Accession Number) 3 (Nasa Cr Or Tmx Or Ad Number

(ACCESSION NUMBER) *-' (THRU)

19 3 (NASA CR OR TMX OR AD NUMBER) NASA Continuing Bibliographies are annotated and indexed compilations of abstracts of reports and journal articles on aerospace subjects. The subjects are selected for their relationship to current developments in the space program and in response to an established interest by the aerospace community. Continuing Bibliographies are updated periodically by supplements. 41

LICATlONS IN THE CONTlNUl ~BLIOGRAPH~PROGRA

High Energy Propellants NASA SP-7002 Lunar Surface Studies NASA SP-7003 Communications Satellites NASA SP-7004 Bibliographies on Aerospace Science NASA SP-7006 Lasers and Masers NASA SP-7009 Aerospace Medicine and Biology NASA SP-7011 Planetary Atmospheres NASA SP-7017 Lubrication, Corrosion and Wear NASA SP-7020

This bibliography was prepared by the NASA Scientific and Technical Information Facility operated for the National Aeronautics and Space Administration by Documentation Incorporated. NASA SP-7017(02)

PLANETARY OSPHERES

A CONTINUING BIBLIOGRAPHY WITH INDEXES

A selection of annotated references to unclas- sified reports and journal articles that were introduced into the NASA Information System during the period June 1966-December 1967.

Scientific and Technical Information Division NATIONAL AERONAUTICS AND §PACE ADMINI§TRATION WASHINGTON, D.C. J u LY 1968 P

This document is available from the Clearinghouse for Federal Scientific and Technical Information (CFSTI), Springfield, Virginia, 221 51, for $3.00 hat Planetary Atmospheres is This publication is the second supplement to the continuing bibliography Planetary b Atmospheres (NASA SP-70 17). It contains references to reports and journal articles announced in NASA abstract journals during the period June, 1966 through December, t 1967.357 references are included. u Previous bibliographies in this series are NASA SP-7017 (January 1962-February 1965) and NASA SP-7017(01) (March 1965-May 1966). Scope of Bibliography References are included for descriptions and properties of the atmospheres of Mars, Venus, Jupiter, Mercury, and Saturn. In addition, references to related subject areas, e.g., extraterrestrial environments, planetary observation techniques, and theories of planetary origin are included.

The bibliography is arranged in Abstracts and Index sections. The Abstracts section contains bibliographic citations and informative abstracts for the references selected from STAR (Scientgic and Technical Aerospace Reports), IAA (International Aerospace Abstracts), and Aerospace Medicine and Biology (NASA SP-7011). The STAR abstracts are listed first, followed by the IAA and the Aerospace Medicine and Biology abstracts. Each set of abstracts is arranged in ascending accession number order. The Index Section contains two indexes, subject and personal author, in that order.

the STAR Abstracts section. Published literature items are referenced in the IAA Abstracts and the Aerospace Medicine and Biology Abstracts sections. 5 The subject index may be used to locate references to specific topics or technical areas; the personal author index may be used to locate references to reports or articles written by a particular individual.

STAR References (N67-10000 Series) NASA Documents. NASA documents (identified by an asterisk in the citation) are available without charge to: 1. NASA Offices, Centers, contractors, grantees, and consultants. 2. Other U.S. Government agencies and their contractors. 3. Libraries in the United States that have arrangements with NASA to maintain collections of NASA documents for public use. 4. Other organizations in the United States having a need for NASA documents in work related to the aerospace program. 5. Foreign governmental or academic organizations that have established reciprocal arrangements for the exchange of publications with NASA, that have current agreements for scientific and technical cooperative activities with NASA, or that have arrangements with NASA to maintain collections of NASA documents for public use. ?SA If you are registered with NASA, send a completed Document Request (Facility Form 492) to:

iii NASA Scientific and Technical Information Facility P.O. Box 33 College Park, Maryland 20740 If you are not registered with NASA, but are eligible to receive documents without charge according to the above information, request Registration Form-Technical Publica- tions (Facility Form 7 13) from the above address. 4 European requesters may purchase NASA documents from ESRO/ELDO Space Documentation Service, European Space Research Organization, 1 14, av. de Neuilly. 92- Neuilly sur Seine, France. t v Non-NASA Documents. Department of Defense documents (identified by the “AD’ number in the citation) are available without charge to U.S. Government-sponsored research and development activities from the Defense Documentation Center (DDC), Cam- eron Station, Alexandria, Virginia 223 14. Department of Defense documents are not available from NASA. Advisory Group for Aerospace Research & Development (AGARD) reports that are not copyrighted will be made available on the same basis as NASA documents. Other non-NASA documents are provided by NASA without charge only to NASA Offices, Centers, contractors, subcontractors, grantees, and consultants. Foreign non- copyrighted documents will be provided by NASA to U.S. Government Agencies and their contractors. Documents that have been placed on microfiche (a transparent sheet of film, approximately 4x6” in size, capable of containing an orderly arrangement of 60 or more pages of information reduced to micro images) are identified with the symbol #. Microfiche are available on the same basis as hard copy. For reference purposes, NASA documents listed in the STAR Abstracts section of this bibliography may be consulted at one of the organizations listed on the inside back cover. Commercial-type publications listed may be consulted in libraries or purchased from publishers or booksellers. The public may purchase NASA documents from either of the following sales ‘hi agencies as specifically identified in the abstract section: Clearinghouse for Federal Scientific and Technical Information (CFSTI) Springfield, Virginia 22151 Superintendent of Documents, U.S. Government Printing Office (GPO) Washington, D.C. 20402 Documents available from CFSTI are sold in hard copy and microfiche form. If a printed hard copy is not available, a facsimile copy is provided. The symbols “HC” and “MF” are used in the abstract section to designate the copy available: “HC” (hard copy) for full size or facsimile; “MF” for microfiche. A unit price policy has been established by CFSTI: $3.00 for printed hard copy or facsimile copy; $0.65 for microfiche. The public may request non-NASA documents by writing to the source or other information systems. Other bibliographic information, e.g., report number, etc., rather than the NASA accession number (Le., N67-12345) should always be provided when requesting such a document from its source. IAA References (A67-10000 Series) All cited documents are available from the AIAA Technical Information Service as * follows: Paper copies are available at $3.00 per document up to a maximum of 20 pages. The charge for each additional page is $0.25. Microfiche are available at the rate of $0.50 per microfiche for documents identified by the symbol # following the accession number. d

iv A number of publications, because of their special characteristics, are available only for reference in the AIAA Technical Information Service Library. Minimum air-mail postage to foreign countries is $1 .OO. Please refer to the accession number, e.g., A67-12345, when requesting documents. Address all inquiries and requests to: Technical Information Service American Institute of Aeronautics and Astronautics, Inc. 750 Third Avenue New York, N.Y. 10017 Aerospace Medicine and Biology References (A67-80000 Series) Journal articles and books included in this section are available in libraries, where they may be borrowed or consulted.

V NASA -N67-107%%*# National Aeronautics and Space Administration. ..9- CO~~QRA~E ACCESSlQN Goddard Space Flight Center, Greenbelt, Md. SOURCE

(Contract NAS12-106) (NASA-TN-D-3678)

crystal with relation to the light beam is very critical. GaAs appears at this time to be the best electro-optic crystal material for a light modulator in the infrared region between 0.9 and 16 microns. Strain-free GaAs can be grown with resistivities exceeding 106 ohm-cm. At this time, the use of HMTA as a light modulator material does not appear promising. Author

NUMBER

NASA AVAILABLE W SPONSORSHI ON MICROFICHE AIAA A UTH 0 R'S AFFILIATION D RADIATIVE HEAT TRANSFER DURING SUPER- BITAL ENTRY. PREVIOUSLY Hoshizaki and K. H. Wilson (Lockheed Aircraft Gorp., Lockheed ISSUED AS: issiles and Space Go., Research Laboratories, Palo Alto, Calif.). (American Institute of Aeronautics and Astronautics, Aerospace AUTHOR Sciences Meeting, 3rd. New York, N. Y., Jan. 24-26, 1966. Paper 7, __I DO-IUD. ) AIAA Journal, vol. 5, Ja TRACT, TITLE OF Contract No. NAS 7-295. NT. OR PERIODICAL The convective and radiative heat transfer to vehicles entering SPONSORSHIP planetary atmospheres at stperorbital velocities is investigated. An integral method is employed to determine the radiative and convective heating around a blunt body. The effect of mass injection, radiative emission and absorption, radiation cooling, and coupling between convection and radiation are included in the analysis. The absorption coefficients of the shock layer gas as well as the injected ablation products are determined as a function of particle number density, temperature and radiation frequency. The results obtained show that self-absorption can reduce the radiative heating by an order of magnitude but has little effect on the convective heating. It was also found that the nose radius which results in th~minimum total heat transfer rate at the stagnation point is much larger (6 to 10 ft diam at U, = 50,000 fps) than the values'indicated by an optically thin analysis. Furthermore, it is shown that the total stagnation point heat transfer rate is a very weak function of the nose radius, contrary to the results obtained from an optically thin analysis. (Author )

vi stracts ...... 1 stracts ...... 29

stracts...... 57 ...... 1-1

ex ...... 1-41

vii ~~ PLANETARY ATMOSPHERES a continuing bibliography with indexes JULY 1968

Improved greenhouse models for the Venus atmosphere are developed and discussed. A two-layer greenhouse model. con- 1966 sisting of a troposphere with arbitrary but constant lapse-rate of temperature, and an isothermal stratosphere in gross radia- STAR ABSTRACTS tive equilibrium, is applied to Venus, Mars, and Earth. For Venus, the computations indicate that the observed high surface temperatures can be the result of a strong greenhouse effect due to an infrared-opaque cloud high in the Venus atmosphere and carbon dioxide or other infrared absorbers in the atmosphere. Estimates of solar radiation absorbed by N66-26263'# IIT Research lnst, Chicago. 111. carbon dioxide in the Venus atmosphere indicate that about LIFE IN EXTRATERRESTRIAL ENVIRONMENTS Quar- 12% of the solar radiation is absorbed by carbon dioxide near terly Status Report, Feb. 15-May 15, 1966 infrared bands. Author Charles A. Hagen [1966] 24 p (Contract NASr-22) (NASA-CR-74969, llTRI-L6023-5) CFSTI HC $1.OO/MF N66-27755"# Georgetown Univ.. Washington, D C. Coli. Ob- $050 CSCL 06F servatory. o Martian environment simulation experiments to study SPECTROSCOPIC STUDY OF SOLAR AND PLANETARY the effects of barometric pressup carbon dioxide concen- ATMOSPHERES Semiannual Status Report No. 6, Aug. 1, trations, and desert soils on 8acillus cereus spores are re- 1965-Feb. 1, 1966 ported. These included earth atmosphere at pressures of Francis J. Heyden [l966] 16 p a0-98 mb; and carbon dioxide concentrations of 37-100% (Grant NsG-362) at pressures of 10-98 mb Spore germination was inhibited (NASA-CR-75488) CFSTI: HC $1.00/MF $0.50 CSCL 038 by carbon dioxide at all concentrations and pressures Ger- This report describes activities performed during this mination was not inhibited at 10 mb with earth atmosphere, period on spectroscopic studies of solar and planetary at- but vegetative cell growth was less than at 98 mb Graphs mospheres. Spectral observations made on Venus and Jupiter are presented showing these effects Soil ecology experi- are discussed. An attempt is being made to prove the exist- ments to determine the minimum numbers of a bacterium ence of nitrogen oxides in the Martian atmosphere by identi- required to survive and grow in different soil types are de- fying spectral lines or bands in the planet's spectrum. The scribed. Inhibition of B cereus spore germination in pulver- main problems in positively identifying these lines and pro- ized felsite/limonite mixture was detected The spores did cedures to circumvent these difficulties are outlined. Infrared not germinate in mixtures of pH 8-84, but did germinate spectral reflectance measurements made of the Martian at- in soil of pH 7. Low numbers of P. aeruginosa and S aureus mosphere are described and the results discussed. R.N.A. did not survive 7 days in a desert soil environment with 99% relative humidity at 1013 mb. N E N. N66-27957# State Univ. of Iowa, Iowa City. Dept of Physics and Astronomy A MARINERDENUS 1967 EXPERIMENT ON SOLAR X-RAY N66-27238'# Geophysics Corp. of America, 'Bedford, Mass ECLIPSE BY THE VENUSIAN ATMOSPHERE THE METEOROLOGY OF MARS A*ND VENUS Final Report J. A. Van Allen 23 Feb. 1966 22 p refs Its Rept.-66-4 George Ohcing. Edward M. Brooks. and Joseph Mariano Mar. CFSTI: HC $l.OO/MF $0.50 1964 116 p refs A physical modification to the Mariner/Venus MC-4 space (Contract NASw-704) probe experimental package is proposed and described. The (NASA-CR-75315; GCA-TR-64-4-N) CFSTI: HC $4 OO/MF modification consists of remounting one of the mica-window $0.75 CSCL 038 Geiger tubes (detector A) so that it is pointed continuously A thermodynamic diagram for the Martian atmosphere is at the sun. The change would make possible the continuous constructed, based upon a model atmosphere. consisting 01 monitoring of soft X-rays (0-14A) from the sun throughout .-83% nitrogen, 11% carbon dioxide, and 6% argon. with a sur the flight, including the measuremeht of the eclipse of solar face pressure of 25 mb. A theoretical study of tides in the X-rays by the Venusian atmosphere. An exemplary calcula- Martian atmosphere indicates that tidal motions play no sig- tion is presented, showing that assuming a time resolution of nificant role in Martian meteorology. An estimate of the annual' 1 second in the data from detector A, it is possible: (1) to 'qadiation budget reveals that below latitude 35" there is a determine the absolute atmospheric density p to an accuracy surplus of radiational energy. and above 35" there is a deficit. of about 20% in the vicinity of ~=2xlO-~g/cm3 and (2) to

1 N66-28011

determine the mean scale height of the atmosphere to an ac- N66-28801*# Maryland Univ I College Park. Dept. of Chem- curacy better than 10% over the density range 2~10-*g/cm3. istry. Several pertinent factors regarding the time resolution, ac- THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMQS- curacy, and the scheme of the experiment are discussed, and PHERES schematic diagrams depicting the geometry of the spacecraft Ellis R. Lippincott. Richard V. Eck, Margaret 0. Dayhoff (Natl. trajectory, and experimental angle are also presented. A plot Biomed. Res. Found.). and Carl Sagan of calculated absorption curves is also given. ' L.S. Biomed. Res. Found. Invest. of Th Production of Complex Compds. Essent. for the Origin of Life 119661 34 p refs (See N66-28800 16-04) CFSTI: HC $4.00/ N66-28011'# Cutler-Hammer, Inc.. Deer Park, N. Y. MF $1.00 INVESTIGATION OF NEW IQNOSOUNDER TECHNIQUES From present information on the composition, pressures. $' Washington, NASA. Jun. 1966 182 p refs and temperatures of planetary atmospheres. we have calcu- (Contract NAS5-9108) lated the expected thermodynamic equilibrium composition (NASA-CR493) CFSTI: HC $5.00/MF $1.25 CSCL 038 of the atmospheres of the Earth, Venus, Mars, and Jupiter. The objective of this report was to study the feasibility Departures from thermodynamic equilibrium must be attrib- of experiments using radio sounding techniques for the investi- uted to special mechanisms. including, on the Earth. biological gation of the ionospheric properties of Mars and Venus. The activity. The major constituents of the terrestrial atmosphere study effort was divided into two areas. Constraints were ap- are found to be in approximate thermodynamic equilibrium; plied in size, weight, and power consistent'with modern space- while many minor constituents have abundances exceeding craft technology. The techniques study was concerned with in- their equilibrium values, there is a marked tendency for equi- strumentation suitable for sounding a planetary ionosphere librium to be restored. It appears that the atmosphere of from nearby to 100.000 km from the planet in flyby or orbit- Venus is in thermodynamic equilibrium, while that of Jupiter ing spacecraft. A parametric analysis related power, resolution. is not. The evidence for Mars is less conclusive, although not frequency, range, and other parameters of importance. A inconsistent with thermodynamic equilibrium. For none of system analysis was performed using the methods of modern these planets is there a molecular species with a large pre- radar systems and applying them to ionospheric sounding. The dicted equilibrium abundance and spectroscopically accessible results were applied to a specific mission, such as a Voyager absorption features which has not been already identified. flight to Mars. with requirements to sound from distances of The predicted equilibrium abundances of oxides of nitrogen 1000 to 40,000 km. A system to accomplish such a mission are extremely low on all planets. Author is described. Author

N66-29298.# Stanford Univ.. Calif. Radioscience Lab. N66-28800'# National Biomedical Research Foundation, SiI- THE STANFORD STUDY OF THE MARINER IV OCCULTA- ver Spring. Md TlON DATA Semiannual Report No. 3, 1 Oct. 1966-31 Mar. INVESTIGATION OF THERMODYNAMIC MECHANISMS 1966 FOR THE PRODUCTION OF COMPLEX COMPOUNDS V. R. Eshleman Jun. 1966 3 p ESSENTIAL FOR THE ORIGIN OF LIFE Final Report, (Grant NGR-05-020-065) 1 Oct. 1965-30 Sep. 1966 (NASA-CR-75816) CFSTI: HC $1.00/MF $0.50 CSCL 22A * Margaret 0 Dayhoff. Richard V. Eck. and Ell~sR Lippincott The large difference in atmospheric surface pressure 11966) 127 p refs (actually more than 50%) between the occultation levels at (Contract NSR-21-003-002) Electris and Mare Acidalium is reported as the most interest- (NASA-CR-74559) CFSTI HC $4.00/MF $1 00 CSCLO6C ing result derived from the analysis of the Mariner IV-Mars occultation experiment and the Martian atmosphere experi- CONTENTS mental models. Both the higher pressure and the smaller 1 THERMODYNAMIC EQUILIBRIA IN PLANETARY radius determined at Mare Acidalium suggest that this region ATMOSPHERES E R. Lippincott (Md Univ ), C. Sagan (Har- is at a lower gravitational level than the bright Electris area. vard Univ.), R~ V Eck, and M. 0 Dayhoff 34 p refs' (See N66- Analyzed data indicated that some of the haze and particle lay- 28801 16-30] ers observed with earth-based telescopes and with the Mariner 2 THERMODYNAMIC EQUILIBRIUM IN THE ORIGIN IV television camera may have been C02 particles. R OF ORGANIC MATTER E R Lippincott, Y. T Pratt (Md Univ 1, R V Eck, and M. 0 Dayhoff 22 p refs (See N66-28802 16-06) 3 EVOLUTION OF THE STRUCTURE OF FERREDOXIN N66-29398*# National Aeronautics and Space Administration. BASED ON SURVIVING RELICS OF PRIMITIVE AMINO Washington, D. C. ACID SEQUENCES R V Eck and M 0 Dayhoff 16 p refs PLANETARY SPECTRA (SPEKTRY PLANET] (See N66-28803 16-04) May 1964 16 p refs Transl. into ENGLISH from Priroda 4 THERMODYNAMIC AND BIOCHEMICALSTUDIES OF (Moscow). no. 6. Jun. 1961 p 39-45 THE ORIGIN OF LIFE Margaret 0 Dayhoff. Ellis R Lippin- (NASA-TT-F-888) CFSTI: HC $l.OO/MF $0.50 CSCL 038 cott. and Richard V Eck 2 p The analysis of data gathered from the earth by the spec- 5 PREDICTIONS OF THE COMPOSITIONS OF THE tral method of investigation is ussed briefly. It is pointed ATMOSPHERES OF THE PLANETS Richard V Eck 1 p refs out that spectroscopic invest ons of the planets have -. 6 THERMODYNAMIC EQUILIBRIUM ON THE PREGIO- developed in three principal directions: study of planetary LOGICAL EARTH M 0 Dayhoff and R V Eck 1 p rotation on the basis of the Doppler shift of spectra lines, 7 PROTEIN SEQUENCES TREATED AS MATHEMAT- photometric study of the continuous spectrum of planets as ICAL PUZZLES. AN ATLAS OF PROTEIN SEQUENCE AND well as the search for new linesand absorption bands. and study of STRUCTURE Richard V Eck and Margaret 0 Dayhoff 1 p already known lines and bands. Reports on the results of these 8 PROGRAM RELATE M 0 Dayhoff and R V Eck 16p investigations are presented in greater detail. A survey of re- (See N66-28804 16-04) search on the following topics is presented: auroras, and carbon 9 PROGRAM ALLELE R V Eck and M 0 Dayhoff 6 p dioxide and water vapor in the Venusian atmosphere; vegeta-v (See N66-28805 16-04) tion on Mars; hydrogen and its compounds in the atmospheres

