHERIC SPIECB. J- PRESSURE AS BASE OF DESI6N FOR MARS ENTRY VEHICLE ANALYSIS OF EQUILIBRIUM SHOCK LAYER RAOIATION FOR A65-82273 MARS ATMOSPHERIC ENTRY N65-32433 SWART. n. SPINRAD. HI EXTRATERRESTRIAL LIFE IN SOLAR SYSTEM. DISCUSSING UPPER LIMIT TO MOLECULAR OXYGEN CONTENT OF VENUS EWIPMENT FOR MARS EXPLORATION. NOTING GULLIVER ATMOSPHERE OBTAINED WITH DOPPLER SHIFT TECHNIQUE PROGRAM. MULTIVATOR AUTOMATIC BIOCHEMICAL TESTINC AN0 (;URVE-OFGRONTH ANALYSIS A65-11189 APPARATUS AND TV MICROSCOPE A6623794

KOZYREV HYDROGEN EMISSION LINES IN IR SYEWSO*. 5. Y. SPECTROlXAMS OF MERCURY NOTINS CORE EMISSION RADIO ASTRONMIY SKETCH NOTIN6 SOLAR. 6ALACTIC AND A65-23491 COSMIC RAY OBSERVATIONS AND INSTRUMENT DIFFICULTIES A65-15368 MERCURIAN ATMOSPHERE FROM HIGH DISPERSION SPECTRAL STUDY OF ABUNDANCE OF CARBON DIOXIDE. OXY6EN AN0 SVTINSKAIA. N. No NITER A65-25226 SEPARATION PROBLEMS OF CAS AND AEROSOL COMPONENTS IN BRIGHTNESS OF ATMOSPHERIC LAYER FOR PHOTOMETRIC EARTH-BOUND OBSERVATIOWS OF SURFACE AN0 ATMDSPHERE DATA PERTAINING TO MARS ATMOSPHERE OF PLANET MARS N65-15491 A6619330

STECHEII. 1. P. JUPITER PHOTOELECTRIC SPECTRAL SCAN IN UV T REPRODUCED AS 6EOMETRIC REFLECTIVITY VS TIIK. w. WAVELENGTH. USING AEROBEE ROCKET ATMOSPHERIC CIRCULATION ON MARS A66-21099 NASA-CR-262 N65-28631

STOVAS. M. U. METEOROLOGY OF PLANETS MARS, VENUS. AND JUPITER SURFACE DISTURBANCES AS POSSIBLE CAUSE OF TECTONIC NASA-CR-280 N65-3072 6 MOVEMENT IN JUPITER ATMOSPHERE - ASTRONOMY 1-439-R N66-10590 ATMOSPHERIC CIRCULATION AN0 CLIMATOLOGY OF VENUS AND MARS STRELKOV. 6. M. NASA-CR-71627 N66-21767 ATMOSPHERIC COMPOSITION OF VENUS AN0 EFFECT ON RADIO EMISSION IN VISIBLE AND NEAR IR SPECTRAL TAYLOI. 1. A- BAWDS A6619325 EARTH REENTRY SIMULATION OF PLANETARY ENTRY ENVIRWMENT WITH EXPONENTIAL ATMOSPHERES OF STRONG. J. WRS AND VENUS TYPE BALLOON BORNE IR SPECTROSCOPY INDICATES VENUS AIAI PAPER 65-218 A65-16bO6 CLOUDS CONSIST OF ICE CRYSTALS A65-14707 TEYFEL. v. 6. DATA RECORDING. DATA REDUCTION AND INTERPRETATION IWCE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL OF INFORMATION ON WATER CONTENT OF VENUS VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN ATMOSPHERE CATHERED BY BALLOON-BORNE INSTRUMENTS DISK IN NEAR IR REGION A66-23504 A65-22097 INTENSITY MEASUREMENTS OF METHANE ABSORPTION IN VENUS ATMOSPHERIC COMPOSITIONI USIN6 BALLOON VISIBLE REGION OF JUPITERS SPECTRUM TELESCOPE OBSERVATION AND IMPLICATIONS FOR MODEL NASA-TT-F-10062 N66-23610 ATMOSPHERE A65-33692 1HO)US. 6. II. WATER VAPOR CONTENT IN VENUS ATMOSPHERE ABOVE EWILIBRIUM AN0 NONEWILIBRIUM STACNATIDN POINT REFLECTING CLOUD LAYER DETERMINEDI USIN6 AUTOMATIC SHOCK LAYER RADIATION IN SIMULATED PLANETARY DAYTIME TELESCOPE AND GRATIN6 SPECTROMETER ATMOSPHERES OF VARYING COMPOSITION A66-18054 A6621773