2 N66-31187

of the giant planets; the meteoric nature of Saturn's rings; Chandrasekhar's planetary problem is reformulated using luminescence and lunar surface color; and the minor planets' an initial-value approach. The problem concerns the diffuse spectra. R.LI. reflection of radiation from a finite atmosphere with a reflecting surface at the bottom. In the direct problem, the angular distribution of multiple-scattered radiation is computationally obtained as the solution of an initial-value problem for ordi- 9I66-29406*# National Aeronautics and Space Administration. nary differential equations for S. a generalization of the Washington, D. C. Chandrasekhar scattering function for an inhomogeneous PROGRESS AND PROBLEMS IN ATMOSPHERE ENTRY atmosphere. In the inverse planetary problem, the properties Alfred J. Eggers, Jr. and Nathaniel 8. Cohen 119651 72 p refs of the atmosphere and the surface are to be estimated, given *resented at the 16th IAF Intern. Congr.. Athens, 13-18 Sep. the angular distribution of scattered radiation. The quasi-lineari- 1965 zation technique for nonlinear multipoint boundary-value prob- (NASA-TM-X-56855) CFSTI: HC $3.00/MF $0.75 CSCL 22C lems provides an effective method for obtaining a computa- Problems of entry vehicle mhion. heating, and heat pro- tional solution to the inverse problem. A Fortran program tection are discussed in the context of current and possible for both the direct and inverse problems is presented in the future space flight missions, including unmanned probes of appendix. Author (TAB) the atmospheres of Mars, Venus, and Jupiter, and manned vehicles appropriate for controlled planetary entry at veloci- *es from orbital to hyperbolic. Problems in reentry physics N66-30187*# TRW Systems Group, Redondo Beach. Calif. such as transition to turbulent flow, turbulent heat transfer THEORETICAL INVESTIGATION: THE SCAlTERlNG at hyper-velocities, and complex radiation flow-field interac- OF LIGHT BY A PLANETARY ATMOSPHERE Final tions and their possible influence on vehicle configuration Report, 15 Sep. 1965-21 Jun. 1966 are discussed. Attention is also given to ground simulation Robert S. Fraser 11 9661 1 19 p refs facilities. such as the expansion tunnel, ballistic shock tun- (Contract NAS5-9678) nel, and high enthalpy arc jet. Finally, some consideration is (NASA-C R-76I 22 ; T R W-4520-6003- R000) C FST I. H C $4.001 given to the comparative features of rocket braking and maneu- MF $0.75 CSCL 20F vering. Author Computed effects of specular reflection at the ground on the radiation scattered from a Raylergh atmosphere are presented. The relative contribution to the ground albedo by each of several components of the radiation field is discussed. NS8-29732.# RAND Corp., Santa Monica. Calif. The characteristics of the neutral points in the degree of RADIATIVECONVECMVE EQUILIBRIUM CALCULATION§ polarization that would be observed from the ground looking FOR A TWO-LAYER MARS ATMOSPHERE up or from above the atmosphere looking down are presented. *C. 8. Leovy May 1966 55 p refs Author (Contract MASr-21(07)) (NASA-CR-75633; RM-5017-NASA) CFSTl: HC $3.00/MF $0.50 CSCL 03 B N66-30788*# National Aeronautics and Space Administration. Preliminary to a numerical experiment in simulating the Marshall Space Flight Center, Huntsville, Ala. circulation of the Mars atmosphere, a computer model that AN INITIAL CONCEPT OF A MANNED MARS EXCUR§lON simulates diurnal and seasonal variation in ground and at- VEHICLE FOR A TENOUS MARS ATMOSPHERE mospheric temperatures on Mars was constructed: it incor- G. R. Woodcock 7 Jun. 1966 55 p refs porates the effects of radiation, small-scale turbulent con- (NASA-TM-X-53475) CFSTI: HC $3.00/MF $0.50 CSCL 228 vection, and conduction into the ground. All calculations are This report summarizes a preliminary investigation of the based on an atmosphere having a surface pressure of 5 mb requirements and characteristics of a manned Mars landing and composed entirely of Cop. as indicated by the Mariner 4 vehicle to: establish how much aerodynamic braking might occultation experiment. Adjustable parameters in the model be feasible with thin atmosphere; determine if parachutes include: the thermometric conductivity of the ground, and the appear feasible and, if not, how can aerodynamic braking be rate of turbulent heat exchange between ground and atmos- phased into rocket braking for a landing; and establish a rough phere. The model is calibrated by adjusting these constants so estimate of the total mass of a Mars landing vehicle. Author that observations of a portionof the diurnal variation in ground temperature are well simulated. An interesting result of the calculations is the prediction of an ice cap composed of solid N66-31187# University Coll.. London (England). Cot whose maximum extent corresponds with that of the AN ANALYSIS OF MARTIAN CLOUDS AND THEIR observed Martian polar cap. Some possible implications of TOPOGRAPHICAL RELATIONSHIPS the computed temperature distributions are also considered, R. A. Wells Paris, ESRO. May 1966 63 p refs along with space probe experiments that could be made to (ESRO-SN-54) CFSTI: HC $3.00/MF$0.75 verify, reject..or improve the model. A simplified model was The-frequency of cloud occurrences distributed against devised to compute soil heat flux that depends on surface heliocentric longitude is displayed in histogram form for the temperature variations rather than on ground temperatures. two chief cloud groups, white and yellow. White clouds show R.LI. two peaks of maximum occurrence, while yellow clouds ap- + pear to show three peaks. Aerographic latitude plots of white and yellow cloud positions against heliocentric longitude re- N66-89969# RAND Corp.. Santa Monica, Calif. veal that the darkening wave is due to the transport of both -A CQMPUTATIONAL APPROACH TO CHANDRASEKHAR'S water vapor and dust from high latitudes towards the equator. PLANETARY PROBLEM An examination of certain white clouds implies that at least R. Bellman. H. Kagiwada. R. Kalaba. and S. Veno May 1966 some of the dark maria are elevations. Order of magnitude 27 p refs estimates of these mountain heights are calculated by a new (Contract AF 49(638)-1700) method. The unusual 'W'-shaped cloud phenomena are ex- (RM-4991-PR; AD-632231 CFSTl: HC $2.00/MF $0.50 plained by orographically-produced air disturbances which

3 N66-3 1 35 1 imply that mountain ridges may be present on the surface liberation of latent heat of water vapor of about 620 cal/qm. with their axes arranged in the general patterns of a 'W'. as that vapor condenses to form clouds The results also bear Author on the radio emissions from Venus L s.

N66-31351*# National Aeronautics and Space Administration. N66-314W0# RAND Corp I Santa Monica. Calif Langley Research Center, Langley Station, Va. COMMENTS ON THE DETECTION OF WATER AND ICE DYNAMIC-MODEL STUDY OF PLANETARY-ENTRY CON- CLOUDS ON VENUS FIGURATIONS IN THE LANGLEY SPIN TUNNEL Diran Deirmendsian In Calif. lnst of Tech. Proc. of the Cal- Peter J. Costigan Washington, NASA. Jul. 1966 23 p refs tech-JPL Lunar and Planetary Conf. 15 Jun. 1966 p 150- (NASA-TN-D-3499) CFSTI: HC $l.OO/MF $0.50 CSCL 22A 154 refs (See N66-31446 18-30) CFSTI: HC $7.00/MF A study has been conducted in the Langley spin tunnel to $1.75 determine the low subsonic speed stability and drag char- The detection of water and ice clouds on Venus by Strong acteristics during vertical descent of a number of entry con- and his collaborators is commented upon. Comparison of figurations being considered for probes of planetary atmos- terrestrial and Venusian reflected spectra lead to the tenta- pheres The models tested were three of a series designateu tive conclusion that the latter represent infrared sunlight dif- as tension shells, two blunted cones, a configuration similar fusively reflected by a dense, unbroken Venusian ice cloud. to the Apollo command module, a sphere, a step-sphere, a The formation of absorption bands by scattering alone. and hemisphere. and two modified spheres. The results of the on cloud scattering in general are discussed with reference study indicate that the tension shells had a limit-cycle oscil- to water or ice particles. An experiment for detecting the glory lation of less than *20" and had the highest drag coefficients of that should be seen through an upper, optically dense. and any of the configurations tested. These configurations would unbroken ice cloud is proposed for verification of the Strong not return to erect positions if launched inverted. but would findings If the visible spectrum is used. the chances would tumble after several increasingly large oscillations An ap- be small; but choosing a narrow region (x1.6~or A2 25~) pendix treats the problem of scaling techniques necessary to where neither vapor nor liquid water has significant absorp- simulate planetary environments other than that of the earth. tion bands should increase the chances of detecting the in- Author frared glory. particularly in regions and at times of thinning of the Venusian ice cloud Other comments on the clouds with respect to particulate and gaseous components are also N66-31446'# California lnst of Tech , Pasadena made. L.S. PROCEEDINGS OF THE CALTECH-JPL LUNAR AND PLANETARY CONFERENCE Harrison Brown. Gordon J Stanley, Duane 0 Muhleman, N66-31465*# Smithsonian Astrophysical Observatory, Cam- and Guido Muench, ed 15 Jun 1966 357 p refs Conf held bridge. Mass. at Calif. lnst of Tech. Pasadena, 13-18 Sep 1965 Pre- PROPERTIES OF THE CLOUDS OF VENUS pared jointly with JPL Carl Sagan and James B Pollack In Calif lnst of Tech. (Contract NSR-05-002-050) Proc. of the Caltech-JPL Lunar and Planetary Conf. 15 Jun (NASA-CR-76142. JPL-TM-33-266) CFSTI HC $7 OO/MF 1966 p 155-163 refs (See N66-31466 18-30) CFSTI $1 75 CSCLO3B HC$7 OO/MF$1.75 Conference papers on lunar and planetary studies for Mars, A method for calculating the fraction of monochromatic Jupiter, and Venus are presented For individual titles see N66- radiation reflected. transmitted. and absorbed by a layer of 31447-N 66-3 148 1 dispersed particles having arbitrary characteristics fluxes is described. and the method is applied to an examination of the clouds of Venus The equation of radiative transfer for monochromatic radiation nonconservatively and aniso- N66-31463'# Johns Hopkins Univ. Baltimore. Md tropically scattered by a aispersed medium is given. and re- BALLOON TELESCOPE STUDIES OF VENUS written in an approximation form which preserves anisot- John Strong In Calif Inst. of Tech. Proc of the Caltech-JPL topies in flux The approximate solutions for the fluxes are Lunar and Planetary Conf 15 Jun 1966 p 147-150 refs compared with exact solutions for a variety of limiting and (See N66-31446 18-30) CFSTI HC$7 OO/MF$l 75 special cases, and with laboratory results, and are presented The amount of water vapor, and the existence of ice clouds in a table The comparisons show the approximation formu- in the atmosphere of Venus were determined by telescopic and lae to be accurate to 5-10% in absolute value, and a few spectrometric instruments suspended from balloons over the percent in relative value. Also tabulated are comparisons of Earth at an altitude that was above 99 9% of the Earth's water the theoretical and observed values of the albedo of Venus. vapor and 97% of the Earth's CO1 Radiation was measured Curves comparing the theoretical and observed normalized in the band at 1 13p. with a qratinq spectrometer of 2 A re- infrared reflectivities of Venus for particle radii 1-20 and solving power once every 10 sec with a set of exit slits arrayed ~~=l8.and for particle radii 1-20 and 71=43 are de- to match water absorption line qroups The radiation passinq picted (r=interaction optical depth) The influence of the through was received by a chilled photomultiplier and its re- size and composition of cloud particle size on the reflec- sponse was recorded on paper A low dispersion qratinq. tion spectrum is discussed The mutual agreement of the utilizing three detectors in place of the slits. was used for the results ~clpports the identification of ice as the principal ice cloud experiments Details of the measured data are qiven constituent of the clouds of Venus L s. The influence of the doppler shift on the recorded data was also measured The existence of water vapor and ice clouds on Venus explained the observations that the temperature of the shady side of the planet dpes not fall more than a few N66-31470"# Academy of Sciences (USSR). Moscow P N degrees short of the temperature! of the sunny side as measured Lebedev Physical Inst. in the 8 to 14p band. even thouqh the shady side has several SOME REMARKS CONCERNING THE RADIOASTRONOMC months to cool off The failure to cool may be due to the CAL OBSERVATIONS OF VENUS

4 N66-3 1475

A. D Kuzmin In Calif lnst of Tech Proc. of the Caltech-JPL of the Mariner IV flight. the flux of ultraviolet radiation and Lunar and Planetary Conf. 15 Jun. 1966 p 184-186 refs charged particles at the surface with respect to living or- (See N66-31446 18-30) CFSTI HC$7 OO/MF$l 75 ganisms. and other selected observations. L s. Theoretical and experimental data curves for an aerosol model are depicted, and discussed with a view toward explaining astronomical results reported in the spectra of Venus N66-31473'# Kitt Peak National Observatory. Tucson, Ariz by absorption of aerosols from the Venus atmosphere. It is Cop BANDS AND THE MARTIAN SURFACE PRESSURE shown that the radio astronomical data rnay be satisfied by Donald M Hunten In Calif lnst of Tech Proc of the Caltech- aerosols containing polar liquid dielectric if the relaxation time JPL Lunar and Planetary Conf 15 Jun 1966 p 240-244 of the dielectric is equal to 1.5x10 -l2to 5x10 -I2sec About refs (See N66-31446 18-30) CFSTI: HC $7.00/MF $1.75 . 0.1 to 0.2 g/cm2 of such an aerosol is needed to obtain cloud '%eights high enough to fit the model. Substances that satisfy Spectroscopic measurements of the vibration-rotation the data for the model can be found in literature reference bands of C02 in the Martian atmosphere were made. using a 60:~nch telescope in conlunction with its spectrograph. to books The data are satisfied for example by some types of determine the surface atmospheric pressure and composition hydrocarbbns such as CH3OH. CeH5CI. etc.. and by super- of the atmosphere on the planet. The results suggest an at- cooled water In addition, calculated curves for electron tem- mosphere in which Cop is the major constituent, if not the peratures of 400°K and 300OK. together with plotted experi- only important one It appears likely that the surface partial mental results are depicted. in support of an explanation of pressure of Cop is in the range of 4 to 7 mb. with the total long wavelength emissions from the Venus ionosphere Also pressure of about 11 to 7 mb. It seems likely that the partial discussed are phase variations of the planet with respect to pressure of otheib gases is not over 3 or 4 mb. This picture of its brightness temperature. L.S. a nearly pure C02 atmosphere is greatly strengthened by the Mariner IV results which suggest a high molecular weight and a pressure of 4 to 7 mb The old photometric and polarimetric N66-31471'# Paris Observatory. Meudon (France) result of 85 mb is discredited The discrepancy rnay have been CONTRIBUTION TO THE CALTECHJPL COLLOQUIUM ON due to additional scattering by aerosols in the atmosphere, or THE MOON AND THE PLANETS: VENUS [CONTRIBUTION to the inherent difficulty of subtracting all the effects of light AU COLLOQUE CALTECH-JPL SUR LA LUNE ET LES from the surface L.S. PLANETES: VENUS] Audouin Dollfus In Calif Inst. of Tech Proc. of the Caltech- JPL Lunar and Planetary Conf. 15 Jun. 1966 p 187-202 N66-31474*# California Univ , Berkeley. refs In FRENCH (See N66-31446 18-30) CFSTI, HC $7.001 SPECTROSCOPIC OBSERVATIONSOF MARS, 1964-5 MF$1.75 Hyron Spinrad In Calif. lnst of Tech Proc of the Caltech- A general review is presented of data on Venus qiven at the JPL Lunar and Planetary Conf. 15 Jun 1966 p 245-246 'lunar and planetary conference The 1959 balloon work of Doll- (See N66-31446 18-30) CFSTI HC$7 OO/MF$l 75 fus is summarized in which 70 p of water vapor above the Doppler-shifted Martian water vapor lines were obtained Venus clouds is reported, as are many photometric and polari- with high resolution spectrograms of Mars The amount of metric observations The photometric data are shown to match water vapor on Mars seems quite small, averaging about 158 "the responses of a Venus atmosphere with a scale height of precipitable when it is detected The location of the Mars 2 8 km, a grain size of 2 p, and a number density on the order H20 apparently varies with Martian season, the weak lines of 3X1O8 ~m-~.Variations in the polarization of reflected light first appearing over the subliming North Polar Cap. and migrat- suggest the presence of water clouds as opposed to dust ing south over the planet. The abundance of C02 in the Mar- clouds In addition to the detection of water content. the tian atmosphere was also redetermined, using the 5u3 C02 study of aerosols in the upper atmosphere of Venus is dis- band at A8700 The preliminary result is wcO2=80 m-atm cussed Consideration is also given to atmospheric pressure C02, which gives a C02 partial pressure near 6 mb Combining in the upper layer of clouds. the polarimetric study of the this result with other recent data on the saturated COz band nature of clouds, and deviations in the direction of polarized at I.Gp,the total Mars surface pressure PS=8?: mb. C02 is light Trans1 by M W R therefore the major constituent.-A portion of the Mars spectrum at the 5v3C02 band is depicted. Positions of the weak rotational lines of COz in the R and P branches are indicated. The clearly visible R12. 10. and 8 lines are noted. L.S. N66-31472'# California Univ , Berkeley THE ATMOSPHERE AND SURFACE OF MARS-A SELEC- TIVE REVIEW D G Rea In Calif Inst. of Tech Proc of the Caltech-JPL N66-31475'# IIT Research lnst, Chicago. 111 Lunar and Planetary Conf 15 Jcn 1966 p 209-238 refs RECENT OBSERVATIONS OF THE PHOTOGRAPHIC SPEC- (See N66-31446 18-30) CFSTI HC$7 OO/MF $1 75 TRUM OF MARS-A PRELIMINARY REPORT A summary review of published reports pertaining to Tobias Owen In Calif. Inst. of Tech. Proc. of the Caltech-JPL the atmosphere and surface of Mars is presented to con- Lunar and Planetary Conf 15 Jun. 1966 p 247-251 refs struct a framework from which subsequent papers can be (See N66-31446 18-30] CFSTI: HC$7.00/MF$1.75 related Some important physical properties of Mars and The C02 abundance in the Martian atmosphere was re- Earth are summarized in a table Important properties of the determined spectroscopically by means of observations in the Martian atmosphere, such as pressure. composition. and weak bands of 8689 A and 1.05 p. One plate of the 8689 A ,particulate content, as well as the presence of clouds. are band which recorded measurable absorptions for lines in discussed with accompanying data curves The CO spectral the P and R branches is reproduced. The means of reducing band of Mars is considered Principal observations (polariza- the data. which included determining the mean atmospheric tion. spectral, brightness. microwave. and temperature stud- temperature, correction of line intensities, and determination ies etc) and interpretations regarding the surface of Mars, of air mass are described; and the result obtained for the Cop '"the white areas at the poles. the bright areas, and the dark abundance from the foregoing parameters is given. The de- areas, are discussed Also discussed are the TV experiment rived value of Cop abundance was 67+20 m-atm. The corre-

5 N66-3 1477 sponding surface pressure was calculated by two independent spectrum of Mars, but that it sometimes appears on certain methods. (method of Moroz. and method of Owen and Kuiper) locations of the planet. Absolute values obtained for the and lies between 8 and 9 mb with a lower limit of 5 mb and luminosity of the light and dark sides of Mars are discussed, an upper limit of 20 mb. The low surface pressure and high and variations in diffusion are graphed as a function of phase C02 content suggests that the present atmosphere of Mars angle and distance from the center of the core. Diffusion of may be similar in composition to the primitive outgassed at- the Martian atmosphere can be determined by measuring mosphere of the earth. with the exception of the low Martian the polarization of light. and curves are plotted for the visual * abundance of water. This implies that Mars may never have and photoelectric spectra from 0.50 to 1.05~.Residual pol- had a more massive atmosphere than it possesses at the pres- lution in the Martian atmosphere and spectroscopic findings ent time. L.S. by Mariner IV are mentioned. It is noted that the dark spots of the Martian soil almost completely disappear in the blue spec- ++>' trum. and transparency of the atmosphere in this region N8631477'# Jet Propulsion Lab., Calif. Inst. of Tech., Pasa- is discussed. Transl. by M.W.R. dena. PRELIMINARY RESULTSOFTHE MARINER IV OCCULTATION MEASUREMENTOF THE ATMOSPHERE OF MARS N66-31488'# Johns Hopkins Univ.. Baltimore. Md. A. J. Kliore. D. L. Cain. G. S. Levy, V. R. Eshleman, G. Fjeldbo BALLOON-TELESCOPE OBSERVATION OF THE PLAN- (Stanford Univ.) et al In Calif. Inst. of Tech. Proc. of the Cal- ETS tech-JPL Lunar and Planetary Conf. 15 Jun. 1966 p 257- John D Strong In VPI Proc. of the Conf on the Exploration 266 refs (See N66-31446 18-30) CFSTI: HC $7.00/MF of Mars and Venus Aug. 1965 8 p refs $1.75 CFSTI HC$7 OO/MF $1 75 (Contract NAS7-100; Grants NGR-05-020-65; NsG-377) The determination of water vapor in the upper atmosphere This paper reviews the preliminary results of the radio of Venus by an automatic telescoix?-spectrometer unit aboard occultation measurement of the Martian atmosphere con- a balloon at an altitude of 27 km is discussed Various aspects ducted as the Mariner IV spacecraft passed behind the planet. of the data recording system. data reduction. and results are Results of the data analysis showed that values of density, presented The 21 positions of the exit slits used are given, pressure, scale height. and temperature near the Martian sur- a single slit scan across the water band is graphed, and a face were lower than expected. Based on the occultation re- double scan showing absorption by water vapor is pictured. sults and terrestrial spectroscopic measurements of CO 2 The reflection spectrum of Venus clouds is graphed to show abundance in the atmosphere of Mars, it is concluded that correction for the upper atmosphere of Venus, and the ter- CO 2must be the primary atmospheric constituent. R.N.A. restrial water above 26 5 km is illustrated It is concluded that, within limits set by the uncertainties of the agreement, the effective cloud reflections determined for radiations of a 1.1, 1.9, and 2.6 microns all lie at essentially the same alti- N66-31478'# Stanford Univ., Calif. tude. It is noted that the Venus cloud surface temperature PRELIMINARY RESULTS OF THE MARINER IV RADIO is about -40°C. and does not vary significantly from light to OCCULTATION MEASUREMENTS OF THE UPPER AT- dark qide The latent heats and freezing of water provide

MOSPHERE OF MARS the mechanism for sustaining this temperature on the dark 6. G. Fjeldbo, V. R. Eshleman, A. J. Kliore. D. L. Cain (JPL), side M.W.R. F. D. Drake (Cornell Univ.) et al In Calif. Inst. of Tech. Proc. of the Caltech-JPL Lunar and Planetary Conf. 15 Jun. 1966 p 267-272 refs (See N66-31446 18-30) CFSTI: HC $7.00/ MF $1.75 N66-31489*# RAND Corp , Santa Monica, Calif (Contract NAS7-100: Grants NGR-05-020-065; NsG-377) SOME ASPECTS OF THE CIRCULATION OF MARS This paper discusses that part of the radio occultation Conway Leory In VPI Proc of the Conf on the Exploration measurement of the Martian atmosphere. conducted as the of Mars and Venus Aug 1965 10 p refs Mariner IV spacecraft passed behind the planet, that is re- CFSTI HC $7 OO/MF $1 75 lated to the upper atmosphere of Mars. An attempt is made Vertical temperature distribution. diurnal heating and to show how the Martian atmosphere changes with altitude, tide%. and differential heating and general circulation at the i.e., the temperature profile, number density profiles, etc., solstices are discussed in connection with the circulation of together with the controlling physical and chemical processes. the Martian atmosphere A schematic diagram of solstice A summary of the more striking features of the upper at- circulation on Mars indicates that the winter hemisphere mosphere of Mars is tabulated. R.N.A. contains strong zonal west winds that increase with height, except for a shallow belt of easterlies near the ground in low latitudes. The summer hemisphere is dominated by easterlies increasing with height. except for a relatively shallow belt of surface westerlies The meridonal circulation associated N66-31481'# Paris Observatory, Meudon (France). with the eddy regime has descending motion toward the equa- CONTRIBUTION TO THE CALTECH-JPL COLLOQUIUM tor of the west wind maximum and ascending motion pole- ON THE MOON AND THE PLANETS: MARS (CONTRIBU- ward of the maximum, and such circulation results from the TION AU COLLOQUE CALTECH-JPL SUR LA LUNE ET zonal momentum produced by the eddies Various circula- LES PLANETES: MARS] tion estimates are given and observations are graphed Audouin Dollfus /n Calif. Inst. of Tech. Proc. of the Cal- M W.R. tech-JPL Lunar and Planetary Conf. 15 Jon. 1966 p 289- * 305 refs In FRENCH (See N66-31446 18-30) CFSTI, HC$7.00/MF$l 75 Attention is given to the measurement of water in the N66-31491'# National Aeronautics and Space Administration, atmosphere of Mars and the photometric properties of the Washington. D C. Martian soil in a review of contributions of the conference. THE SYSTEMATIC INVESTIGATION OF THE METEOROL- It is noted that water vapor is not always detectable in the OGY OF MARS

6 N66-31819

Morris Tepper In VPI Proc. of the Conf. on the Explora- We have obtained in the Schuster-Schwarzschild approx- tion of Mars and Venus Aug. 1965 14 p ref imation theoretical formulae describing the monochromatic CFSTI: HC $7.00/MF $1.75 transmissivity. reflectivity. and absorpiiviry of a cloud layer Weather observation and prediction for the manned Mars characterized by an arbitrary single scattering albedo and landing program is discussed Four approaches used in fore- anisotropic phase function The application of this formalism casting are briefly summarized: analogue, statistical, em- combined with exact solutions to the Mie theory problem to rpirical. and numerical. The dynamical or numerical approach the observed visual and near infrared reflectivity of Venus per- is chosen as the most applicable to Mars. The acquisition mits the determination of a number of properties of the Cyther- of atmospheric data globally on Mars is described as anal- ean cloud layer We confirm Strong's identification of ice as ogous to observations on Earth. A solution to the problem of. the principal constituent of the clouds. In addition the mean %obtaining data lies in the use of Earth orbiting satellites. The radius of cloud particles lies between 7.5~and lop. while satellite is discussed as an instrument platform and as a data the interaction optical depth of the layer is between 18 and collection and relay device. s. P. 43. Clouds with these properties allow a sizeable fraction of the incident sunlight to penetrate to the surface, but are extremely opaque to radiation thermally produced by the planet. N88-31639'# Smithsonian Astrophysical Observatory. Cam- A greenhouse mechanism therefore appears to be operative bridge, Mass. which can explain the high surface temperature of Venus. Author SELECTED STUDIES IN EXOBIOLOGY, PLANETARY ENVIRONMENTS, AND PROBLEMS RELATED TO THE ORIGIN OF LIFE Semiannual Progress Report No. 1. 1 Oct. 1986-31 Mar. 1988 N66-31642*# Smithsonian Astrophysical Observatory. Cam- Carl Sagan Jun. 1966 130p refs bridge. Mass. (Grant NGR-09-015-023) THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOS- (NASA-CR-76106) CFSTI: HC$4.00/MF$1.00 CSCLO6F PHERES Ellis R. Lippincott (Maryland Univ.), Richard V. Eck (Natl. CONTENTS: Biomed. Res. Found.). Margaret 0. Dayhoff, and Carl Sagan 1. AN ANALYSIS OF THE MARINER 2 MICROWAVE In its Selected Studies in Exobiol., Planetary Environments. OBSERVATIONS OF VENUS J. B. Pollack and C. Sagan 69 p and Probl. Related to the Origin of Life Jun. 1966 37 p refs refs (See N66-31640 18-40) (See N66-31639 18-04) CFSTI HC$4OO/MF $1.00 2. PROPERTIES OF THE CLOUDS OF VENUS C. Sagan The thermodynamic equilibrium composition of all pos- and J. B. Pollack 16p refs (See N66-31641 18-30] sible combinations of the elements C, H. 0. and N at reason- 3. THERMODYNAMIC EQUILIBRIA IN PLANETARY able average pressures and temperatures have been calculated ATMOSPHERES E. R. Lippincott (Md. Univ.), R. V. Eck. M. 0. for the atmospheres of Earth, Venus, Mars. and Jupiter All Dayhoff (Natl. Biomed. Res. Found.). and C. Sagan 37 p refs regions of the composition diagram consistent with the ob- (See N66-31642 18-30) served molecular abundances are located and discussed The atmosphere of Venus seems likely to be in thermodynamic equilibrium It then follows that the measured upper limits on * the abundances of CH4. NH3. and CO are all inconsistent with N86-31640*# Smithsonian Astrophysical Observatory. Cam- the possibility of elemental carbon or hydrocarbons in contact bridge. Mass. with the atmosphere, either on the surface or as clouds. Venus AN ANALYSIS OF THE MARINER 2 MICROWAVE OB- must have begun itsevolutionary history with a [C/O] abundance SERVATIONS OF VENUS ratio50 5. a value consistent with several cosmic abundance James B. Pollack and Carl Sagan In its Selected Studies in estimates The evidence for Mars is not inconsistent with Exobiol.. Planetary Environments. and Probl. Related to the thermodynamic equilibrium. Equilibrium abundances of all Origin of Life Jun. 1966 69 p refs (See N66-31639 18-04) oxides of nitrogen are extremely low even if computed with a CFSTI: HC $4.00/MF $1 00 considerable excess of 02. Under equilibrium conditions at low Limb-darkening observations of Venus by 19 mm micro- temperatures Jupiter also cannot contain significant amounts wave channel onboard Mariner 2 spacecraft were analyzed of any molecule not yet observed. However, at high tempera- and compared with ground-based measurements in a hot- tures simple hydrocarbons and cyanides. polycyclic aromatics. surface context. Peak brightness temperatures near the center and a variety of nitrogen compounds would be expected. Some of each scan. temperatures of the emitting level, and total of these compounds are brightly colored and possibly con- optical depths of the microwave attenuators were related to tribute to the observed variable coloration of Jupiter. Author the five following capacity models (1) transition of C02 and N 2 throughout the atmosphere, (2) water vapor absorption; (3) aerosol of absorbing dust; (4) isothermal absorbing cloud N66-31819*# AVCO Corp.. Lowell, Mass Space Systems layer: and 15) an aerosol of scattering particles. arbitrarily dis- Div tributed with altitude. Results rendered the C02-N2, the water COMPARATIVE STUDIES OF CONCEPTUAL DESIGN AND vapor, and the absorbing dust models untenable and suggested QUALIFICATION PROCEDURES FOR A MARS PROBE/ that the observed radiation arises from a hot surface and at- LANDER. VOLUME 111: PROBE, ENTRY FROM ORBIT. mosphere. G.G. BOOK 1: SYSTEM DESIGN Final Report T. R. Ellis et al 11 May 1966 302 p (Contract NASl -5224) N66-31641'# Smithsonian Astrophysical Observatory. Cam- (NASA-CR-66131; AVSSD-0006-66-RR. V 111, Bk-1) CFSTI bridge. Mass. HC$4.25/MF$l 75 CSCL22B PROPERTIES OF THE CLOUDS OF VENUS The system design of a nonsurvivable probe to perform Carl Sagan and James B Pollack In Its Selected Studies in engineering experiments for the determination of Mars at- Exobiol.. Planetary Environments, and Probl Related to the mospheric and terrain properties is presented The flight cap- Origin of Life, Jun. 1966 16 p refs (See N66-31639 18-04) sule is to be deployed from the flight spacecraft while in Mars CFSTI: HC$4.00/MF $1.00 orbit to allow use of shallow entry angles required by model

7 N66-31926

atmospheres which vary from 5- to 10- millibars surface ticles. planetology. planetary atmospheres and general top- pressures. The study includes all necessary parametric and sys- ics are presented. For individual titles see N66-32007-N66- tems analyses leading to a conceptual design. with particular 32043 emphasis on critical tradeoff regions and the necessary assumptions and decisions which have led to the conceptual design Experiment designs for television. surface hardness penetrometers. and wind measurement instrumentation which N66-32034*# National Aeronautics and Space Administration a is included in the science payload are discussed Mission con- Goddard Space Fliqht Center. Greenbelt. Md straints. subsystem characteristics. entry vehicle design. de- THE ORIGIN OF THE ATMOSPHERES OF VENUS AND orbif techniques. attitude control svstem tradeoffs. and cap- THE EARTH sule telecommunications are also reported. A. 0 A. G W Cameron In /ts Pub1 of Goddard Space Flight Center, 1963, Vol. I [1963] p 1337-1345 refs (See N66-32006 18-30) GPO HC$9 75. CFSTI. MF$7 50 Evidence regarding the Earth's atmosphere IS reviewed N66-31926'# Minnesota Univ . Minneapolis School of and it is concluded that there are no detectable traces of the Physics primitive solar nebula survivinq in it Evidence concerninq the A STUDY OF THE FEASIBILITY OF EMPLOYING A MAG- Venus atmosphere is analyzed and it IS concluded that it Drob- NETIC MASS SPECTROMETER FOR THE ANALYSIS OF ably contains of the order of 100 times the amount of nitroqen THE MARTIAN ATMOSPHERE in the Earth's atmosphere and neqliqible amounts of water Alfred 0 C Nier 20 Dec 1962 58 p refs Prepared for JPL vapor It is very difficult to see how the two atmospheres can (Contracts NAS7-100. JPL-950241) (NASA-CR-76498) CFSTI HC $2 50/MF $0 50 CSCL 03A have had a common oriqin. and it is proposed that the bulk of the Venus atmosphere is a remnant of the primitive solar A study of magnetic-sector mass spectrometers has been conducted to test the feasibility of employing such instruments nebula In order to account for the absence of primitive qases from the Earth's atmosphere, a modified form of the for making analyses of planetary atmospheres A number of designs of spectrometers were tried. as were appropriate Darwin-Wise hypothesis is proposed. according to which the transistorized electronic circuits A preliminary study of a Moon is formed as a result of the Earth's rotational instability induced for formation of the iron core Durinq such rota- miniature sputter ion pump was also carried out The investigations showed that essentially all but the weight specifica- tional instability the primitive qases would be entirely lost A discussion IS qiven of the circumstances surroundinq the tion given in SW-2751 could be met It is likely that further period of rotational instability Author studies will result in weight reductions. This would certainly be the case if a reconsideration of the entire problem showed that some of the other specifications could be modified Author

N66-32039'# National Aeronautics and Space Administration. a Goddard Space Fliqht Center, Greenbelt. Md N66-31944*# National Aeronautics and Space Administration. STRUCTURE OF PLANETARY ATMOSPHERES Marshall Space Flight Center, Huntsville, Ala S I Rasool In Its Pub1 of Goddard Space Flight Center. 1963. THE ATMOSPHERE OF MARS: A DERIVATION OF EN- Vol I [1963] p 1464-1485 refs (See N66-32006 18-30] 8r GINEERING AND DESIGN PARAMETERS GPO HC$9 75. CFSTI MF$7 50 W T Roberts and George S West 29 Jun 1966 38 p refs The properties of the atmospheres of Mars, Venus, and (NASA-TM-X-53484) CFSTI HC $2 OO/MF $0 50 CSCL Jupiter are reviewed in the liqht of the observational results 03 B stemminq from intensified research activity in the field of Three model atmospheres have been derived for use in planetarv atmospheres Temperature is the most siqnificant mission planning, aerospace lander design, and Martian parameter in studying planetary atmospheres, and as an aid orbiter and flyby studies Atmospheric parameters for these to the discussion. the temperature structure of the Earth's at- three models have been calculated from the planetary sur- mosphere is examined In order to fit the observed data. new face to 10,000 kilometers These three model atmospheres model atmospheres for the planets considered were derived The of differing atmospheric composition. surface pressure, and discussion of these models includes. atmospheric composition surface temperature are the upper density model (60 per- and pressure, vertical dtstribution of temperature. upper atmos- cent COz and 40 percent NZ). the mean density model (100 per- phere and ionosphere. and radiation belts HSW cent COz). and the lower density model (80 percent COz and 20 percent Ar) The general program of Kern and Schilling. with a few revisions. was used, this publication contains the details of the mathematical basis and program routines N66-32064'# National Aeronautics and Space Administration. in considerable depth The models chosen should provide Goddard Space Flight Center. Greenbelt. Md. values which will be of use as guidelines for the engineering ATMOSPHERIC SAMPLING INSTRUMENTATION and design of orbiting and landing vehicles Author Nelson W. Spencer In its Publ. of Goddard Space Flight Center, 1963, Vol. II [1963] p 583-586 CFSTI: HC $7.00/MF $5.00 N66-32006'# National Aeronautics and Space Administration The use of a capsule as instrument carrier for Martian Goddard Space Fhqht Center. Greenbelt. Md atmospheric measurements is advocated as a reliable and PUBLICATIONS OF GODDARD SPACE FLIGHT CENTER, safe exploration device. The capsule will enter the planetary 1963. VOLUME I: SPACE SCIENCES atmosphere by parachute and deploy its antennas and sensors * [1963] 1556 p refs during descent to the surface. Its sensors will obtain the fol- (NASA-TM-X-57737) GPO HC $9 75, CFSTI MF $7 50 lowing measurements: (1) atmospheric temperature and CSCL 03 B pressure data from thermistors and potentiometer gauges; A collection of articles, papers. talks, and reports on as- (2) mean molecular mass and air density from acoustic de- tronomy and astrophysics. celestial mechanics and geodesy. vices: and (3) the total amounts of C02 Hz0. and 03 for the @ solar physics. ionosphere and radio physics. fields and par- area between the sensor and the sun by-infrared absorption

8 N66-33526

detector. The obtained information can then be utilized to tion method has been employed. The analysis indicates a determine the temperature, pressure, density. and gross com- small but statistically significant negative correlation between position profiles of the Martian atmosphere. G.G. the extent of blue clearing and meteor shower activity. This result combined with the optical properties of the Martian atmosphere and the close resemblance between the characteristics of the blue haze and those of the terrestrial noctilu- N66-32302'# Southwest Center for Advanced Studies, Dallas. cent clouds suggests that variable amounts of interplanetary 'Tex dust are suspended in the Martian atmosphere and that the THE ATMOSPHERE OF MARS occasional clearings of the blue haze are caused by a diminish- Francis S Johnson 119661 16 p refs Presented at the COSPAR ing influx of these dust particles. Author 7th Intern. Space Sci Symp.. Vienna, 10-19 May 1966 (Grant NsG-269) (NASA-CR-76666) CFSTI. HC $l.OO/MF $0.50 CSCL 038 Much ne-w information has become available in recent years N66-33437'# New York Univ.. N. Y. Dept. of Meteorology on the Martian atmosphere Mariner IV data have shown that and Oceanography. the surface pressure is below ten millibars. a result that is not PROJECT HlAM Informal Report, Dee. 1966-May 1966 inconsistent with the most recent spectroscopic studies If Wayne E. Mc Govern 119661 21 p refs the Mariner IV ionospheric data are interpreted in terms of an (Grant NsG-499) F2 peak, the atmosphere must be very cold at all levels and (NASA-CR-77048) CFSTI: HC $1 .OO/MF $0.50 CSCL.01 B the exospheric temperature must be near 85°K This result is Progress is reported on a number of astrophysical and in disagreement with studies of radiative equilibrium tempera- geophysical studies. They include the atmosphere of Mercury. tures. which indicate a relatively warm exosphere. the tem- the atmosphere of Mars, the ashen light emission from the perature being in the vicinity of 400°K As a consequence of dark side of Venus, the 26-month oscillation of ozone con- this inconsistency and others of a similar nature. there is still centration, calculation of average single particle scattering a wide range of speculation concerning the properties of the functions for clouds and aerosols, calculation of the distribu- Martian atmosphere These inconsistencies will probably be tion of scattered radiation in a plane parallel atmosphere, resolved only after more detailed observations have been made heat budget of the earth, the earth's albedo, degradation of in planetary probes, such as the distribution of resonance the Tiros VI1 radiometers, optical constants of ammonium scattering of sunlight by atomic oxygen Author sulfate and sulfuric acids. and atmospheric breaking waves. R. N.A.

N66-33271# Army Electronic Proving Ground, Fort Hua- chuca, Ariz Research Div N66-33526+# Israel Program for Scientific Translations. Ltd , NUMERICAL SOLUTION OF THE TRANSPORT AND EN- Jerusalem ERGY EQUATIONS IN THE PLANETARY BOUNDARY PHYSICS OF THE MOON AND THE PLANETS LAYER 1. K. Koval'. ed. 1966 116 p refs Trans1 into ENGLISH of William D. Ohmstede Apr 1966 156 p refs "Fizika Luny i Planet" Kiev, Naukova Dumka. 1964 Prepared (ECOM-6020. AD-633694) CFSTI HC $5.00/MF $1.00 for NASA and NSF This report presents the development of an algorithm for (NASA-TT-F-382; TT-66-51019) CFSTI: HC $4.00/MF the approximate prediction of the physical behavior of the $1.00 CSCL 038 planetary boundary layer. For the sake of brevity, the problem is restricted to one which displays most of the essential fea- CONTENTS. tures involved By means of various approximations. the prob- 1. POLYCHROMATIC POLARIMETRY OF SOME lem is stated in mathematical terms The behavior of the LUNAR REGIONS V. V. Avramchuk p 1-10 refs (See N66- planetary boundary layer IS described by a system of non- 33527 19-30) linear partial differential equations of the parabolic type. and 2. SPECTROPHOTOMETRY OF SOME LUNAR OB-. boundary conditions at the earth's surface are developed in JECTS M. N. Mironova p 11-22 refs (See N66-33528 terms of the energy balance principle. through a priori anal- 19-30) ysis. It is ,nferred that the problem is well-posed. Various 3. SPECTRAL STUDIES OF THE LUNAR SURFACE finite-difference operators are proposed and shown to be con- A. N. Sergeeva p 23-33 refs (See N66-33529 19-30) sistent with the differential operators The boundedness and 4. ON THE STUDY OF THE OPTICAL PROPERTIES computational stability of the solutions of the finite-difference OF THE ATMOSPHERE AND SURFACE OF MARS 1. K. operators are discussed. It is concluded that the pure implicit Koval' p 34-39 refs (See N66-33530 19-30) nonlinear operator is the most satisfactory for the develop- 5. THE BRIGHTNESS DISTRIBUTION IN THE MARGI- ment of the algorithm. The algorithm is developed in detail NAL ZONE OF MARS L. A. Bugaenko. 0. 1. Bugaenko. 1. K. and several solutions are presented to illustrate the results Koval', and A. V Morozhenko p 40-42 refs (See N66-33531 obtainable from it. Author (TAB) 19-30) 6. RESULTS OF POLARIMETRIC OBSERVATIONS OF MARS IN 1962-1963 A. V. Morozhenko p 43-60 refs (See N66-33532 19-30) N66-33414'# California Univ., Berkeley. Space Sciences Lab. 7. DETERMINATION OF OPTICAL PARAMETERS THE BLUE HAZE OF MARS OF THE ATMOSPHERE AND SURFACE OF MARS A. V. Ann Palm 7 Dec. 1964 25 p refs Submitted for Publication Morozhenko and E. G. Yanovitskii p 61-68 refs (See N66- ltsSer No.5.lssueNo 70 33533 19-30] (Grant NsG 243-62) 8. APPROXIMATE SOLUTION OF THE PROBLEM OF (NASA-CR-59938) CFSTI. HC $l.OO/MF $0.50 CSCL 038 DIFFUSE REFLECTION AND TRANSMISSION OF LIGHT The extent of blue clearings is investigated as a function IN PLANETARY ATMOSPHERES WITH AN ARBITRARY '* of the number of the meteor showers intersecting Mars' SCATTERING INDICATRIX E. G. Yanovitskii p 69-82 refs orbit, at 10" intervals of heliocentric longitude. A rank correla- (See N66-33534 19-30)

9 N66-33530

9. DIRECT-READING RECORDING ELECTROPWAR- E. G. Yanovitskii In its Phys. of the Moon and the Planets IMETER OF THE MAIN ASTRONOMICAL OBSERVATORY 1966 p 69-82 refs (See N66-33526 19-30) CFSTI: HC OF THE ACADEMY OF SCIENCES OF THE UKRAINIAN $4.00/MF $1 .OO SSR 0. 1. Bugaenko p 83-93 refs (See N66-33535 19-30) Approximate methods are considered for the solution of 10. TYPES OF COMETARY TAILS A. A. Demenko the equation of radiative transfer in planetary atmospheres. p 94-103 refs (See N66-33536 19-30) and formulas for brightness factors are derived by a method based on certain Chandrasekhar relations. Both a medium of I infinite optical thickness and an atmosphere of finite optical thickness and an atmosphere of finite optical thickness are N66-33630'# Israel Program for Scientific Translations, Ltd.. treated. with appropriate formulas evolved for each case. The Jerusalem. accuracy of the formulas was estimated for a plane layer of ON THE STUDY OF THE OPTICAL PROPERTIES OF THE finite optical thickness, and the resultant graphs indicate that ATMOSPHERE AND SURFACE OF MARS the error in the calculations does not exceed 10% for the 1. K. Koval' In its Phys. of the Moon and the Planets 1966 simplest nonspherical indicatrix. It is concluded that, in p 34-39 refs (See N66-33526 19-30) CFSTI: HC $4.00/ the majority of cases, this estimate applies also to brightness MF $1.00 factors of the diffusely reflected and diffusely transmitted radi- Following a review of various findings dealing with the sur- ation. M.W.R. face of the moon. it is concluded that the distribution of energy in the visible spectrum of Mars and its color depend N88-34373*# National Aeronautics and Space Administration. mainly on surface energy distribution. The surface of Mars Langley Research Center. Langley Station, Va. may be regarded as covered by a powdered limonite which is DIRECT CALCULATION OF SPECIFIC HEATS AND RE- orange in color; and the visual albedo of Mars and the albedo LATED THERMODYNAMIC PROPERTIES OF ARBITRARY of the true surface may differ slightly from each other. During GAS MIXTURES WITH TABULATED RESULTS clear periods. fluctuations of the visual albedo in the violet Perry A. Newman and Dennis 0. Allison Washington, NASA, region may not be noticed. The true continent-mare contrast Aug. 1966 57 p refs at A = 400 mp is usually entirely blurred by an atmospheric (NASA-TN-D-3540) CFSTI: HC $2.50/MF $0.50 CSCL 20M veil produced by light scattering in the Martian atmosphere. It is shown that the partial derivatives.of the species In the 400 to 650 mp range, the light is scattered in the same concentrations can be computed using the same matrix of sense as Rayleigh scattering.so that toward lower wavelengths coefficients as that used in the free-energy minimization iterations the rate of limb darkening of the apparent disk is more gradual. to determine the equilibrium concentrations. The second-order At even greater wavelengths, coarse .particles float in the thermodynamk properties directly computed from these de- Martian atmosphere and result in a decrease in the limb dark- rivatives agree very well with existing properties (both directly ening to the infrared. M.W.R. and numerically obtained) for air considered as a mixture of ' ideal gases. Comparison of these results with recent imper- fect air results shows that the "mixture of ideal gases approximation" produces acceptable engineering data (error less than N66-33533"# Israel Program for Scientific Translations, Ltd.. 5percent) for temperatures 5 15.000" K and pressures 5102 at- Jerusalem mospheres. Tabulated results for the high-temperature thermo- ~ DETERMINATION OF OPTICAL PARAMETERS OF THE dynamic properties of NASA engineering model Mars at- ATMOSPHERE AND SURFACE OF MARS mosphere 3 are given for 36 pressures at each of 56 temper- A V. Morozhenko and E G. Yanovitskii In rts Phys. of the atures. Author Moon and the Planets 1966 p 61-68 rcfs (See N66-33526 19-30) CFSTI HC $4.00/MF $1 00 N66-34667*# Hamilton Standard Div.. United Aircraft Corp., The known brightness distribution of the Martian disk was Windsor Locks. Conn. used to determine the optical parameters of its atmosphere CONTINUATION OF STUDIES IN STATISTICAL DECI- and surface from absolute photometric data. A computa- SION THEORY IN LARGE SCALE BIOLOGICAL EXPERI- tional procedure and related tables are given which enable MENTS Final Report, 1 May 1966-31 Jul. 1966 the calculation of these optical parameters with relative ease Dian R. Hitchcock and Gordon B. Thomas 31 Jul. 1966 65 p and accuracy. It is assumed that the Martian highlands are refs orthotropically reflecting, that these parameters are con- (Contract NASw-871) stant for all scanned points of the highland from which the (NASA-CR-77234; SLS-6309R) CFSTI: HC $3.00/MF $0.75 brightness distribution curve is plotted, and that the atmos- CSCL 06C The empirical implications of the viewpoint that iiving phere of Mars does not absorb selectively in the entire range organisms characterized by some feature equivalent to or of wavelengths used in Martian photometry. In the 450 to 850 are implied by the negative entropy assumption is examined. The mp range, the Martian atmosphere is purely scattertng. below biological significance of atmospheric compositions and sur- this true absorption is felt which increases with decreasing wavelength During dust storms. the optical thickness of the face atmosphere reactions were studied, with emphasis placed Martian atmosphere in the infrared decreases with increasing on demonstrating the validity of a characterization of life in maintain a free energy wavelength because of the presence of coarse dust particles. terms of its ability to establish and M W R. gradient between itself and some portion of its environment. The Martian analysis atmosphere is analyzed, and the extra- polation of these results to a life detection experiment is considered. The distribution of n-alkanes in materials of biotic. abiotic. and unknown origin was observed to determine e N66-33534'# Israel Program for Scientific Translations. Ltd.. whether the order in these distributions could be computed Jerusalem. from a digitized gas chromatogram. A class of processes was APPROXIMATE SOLUTION OF THE PROBLEM OF DIFFUSE selected which are described in terms of the information which REFLECTION AND TRANSMISSION OF LIGHT IN PLANE- some subset of the ordinates of the observed chromatogram TARY ATMOSPHERES WITH AN ARBITRARY SCATTER- conveys about the whole chromatogram. Comparative data ' ING INDICATRIX on the various materials are presented. M.G.J.