REFLECTION SPECTRUM OF CLOUDS IN VENUS THOIIPSON. TI R- ATMOSPHERE MEASUREO. USING TELESCOPE MOUNTED ON EMISSION AND ABSORPTION OF RADIANT ENERGY IN MODEL HELIUM B&LLOON. NOTING DETAILS OF INSTRUUENT NARTIAN ATMOSPHERE COMPOSE0 OF 15 PERCENT CARBON A66-18055 DIOXIDE AND 85 PERCENT NITROGEN BY VOLUME A6615777 DATA RECORDING. DATA REDUCTION AND INTERPRETATION OF INFORMATION ON NITER CONTENT OF VENUS THOILSO)I. E. 0. ATIYISPHERE GATHERED BY BALLOON-BORNE INSTRUMENTS WEIGHT AND ENERGY REQUIREMENTS OF VEHICLE SYSTEMS A66-21109 FOR MANNED EXPLORATION OF MARS AIAA PAPER 64-403 1165-33549 STRUWLD. H. POSSIBLE WATER SOURCE BENEATH MARS SURFACE OUST TIMOFEEVA. 6. 1. AND ICE MAY CONSTITUTE POTENTIAL BIOSPHERE RADIO ASTRONOMICAL OBSERVATlONS OF VENUS NITH A65-26720 HIGH RESOLVINC POWER NRL-TRANS-936 N65-17990

1-51 TITOV. V. N. PERSONAL AUTHOR INDEX

TITOV. V- N. MOWLATION MICROWIVE RADIOMETER FOR MEASURING W JUPITER RADIATION INTENSITY IN 700 MC RANGE A65-18553 WALSHAY. C- 0- I R COOL,ING RATE IN PLANETARY ATMOSPHERES, NOTING MOWLATION MICROWAVE RADIOMETER FOR MEASURING CURTIS- GODSON APPROXIMATION, OOPPLER LINE JUPITER RADIATION INTENSITY IN 700 MC RANGE SHAPE, WATER VAPOR ROTATION BAND, ETC A65-27146 A66-22264

TOMBAU6H. C. W- WANG P. K- C- PHOTOGRAPHIC RECORDING OF JUPITER ATMOSPHERE EQUATIONS OF MOTION FOR ELASTIC BODIES ENTERING NASA-CR-50303 N65- 1465 3 PLANETARY ATMOSPHERE AT HYPERSONIC VELOCITIESN66-21667

TRAFTON. Lo M. JOVIAN ATMOSPHERE AND ENVIRONMENT - COMPOSITION, WARNECK. Po STRUCTURE, AN0 PHOTOMETRIC PROPERTIES OF MARS ATMOSPHERE OZONE DISTRIBUTION ANALYSIS ATMOSPHERE, PERIOD OF ROTATION, MAGNETIC FIELD, INCLUDING PHOTOCHEMICAL REACTIONS AN0 DISCREPANCY AN0 JOVIAN RAOIOFREQUENCY SPECTRUM FACTORS A65-25020 NASA-CR-63116 N65-24983 PHOTOIONIZATION MASS SPECTROMETER WITH 180 OEG TRUNOVA. Z- 6. MAGNETIC ANALYZER AN0 USE AS GAS ANALYZER N66- 196 36 MODULATION MICROWAVE RADIOMETER FOR MEASURING NASA-CR-71210 JUPITER RAOIATIDN INTENSITY IN 700 MC RANGE ~65-it3553 WARREN. Yo Re. JR. MOWLATION MICROWAVE RADIOMETER FOR MEASURING SIMULATION OF HEAT TRANSFER ENVIRONMENTS OF SPACE VEHICLE ENTERING PLANETARY ATMOSPHERE WITH JUPITER RADIATION INTENSITY IN 700 MC RANGE A65-27146 SUPERORBITAL VELOCITY N65- 15600 R64S073

TSITSIN, F. A. HVPERVELOCITY HEAT TRANSFER STUDIES IN SIMULATED PHYSICAL CHARACTERISTICS OF UNIVERSE AN0 PLANETARY ATMOSPHERES BIOGENESIS OF EXTRATERRESTRIAL LIFE NASA-CR-57508 N65-19884 A66-80742