10 N66-36942

N66-34876# RAND Corp.. Santa Monica, Calif. expressions corresponding to physical quantities such as directional REDUCTION OF THE EQUATIONS OF RADIATIVE TRANS- radiation and total fluxes emerging from a Rayleigh scattering FER FOR A PLANE-PARALLEL, PLANETARY ATMOS- atmosphere are also derived. Author (TAB) PHERE, PART I Zdenek Sekera Jun. 1966 84p refs (Contract AF49(638)-1700; Proj. RAND) ' (RM-4951-PR, Pt. I; AD-635284) N86-36683*# Avco Corp.. Wilmington. Mass. Research and A discussion is presented of the reduction of the equa- Technology Labs. tions of radiative transfer when the phase matrix is separable. FEASIBILITY STUDY OF AN OPTICAL RADIOMETER FOR A separable matrix is one that can be expressed as the prod- DETERMINING THE COMPOSITION OF THE MARS AT- * uct of two matrices, one whose elements depend on the di- MOSPHERE FROM SHOCK LAYER RADIATION DURING rectional parameters of the incident beam alone, and the ENTRY, VOLUME II Final Report other whose elements depend on the directional parameters J. A. Hull, R. N. Schweiger. and J. Shumsky May 1966 129 p of the scattered beam alone. When the phase matrix can be refs developed as a harmonic series in the azimuth difference be- (Contract NASw-1208) tween the vertical planes containing the scattered and in- (NASA-CR-73027) CFSTl: HC $3.00/MF $1.00 CSCL 2OF cident beams and each term of this series is separable. The This report describes the results of the instrumentation radiative transfer equations have series solutions with each feasibility and development program. The instrument require- term in these series being given by a product of three mai- ments are discussed considering both the experimental and rices; one of these is azimuth-independent; the other two, engineering problems. Filters and sensors are examined in which post- and pre-multiply this matrix, are the same mat- detail as to performance and survival of sterilization. Elec- rices whose product forms the corresponding term in the tronic circuitry is described and design considerations leading to choice of optical and electronic system configurations are phase matrix. Author (TAB) discussed. A brassboard instrument was constructed and is described with some preliminary calibration and operational data given. An error analysis was performed to establish the N66-35309*# National Aeronautics and Space Administration. accuracy requirements of the measurements. Author Goddard Space Flight Center, Greenbelt, Md. CONDITIONS OF ENCOUNTER BETWEEN DUST AND THE PLANTERS N68-38130"# National Aeronautics and Space Administration, Curtis W. Mc Cracken [1965] 30 p refs Submitted for Publi- Washington. D. C. cation PLANETARY ATMOSPHERES-A CONTINUING BIBLIO- (NASA-TM-X-57009) CFSTI: HC $2 OO/MF $0.50 CSCLO3B GRAPHY, FEBRUARY-MAY 1966 The conditions of encounter between interplanetary dust Aug 1966 135 p refs With Indexes particles and the planets are investigated for the range of (NASA-SP-7017(01)) CFSTI. HC $1.50/MF $1.00 CSCLO3B particle size where the force of solar radiation is not negligible in A continuing annotated bibliography. together with personal comparison with the force of solar gravity. The action of solar author and subject indices, on planetary atmospheres is presented. radiation pressure in reducing the heliocentric orbital speed of a Most of the entries pertain to investigations of Mars and Venus, small dust particle makes possible very low planetocentric speeds many of which are the result of the successful probes of the at encounter for an entire class of heliocentric orbits of non-zero atmospheres of Venus by Mariner II and Mars by Mariner IV. A eccentricity and fairly low inclination. The speed at encounter and limited number of references to the atmospheres of Jupiter, Mercury. the apparent radiant depend on the size of the dust particle for and Saturn is also included. References to such specific topics as the a given heliocentric orbit throughout the range of particle size theory of planetary origins, extraterrestrial environment, planetery being investigated by means of dust particle sensors mounted on exploration and spacecraft entry, and the physical properties of spacecraft. Author the planets are provided. Pertinent references to the techniques of planetary observation and measurement, e.g.. those involving photography, photometry, spectroscopy, astronomy, and meteorology, are also given. R.N.A. N66-35579# RAND Corp , Santa Monica, Calif. REDUCTION OF THE EQUATIONS OF RADIATIVE TRANSFER FOR A PLANE-PARALLEL, PLANETARY ATMOSPHERE, PART N88-38942# Observatoire de Paris (France). Section II d'Astrophysique Zdenek Sekera Jul. 1966 69 p refs POLARIMETRIC STUDY OF THE PLANET MARS Final (Contract AF 49(638)-1700; Proj. RAND) Scientific Report (RM-5056-PR; AD-635847) CFSTI: HC $6.00/MF $0.75 Audouin Dollfus and John H Focas 30 Apr. 1966 61 p refs A presentation of mathematical techniques necessary in unique (Contract AF 61(052)-508) solution of equations of radiative transfer in a homogeneous (AFCRL-66-492: AD-635928) CFSTI' HC $3.00/MF $0.75 atmosphere with Rayleigh scattering. The singular linear integral Analysis was made of five thousand two hundred measures equations for the x- and y-matrices appearing in the of the polarized light of Mars, collected during the last nine azimuth-independent terms of the reflection and transmission matrices apparitions of this planet, since 1948 The polarization curves for for the emerging radiation from a homogeneous, plane-parallel the bright and the dark areas of the planet are reproduced for atmosphere with Rayleigh scattering are reduced to four pairs of each one of the apparitions. The variation of the polarization for scalar equations of the forms discussed by T. W. Mullikin. The the spectral range 1.05 to 0.45 micron is examined A polarimetric nonuniqueness in the solutions of one of these pairs of equations and photometric study of selected samples of minerals indicated is removed by using linear constraints. The solutions are finally the presence, in the bright areas of the planet. of a fine powder expressed as linear combinations of Chandrasekhar's functions and of hydrated iron oxide of the limonite type. The seasonal variation are brought to the same form as that derived by Chandrasekhar, of the polarizing properties of the dark areas of Mars follows but by completely different methods. The new forms of the closely the variation of their darkness at Martian spring: this suggests solutions are particularly suitable from the computational point of a seasonal modification of their microscopic contexture The view when large optical thicknesses are involved. Mathematical luminance of the atmosphere of the planet amounts, for a

11 N66-37027 wavelength of 0 61 micron. to Ka (0.61 Micron) = 0.0006 stilb/phot; Three models for the atmosphere of Mars are compared. this corresponds to a surface pressure of 30 millibars. The In the Fp models, COZ is dissociated by solar ultraviolet radiation scattering coefficient of the atmosphere at 0.47 micron is K,(0.47 at 70 km altitude. and atomic oxygen predominates above 80 micron) = 0.00151 stilb/phot. This value shows that the kin The principal ion in the daytime ionospheric layer would be atmosphere of the planet is much too transparent in the blue to O+, and the topside of the layer would be isothermal at 90°K. mask the markings of the soil. Author The mesopause temperature minimum would be at or below the freezing point of Cop. and dry ice particles would form In the F1 models. molecular constituents predominate in the upper N66-37027*# Lockheed Missiles and Space Co, Palo Alto, atmosphere to 225 km, and molecular ions formed by solar Calif ultraviolet radiation and various chemical reactions would make CONVECTIVE AND RADIATIVE HEAT TRANSFER DURING up the ionospheric layers. The temperature in the isothermal height SUPERORBITAL ENTRY region would be between 150' and 250°K In the E model the H Hoshizaki and K. H Wilson Washington, NASA, Sep 1966 main ionization layer is formed by solar X-rays in a mixed upper 69 p refs atmosphere. The mass dens~tyin the upper atomosphere for the (Contract NAS7-295) E model would be more than two orders of magnitude larger (NASA-CR-584) CFSTI HC $2 50/MF $075 CSCL 20M than for the F1 models. and about lo4 times the mass density The convective and radiative heat transfer to vehicles entering at the same altitudes in the F2 models. The F2 models fit theory planetary atmospheres at superorbital velocities IS investigated and observation best. and identify the reacfion which is critical in An,integral method is employed to determine the radiative and defining a particular F2 modei. However. an F1 model might convective heating around a blunt body The effect of mass injection. result if photodissociation and diffusive separation are markedly radiative emission and absorption. radiation cooling. and coupling less than would be expected by analogy with the earth's upper between convection and radiation are included in the analysis atmosphere Author The absorption coefficients of the shock-layer gas. as well as the injected ablation products are determined as a functlon of particle-number density. temperature, and radiation frequency The N66-37946' # National Aeronautics and Space Administration. esults obtained show that self-absorption can rsduce the radiatve Goddard Space Flight Center, Greenbelt, Md. heating by an order of magnitude but has little effect on the' PUBLICATIONS OF GODDARD SPACE FLIGHT CENTER, convective heating The nose radius which results in the minimum 1964. VOLUME I: SPACE SCIENCES total heat-transfer rate at the stagnation point is much larger (6 119651 1636 p ref ft to 10 ft diam at U, =50,000fps) than the values indicated by (NASA-TM-X-57969) GPO HC $8 50. CFSTI MF $7 50 CSCL an optically thin analysis It is shown that the total stagnation-point 03 B heat-transfer rate is a very weak function of the nose radius. A collection of articles on astronomy. astrophysics. celestlal contrary to the results obtained from an optically thin analysis mechanics. .geodesy. solar physics. ionosphere and radio physics, Author fields and particl6s. planetology, and planetary atmospheres arr; (L presented For individual titles see N66-37947-N66-37973.

N66-37122'# Lockheed Missiles and Space Co., Palo Alto, Calif N66-37965'# National Aeronautics and Space Administration SPHERICAL PARTICLE TERMINAL VELOCITIES IN THE Goddard Space Flight Center, Greenbelt, Md a,' MARTIAN DAYTIME ATMOSPHERE FROM 0 TO 50 KILO- ORlOlN AND EVOLUTION OF ATMOSPHERES AND OCEANS METERS A G. W. Cameron, P. J. Brancazio. and N. W. Panagakos In its Albert D Anderson Sep 1966 37 p refs Publ. of Goddard Space Flight Center. 1964 Vol 1. Space Sci. (LMSC-6-76-66-21) CSCL 038 [I9651 p 907-91 1 Submitted for Publication (See N66-37946 The terminal velocities of spherical particles (density=3.0 23-30) GPO. HC $850 CFSTl MF $7 50 gm cm-3), with diameters from one to 10,000 microns. are Recent evidence for mechanisms which might add to or sub- presented for seven Martian daytime model atmospheres tract from the contents of planetary atmosphere and oceans are from 0 to 50 km. The model atmospheres are based on re- reviewed. Findings concerning the Earth's atmospheric origins and sults from the Mariner IV occultation experiment which gave composition are discussed, with emphasis on isotopic abundance densities in the Martian atmosphere that were much lower New data about the atmospheric composition of Mercury. Venus, than previous estimates. The following conclusions are reached Mars. Jupiter, and Saturn are mentioned. and uncertainties are concerning the yellow (dust) clouds. (1) The vertical velocities pointed out N E.N required to keep yellow-cloud particles of sizes 10 p or less aloft are greater on Mars than on earth, (2) The minimum N66-38722'# Johns Hopkins Univ.. Baltimore. Md. size of the grains primarily responsible for the local surface ULTRAVIOLET MEASUREMENTS IN PLANETARY yellow-cloud obscurations is about 20 microns (3) Particies ATMOSPHERES as small as 3 microns could be responsible for the rarer William G. Fastie [19661 29 p refs Submitted for Publication planet-wide obscurations lasting a month or more It is con- (Grant NsG-193) cluded that the tops of the dust clouds normally extend to (NASA-CR-78485) CFSTI: HC $2 OO/MF $0.50 CSCL 04A the tropopause (5-9 km), which usually limits the convec- The impact of the latest optical and electronic component tion in the Martian atmosphere Author developments on far ultraviolet rocket spectrophotometry is discussed Results of some recent experiments studying earth airglow N66-37214'# Stanford Univ , Calif Radioscience Lab and aurorae are reviewed. It is shown that weaker spectral THE ATMOSPHERE OF MARS: A COMPARISON OF features can be measured in the region 1100 to 3000 A than at DIFFERENT MODEL STUDIES BASED ON MARINER IV any longer wavelength. Author OCCULTATION DATA Scientific Reports 16 and 3 Gunnar Fjeldbo. Wencke C. Fjeldbo. and Von R Eshleman Jun 1966 24 p refs N66-38994# Air Force Systems Command, Wright-Patterson (Contract NgR-05-020-065. Grant NsG-377) AFB, Ohio. Foreign Technology Div. (NASA-CR-78134; SEL-66-054) CFSTI HC $1 OO/MF $0 50 THE NATURE OF RADIO NOISE EMISSION FROM THE CSCL 038 SURFACE OF VENUS

12 N67-12665

V. M. Vakhnin and A. I. Lebedinskiy In its Cosmic Res., Vol. Ill. Summary data are presented on an experimental program No 6 [19661 p 177-197 refs (See N66-38986 24-30) being conducted to measure and compare the total (over the CFSTI. HC $6.00/MF $1 25 whole body) equilibrium shock layer radiative beat transfer for three The somewhat high level of radio noise emission of Venus entry body shapes in a simulated Mars atmosphere. Simulated (600"-7OO0K) can be accounted for by "quiet" or "glow" discharges flight conditions are listed, similar to those expected to be

I in the upper atmosphere, which produce a 200°-300"K iccrease encountered in typical hyperbolic Mars entry trajectories where in radio noise above the true thermal emission. The main factor maximum stagnation point convective or radiative heat transfer determining the "quiet" or "glow" atmospheric discharge on Venus occur. The use of a ballistic range, a shock tube, and a shock would not be the electrical-storm phenomena characteristic for tunnel for measuring total radiation is proposed; the relative the earth, but may be the extremely slow rotation of the planet and advantages and disadvantages of each method is assessed. Figures )i the resulting low-turbulence, very intense atmospheric circulation depict the blunt cone, modified Apollo, and tension shell entry covering almost all of its surface. Calculations of the efficiency body shapes. Preliminary data from the ballistic range tests with which solar thermal energy is converted into radio-noise energy indicate that the modified Apollo shape is subject to much higher through intermediate stages-into energy of atmospheric circulation equilibrium shock layer radiation than either the blunt cone or and into electrical-current energy-indicates that the proposed tension shell. M.G.J. "gasdischarge" model of the radio noise is realistic. Author

N67-12128*# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadena. N66-39579# RAND Corp., Santa Monica, Calif. GAS CHROMATOGRAPHY COLUMN DEVELOPMENT FOR ANALYSIS OF THE MARTIAN ATMOSPHERE MANNED SATELLITE OBSERVATIONS AND PLANETARY W. F. Wilhite In its Space Programs Sum. No. 37-40, Vol. IV RESEARCH 31 Aug. 1966 p 119-123 CFSTI: HC $3.75/MF$1.25 D. Deirmendjian Aug. 1966 12 p refs Presented at the 17th By using a recently-developed porous polymer bead column Intern. Astron. Congr.. Madrid, 9-1 5 Oct. 1966 packing material, resolution of nearly all the components of interest (P-3418, AD-637780) CFSTI. HC $1 .OO/MF $0 50 in the Martian atmosphere can be obtained with one gas chromato- Certain terrestrial observations from a manned geophysical graphic column for a period of less than 15 min. Development of satellite are considered as a training ground for research on other the combined gas chromatograph-massspectrometer experiment to planets In particular, it is shown that the experience thus acquired separate atmospheric constituents is discussed, and the various is essential in solving some of the outstandmg problems of the constituents that require identification a[e listed. Th-e poor baseline Venusian atmosphere by means of a properly designed flyby stability that resulted from the use of temperature programming mission to that planet Author (TAB) during the separation of N and CO is noted: and the excellent stability obtained through the use of better flow control and a 50-80 mesh Porapak Q is reported. Further improvements permitted the resolution of all components of interest except oxygen. argon. and carbon monoxide which can easily be determined by mass spectrometry. The peak shape for all the components is excellent. 1967 except for ammonia and nitrogen dioxide which tail M.W R s STAR ABSTRACTS

N67-12664# Tel-Aviv Univ (Israel). lnst of Planetary and Space Science. BATSHEVA SEMINAR ON PLANETARY PHYSICS 1966 N67-12052*# Goodyear Aerospace Corp., Akron, Ohio. Final Report, Aug. 1Sep. 9.1966 STUDY OF EXPANDABLE, TERMINAL DECELERATORS FOR Uri Shafrir 13 Sep. 1966 69 p refs MARS ATMOSPHERIC ENTRY. VOLUME 11: SUPPORTING CFSTI: HC $Q.OO/MF $0.75 DATA AND TECHNICAL ANALYSIS Jay L. Musil 3 Oct. 1966 286 p refs Prepared for JPL CONTENTS: (Contracts NAS7-100; JPL-951153) 1. TWO FREQUENCY BEAT OCCULTATION EXPERI- MENT FOR A MARS ORBITER 2. Houminer (Natl. Committee (NASA-CR-79496: GER-12842, VOI.II) CFSTI: HC $6.00/MF for Space Res.) p 11-26 refs (See N67-12665 03-30) $0.50 CSCL 228 Aerodynamic characteristics. thermal environment and analytical 2. MEASUREMENTS OF SURFACE AND ATMOS- details, as well as preliminary design. development and testing of PHERIC PARAMETERS BY POLARiZATlON EXPERIMENTS expandable, terminal decelerator for application to Mars atmospheric FROM A MARTIAN ORBITER A. Yaniv and N. Levanon entry are delineated. Also considered are details on: sterilization p 27-39 refs (See N67-12666 03-30) and materials, decelerator envelope size established by thermal 3. MEASUREMENTS OF SURFACE AND ATMOS- requirements, auxiliary gas-inflation means for the decelerators, and PHERIC PARAMETERS BY GAMMA-SPECTROSCOPY free-flight test simulation. Further technical details are given on FROM A MARTIAN ORBITER G. Asaf and S T. Kruger weight calculations for several fabric decelerators for a Mars entry p 40-45 refs (See N67-'12667 03-30) capsule. Appendixed is a digital computer program for simulating 4. THE MEASUREMENT OF WATER VAPOR ON MARS the motion of re-entry vehicles with either rigidly erected or BY 6.3~ABSORPTION EXPERIMENT FROM AN ORBITER tethered deceleratory systems. R.LI. Y. Ben-Aryeh p 46-49 refs (See N67-12668 03-30) 5 PANEL DISCUSSION: "WHAT SHOULD BE THE PART OF ISRAEL IN SPACE-RELATED ACTIVITIES"? ., p 50-61 N67-12109*# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadena. COMPARISON OF ENTRY-BODY SHAPES FOR TOTAL EQUILIBRIUM RADIATION UNDER MARS ENTRY N67-12665# National Committee for Space Research, Tel Aviv ' CONDITIONS (Israel). H. J. Stumpf In its Space Programs Sum. No. 37-40. Vol. IV TWO FREQUENCY BEAT OCCULTATION EXPERIMENT FOR 31 Aug. 1966 p 28-31 refs CFSTI. HC$3.75/MF$1.2C A MARS ORBITER