WATANABE. K. U ABSORPTION AN0 PHOTOIONIZATION COEFFICIENTS OF URBAN. V. M- PROPYLENE AN0 BUTENE 1 IN VACUUM ULTRAVIOLET - PLANETARY RADIATION AND ALBEDO EFFECTS ON THERMAL PLANETARY AERONOMY BALANCE OF SPACECRAFT ORBITING MARS AN0 VENUS NASA-CR-18 N65-17265 NASA-CR-67813 N66-10684 WAYNE. J. F- USHAKOFF. 0. Y. ORBITER INJECTED STERILIZED BALLISTIC SKIPOUT RADIO OBSERVATION OF PLANETARY AND STELLAR CAPSULE FOR IN FLIGHT MARTIAN STRATOSPHERE EMISSION AND EFFECTS OF TERRESTRIAL ATMOSPHERE MEASUREMENTS, USING NONABLATIVE HEAT SHIELD AN0 A66-20289 OUTSIOE ATMOSPHERIC PROPULSION MANEUVERS AIAA PAPER 65-23 A6515944 RADIO ASTRONOMV - PASSIVE RECEPTION OF RADIATION IN RADIO WAVELENGTHS FROM EXTRATERRESTRIAL WEAVER. R- W. SOURCES SUCH AS MOONlLUNAR THERMAL EMISSION, AND LOW SUBSONIC DYNAMIC STABILITY DATA FOR EVALUATION PLANETARY RADIO EMISSION N66- 10998 OF BALLISTIC DECELERATION VEHICLE ENTERING MARS ATMOSPHERE V NASA-CR-63117 N65-24985 VAKHNIN. V- M. WEBER. J. Q. RADIO NOISE EMISSION FROM VENUS SURFACE EXPLAINED THEORETICAL FUEL-BASE0 SPECIFIC IMPULSE LIGHT IN TERMS OF GLOW DISCHARGE A66-17 17 4 METAL-NITROGEN SYSTEM FOR RAMJET AN0 TURBOJET PROPULSION IN MARTIAN ATMOSPHERE VAN ALLEN. J. A. A65- 15610 ABSENCE OF ELECTRONS IN MARS ATMOSPHERE AN0 IMPLICATIONS THEREOF YELLS. R. A. NASA-CR-64870 N65-33919 1924 AND 1926 OPPOSITIONS OF MARS IN Y. H. WRIGHT PLATES NOTING MARS OIAMETER IN IR VAN TASSEL. R. A. AN0 UV A65-20633 PLANETARY ENVIRONMENTS IN VARIOUS MODELS A66-20287 YESTOII..~ C, R. MARS ENVIRONMENTAL CONDITIONS, LIFE ORGANISM PLANETARY ENVIRONMENTAL MODELS OF VENUS, MARS, DETECTION, EVALUATION AN0 LIMITING EFFECTS MERCURY, JUPITER, PLUTO, NEPTUNE, AN0 URANUS A66-22715 AN0 SATELLITES ATMOSPHERIC COMPOSITION, TEMPERATURES, AN0 CIRCULATION N66-10996 WLSTPHAL. J- Ao 1 R ASTRONOMY, DETECTION DEVICES AN0 EVALUATION OF VICTOR. 6- A. OBSERVATIONS OF MOON AND PLANETS COUPLE0 HARTREE- FOCK APPROXIMATION FOR A65-30119 CALCULATING FREQUENCY-DEPENDENT REFRACTIVE INDEX OF HELIUM GAS VENUS ATMOSPHERE BRIGHTNESS-TEMPERATURE MAPPING OF NASA-CR-68991 N66-14281 8-14 MICRON RADIATION BEFORE 1964 CONJUNCTION A65-35025 VO6Lp J. L. ARGON ABUNDANCE IN MARTIAN ATMOSPHERE DETECTOR, WHIPPLE. F. L- USING CYLINDRICAL IONIZATION CHAMBER CONTAINING METEOR PHENOMENA, UPPER ATMOSPHERE WINO FIELDS IRON 55 X-RAY SOURCE A65-23098 .FROM .METEOR - TRAILS. AN0 PHOTOMETRY OF A AN0 B RINGS OF SATURN VSEKHSVIATSKIIr 5. K- AFCRL-65-33 N65-36000 CONCEPTS CONCERNING JUPITER SURFACE REVISE0 FOLLOWING TRANSFORMATIONS OBSERVE0 SINCE 1962 AND WHISTLER. W- J- ESTIMATION OF ASH PARTICLES IN PLANET ATMOSPHERE MASS SPECTROMETER INSTRUMENTATION FOR ANALYSIS OF A65-30238 MARS ATMOSPHERE NASA-CR-67959 N66-11743

1-51) PERSONU. AUTHM INDEX

WILDEY. R. I.. A6t-16323 THERMAL EMISSION OBSERVATIONS OF SHADOWS CAST ON JUPITER BY SATELLITES GANYMEDE* EUROPA AN0 IO 115-18223 Z LA*DEII. 1. THERMAL EMISSION MAPS OF JUPITER. OISCUSSIW STRATOSPHERIC BALLOON OBSERVATIONS OF VENUSIAN SOURCE Of NOISE FROM TRACKING ERRORS AN0 CLOUDS INOICATE COMPOSITION OF ICE CRYSTALS PHOTOMETRIC ERRORS A65-31279 1165-28654