13 N67-12666

Zwi Houminer In its Batsheva Seminar on Planetary Phys. 1966 An absorption spectroscopic method of quantitatively 13 Sep. 1966 p 11-26 refs (See N67-12664 03-30) CFSTI: determining the abundance of water vapor in the atmosphere of HC $3.00/MF $0.75 Mars from instrumentation aboard an orbiter is suggested. A band A two frequency beat occultation experimental procedure model theory for determining the atmospheric transmission function for studying planetary atmospheres is described. The techniques is described: and a geometric diagram of the suggested experiment can be used by a Mars orbiter. When an orbiter passes behind the is depicted. The use of infrared radiometric instruments aboard " planet as viewed from the earth, the radio ray path from transmitter planetary space probes to measure radiation from the sun is also to receiver passes tangentially through the ionosphere and discussed. LS. atmosphere and is occulted at the limb. The presence of an atmosphere and ionosphere causes the velocity of propagation of the radio signal to deviate from that in free space. because of the N67-12754# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadena. ~ non-unity refractive index of the neutral and ionized media. MARINER IV MEASUREMENTS NEAR MARS-INITIAL Calculations for the electron density of the ionosphere, and for the RESULTS: OCCULTATION EXPERIMENT: RESULTS OF refractivity profile of the neutral atmosphere, are presented. Data THE FIRST DIRECT MEASUREMENT OF MAR'S results from the Mariner IV occultation experiment are given, and are ATMOSPHERE AND IONOSPHERE discussed. It is concluded that the two frequency beat occultation Arvydas Uiore. Dan L Cain. Gereld S. Levy, Von R. Eshleman, method is a good technique for studying planetary atmospheres Gunnar Fjeldbo (Stanford Univ.) et al In NAS-NRC Exhaterrest. because it is simple to perform and does not add much to the Life 1966 p 362373 refs Reprinted Prepared jointly with orbiter weight. In addition, the method permits diurnal and seasonal Stanford Univ. Available from NAS-NRC, changes in different regions of the atmosphere to be studied from Washington. D. C.: $6.00 a single orbiting satellite. L.S. (Contract NAS7-100; Grants NGR-05-020-065; NsG-377) Changes in the frequency, phase, and amplitude of the Mariner IV radio signal, caused by passage through the atmosphere and ionosphere of Mars, were observed immediately before and N67-12666# Tal-Aviv Univ. (Israel). Inst. of Planetary and Space after occultation by the planet. Preliminary analysis of these effects has Science. yielded estimates of the refractivity and density of the atmosphere MEASUREMENT OF SURFACE AND ATMOSPHERIC near the surface, the scale height in the atmosphere, and the PARAMETERS BY POLARIZATION EXPERIMENTS FROM A electron density profile of the Martian ionosphere. The atmospheric MARTIAN ORBITER density, temperature, and scale height are lower than previously Akiva Yaniv and Nadav Levanon In its Batsheva Seminar on predicted, as are the maximum density, temperature, scale height, Planetary Phys. 1966 13 Sep. 1966 p 27-39 refs (See and altitude of the ionosphere. Author N67-12664 03-30) CFSTI: HC$3.00/MF$0.75 A means of measuring Martian surface and atmospheric parameters (chemical and physical surface structure, cloudiness N67-13018*# GCA Technology Div.. GCA Corp., Bedford, Mass. w and turbidity of the atmosphere, pressure profile of atmospheric TEMPERATURE DETERMINATION OF PLANETARY density, ice cap composition, and ice cap geometry as a function ATMOSPHERES. OPTIMUM BOUNDARY CONDITIONS FOR of season) by light polarization experiments using instrumenta- BOTH LOW AND HIGH SOLAR ACTIVITY tion aboard a Martian orbiter space probe, is described. The R. A Minzner and G. 0. Sauermann Feb. 1966 55 p refs polarization phenomenon, the instrumentation. and the geom- u (Contract NASw-1225) etry of the proposed experiment are also described. Tables of (NASA-CR-79525; GCA-TR-66-6-N) polarization data for basalt, granite, quartz sandstone, red CFSTI: HC $3.00/MF $0.50 CSCL 038 sandstone, and water droplets are given. The data indicate how One-gas and two-gas methods are proposed for obtaining material type, size, roughness, or smoothcess, or water vapor accurate temperature-altitude profiles. Using atmospheric models affect changes in the polarization readings. L.S. for both high and low solar activity. analytical and numerical examinations of the single gas and double gas equations for both high and low altitude reference levels indicate the conditions which N67-12667# Weizmann Inst. of Science, Rehovoth (Israel). optimize each type of calculation. The method depends upon the MEASUREMENTS OF SURFACE AND ATMOSPHERIC use of airborne mass spectrometers with detection sens PARAMETERS 5Y GAMMA-SPECTROSCOPY FROM A the order of lo4 to 105 particles per cubic centimeter. To verify MARTIAN ORBITER the relative suitability of the several approaches, a rigorous error Gad Asaf and Steve T. Kruger In Tel-Aviv Univ. Batsheva Sminar analysis based on the Gaussian method was performed for each on Planetary Phys. 1966 13 Sep. 1966 p 40-45 refs (See case considered. The results show: (1) For optimum conditions, N67-12664 03-30) CFSTI: HC$3.00/MF$0.75 the high altitude reference level should be chosen as the altitude A proposed method of measuring the surface and atmospheric for which the uncertainty in observed number-density data is parameters of Mars by means of a gamma ray spectrometer 100%. (2) Absolute temperature uncertainty is not strongly aboard the Voyager orbital mission is discussed. Possible information influenced by variations in number-density models associated with on the composition and past history of Mars which might be variations in solar activity. (3) The percentage uncertainty at high obtained through measurements of the gamma rays emerging from altitudes, however, is strongly influenced by such variations in the Martian surface and atmosphere are examined in ;3ieneral number-density models. M.G.J. way. Natural radioactivity sources @, TQS, and U , and cosmic ray induced radioactivity are discussed. A Csl(tl) crystal instrumentation system is described; and tables of data regarding N67-15280*# RAND Corp., Santa Monica, Calif. radionuclides are given. L.S. A NUMERICAL GENERAL CIRCULATION EXPERIMENT FOR THE ATMOSPHERE OF MARS C 8. Leovy and Y. Mine Dec. 1966 48 p refs N67-12668# Israel Inst. of Tech., Haifa. Dept. of Physics. (Contract NASr-2 1J THE MEASUREMENT OF WATER VAPOR ON MARS BY (NASA-CR-81146: RM-5110-NASA) CFSTI: HC $3 OO/MF $0.65 6.3~ABSORPTION EXPERIMENT FROM AN ORBITER CSCLO3B Yacob Ben-Aryeh In Tel-Aviv Univ. Batsheva Seminar on Planetary A numerical model for simulating the general circulation as Phys. 1966 13 Sep. 1966 p 46-49 refs (See N67-12664 of the atmosphere of Mars IS described and preliminary results 03-30) CFSTI: HC $3.00/MF $0.75 from an initial experiment are given. The experimental conditions

14 N67-16801

correspond to the Northern Hemisphere winter solstice on a planet, progress was achieved on observation of noctilucent clouds in in the orbit of Mars. having an atmosphere composed entirely of planetary atmospheres. S.P. Cqand an initial surface pressure of 5 mb. The important features indicated by the model are development of a fluctuating wave regime in the winter hemisphere. a large amplitude diurnal tide, N67-16722*# General Electric Co.. Philadelphia, Pa. Space and condensation of COz to form a winter polar ice-cap. The Sciences Lab.

S, S, preliminary character of this experiment is stressed and some future STUDY OF EQUILIBRIUM AIRTOTAL RADIATION improvements are proposed. Author J. S. Gruszaynski and W. R. Warren, Jr. 1966 51 p refs (Contract NASw-939) (NASA-CR-81315) CFSTI: HC$3.00/MF$0.65 CSCL 20M N67-15764*# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadeha. Results are presented from a study of high temperature air VENUS CAPSULE SCIENCE radiance applicable to superorbital reentry vehicles. Consideration R. G. Brereton. R. W. Davies, and C. E. Griffin In its Space is given to equilibrium radiation in air and gas mixtures assumed to Programs Sum. No. 37-41, Vol. IV 31 Oct. 1966 p 285-289 represent the atmospheres of the near planets. Several theoretical refs CFSTI: HC$3.00/MF$0.65 approaches to the problem are reviewed and compared. A shock Instruments for measuring the altitude dependent physical tube experiment has shown that an electrically driven conventional properties of the Cytherean atmosphere from an entry capsule are tube is capable of producing useful model stagnation region test flows described. The purpose of these measurements is to establish an to the 60,000 ft/sec flight velocity simulation level. Experimental altitude profile of gas density, temperature. pressure. and gas radiance data, obtained in the vicinity of a simulated 38,000 composition. A suggested capsule scientific payload weighing about ft/sec flight velocity, show that there is a significant contribution 16 Ib. is discussed which consists of a thermodynamic variables to intensity in the vacuum ultraviolet portion of the spectrum. package, atmospheric composition experiment, impact Also. there appears to be a contribution to intensity in the wavelength accelerometer, visual and/or UV photometer, and triaxial region between the quartz and LiF cut-off values. A.G.O. accelerometer. A.G.O.

N67-16801*# National Aeronautics and Space Administration, N67-15904*# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadena Washington, D. C. ENTRY CAPSULE ORBIT DETERMINATION ACCURACY PROBLEMS IN ASTROPHYSICS. INVESTIGATION OF THE C. Scranage In its Space Programs Sum. No 37-42, Vol. 111 30 ATMOSPHERES OF VENUS AND MARS Nov. 1966 p 8-12 CFSTI: HC $3.00/MF$0.65' 1. K. Koval', ed. Jan. 1967 169 p refs Transl. into ENGLISH The feasibility of an on-board tracking system of two-way of the Book "Voprosy Astrofiziki. lssledovaniye Atmosfer Venery i coherent doppler between an entry capsule and an orbiting bus Marsa" Kiev, Izd. Naukova Dumka, 1965 Papers Presented at for determining the orbit of an entry capsule and estimating Conf. of the Working Group on Invest. of Venus and Mars, Kiev, atmospheric parameters was studied Presented is a discussion of Jun. 1964 entry and impact statistics of the orbital parameters, a description (NASA-TT-F-394) CFSTI: HC$B.OO/MF $0.65 CSCL 036 of computer programs and procedures, and a presentation of the estimated uncertainties on the atmospheric constants. Results CONTENTS ~~ indicate that: (1 The proposed system is a highly reliable observable 1. SPECTROSCOPIC INVESTIGATION OF THE COMPOSI- for determining the orbit of an entry capsule and estimating TION OF THE ATMOSPHERE OF VENUS V. K. Prokof'yev atmospheric parameters: and (2) The uncertainties on the estimates p 1-5 (See N67-16802 07-30) of the parameters do not appear to be as dependent on the 2. NOCTURNAL AIRGLOW OF VENUS N. A. Kozyrev inherent accuracy of the system as with an Earth-based system. p 6 (See N67-16803 07-30) Most significant of the results is that this new observable 3. THE IONOSPHERIC HYPOTHESIS OF RADIO EMISSION determined the stratosphere scale height, surface temperature, and , FROM VENUS A. D. Danilov and S. P. Yatsenko p 7-12 refs stratosphere base temperature to a greater accuracy than was (See N67-16804 07-30) attained by the Mariner IV Mars occultation experiment. S.C.W. 4. EFFECT OF VENUS CLOUD COVER IN RADIO EMISSION OF THE PLANET IN THE CENTIMETER AND MILLIMETER BANDS G. M. Strelkov p 13-37 refs (See N67-16805 07-30) N67-16515*# GCA Technology Div.. GCA Corp.. Bedford, Mass. 5. RESULTS FROM A PRELIMINARY ANALYSIS OF SOME EXPERIMENTAL AND THEORETICAL STUDIES IN SPECTROGRAMS OF VENUS TAKEN IN APRIL 1964 V. V. PLANETARY AERONOMY Quarterly Progress Report, 17 Avramchuk and 1. K. Koval' p 38-42 refs (See N67-16806 Sep.-30 Nov. 1966 07-30) F. F. Marmo Dec. 1966 131 p refs 6. OPTICAL PROPERTIES OF THE MARTIAN ATMOSPHERE (Contract NASw-1283) FROM DATA OF PHOTOMETRIC OBSERVATIONS N. P. (NASA-CR-81262; QPR-7) CFSTI: HC $3.00/MF $0.65 CSCL Barabashov p 43-51 refs (See N67-16807 07-30) 038 7. SOME REMARKS ON HYPOTHESES OF AN ABSORPTIVE Technical summaries are presented for studies in ATMOSPHERE ON MARS V. V. Sharonov p 52-60 refs (See photochemistry of planetary gases, planetary aeronomy, and N67-16808 07-30) experimental investigations in the VUV (2000-1000 A) and the 8. A. MODEL FOR THE MARTIAN ATMOSPHERE AND EUV (below 1000 spectral regions. Results are discussed for the PLANETARY SURFACE FROM THE STANDPOINT OF A photochemistry of planetary gases in the EW and for investigations HYPOTHESIS ASSUMING AN ATMOSPHERE WITH PURELY of ion-molecule reactions in planetary atmospheres. Theoretical SCATTERING PROPERTIES V. V. Sharonov p 61-65 refs (See - studies included work on the cooling rates of hot electroncs in the N67-16809 07-30) Earth's atmosphere. Absorption and photoionization cross sections 9. SOME CONSIDERATIONS ON THE AEROSOL were measured for the atomic atmospheric species in the VUV COMPONENT OF THE MARTIAN ATMOSPHERE N. N. and EUV. The kinetic energy and spatial distribution of ejected Sytinskaya p 66-68 (See N67-16810 07-30) photoelectrons due to VW and EUV photoionization was measured. 10. ON THE AEROSOL COMPONENT OF THE MARTIAN Experimental devices such as windows. filters, and counters. were ATMOSPHERE E. G. Yanovitskiy p 69-78 refs (See N67-16811 designed for use in the VUV and EUV investigations. Significant 07-30)

15 N67-16802

11. THE COLOR OF MARS AS A RESULT OF THE OPTICAL N67-16804*# National Aeronautics and Space Administration, PROPERTIES OF ITS ATMOSPHERE N. A. Kozyrev p 79 (See Washington, D. C. N67-16812 07-30) THE IONOSPHERIC HYPOTHESIS OF RADIO EMISSION 12. CHEMICAL COMPOSITION, PRESSURE AND FROM VENUS TEMPERATURE OF THE MARTIAN ATMOSPHERE FROM DATA A. D. Danilov and S. P. Yatsenko In its Probl. in Astrophysics. OF INFRARED SPECTROSCOPY V. 1. Moroz p 80 (See Invest. of the Atmospheres of Venus and Mars Jan. 1967 p 7- N67-16813 07-30) 12 refs (See N67-16801 07-30) CFSTI: HC $3.00/MF $0.65 * 13. BRIEF ANALYSIS OF A PHOTOMETRIC STUDY OF The hypothesis proposed by Strelkov that the high tempera- BRIGHTNESS DISTRIBUTION ACROSS THE MARTIAN DISK 1. K tures of centimeter radio waves emitted from Venus is explained Koval' p 81-84 refs (See N67-16814 07-30) by radioactive heating of the planetary surface is discussed. The 14. USING SPECTROPHOTOMETRIC DATA TO VERIFY hypothesis is weakened by observations that indicate Venus THE HYPOTHESIS OF A LIMONITE COVERING ON MARS 1. 1. has a thick ionosphere. Detailed analysis shows that the ion- Lebedeva p 85-90 refs (See N67-16815 07-30) ospheric model may be used as a basis for a complete explana- 15. USE OF INDICATOMETRY FOR VERIFYING THE tion of the spectrum of brightness temperatures observed in HYPOTHESIS OF A LIMONITE SURFACE COVER ON MARS T. D. the radio emission from Venus, although a much stronger en- Bessonova p 91-94 refs (See N67-16816 07-30) ergy source would be needed than that provided by the Earth's 16. POLARlZATlON STUDIES OF RADIO EMISSION FROM ionosphere. Available data show a possible correlation between THE UPPER LAYER AND SURFACE COVERING OF THE solar activity and the brightness temperatures of centimeter PLANETS A. Ye. Basharinov. M. A. Kolosov. and A. A. radio emission from Venus. A positive confirmation of this cor- Kurskaya p 95-96 refs (See N67-16817 07-30) relation would be an important factor in explaining the mech- 17. POLYCHROMATIC POLARIMETRY OF LIGHT IN THE anism responsible for this radio emission. Author TWILIGHT AND DAYTIME SKY AT THE ZENITH V. V.' Avramchuk p 97-104 refs (See N67-16818 07-1 3) N67-16805*# National Aeronautics and Space Administration. 18. INTENSITY MICROPHOTOMETER BASED ON THE Washington, D. C. MF-4 L. A. Bugayenko and K. Ye. Skorik p 105-109 refs EFFECT OF VENUS CLOUD COVER ON RADIO EMISSION (See N67-1681907-14) OF THE PLANET IN THE CENTIMETER AND MILLIMETER 19. TAKING ACCOUNT OF SCATTERING ANISOTROPY IN BANDS DETERMINING THE OPTICAL PARAMETERS OF THE MARTIAN G. M. Strelkov In its Probl. in Astrophysics. Invest. of the ATMOSPHERE AND SURFACE A. V. Morozhenko and E. G. Atmospheres of Venus and Mars Jan. 1967 p 13-37 refs (See Yanovitskiy p 110-1 14 refs (See N67-16820 07-30) N67-16801 07-30) CFSTI: HC$3.00/MF$0.65 An atmospheric model with structural parameters determined by astronomical observations is used to explain the high effective temperature of radiation emission from Venus in the centimeter N67-16802*# National Aeronautics and Space Administration, band. It is assumed that the cloud cover of Venus has a 3 km I$ Washington, D. C. layer of water droplets under an 8 km layer of ice qrystals; and SPECTROSCOPIC INVESTIGATION OF THE COMPOSITION spectral characteristics of the brightness temperature for 0.3 to 22 THE ATMOSPHERE OF VENUS OF cm emissions were calculated for surface pressures of 5 and 10 V. K. Prokof'yev In its Probl. in Astrophysics. Invest. of the atm. Comparison of these characteristics with measured data at , Atmospheres of Venus and Mars Jan. 1967 p 1-5 (See various wavelengths indicates that ?he planetary cloud cover contains N67-16801 07-30) CFSTI: HC$3.00/MF$0.65 neither water nor solid nonconductive powders. Emission from the Basic components of the Venutian abnosphere, as determined by heated interior is considered as an explanation for the high effective spectroscopic studies, are discussed. The hypothesis that nitrogen temperature of radio emission from Venus in the centimeter range; is the main atmospheric component is considered fairly well with the depths of these layers dependent upon optical thickness ascertained: and attention is given to the carbon dioxide, oxygen, of the rocks making up the planetary crust. High temperature water vapor, and other gaseous components. Various investigations gradients in the subsurface layers of the soil are not considered to are mentioned, including the interpretation of a banded structure be involved. M.W.R. as a formaldehyde emission. It is acknowledged that the spectrum of Venus is not an exact duplicate of the solar spectrum, and that N67-16806*# National Aeronautics and Space Administration, there are data to indicate that absorption in carbon dioxide bands undergoes changes. M.W.R. Washington, D. C. RESULTS FROM A PRELIMINARY ANALYSIS OF SOME SPECTROGRAMS OF VENUS TAKEN IN APRIL 1964 V. V. Avramchuk and 1. K. Koval' In its Probl. in Astrophysics. N67-16803'# National Aeronautics and Space Administration. Invest. of the Atmospheres of Venus and Mars Jan. 1967 Washington, D.C. p 38-42 refs (See N67-16801 07-30) CFSTI: HC $3.00/MF NOCTURNAL AIRGLLOW OF VENUS $0.65 N. A. Kozyrev In its Probl. in Astrophysics. Invest. of the At- A spectrogram of Venus taken on April 21, 1964, reveals a mospheresof Venus and Mars Jan. 1967 p 6 (See N67-16801 bright detail with a diameter of approximately 4 in: with the 07-30) CFSTI: HC $3.00/MF $0.65 spectrograph slit oriented along the line through the horns of Spectral observations indicate that the Venus night airglow the crescent close to the middle zone of the terminator. This is composed of both luminescence from the lower atmospheric spot is well defined in the ultraviolet region, gradually fades layers that is uniformly distributed over the dark side, as well as toward the long wave end of the spectrum, and vanishes at M=p. ionospheric luminescence that presents a narrow ring at the Another spectrogram taken April 27, with slit orientation along edge of the planete- luminescence from the lower the intensity equator was analyzed to determine the energy

atmospheric layers 3;: le of the two. has the spectrum range in the 370 to 500 M=F range. A considerable drop in the * of formaldehyde 8 ~ . the result of hydrocarbon oxi- curve for monochromatic albedo is noted for the point on the dation in the ir - ;urface of Venus. Ionospheric limb toward the ultraviolet end of the spectrum: and there is a luminescence ic changes, and there appears lesser drop for the terminator. The difference in the curves of :h luminescence and solar monochromatic albedo for the limb and terminator of Venus activity. Emisss scence have been identified may explain the change in the color of the planet with phase, as $ by various au' ' d?n, or carbon dioxide under well as the difference in violet absorption observed at different the influence I M.W.R. times. M.W.R.