VENUS ATMOSPHERE BRIGHTNESS-TEMPERATURE MAPPIN6 OF VENUS ATMOSPHERIC COMPOSITION. USING BALLOON 8-14 MICRON RADIATION BEFORE 1964 CONJUllcTIOW TELESCOPE OBSERVATION AN0 IMPLICATIONS FOR HODEL A65-35025 ATMOSPHERE 1165-33692

WILDTI R. REFLECTION SPECTRUM OF CLOUDS IN VENUS JUPITER ATMOSPHERE* USING SfECTROPHOTOGRAPHIC ATMOSPHERE MEASURED* USING TELESCOPE MOLNTED ON OBSERVATIONS A65-33303 HELIUM BALLOON. NOTING DETAILS OF INSTRUMENT A6618055 SEPARATION BETWEEN FLUID PHASES IN MULTICMPONENT ATMOSPHERE AS POSSIBLE EXPLANATION OF JUPITER ZAVITSANOS. C- Do GREAT REO SPOT A66-19592 MASS SPECTROMETER ABOARD HYPERSONIC ENTRY VEHICLE FOR CHEMICAL COMPOSITION STUDY OF MARTIAN HOPF ANALYTICAL SOLUTION FOR VALUES OF RATIO OF ATMOSPHERE GRAY ABSORPTION COEFFICIENTS FOR INSOLATIW AN0 NASA-CR-71307 N66-23779 ESCAPING RAOIATION /GREENHOUSE PARAMETER/ ASSUME0 CONSTANT AT ALL DEPTHS* PRESENTING TEMPERATURE LntLEZNI4KOV~V. V. OISTRIBUTION 6RAPHS A66-21204 MONOGRAPH ON RADIO EMISSION OF SUN AWO PLANETS A65-16909 HOPF ANALYTICAL SOLUTION FOR GREENHOUSE PARAMETER IN GRAY PLANETARY ATMOSPHERE ZMII(MA. A- I- NASA-TM-X-56621 N66-22218 CHAMBER AN0 ELECTRICAL CIRCUIT USED TO SIMULATE MARTIAN CONOITIONS FOR MICROBIOLOGICAL WILLIS* E- Am* JR. INVESTIGATIONS A65-25099 ALTERNATE MISSION PROFILES FOR MANNED MARS LANDING MARTIAM CONOITIONS SIMULATED FROM ASTROPHYSICAL NASA-TN-0-3181 N66-14703 DATA FOR MICROBIOLOGICAL INVESTIGATIONS A65-30682 WITTING J. M- JUPITER FLYBY MISSIONS - FUTURE STUDIES ON PLANET ATMOSPHERE AND MAGNETOSPHERE NASA-CR-69561 N66-15807

WOLF. F. ANALYSIS OF EQUILIBRIUM SHOCK LAYER RADIATION FOR MARS ATMOSPHERIC ENTRY N65-32433 uOODCOCK* 6. Re PROPULSION ORIENTED STUDY OF MISSION MODES FOR MANNED MARS LANDING NASA-TM-X-53265 N65-28960

WOODS. R. 0. INSTRUMENTATION FOR ANALYSIS OF MARS ATMOSPHERE AFTER SOFT LANOING NASA-CR-62870 N65-24307 WOOWARD. H. To SPECTRAL AND TOTAL RADIATION STUDIES OF aooiEs TRAVELING AT HYPERSONIC SPEED IN SIMULATED MARTIAN AND VENUSIAN ATMOSPHERES AIM PAPER 65-116 A65-15068

WUNDER. C. C. BIOLOGICAL PROBLEMS IN SPACE-TEXTBOOK A66-80836 Y YATSENKO. 5. P. VEWS NIGHT ATMOSPHERE INVESTIGATE0 BY STlDYIW IONOSPHERIC ELECTRON DENSITY AN0 ELECTRON RECOMBINATION IN NIGHT ATMOSPHERE OF EARTH NASA-TT-F-8244 N65-22589

YOU16. A. 1, MARS NITROGEN OXIDES OBSERVED AT DIFFERENT WAVELENGTHSI COMPUTING PMCTOCHEMICAL EQUICI8RIA POINT AN0 ROLE IN BLUE HAZE A65-17992 yOUN6. RO 5. ATMOSPHERES CAPABLE OF PROOUCING ORGANIC COMPOUWDS DISCUSSED. STUOYING ABIOGENIC SYNTHESIS IN MARS SIMULATOR A65-30683

mas ENVIRONMENTAL FACTORS SUGGESTING BIOLOGICAL POSSIBILITIES AND LIFE DETECTION EQUIPMENT TO PREVENT CONTAMINATION A6582218

AUTOMATED LIFE DETECTION ON MARTIAN ENVIROWnENT BASED ON METABOLISM. REPRODUCTION AND CHEMISTRY

1-59 NASA-Langley, 1966