16 N67-16817

N67-16807*# National Aeronautics and Space Administration, N. N. Sytinskaya In its Probl. in Astrophysics. Invest. of the Washington, D. C. Atmospheres of Venus and Mars Jan. 1967 p 66-68 (See OPTICAL PROPERTIES OF THE MARTIAN ATMOSPHERE N67-16801 07-30) CFSTI: HC$3.00/MF$0.65 FROM DATA OF PHOTOMETRIC OBSERVATIONS Particles suspended in a gas may have a strong effect N. P. Barabashov In its Probl. in Astrophysics. Invest. of the on the scattering properties of the medium without changing its Atmospheres of Venus and Mars Jan. 1967 43-51 refs (See mass and density to any great extent. For this reason, photometric 'N67-16801 07-30) CFSTI: HC $3.00/MF $0.65 data on mass, density and surface pressure for the Martian An analysis of photometric data for Mars based on the atmosphere must be analyzed to isolate the contributions from gas theory of light scattering in planetary atmospheres indicates and aerosol to the brightness of the atmospheric layer. Since that the atmosphere probably has a low optical thickness. The there have been no satisfactorily reliable methods proposed for this %scattering properties of the Martian atmosphere are chiefly in purpose, the author reverses the process and uses pressure data the visible region of the spectrum. The true absorption increases obtained by other methods for a photometric study of the suspended toward the short-wave end of the spectrum, although even here particles. Author the optical thickness of the atmosphere is relatively low. Many areas in maria show a greenish hue. Author N67-16811*# National Aeronautics and Space Administration, Washington, D.C. N67-16808*# National Aeronautics and Space Administration, ON THE AEROSOL COMPONENT OF THE MARTIAN AT- Washington, D. C. MOSPHERE SOME REMARKS ON HYPOTHESES OF AN ABSORPTIVE E. G. Yanovitskiy In its Probl. in Astrophysics. Invest. of the ATMOSPHERE ON MARS Atmospheres of Venus and Mars Jan. 1967 p 69-78 refs V. V. Sharonov In its Probl. in Astrophysics. Invest. of the At- (See N67-1680107-30) CFSTI: HC$3.00/MF$0.65 mospheres of Venus and Mars Jan. 1967 p 52-60 refs (See Consideration is given to the discrepancy between data for N67-16801 07-30) CFSTI: HC $3.00/MF $0.65 the atmospheric pressure on the Martian surface from spec- Models for the atmosphere and surface of Mars are re- troscopic measurements and data for this pressure according viewed that assume that the atmosphere has absorptive rather to photometric and polarimetric observations. This difference than scattering properties and that the red color of the planet is explained by the fact that light scattering by aerosol particles is due to selective absorpticg ,in the atmospheric layer. The with radii r<10-6 cm is not considered when using photometric Carrer-Kiess hypothesis, which atfributes selective extinction and polarimetric observations for determining surface pres- to nitrous oxide in the Martian atmosphere, is inadmissible sure. The terrestrial atmosphere is used as an example to since the absorption band for this compound in the spectrum confirm this assumption. It is found that the number of aero- of the planet is either absent or extremely weak. The model sol particles with radii of the order of cm in a column of proposed by N. A. Kozyrev is not in accord with the observed Martian atmosphere with a base of 1 cm2 IS 1015 l/cm2. brightness distribution along the radius of the disk as has al- It is shown that the Martian atmosphere has a higher satura- * ready been pointed out in a number of articles. Opiks calculation of fine particles of aerosol per unit of mass than that of tions are self-consistent. although they assume optical proper- the Earth Author ties in the atmosphere that have no sound physical basis. It IS considered extremely improbable that the Martian atmosphere .. has absorptive properties. Author N67-16813* # National Aeronautics and Space Administration, Washington, D.C. CHEMICAL COMPOSITION. PRESSURE AND TEMPERA- N67-16809*# National Aeronautics and Space Administration. TURE OF THE MARTIAN ATMOSPHERE FROM DATA OF Washington. D. C. INFRARED SPECTROSCOPY A MODEL FOR THE MARTIAN ATMOSPHERE AND PLAN- V. 1. Morov In its Probl. in Astrophysics. Invest. of the At- ETARY SURFACE FROM THE STANDPOINT OF A HY- mospheres of Venus and Mars Jan. 1967 p 80 (See N67- POTHESIS ASSUMING AN ATMOSPHERE WITH PURELY 16801 07-30) CFSTI: HC $3.00/MF $0.65 SCAlTERlNG PROPERTIES Infrared spectroscopy of Mars revealed a series of new V. V. Sharonov In its Probl. in Astrophysics. Invest. of the C120216 bands, the C'3021s band, and four new unidentified Atmospheres of Venus and Mars Jan. 1967 p 61-65 refs bands. The C120zr6 bands at 1.6 and 2.05 p give a (See N67-16801 07-30) CFSTI: HC $3.00/MF $0.65 product of CO2 by pressure equal to 170 g/cm2mbar: and The author reviews the state of the art in attempts tc apply other studies have indicated the pressure in the Martian at- photometric data for explaining the nature of Mars It is pointed mosphere is about 15 mbar clase to the surface. It is. therefore. out that this problem has no unique solution since the rela- assumed that the pressure is in the 10 to 30 mbar range, which tionship between brightness across the disk and optical charac- is considerably lower than previous estimates from photometric teristics of the atmosphere depends on atmospheric composi- and polarization data. tion and structure. Thus all calculations of atmosphgr c characteristics such as optical thickness, mass and surfack pressure are always based on some predetermined model. Since there is N67-16817*# National Aeronautics and Space Administration, an infinite selection of possible models, analogy with terres- Washington. D. C. trial conditions is assumed to be most probable. This point of POLARIZATION STUDIES OF RADIO EMISSION FROM THE view gives preference to a model in which the visible region of UPPER LAYER AND SURFACE COVERING OF THE the atmospheric spectrum is assumed to have purely scattering properties and the surface is considered to be covered with PLANETS limonite dust. The nature of the polar caps and the violet layer A. Ye. Basharinov. M. A. Kolosov, and A. A. Kurskaya In its Probl. in Astrophysics. Invest. of toe Atmospheres of Venus and are problems which are still unsolved. Author Mars Jan. 1967 p 95-96 refs (See N67-16801 07-30) CFSTI: HC$B.OO/MF $0.65 Polarization studies of inherent and reflected radio emission N67-16810*# National Aeronautics and Space Administration, in the centimeter and decimeter bands were used to obtain Washington, D. C. information on the structure of the upper layer and surface coverings SOME CONSIDERATIONS OF THE AEROSOL COMPONENT of the planets. Polarization properties of the inherent radio emission OF THE MARTIAN ATMOSPHERE from the moon in the centimeter range were used to obtain a

17 N67-16820

more precise determination of the dielectric constant, and to evaluate implications of a nonsynchronous rotation of the planet on the the roughness of the upper surface layer. Similar data were atmosphere are discussed. Several atmosphere models consistent obtained from polarization studies of radio echoes from Venus on with observations are constructed in an attempt to determine if a 12 cm wavelength. Instrumentation used for the polarization they are stable against depletion of the atmosphere by gravitational studies are mentioned; and other polarization data in the SHF escape. Results are discussed fmm the viewpoint of the atmospheric range are briefly reviewed. L.S. surface. R.N.A. *

N67-16820*# National Aeronautics and Space Administration, N67-18280*# National Aeronautfcs and Space Administration. Washington, D. C. Goddard Space Flight Center, Greenbelt Md. TAKING ACCOUNT OF SCATTERING ANISOTROPY IN ON THE LIMB DARKENING OF PLANETARY DETERMINING THE OPTICAL PARAMETERS OF THE ATMOSPHERES IN THE THERMAL INFRARED MARTIAN ATMSOPHERE AND SURFACE Robert E. Satnueleon [1965] 12 p refs Submittedfor Publication A. V. Morozhenlqo and E. G. Yanovitskiy In its Probl. In (NASA-TM-X-57359) CFSTI: HC$3.00/MF$0.65 CSCL 038 Astrophysics. Invest. of the Atmospheres of Venus and Mars. Jan. Thermal maps of Venus and Jupiter have demonstrated 1967 p 110-1 14 refs (See N67-16801 07-30) CFSTI: HC that limb darkening in the 8 to 14 micron wavelength interval is $3.001 MF$0.65 pronounced for these two planets. Sinca both planets are mpletely Absolute photometric data for spherical and elongated cloud anrered, it is possible that both anisotropic multiple scattering indicatrices are used for determining the optical parameters of the and a temperature gradient are responsible. An attempt is made Martian atmosphere and surface. A mparison of these parameters to demonstrate how exact solutions to the standard problem. that shcws that the optical thickness increases considerably with of describing the angular distribution of outgoing radiation from a elongation of the scattering indicatrix (if the albedo for single slab of material bounded on both sides by a vacuum, may be scattering is close to unity). Author expressed in terms of Chandrasekhar's $ and 4 functions of zero order when both scattering and temperature gradient effects are present. Author N67-17629*# National Aeronautics and Space Administration, Ames Research Center, Moffett Field, Calif. PREDlCTlONS OF SHOCK-LAYER RADIATION FROM N67-18435* National Aeronautics and Space Administration. MOLECULAR BAND SYSTEMS IN PROPOSED PLANETARY Goddard Inst. for Space Studies, New York. ATMOSPHERES EARTH AN0 VENUS-THE SISTER PLANETS? Henry T. Woodward Washington, NASb, Feb. 1967 49 p refs R. Jastrow and S. I. Rasool Feb. 1966 32 p refs Submitted (NASA-TN-D-3850) CFSTI: HC$3.0O/MF$0.65 CSCL 03A for Publication Concentrations of radiating molecules and radiation from a (NASA-TM-X-57351) CFSTI: $3.00 CSCL 038 number of band systems are presented for equilibrium shock-layer Various features of Venus, including its climate, surface ~ temperatures and densities of vehicles entering proposed Martian temperature. atmosphere, greenhouse effect, radiation. C02 and and Venusian atmospheres The atmospheres selected consist of water vapor content, surface characteristics derived from radar various proportions of COz, Nz. and A. Charts relate these observations. and rotation are discussed and compared with those equilibrium shock-layer properties to flight velocity and ambient of the Earth. R.N.A. , density through the normal shock conservation equations. These w data can be used to estimate stagnation-point radiative heat transfer for entry trajectories. Estimates for some flight conditions are N67-18662* National Aeronautics and Space Administration. discussed and compared. Author Goddard Inst. for Space Studies, New York THE UPPER ATMOSPHERE OF MARS S. H. Gross (Airborne Instr. Lab.). W. E. McGovern (New York N67-17793*# Johns Hopkins Univ., Baltimore, Md. Univ.), and S. 1. Rasool [1965] 16 p refs Submitted for publication ULTRAVIOLET MEASUREMENTS IN PLANETARY (NASA-TM-X-57327) CFSTI: $3.00 CSCL 038 ATMOSPHERES The thermal structure of the upper atmosphere of Mars William G. Fastie ln NASA. Electron. Res. Center Aerospace has been theoretically investigated. It is found that the exospheric Meas. Tech. 1967 p 203-216 refs temperature, for a pure COzmodel atmosphere, lies between GPO HC$1.00; CFSTI: MF$0.65 400-700°K The origin of the Martian atmosphere is discussed in The techniques and optical components which are employed the light of these results. Author in ultraviolet space measurements are described. and some of the experimental data which have been obtained are presented. The instrumentation considered is applicable to all spectral ranges above the cutoff wavelength of lithium fluoride windows at about N67-19022*# National Aeronautics and Space Administration, 1050 A. Specific areas receiving emphasis include energy Washington, D. C. relationships, unit of brightness, differential filter photometry below SIGNIF~CANTACHIEVEMENTSIN SPACE SCIENCE, 1965 Homer E. Newell 1967 222 p refs 2000 A, Ebert spectrometer properties. measuring Circuits. and collecting optics. A G.O. (NASA-SP-136) GPO HCb1.00, CFSTI: MFL0.65 CSCLO3B

CONTENTS: 1. SPACE ASTRONOMY F. T. Haddock (Mich. Univ.). A. G. N67-18273*# National Aeronautics and Space Administration. W. Cameron, and J. K. Gleim p 1-15 refs (See N67-19023 Goddard Inst. for Space Studies, New York. 08-30) THE ATMOSPHERE OF MERCURY 2. IONOSPHERES AND RADIO PHYSICS E. R. S. H. Gross (Airborne Instr. Lab.). W. E. McGovern. (N. Y. Univ.). Schmerling p 17-30 refs (See N67-19024 08-13) and S. 1. Rasool Jan. 1966 54 p refs Submitted for Publication 3. PARTICLES AND FIELDS A. W. Schardt and (Grant NSG-499) A. G. Opp p 31-88 refs (See N67-19025 08-29) (NASA-TM-X-57322) CFSTI: HC$3.00/MF$0.65 CSCL 038 4. PLANETARY ATMOSPHERES R. Horowitr. R. F. Available information on the temperature, composition, Fellows, and H. Hipsher p 89-111 refs (See N67-19026 ' and surface pressure of Mercury's atmosphere is reviewed and the 08-30)

18 N67-21180

5. PLANETOLOGY M. W. Molloyand U. Liddel p 113-195 G. V. Rozenberg 17 Jun. 1966 20 p ref Transl. into ENGLISH refs (See N67-19027 08-30) from IN. Akad. Nauk SSSR, Fiz. Atmosfery i Okeana (USSR), v. 6. SOLAR PHYSICS P. J. Dickerman (IIT Res. Inst.) 1, no. 4,1965 p 377-385 and H. J. Smith p 197-218 refs (See N67-19028 08-29) (FTD-MT-65-400: TT-66-62496; AD-640725) CFSTI: HC $3.00/MF $0.65 Translation of Russian research: On Twilight Investigations * N67-19026*# National Aeronautics and Space Administration, of Planetary .Atmospheres from Space Ships. TAB Washington, D. C. PLANETARYATMOSPHERES N67-19904*# Stanford Research Inst.. Menlo Park, Calif. Richard Hwowitz, Robert F. Fellows, and Harold Hipsher In its CHEMICAL ORIGIN OF THE VENUSIAN CLOUDS Interim Significant Achievements in Space Sci., 1965 1967 p 89-1 11 ’* Report, 1 Oct. 196640Jan. 1967 refs (See N67-19022 08-30) GPO: HC 81.00; CFSTI MF R. C. Robbins 24 Feb. 1967 12 p refs $0.65 (Contract NASr-49(25); SRI Proj. PAU-6128) A description of the diurnal density bulge in the Earth’s (NASA-CR-82960; IR-2) CFSTI: HC $3.00/MF $0.65 CSCL atmosphere involving composition. temperature, and airglow is 038 presented. Tabulated are the number densities of the neutral A laboratory study was made of chemical reactions which atmospheric constituents. Experiments aboard Explorer XVll represent may be important in the atmosphere of Venus. It has been found the first attempt toward measuring on a global scale the that the reaction between excited hydrogen atoms and carbon composition the neutral atmosphere and its temporal variations. of monoxide yields intermediate radical and atom species which undergo The thermosphere probe temperature measurements, based on rapid secondary reactions to produce water and organic compounds. the scale height of the molecular-nitrogen density obtained under The principal organic cwnpounds formed are ethylene, formaldehyde. different atmospheric conditions. are summarized. Sodium release and glyoxal, all readily polymerizable substances. Since the reaction during rocket flights has revealed that strong shear zones exist at course proceeds in this fashion under laboratory conditions, with altitudes from 70 to 120 kilometers. A wavelike structure has the formation of these reactive monomers, it is altogether possible been detected in some neutral temperature profiles, possibly revealing that the same reactions and products are important in the high the presence of gravity waves. Simultaneous measurements of Venus atmospheres. Author midlatitude night airglow and particle precipitation indicate that the midlatitude 5577 A night airglow is not excited by charged particle bombardment as it is in auroras. Spectroscopic measurements made during the recent Mars opposition yield values between 7 N67-19929*# Geophysics Corp. of America, Bedford, Mass. and 13 millibars for the surface pressure. Radio measurements of Technology Div. Venus indicate a surface temperature of approximately 600°K and EXPERIMENTAL AND THEORETICAL STUDIES IN a surface pressure ranging from = 10 to z 200 Earth atmospheres. PLANETARY AERONOMY *r S.P. F. F Marmo Sap. 1966 84 p refs 1 (Contract NASw-1283) - _I (NASA-CR-82937: GCA-TR-66-19-N) CFSTI: HC $3 OO/MF $0.65 N67-19113* Yale Univ., New Haven, Conn. CSCL 04A

*I SPACE RECEIVER OBSERVATIONS OF JOVIAN Summaries, bibliographies, and abstracts of individual DECAMETER FLUX Progress Report publications on the physics of planetary atmospheres are presented Louis Pataki fl9661 7 p along with technical summaries of unpublished results. The broad (Grant NsG-407) variety of scientific areas which have been considered are discussed (NASA-CR-82654; PR-3) CFSTI: $3.00 CSCLO3B under the following major categories: (1) photochemistry of A third flux monitoring station was set up which led to planetary atmospheres. (2)theoretical studies, (3) laboratory confirmation of the velocity of the interplanetary electron clouds investigations in the vacuum and extreme ultraviolet spectral regions. responsible for the second long I-pulses. The addition of this and (4) planetary aeronomy. A G.O. station has led to a study of the direction of this motion, and will allow the calculation the shape of the irregularities in the of N67-20169*# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadena. interplanetary medium.’ Described are techniques used to analyze THE UTILIZATION OF POWDERED METALS AS FUELS either spherical or randomly oriented irregularities causing the IN THE ATMOSPHERES OF VENUS, EARTH, AND MARS L-pulses. As a basis for first analysis the contours correlation of R. A. Rhein 28 Feb. 1967 15 p refs are treated as circular. Data on the directions of the velocity vector (Contract NAS7-100) in the plane perpendicular to the line of sight of Jupiter are (NASA-CR-82878: JPL-TR-32-1073) CFSTI: HC $3.00/MF $0.65 presented for the event of October 23, 1965. Velocity data obtained CSCL 21 B from the three stations was in agreement. This indicates that The ignition temperatures of a number of powdered metals even if correlation contours are elliptical and not strictly circular, the have been measured in air, in a simulated Venus atmosphere, and their motion is not such as would give a misleading projected in a simulated Mars atmosphere. Each atmosphere was thought velocity between two stations. An extension of the theory derived to consist of mixtures of argon, carbon dioxide, and nitrogen. This for ionospheric work and its casting in a form suitable for computer study was conducted to show that the atmospheres of the planets analysis is under way. This will allow calculation of the shape of Mars and Venus might be utilized as sources of oxidizers for the correlation contours and thus of the mean shape of the chemical energy. The heat liberated from the combustion of lithium. irregularities in the interplanetary medium. Records are being diii(ized beryllium, and boron in the simulated Venus and Mars atmospheres for this purpose. It is surmised that their analysis will give data was calculated from the compositions of the products formed at various values hour angle and Jovian longitude thus allowing of from the combustion of these metals in the simulated Venus and a careful analysis of the interaction of the L-pulse phenomena - Mars atmospheres. The product compositions were determined by with other astronomical parameters. S.C.W. chemical analysis. Author

N67-19543# Air Force Systems Command, Wright-Patterson -- AFB. Ohio. Foreign Technology Div. ON TWILIGHT INVESTIGATIONS OF PLANETARY N67-21180*# Jet Propulsion Lab., Calif. Inst. of Tech. Pasadena. ATMOSPHERES FROM SPACE SHIPS THE MARS 1964-1965 APPARITION

19 N67-22562

C. F. Capen 15 Dec. 1966 204 p refs Simon C. Sommer. Alfred G. Boissevain, Layton Yee, and Roger (Contract NAS7-100) C. Hedland Washington. NASA, Apr. 1967 56 p refs (NASA-CR-83123: JPL-TR-32-990) CFSTI: HC $3.00/MF $0.65 (NASA-TN-D-3933) 6FSTI: HC$3.00/MF$0.65 CSCL 038 CSCL 03A A method has been developed for determining the structure A multicolor photographic and visual patrol of the planet of a planetary atmosphere from measurements of pressure, Mars was carried out for an entire terrestrial year that covered temperature, and acceleration made on board an entry vehicle. the Martian northern hemisphere spring and summer during the Determination of the average molecular weight of the atmosphere "Ir 1964-1 965 apparition. The spectral range of the photographic is an important by-product of this type of measurement. Data program included the ultraviolet, visual. and infrared in seven discrete obtained from drop tests of instrumented capsules into the earths pass-bands. The nightly visual record was obtained with the aid atmosphere from high altitude have been analyzed. The atmosphere of six color filters spaced across the visual spectrum. Good structure and the vehicle trajectory determined from these data d" observational coverage was obtained of the Mariner IV scan are in excellent agreement with those obtained from ground-based region (1 10"-200" long.) before, during. and after the photographic observations and meteorological measurements. The deduced contact of July 15. 1965 UT, in an effort to predict and describe molecular weight was within 3 percent of the average value of air. atmospheric and surface conditions during encounter. A summary Author of Martian seasonal events is given. Martian polar regions are explored and North Polar Cap regression curves obtained from orange-red and green plate measurements are presented N67-23425# Smithsonian Astrophysical Observatory. Cambridge, Atmospheric and meteorological observations are thoroughly analyzed. Mass. A daily observation report of surface conditions and atmospheric ON THE SCATTERING OF LIGHT IN PLANETARY phenomena. a Mars pictorial atlas. and Mariner IV photographic ATMOSPHERES. ON THE PROBLEM OF DIFFUSE data are presented. Author REFLECTION OF LIGHT BY A TURBID MEDIUM V. A. Ambartsumyan [1966] 36 p refs Transl. into ENGLISH from Russian Its Astron. Papers Translated from the Russian, No. N67-22562# RAND Corp.. Santa Monica, Calif 7 A NEW APPROACH TO THE AUXILIARY EQUATION WITH The problems of scattering of light in planetary atmospheres APPLICATION TO THE GREENHOUSE EFFECT and diffuse reflection of light by a turbid medium are considered. An integral equation from scattering theory for the case of spherical H. H. Kagiwada, R. Kalaba, and Rupert Wildt Jan. 1967 E. indicatrix is given, and its solution reduces the problem to a 20 p refs functional equation that is easy to solve numerically. Results obtained (Contract AF 44(640)67-C-0045) are used to determine the distribution of intensity over the disk (RM-5076-PR; AD-645565) CFSTI. HC$3 OO/MF$0.65 of a planet at different phases A particularly simple result is Part of the heating of the atmosphere is due to the fact obtained for the case when the planet is in opposition. From the that the incident solar radiation has one absorption coefficient and auxiliary functions introduced the plane albedo of the medium, * the escaping planetary gas another. This is referred to as the Le.. the ratio of the flux scattered by the medium to that.incident greenhouse effect. An idealized theory of the greenhouse effect for on it, is determined. The problem of diffuse reflection of light by a gray planetary atmosphere of infinite depth was developed by a medium which both scatters and absorbs light is solved with a R Wildt of Yale University in previous work. Numerical results new method that leads to a linear integral equation. This method for the temperature profile were given. These employed accurate ab does not resort to the calculation of quantities which characterize numerical values for the Hopf q function and the Chandrasekhar H the behavior of light within the medium, and it allows confinement function, which are now available. This memorandum shows how to an analysis of the conditions at the boundary. S.P. to treat the problem for the case of an atmosphere of finite depth. First an initial value problem for the basic integral equation for the source function is obtained. Then an effective numerical procedury is described, and some computational results are presented. N67-23655*# Jet Propulsion Lab. Calif. lnst of Tech. Pasadena Author (TAB) RESEARCH AND ADVANCED CONCEPTS In ~tsSupporting Res and Advanced Develop 28 Feb 1967 p 202-223 refs N67-22577# RAND Corp., Santa Monica, Calif. Apparent optical properties of window-covered spherical INTRODUCTORY COMMENTS ON VENUS LOWER cavities are reported along with an illustration of the Greenhouse ATMOSPHERE effect Results obtained with an annular hohlraum are given for D. Deirmendjian Jan. 1967 10 p Presented at Conf. on the the thermal radiation from ionized argon, and a nonrotating Rankine Atmospheres of Mars and Venus, Tucson, Ariz ,28 Feb 1967 cycle liquid metal magnetohydrodynamic (MHD) system is under (P-3513; AD-645956) CFSTI: HC$3.00/MF$0.65 investigation This liquid MH D power conversion system uses The difficulties in distinguishing between an upper and lower lithium that is accelerated by cesium vapor in a two-phase nozzle, Venusian atmosphere are pointed out. The lack of reliable basic separated from the cesium, decelerated in an MHD generator, and data, such as surface pressure and temperature, temperature returned to the nozzle by a diffuser and heat source Gaseous gradients, gaseous and particulate composition, large and small breakdown from an applied electric field for three component gases scale air motion, related to the denser parts of the atmosphere are are studied as possible atmospheres of Mars and Venus Paschen noted. The wide variation of surface pressure estimates, ranging curves for the gas mixtures and for extra high purity dry nitrogen between 3 and 1000 atmospheres, advanced by various authors and spectroscopic grade argon are included Despite the similarity recently is displayed graphically. No critique of these is attempted between the curves for the proposed planetary atmospheres and because the corresponding models are not sufficiently well defined the nitrogen, it is noted that a slight amount of impurity of an nor thoroughly analyzed. Author (TAB) unknown minor constituent could have considerable effect on the breakdown potential MWR.

N67-23302*# National Aeronautics and Space Administration. Ames Research Center, Moffett Field, Calif. N67-23660*# Jet Propulsion Lab, Calif Inst. of Tech, Pasadena THE STRUCTURE OF AN ATMOSPHERE FROM ON-BOARD LUNAR AND PLANETARY SCIENCES MEASUREMENTS OF PRESSURE, TEMPERATURE, AND R. H. Norton In its Supporting Res. and Advanced Develop. 28 ACCELERATION Feb 1967 p 293-305 refs

20 N 67-2 6454

The Cwd6 facility for the Table Mountain Observatory 24-inch 31 Jan. 1967 32 p telescope is described, and observations are reported for the radio (Contract NAS7-100) emission from Venus at 1 5 cm wavelength by using a tunable. (NASA-CR-83745: JPL-SPS-37-43. VOI. VI) CFSTI: HC $3.00/MF narrow passband Dicke-type radiometer. For the latter, brightness $0.65 CSCL 228 temperatures of Venus cannot be determined from the autumn measurements because of effects from the Sun in the far sidelobes CONTENTS: of the antenna and too-large antenna offsets during the observing 1. SURVEYOR PROJECT: THE LUNAR PROGRAM cycle The emission feature near 2300 GHz for the spring data p 1-6 (See N67-25093 13-31) appears to be more pronounced relative to neighboring points as 2. MARINER VENUS 67 PROJECT THE PLANETARY- the illumination of the Venusian disk increases. and atmospheric INTERPLANETARY PROGRAM p 7-1 1 (See N67-25094 13-31) 'c extinction appears near the center of the water line. The effects of 3. MARINER MARS 1969 PROJECT: THE PLANETARY- thermally nonuniform sources on the emission spectra of INTERPLANETARY PROGRAM p 12-14 (See N67-25095 13-31) silicates are investigated to shed light on planetary petrology and 4. DSN CAPABILITIES AND FACILITIES. THE DEEP mineralogy M.W.R. SPACEMETWORK p 15-16 (See N67-25096 13-31) 5. DSlF DEVELOPMENT AND OPERATIONS. THE DEEP SPACENETWORK p 17-22 (See N67-25097 13-31) N67-24229# Grumman Aircraft Engineering Corp.. Bethpage. N. Y. Research Dept. DETERMINATION OF THE BRIGHTNESS OF THE ATMOSPHERE OF THE PLANET MARS N67-25094*# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadena. A. Dollfus Jul. 1966 13 p refs Transl. into ENGLISH from Compt. MARINER VENUS 67 PROJECT: THE PLANETARY- Rend. SOC.(Paris), v 262. ser. B, 14 Feb. 1966 p 519-522 INTERPLANETARY PROGRAM (TR-34) CFSTI: HC$3.00/MF$0.65 ln its Space Programs Sum. No. 37-43, Vol. VI 31 Jan. 1967 The measurements of the variation of polarization of light p 7-1 1 (See N67-25091 13-311 of the planet Mars between the center and the edge of its disk Various design changes in the Mariner spacecraft are reported gives the brightness of the atmosphere, in the absence of haze or on the Venus 67 project. Such changes to the spacecraft were clouds, as 6x10 -4 sb/phot. If the air is devoid of aerosols, the necessitated by the fact that the M67-2 flight spacecraft travel is pressure at the surface should be 30 mb. Author oriented toward, rather than away from, the Sun. Also. conversions to accommodate the revised encounter sequencing and science payload were taken into account. Brief technical details are given on the attitude-control subsystem, planet sensor, sun shade. and N67-24309# National Aeronautics and Space Administration, space simulator radiometers. R.LI. Washington, D. C. NASA AND THE MANNED SATELLITE PROGRAM .V Morris Tepper ln Natl. Center for Atmospheric Res. Satellite Data N67-26096*# Jet Propulsion Lab.. Calif. Inst. of Tech.. Pasadena. in Meteorol Res. Dec 1966 p 333-340 MARINER MARS 1969 PROJECT: THE PLANETARY- NASAs flight program plans for the Tiros/TOS satellites, INTERPLANETARY PROGRAM Applications Technology Satellites. and Manned Meteorology ln its Space Programs Sum. No. 37-43. Vol. VI 31 Jan. 1967 '' Satellites: and projected post-1970 flight programs: are summarized. p 12-14 (See N67-25091 13-31) Also reviewed are procedures for participating in space flight In connection with the Mariner Mars 1969 Project, the initial investigations. and the requirement for meteorological research on formal issue of the spacecraft design book, containing system and Mars. s C.W. subsystem functional requirements and defining the system design, was completed. Technical details are given on orbit determination. planetary quarantine, and central computer and sequencer for guidance and control. R.LI. N67-25054*# SDS Scientific Data Systems, Pomona. Calif IMPROVED ION SOURCES Washington, NASA, May 1967 61 p refs (Contract NAS5-3453) (NASA-CR-7754) CFSTI: HC$3.00/MF$0.65 CSCL 20F N67-26097*# Jet Propulsion Lab., Calif. Inst. of Tech.. Pasadena. A study was performed of ion sources having a magnetically DSlF DEVELOPMENT AND OPERATIONS. THE DEEP aligned electron beam, and which are compatible with a previously SPACE NETWORK designed quadrupole mass spectrometer for planetary atmospheric ln its Space Programs Sum. No. 37-43, Vol. VI 31 Jan. 1967 analysis A primary objective was to use the rigid alignment of p 17-22 (See N67-25091 13-31) the electron beam to minimize electron bombardment of the ion Technical details are presented on various NASA Programs, source surfaces thereby removing one of the obstacles to stable, including their instrumentation developments, and design long-term operation A second objective was to formulate the modifications. Some of those reported are: Surveyor Project, Mariner relationships of size, pressure. electron current and applied potentials Mars 1964 Project. Lunar Orbiter Project, and Pioneer Project. for a simple model of a magnetic ion source in order to scale the DSS equipment installation and testing results are given on Pioneer, dimensions and pressure over wide ranges. Using derived scaling Echo. Venus, and Mars DSS. Brief details are also reported on factors a crossed magnetic field ion source was designed for communications development and testing. R.LI. operation at 10 -'torr internal pressure. A model, having an internal volume of 4.7~10-~cubic centimeters and tunnel apertures of 0.0025 centimeter diameter was constructed and subjected to test. Author N67-2%4€4*# Army Missile Command. Huntsville. Ala. '. MERCURY ATMOSPHERE AND SURFACE Herbert H. Hoop 31 Jan. 1967 86 p refs N67-26092*# Jet Propulsion Lab.. Calif. Inst. of Tech., Pasadena. (NASA-CR-84113; RSIC-633) CFSTI: HC $3.00/MF $0.65 CSCL SPACE PROGRAMS SUMMARY NO. 37-43, VOLUME VI 038 FOR THE PERIOD NOVEMBER 1,1966 TO DECEMBER 31, This summary and bibliography is a selection of the more 1986. SPACE EXPLORATION PROGRAMS AND SPACE accepted literature tiom the sizable quantity which covers the range SCIENCES of hypotheses as to rotation of the planet Mercy, temperature,

21 N67-2646 1 atmosphere, surface, and terrain. Various hypotheses and the few vapor with nitrogen were applied to an analysis of the observed generally accepted facts are discussed. Included is a selected microwave emission spectrum of Venus with regard to the bibliography and author index. Author composition and structure of its atmosphere. It is reported that from spectroscopic evidence, the only gases definitely identified in the Venus atmosphere are carbon dioxide and, in very small amounts. water vapor. A large-area X-ray collector is reported for N67-26461# Boeing Scientific Research Labs., Seattle, Wash. flight in an Aerobee 150 sounding rocket. R.LI. G EO-ASTROPHYSICS LABORATORY REVIEW, JANUARY- JUNE 1966 Jun. 1966 25 p refs CFSTI: HC$3.00/MF$0.65 N67-27042# RAND Corp., Santa Monica. Calif. The work on geomagnetic micropulsations has proceeded PLANETARY CONTAMINATION. II: SOVIET AND U.S. to the point where seasonal variations in the diurnal rate of PRACTICES AND POLICIES occurrence of the high-frequency component. i.e., the so-called pearls Bruce C. Murray, Philip K. Eckman (Calif. Inst. of Tech.), and in the frequency regime 0.2-2.0 Hz, are apparent. A limited Merton E. Davies Mar. 1967 25 p refs amount of data has also been obtained from stations near the (AD-648864) CFSTI: HC $3.00/MF $0.65 north and south geomagnetic poles. Experimental and theoretical It was concluded that viable terrestrial micro-organisms investigations established conclusively that plane-wave theory in which are transported to Mars inside solid components in sealed scattering of electromagnetic radiation by random media is spaces have a low probability of being released to the surface or inadequate, and that it is necessary to consider spherical waves. atmosphere, and if any are released they are not likely to infect Experimental work and associated analysis have continued in fields the planet. TAB of radio star scintillations, photoionization, and photodissociation with molecular beams. Other theoretical work has dealt with flow of a conducting fluid past a magnetic source, propagation of solar N67-27295* National Biomedical Research Foundation, Silver protons in the interplanetary magnetic field. and radiative cooling Spring, Md. of stellar material. A relatively inexpensive and simple system for THERMODYNAMIC EQUILIBRIUM IN PREBIOLOGICAL displaying cloud photographs taken by the weather satellites ESSA JI ATMOSPHERES OF C, H, 0, N. P, S. AND CI and Nimbus C was developed. The system utilizes-an oscilloscope M. 0. Dayhoff. E R Lippincott. R. V. Eck. and G. Nagarajan and Polaroid camera, rather than an expensive facsimile recorder. Washington, NASA, 1967 274 p refs Author (Grant NSR-21-003-002; NGR-21-002-059: NGR-09-015-023) (NASA-SP-3040) CFSTI. HC$3 OO/MF$O 65 CSCLO7B A computational system for the equilibrium of many N67-26507*# Ludwig-Maximilians-Universitat, Munich (West compounds in an ideal gas mixture was developed in connection Germany). with the study of the thermodynamic equilibrium of prebiological ON THE INFLUENCE OF ATMOSPHERIC TRANSMISSION atmospheres containing varying amounts of C. H. 0. N. P, S. and CI. FUNCTIONS ON lNFRARED MEASUREMENTS IN An introduction to the methodology, the tables for the computer PLANETARY ATMOSPHERES, PART I1 Final Report survey, and the mathematical models are presented Appendixes I Tannhaeuser Jan 1967 75 p refs deal with thermodynamic equilibria in planetary atmospheres, and (Grant NsG-305) relate thermodynamic equilibrium to the inorganic origin of organic (NASA-CR-84157) CFSTI. HC$3.00/MF $0.65 CSCL 038 compounds. M.W.R. Various methods to represent atmospheric radiation spectra and discrepancies in the results are discussed A comparison is made of present calculations in the 4.5 micron region, where the N67-27370*# Smithsonian Astrophysical Observatory, Cambridge, bands of C02, N20, and CO are overlapping The difference of Mass. calculated equivalent temperatures of the outgoing radiation are MARTIAN IONOSPHERE: A COMPONENT DUE TO SOLAR seen to be higher than 8°K Approximate calculations in the Nimbus PROTONS I HRlR region (3.4 to 4.2 micron) show that the bands of C02 Carl Sagan and Joseph Veverka Apr. 1967 14 p refs and N20 can be responsible for observed discrepancies These (Grant NGR-09-015-023) gases account for about 2°K of the equivalent temperature. Detailed (NASA-CR-84411; Rept -703-24) CFSTI. HC $3.00/MF $0.65 results for clouds of various heights and emissivities are tabulated. CSCL 20H Approximate calculations in the long wave length wing of the 6.3 The small magnetic field strength observed by Mariner 4 micron H2O-band show that the neglection of N20 and CH4 near Mars suggests that protons from the solar wind may enter against the H$ transmission may cause an error of about 9°K the Martian atmosphere and produce ionization in addition to that between 7.25 and 7.75 microns. A general method for the produced by ultraviolet light and X-rays. It is found that solar representation of atmospheric spectra is given, based on laboratory protons produce a thin ionized layer at a rate ~3x10~c~n-~ sec-l at a depth corresponding to the F1 region in the terrestrial transmission functions. Its applicability to the 130611 550 CH4, atmosphere. Unless the effective recombinative coefficient is very 256312461 N20, 3020 CH4, 2143 CO, 2224 N20-bands. and large cm3 sec-’), or unusual diffusion effects are the 6.3 micron H20 and 4.3 micron C02-bands is demonstrated. Author present, this layer should have been detected by Mariner 4, and therefore must be present in one of the observed ionized regions. Because of its very compact shape, the subsidiary maximum near 95 km discovered in the Mariner-4 occultation experiment may be N67-26620*# Columbia Univ , New York. Columbia Radiation the proton ionization peak. If so. the major 120-km maximum is Lab. an F2 layer Distinction between photon and proton ionization RADIO AND X-RAY ASTRONOMY regions can be made by microwave occultation experiments aboard ln its Res. Invest Directed Toward Extending the Useful Range of planetary orbiters. Author the Electromagnetic Spectrum 31 Oct. 1966 p 93-102 refs Radio and X-ray astronomy research is briefly outlined under the trichotomy. X-ray telescope, X-ray polarization. and models of N67-27633*# International Information. Inc.. Philadelphia, Pa. planetary atmospheres. Microwave absorption coefficients measured BEYOND THE DOOR IS AN UNKNOWN PLANET [ZA for mixtures of carbon dioxide with nitrogen and argon, and water DVER’Y U-N EZNAKO MAYA PLANETA]

22 N67-29983

L. Repin May 1967 4 p Transl. into ENGLISH from The paper treats some of the technical characteristics of Komosomol'skaya Pravda (USSR). 21 Jan. 1967 lifting spacecraft and considers some problems of testing Some (Contract NASw-1499) general observations about operating lifting spacecraft in the (NASA-TT-F-11062) CFSTI: HC$3.00/MF$0.65 CSCL 148 'atmospheres' of other planets were included in the hope of This article discusses a special device cepable of reproducing stimulating thought and discussion of such future possibilities. the environmental conditions of other planets This planetary Author (TAB) * stimulator, called "Photostat-1" is essentially a pressure chamber capable of modeling the atmospheric composition, pressure, and the daily variations of Mars and other planets. This facility is the N67-28785*# Pittsburgh Univ., Pa. Dept. of Physics. first which is capable of stimulating the UV radiation on other THE PROBLEM OF USING MARINER IV IONOSPHERIC b planets Special lighting fixtures can imitate the entire solar spectrum, DENSITIES TO DEDUCE A MODEL OF THE MARTIAN including a wide range of UV rays and individual lines of the solar ATMOSPHERIC STRUCTURE spectrum. Experiments with the "Photostat" indicate that various living creatures may be able to survive in a wide range of alien T. M. Donahue 7 Apr. 1967 24 p refs Presented at the Conf. on the Atmospheres of Mars and Venus, Kitt Peak Natl. Lab., conditions Author Feb. 1967 (Contract NASr-179) N67-28001*# California Univ.. Berkeley. (NASA-CR-84825; SRCC-41) CFSTI: HC $3.00/MF $0.65 CSCL UPPER LIMITS ON LIQUID WATER IN THE VENUS 04A ATMOSPHERE An F 1 layer maximum would apparently occur fifteen kilometers W. J. Welch and D. G. Rea [1966] 9 p refs too high in the Martian ionosphere even though the atmosphere (Contract NASr-220; Grants NsG-101-61; NsF GA-527) were pure CO2 in a model with high temperature mesopause and (NASA-CR-84001) CFSTI: HC$3.00/MF$0.65 CSCL 038 thermopause. It is pointed out, however, that a similar calculation A consequence of the discovery of HCI and HF in the of electron densities in the earth's ionosphere starting with a atmosphere of Venus, namely, that there cannot be much liquid reasonable model for neutral structure and temperature would also water in the Venus atmosphere due to the presence of HCI, is disagree with the observed profile of electron density in the F1 discussed. The statement is based on microwave observations of region. It is argued that where no ionospheric model based on the planet. The HCI is highly soluble in water, and the resulting unforced assumptions manifestly supports any atmospheric model it acid has a high DC conductivity. If there were much of this acid in is unreasonable to rely on ionospheric properties to discriminate the Venus atmosphere. the long wavelength radar signals would between models. Author be strongly attenuated, whereas the radar signals appear to reach the planet's surface with little attenuation. An even smaller upper N67-28789*# Astro Research Corp.. Santa Barbara, Calif. limit on the liquid water content of the Venus atmosphere is DESIGN CRITERIA FOR LIGHTLY LOADED INFLATED obtained by another less direct argument. The microwave emission STRUCTURES IN A NEAR-PLANETARY ATMOSPHERE spectrum of the planet resulting from a cool acid cloud above the Peter G. Niederer 16 Feb. 1967 69 p refs warm surface is considered. P. s. (Contract NAS7-427) (NASA-CR-84829; ARC-R-246) CSCL 20K N67-28368*# Cutler-Hammer, Inc., Deer Park, N. Y. For inflating a lightly loaded membrane. the simplest solution INVESTIGATION OF PLANETARY IONOSPHERES is offered by carrying a pressurization medium directly within the B. Mohr. 2. Poznanski. D. Luganski. G. Kraft, and S. H. Gross structure. The difference of state of this medium between the Washington. NASA, May 1967 205 p refs packed condition at the launching site and the deployed condition (Contract NAS5-9108) in the operating environment is used to deploy the body and then (NASA-CR-689) CFSTI: HC$3.00 CSCL 03A to rigidize it. Two near-earth environments and one near Mars are The feasibility of usiny radio-sounding techniques to investigate chosen for closer investigation. An exact knowledge is required of the ionospheric properties of the planets was studied Principal the equilibrium temperature a body attains due to radiative sources concern was with overall systems evaluation, signal processing, and in space. Temperature can be regulated by the appropriate transmitter design for an advanced long-range sounder system. choice of the solar absorptivity and emissivity of the body surface. Sounding ranges of interest were from nearby to 40,000 km. Pressurization substances are examined and their abilities to develop Application of the new sounder system was made to typical planetary a certain pressure by varying the quantity used to inflate a given missions such as the Voyager-Mars Orbiter and the Mariner-Mars volume are investigated. An analysis is made to minimize the flyby spacecrafts. The signal-processing design study was based weight of an inflated body for a given task. The theory is applied on a previous program, which concluded that digitized to the bracing system of an X-brace Stokes flow decelerator. pulsecompression and integration techniques were the most desirable Author methods to be used in advancing the state of the art of ionospheric sounding. Investigations of these techniques and their applications N67-29983* National Aeronautics and Space Administration. to typical planetary sounding systems resulted in detailed Marshall Space Flight Center. Huntsville, Ala. circuits, components, and characteristics. The design THE ENVIRONMENT OF VENUS: A DISCUSSION OF ITS ct toward providing a sounding capability from ATMOSPHERE AND SURFACE extremely long ranges, as well as from nearby, over a wide band Robert B. Owen, C. L. Hasseltine. William T. Roberts. George S. of frequencies. The transmitter design consisted mainly of West, and Jeanette A. Scissum 1 May 1967 142 p refs breadboarding efforts to realize a wide-band untuned system entirely Supersedes NASA-TM-X-53327; see N65-35976 of solid-state components. The task also included a study of the (NASA-TM-X-53497; NASA-TM-X-53327) CFSTI: $3.00 CSCL design of matching networks for dipole antennas Author 03 B * Presented is a self-consistent model atmosphere for the planet Venus, with emphasis on parameters of general use in N67-28513# RAND Corp.. Washington, D C. developing vehicle design criteria. Kern and Schilling's program for AERODYNAMIC ASPECTS OF FUTURE SPACE VEHICLES generation of atmospheric parameter values is coupled with the AND IMPLICATIONS FOR TESTING most recent estimates of surface conditions in order to derive the F. S. Nyland Mar. 1967 21 p refs atmosphere environment at different altitudes. A range of initial (P-3559; AD-649512) CFSTI: HC$3.00/MF$0.65 values is used to produce a parametric band most representative of

23 N67-30624 actual conditions. Because of the extreme pressures and N67-31336* California Univ.. Berkeley. Dept. of Chemistry. temperatures involve$ it is felt that design for such an environment INFRARED SPECTROMETER DEVELOPMENT FOR SPACE presents an engineering problem of the first magnitude. Author VEHICLE STUDY OF PLANETARY ATMOSPHERES Final Report George C. Pimentel Jun. 1967 1 16 p N67-30624*# GCA Technology Div . GCA Corp , Bedford. Mass. (Contract NASr-212) PLANETARY METEOROLOGY Final Report (NASA-CR-85797) CSCL 20F .L George Ohring. Wen Tang. and Joseph Mariano Mar. 1967 A filter-wedge spectrometer concept was found to be feasible 73 p refs with resolution of 1% and scan times of a few seconds. Infrared (Contract NASw-1227) spectra were recorded in the laboratory using a black body at dry (NASA-CR-85569; GCA-TR-67-5-N) CSCL 036 ice temperature (195'K) as the radiation source at 2% resolution *. In the first of two studies the seasonal and latitudinal over the wavelength range of 6 to 15 microns in a 3min scan time. variations of the average surface temperature and vertical profile of This optical design has the advantages of low power. ruggedness, atmospheric temperature on Mars are computed using a thermal and light weight. Laboratory research was performed to permit equilibrium model. The computed temperature profiles satisfy the the design of an instrument suited to the Mariner spacecraft; and following equilibrium conditions: (1) a balance at tne top of the a ground-based model was also developed for balloon or atmosphere between net incoming solar radiation and outgotng ground-based telescopic study of the terrestrial and planetary infrared radiation; (2) a balance at the surface between the net atmospheres. This adaptation is useable for Mars and Venus studies gain of heat by radiation and the loss of heat by convective in the 12 micron spectral region. M.W.R. transport into the atmosphere, the amount of convective loss being determined from the net integrated radiative cooling of the convective layer. I e. the troposphere; and (31 the stratosphere is in radiative N67-32308*# Volt Technical Corp., Washington, D. C. equilibrium In the second study. two dynamic models simulating SOMETHING NEWABOUTVENUS [NOVOYE 0 VENEREl the Martian atmospheric circulation are constructed Model 1, based D. Martynov 22 Jun. 1967 4 p Transl. into ENGLISH from on terrestrial atmospheric circulation, is a vertically integrated Pravda (Moscow), no. 165, 1967 model for computing meridional profiles of mean mid-atmospheric (Contract NAS5-12487) zonal wind and temperature for both northern and southern (NASA-CR-86635; ST-PR-LPS-10628) CFSTI' HC $3 OO/MF hemispheres of Mars during the two equinoxes and the two solstices $0.65 CSCL22A Model II, a more sophisticated two-level quasi-geostrophic numerical A general discussion of the planet Venus is presented in model. can be used for computing similar Martian temperature terms of atmosphere, temperature measurements, cloud cover, and wind characteristics K. W and length of day. Implications of the high temperatures of Venus are noted; and mention is made of the Soviet cosmic rocket, Venus-4, launched June 12, 1967. M.W.R. N67-30793# Ludwig-Maximilians-Universitat, Munich (West Germany) Meteorogisches lnstitut -e METHODS TO CALCULATE THE INFRARED RADIATION N67-32463# RAND Corp., Santa Monica, Calif. FROM PLANETARY ATMOSPHERES [METHODE ZUR CHANDRASEKHAR'S PLANETARY PROBLEM WITH BERECHNUNG DER VON PLANETEN-ATMOSPHAEREN INTERNAL SOURCES AUSGESANDTEN INFRAROTSTRAHLUNGJ R. Bellman. H. Kagiwada. R. Kalaba. and S. Ueno May 1967 4 I Tannhaeuser Feb. 1967 12 p refs 24 p refs (BMWF-FB-W-67-02) (Contract F44620-67-C-0045; Proj. RAND) The spectrum of the outgoing radiation in the region between (RM-5229-PR; AD-652832) CFSTI: NC$3.00/MF$0.65 4 to 5 microns is given for different cloud heights. From this, the Invariant imbedding equations are developed for the radiative effect of the atmospheric gases between the cloud level and determination of the vertical stratification of terrestrial and other the receiver can be deduced. The product functions corresponding planetary atmospheres on the basis of satellite observations. The to the weighting function are also shown; the former give a more top altitude of a cloud. for example. can be estimated from the realistic impression than the latter. In addition to being accurate relative spectral intensities of the solar radiation reflected from the and simple. the method is especially applicable to the inversion cloud in the oxygen A band at 7600 angstrom, and in a nearby problem and for the atmospheres of other planets, since the window. The results of RM-5245-PR are extended to solve the parameters in the atmospheric transmission functions may be varied Chandrasekhar planetary problem for atmospheres with or without without expending much computing time. Author internal energy sources. and with or without bottom surface reflectivity, either Lambert or nonorthotropic. The differential-integral equations may be approximated by systems of stable initial-value N67-31108*# New Mexico State Univ.. Las Cruces. problems that are readily and accurately solved by digital computers. JUPITER'S RED SPOT IN 196666 TAB H. Gordon Solberg. Jr. [I9671 17 p refs (Grant NsG-142-61) (NASA-CR-85560; TN-701-67-14) CSCL 038 N67-32494*# RAND Corp.. Santa Monica. Calif. The latitude and longitude of Jupiter's Red Spot were measured SOME ASPECTS OF THE CIRCULATION OF MARS from photographic plates obtained between 1 July 1965 and 4 Conway Leovy Nov. 1965 27 p refs Presented at Conf. on Spot increased irregularly in Sptm I1 longitude Exploration of the Planets, Blacksburg, Va.. 16-20 Aug. 1965 965 to 28" in June 1966. The zenographic (Contract NASr-21(07)) Spot remained near its mean value of -22.3". (NASA-CR-86912. P-3262) CFSTI: HC $3.00/MF $0.65 CSCL 03B Numerous fluctuations in the position and dimensions of the Red Estimates of the vertical temperature structure and heat balance s Spot were noted, and evidence for a relationship between the Red Spot and rapidly moving features of the South Temperate Belt of Mars are reviewed and compared with the corresponding ~sTB)is cited. An oscillation in the longitude of the Red Spot quantities on the Earth. The probable resulting circulation is with a period of 88110 days may have been produced by rapidly discussed, and reasons for expecting a stronger solstice circulation moving dark spots on the north edge of the STB. which moved on Mars than on the Earth are given. The problem of thermally 360" in longitude with respect to the Red Spot in 91 days driven tides is reviewed. The amplitude of such tides is likely to Author be small. Author

24 N67-34596

N67-32719*# Avco Corp., Lowell, Mass. scattering and Lambert reflectivity, the flux is determined for a A FEASIBILITY STUDY OF AN EXPERIMENT FOR wide range of solar elevations, ground reflectivities, and optical DETERMINING THE PROPERTIES OF THE MARS depths. For very large surface reflectivities there is more radiation ATMOSPHERE. VOLUME I: SUMMARY downward onto a planet at the bottom of a thick atmosphere Steven Georgiev Washington, NASA, Jul. 1967 141 p refs than is received at the top because the radiation that does penetrate (Contract NAS2-2970) undergoes multiple reflection. The total radiation absorbed by the * (NASA-CR-530) CFSTI: $3.00 CSCLO3B surface plus the corresponding diffuse upward radiation always A feasibility study of a Mars probe for obtaining vertical equals the input flow. Bond albedo is determined by numericaly profiles of pressure, temperature, and density is reported. The integration. It approaches the value of the ground reflectivity as most important mission objectives and constraints aresummarized. The optical thickness approaches zero. and approaches 1 as it becomes 'h launch-to-probe/spacraft separation. probe/spacecraft separation, very large. Author (TAB) and probe entry sequences are outlined. The overall probe system is described, and details are given on the entry probe, sterilization canister. pr.obespacecraft integration, and the probe. separation, N67-33596* Purdue Univ.. Lafayette, Ind. School of Electrical stabilization, and propulsion subsystem. Alternate mission modes Engineering. and earth entry test program are also covered. It is felt that the OPTIMAL CONTROL THEORY engineering feasibility is established and the preliminary design /n its [Res. Areas in the School of Elec. Eng. of Purdue Univ.] satisfactory. N.E.N. Jan. 1967 p 8-28 refs (Grant NGR-15-005-021; Contract JPL-950670) Electric engineering developments in optimal control theory N67-32849*# National Aeronautics and Space Administration. and information systems cover such topics as: error in linear Goddard Space Flight Center, Greenbelt, Md. systems with bounded input; control of systems with inaccessible lNVERSE PROBLEMS IN RADIATIVE TRANSFER: A states; time optimal feedback control; minimum sensitivity optimal REVIEW control: stochastic cooperative games; pursuit problem applied to Barney J. Conrath Feb. 1967 35 p refs synthesis of stochastic optimal controller; specific soft-lander (NASA-TM-X-55857; X-622-67-57) CFSTI: HC $3.00/MF $0.65 control problem; and maneuverable landing in Martian atmosphere. CSCL 20M R.LI. An elementary introduction to the inverse problem of radiative transfer as applied to remote measurements of infrared radiation from planetary atmospheres is presented, along with a review of N67-33758 Douglas Aircraft Co.. Inc.. Huntington Beach, Calif. work which has been done on the problem. Particular attention is Missile and Space Systems Div. given to the problems of inferring vertical temperature profiles and DETERMINATION OF MARTIAN AND CYTHEREAN water vapor distributions in the earth's atmosphere. The principle ATMOSPHERIC COMPOSITION WITH AN ENTRY PROBE methods which have been developed for solving these problems BY MEASUREMENT OF ULTRAVIOLET AND X-RAY are discussed briefly. Examples of applications of temperature and ATTENUATION water vapor inversions to both synthetic data and data taken with F. F. Fish and V. A. Sirounian April 1967 23 p refs an IRIS instrument at balloon altitudes are presented. (DAC-60627) Detailed is the manner in which Martian atmospheric composition and structure can be obtained applying the technique N67-32936*# National Aeronautics and Space Administration. which focuses on the use of ultraviolet and absorption Goddard Space Flight Center, Greenbelt, Md. measurements from an entry probe or flyby. Also discussed is the THEORETICAL COMPUTATIONS OF THE OUTGOING applicability of the technique to studies of the Cytherean INFRARED RADIANCE FROM A PLANETARY ATMOSPHERE atmosphere. S.C.W. Virgil G. Kunde Washington, NASA, Aug. 1967 121 p refs (NASA-TN-D-4045) CFSTI: $3.00 CSCL 036 The solution to the radiative transfer equation for a non-gray N67-34136 General Electric Co.. Philadelphia, Pa. Missile absorbing atmosphere in local thermodynamic equilibrium was and Space Div. programmed for an IBM 7094 computer to calculate theoretically the TABLES OF THERMODYNAMIC PROPERTIES OF MARS outgoing infrared radiance in five wave number spectral intervals. ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOW The spectral range covered is from 5 to 20 microns. The theoretical -FIELDS, PART I outgoing radiances may be utilized in several ways: (1) to assist C. L. Kyriss and A. Milas 12 Dec. 1966 35 p refs in selection of the desired spectral characteristics for infrared (ATDM-86-11 satellite experiments, (2) to test the validity of balloon and satellite Thermodynamic data for three Martian model atmospheres observations, and (3) to aid in the analysis of planetary infrared have been processed for use in the GE-RSD flow field system for radiation data. Theoretical thermal emission spectra were computed real gases in chemical equilibrium. The results of this work are for several representative model atmospheres for Earth and Mars. reported in three parts. Part I treats the model composition: 4.9% These spectra illustrate that a considerable amount of information COp95.1% N 2 by volume, over the temperature range 9073 is available from radiation data of five wave number resolution. to 27.000"R and loglo p/po range -7.6 to 1.0. Part II treats This information allows the recovery of the atmospheric and surface the model composition: 9% C@-90% N2-1% A by volume, parameters from measured thermal emission spectra. Author over the temperature range 90"R to 27.00TR and loglo p/po range -7.0 to 1.8. And Part 111 treats the model composition: 48.8% CO2-51.2% N2 by volume. over the temperature range N67-32966# RAND Corp.. Santa Monica. Calif. 90"R to 17,100"K and loglo p/po range -7.0 to 1.0. Author GLOBAL RADIATION EMERGING FROM A RAYLEIGH - SCATTERING ATMOSPHERE OF LARGE OPTICAL THICKNESS N67-34596# Lockheed Missiles and Space Co., Palo Alto, Calif. Anne 6. Kahle May 1967 29 p refs Research Lab. (Contract F44620-67-C-0045) DUST PARTICLE TERMINAL VELOCITIES IN VENUS (RM-5343-PR; AD-652646) CFSTI: HC$3.00/MF$0.65 ATMOSPHERE FROM 0 TO 100 KILOMETERS Calculations of the total radiation emerging from planetary Albert D. Anderson May 1967 18 p refs atmospheres optically thicker than those of the earth. For Rayleigh (LMSC-6-77-67-18)

25 N67-34775

In order to better undersfand the possible generation, N67-35341# RAND Corp., Santa Monica, Calif. persistence, and particle size range of dust in the Venus atmosphere, THE TWILIGHT CUSP EXTENSION OF VENUS terminal velocities are calculated for spherical particles with G. F. Schilling and R. C. Moore Jun. 1967 11 p refs Submitted diameters from one to 10.000 microns for three model atmospheres for publication over the altitude range 0 to 100 km. The model atmospheres are (P-3621: AD-654628) based on minimum (30 atm: 620°K). most probable (50 atm: It has been known since about 1790 that when Venus 688°K). and maximum (300 atm: 720°K) surface pressures and is near inferior conjunction, the cusps of her crescent extend far * temperatures. Assuming a solid surface and the availability of dust beyond a half-circle. It is further known that Venus, at greatest on the ground, the following conclusions are reached: (1) The elongation, does not present the expekted half-moon shape. but falling rates for the smaller dust particles (less than 50 microns) rather appears convex towards the illuminated side. This leads to show the least sensitivity to the model used at the lower altitudes a discrepancy of the order of days between date of apparent and e’ (less than 40 km) and the greatest sensitivity at tbe higher geometric dichotomy, not satisfactorily explained to date. On the altitudes (90-100 km): (2) For all sizes considered. the vertical basis of our study, we are forced to infer that the scattering winds required to maintain particles aloft in the lower Venus atmosphere of Venus extends to considerable heights above the atmosphere are less than one-half those needed on earth. Therefore, cloud deck, and that its luminosity characteristics are not too far for the same degree of convective activity, one should expect different from those of the earths atmosphere. Height variations of more dust, consisting of larger particles ranging in size up to several the scattering atmosphere itself appear therefore to be Immaterial. hundreds of microns in diameter; (3) If, as is probable, Venus has but small height variations of the probably uneven top of the much more convective activity than earth, then it is likely that a opaque cloud deck would explain observed effects. TAB great deal more dust exists there, whose maximum size is on the order of one thousand microns in diameter. These last two conclusions lend support to Opik‘s Aeolosphere Model. Author N6735919# White Sands Missile Range, N. Mex. Atmospheric Sciences Lab. SPACIAL AND TEMPORAL DISTRIBUTION OF THE N67-34775*# Jet Propulsion Lab., Calif. Inst. of Tech., Pasadena. GRADIENT RICHARDSON NUMBER IN THE SURFACE AND LUNAR AND PLANETARY SCIENCES PLANETARY LAYERS In irs Space Programs Sum. No. 37-45, Vol. IV 30 Jun. 1967 FrankV. Hansen May 1967 30 p refs p 235-243 refs (ECOM-5123: AD-654993) The Richardson number (Ri) as a function of height. time To provide an experimental basis for the geologic interpretation of spectral reflectance measurements oj planetary surfaces, and stability classification method has been investigated by the use of wind and temperature profiles observed in the surface and laboratory studies were made of particulate rocks. Changes in the wavelength distribution of reflected light were measured as functions planetary boundary layers. It was found that a reference height of of rock composition and mineralogy, particle size, particle shape, three to six meters above the surface provides the best estimate of the Richardson number in respect to the energy balance of the * particle packing, and angle of illumination. Experimental results indicate that powdered silicate rocks can be classified as rock air-earth interface. Further investigation revealed that nearly all glasses, crystalline acidic rocks, or crystalline basic-ultrabasic rocks, boundary layer processes can be related to the Richardson number including a hypothesis in the form of wind and temperature profiles on the basis of spectral reflectance in the 0.4 to 2.0 fl wavelength Author (TAB) region. This led to the conclusion that a combination of several for a diabatic surface boundary layer. spectral reflectance properties is capable of giving some gross composition information on silicate rock powders. Summary data are provided on determinations of cloud-top pressure and hydrogen N6737243# RAND Corp.. Santa Monica, Calif. abundance in the Jupiter atmosphere. Also considered are four THETWILIGHT ATMOSPHERE OF VENUS methods of analyzing the visible and near-infrared spectrum of G. F. Schilling and R. C. Moore Jul. 1967 97 p refs solar energy returned from the lunar surface: photometry. polarimetry. (Contract F44620-67-C-0045; Proj. RAND) luminescence, and spectrophotometry. Pictorial data are included (RM-5386-PR; AD-656307) to show the linear Martian features obtained from Mariner IV An investigation of the discrepancies between the theoretically photographs. M.G.J. predicted and the actually observed shape and periodic appearance of Venus. Current astronomical methods of observation of the twilight sky of Venus are investigated by combining a rigorous celestial geometry with a determination of the physical effects exerted by the relative luminances of the atmospheres of Venus and the N67-34884*# National Aeronautics and Space Administration, Earth. Analysis shows that the discrepancy between the expected Electronics Research Center, Cambridge, Mass. and observed times of dichotomy corresponds to a range in FLYBY MEASUREMENTS OF THE PROFILES OF WATER position angle from about 92 to 98 degrees, which implies a VAPOR, PARTICULATE MATTER, AND CARBON DIOXIDE minimum height of the effectively scattering atmosphere from 13 INTHE MARTIAN ATMOSPHERE to 23 km. There are indications that the true height may be Alfred E. Barrington, Anthony J. Caruso. and Gene G. Mannella several tens of kilometers. TAB Washington, NASA, Aug. 1967 16 p refs (NASA-TN-D-4115) CFSTI: HC$3.00/MF$0.65 CSCL 038 A study of infrared absorption measurements in the Martian N6738348*# Volt Technical Corp.. Washington, D. C. atmosphere for the determination of the profiles of water vapor A TWO-LAYER MODEL OF VENUS ATMOSPHERE and carbon dioxide is presented in quantitative detail. Using the (INTERPRETATIONS OF RADAR OBSERVATIONS) best available data on the Martian atmosphere, it is shown that [DVUSKHSLOYNAYA MODEL‘ ATMOSFERY VENERY (OB with stateaf-the-art instrumentation the following can be measured: INTERPR ETATSlI RADIO LO KATSIONNY KH NABLY UDENIY)] * an upper limit of water vapor of g/cn?-column (at 6.3 Y. N. Vetukhnovskaya and A. D. Kuz’min 10 Oct. 1967 6 p p). scattering by particulate matter (at 3.5 p), and the carbon Transl. into ENGLISH from Astron. Vestn. (USSR). v. 1, no. 2 dioxide profile above an altitude of 50 km (at 4.3 a). The choice p 85-88 of wavelengths and of experimental instrumentation is based on (Contract NAS5-12487) 4 a realistic appreciation of Martian atmospheric characteristics and (NASA-CR-88980: ST-LPS-RA-10654) CFSTI: HC $3.00/MF experience gained during the Mariner II Venus mission. Author $0.65 CSCL 038

26 N67-40462

A two-layer model atmosphere of Venus is considered. N67-40004* Douglas Aircraft Co., Inc., Santa Monica, Calif. It satisfies the data of both the radioastronomic and radar Missile and Space Systems Div. measurements. including the measurements at 3 cm. It shows a STUDY OF DUST DEVILS IN RELATION TO THE MARTIAN considerable decrease of the effective cross-section of Venus' YELLOW CLOUDS Quarterly Progress Report, 1 Jun.31 reflection at short wavelengths. The first upper absorbing layer, Aug. 1967 being "cold". determines the spectrum of its proper radiation, but J. A. Ryan and F. F. Fish, Jr. 31 Aug. 1967 116 p refs -is transparent for the radiation with wavelength h > 3 cm. This (Contract NASw-1670) is why it does not affect the results of radar observations. The (NASA-CR-89578; QPR-1) CSCLO3B second absorbing layer, being near the planet's surface, and therefore A study is being conducted to determine whether dust "hot". absorbs the centimeter radiation and determines the devils could occur on Mars and be responsible for the observed frequency dependence of the effective Venus' reflection but does yellow clouds. Emphasis is being given to field studies and during not influence the brightness temperature of the planet, for the this period field data were obtained in the Mojave Desert of temperature of this layer is similar to that of planet's surface. A Southern California. Quantities measured were temperature as a surface absorbing layer may be a lower row of clouds, containing function of height and time, background wind velocity. wind direction, (li2) .lo3 g/cm2 of dust or about 2 g/cm2 of polar liquid pressure, dust devil diameter, dust column height, height of dust with equipartition time of (1 i2) .lo-" sec. Author devil associated turbulence, and horizontal wind velocity inside the dust devil. Temperature measurements were initially taken up to N67-39468# Ohio State Univ., Columbus. Aeronautical and 150 meters, but on occasion the temperature lapse rate remained Astronautical Research Lab. superadiabatic above this height. Accordingly, measurements were CHEMICAL KINETICS OF ENTRY INTO THE MARTIAN extended up to 1540 meters above the surface using a light ATMOSPHERE Final Report plane. The maximum dust devil velocity recorded to date was 45 E. Stokes Fishburne. K. R. Bilwakesh, and Rudolph Edse km/hr under strongly superadiabatic conditions. Dust devil Wright-Patterson AFB. Ohio. ARL, May 1967 47 p refs associated turbulence was found as high as 3600 meters above (Contract AF 33(657)-8951) the surface and the maximum dust column height was 450 meters. (ARL-67-0113; TR-6; AD-657778) The data demonstrate that a superadiabatic lapse rate is necessary The reactions between carbon monoxide and oxygen to form for dust devil generation and their considerable vertical extent. carbon dioxide have been examined in two separate experimental Author studies. In the first study a mixture of carbon monoxide and oxygen was introduced into a shock tube. The mixture then was heated by a shock wave and the rate of formation of carbon N67-40462*# Stanford Univ , Calif dioxide was determined. The carbon dioxide concentration was RELATIONSHIP OF PLANETARY QUARANTINE TO followed by observing the intensity of the infrared radiation at 4.25 BIOLOGICAL SEARCH STRATEGY mu emitted by the heated carbon dioxide. Rate constants were E C. Levinthal, J Lederberg. and Carl Sagan (Harvard Univ, obtained. However. it was shown that if the amount of water Cambridge, Mass ) [1967] 15 p refs vapor in the system was greater than 7 ppm the primary reactions (Grant NsG-81) were governed by the hydrogen-oxygen system of reactions. Hence, (NASA-CR-89772) CFSTI: $3.00 CSCL 22A it was impossible to obtain reliable rate constants for the CO-02 Decision theory search strategies are discussed for Mars system of reactions. The elimination of such minute quantities of missions, emphasizing planetary quarantine considerations. In moisture is almost impossible. The second experimental study addition to the detection and characterization of life on Mars, involved expanding a high temperature mixture of C02. CO, 0, and attention is directed to the importance in mission decision analysis 02 through a supersonic expansion nozzle. From a measurement of judging the future utility of Mars and the possibilities of of the pressure profile down the nozzle the chemical state of the gas modifying Mars atmosphere, and of arriving at an explicit statement can be determined. Extensive computer programs were formulated of the probabilities of back contamination of the Earth. A method for this phase of the investigation. Unfortunately the contract of analysis used in a pilot problem of a simplified version of the period came to an end at the conclusion of the calibration decision required in selecting Voyager-Mars mission configurations experiments. Hence, no information was obtained concerning the is also examined. E.C. recombination of carbon dioxide. TAB

N67-39518# RAND Corp.. Santa Monica, Calif. LIFE IN THE UNIVERSE S. H. Dole Sep. 1967 21 p Presented at Hawthorne School, Beverly Hills. Calif.. 28 Jul. 1967 (P-3669; AD-658009) If life will appear whenever the conditions are tolerable. as stated by many modern scientists. and if there are numerous planets in the right mass range orbiting at the proper distance around suitable stars. then life must be quite common. Assuming here that the word life. wherever it appears, implies life based on water and on carbon compounds, that is, life as-we-know-it and as found on the surface of the earth. There are some very good arguments in support of this. Another argument depends on the very unusual properties of water and of the compounds of carbon. Water is an amazing material--there is no other compound that comes close to it in many of its properties. Similarly, no other element but carbon has the property of being able to form such an enormous variety of complicated long-chain compounds--as are demanded by life processes. Something like half-amillion compounds of carbon have been identified--which is perhaps 50 times as many as all the chemical compounds that do not contain carbon. TAB

CEDING PAGE BLANK NOT FILMED. A66-25275,

on the feasibility of performing the aerobraking maneuver and a number of functtonal Tequirements are considered in the light of the 1966 Mariner 4 atmospheres, as well as a number of other model atmospheres that have been postulated. Although the most recently reported low-density atmospheres have served to further constrain IAA ABSTRACTS the available entry window, aerobraking is still thought to be feasible. A. B. K.

A66-25169 # A66-25273 # EQUILIBRWM AND NON-EQUILIBRIUM RADIATION IN SIMULATED SOME REQUIREMENTS ON LIFTING VEHICLES FOR MANNED PLANETARY ATMOSPHERES. MARS OPERATIONS. J. S. Gruszczynski and K. M. Thomas (General Electric Co., Mis- B. L. Swenson, R. W. Carlson, and E. L. Tindle (NASA, Office sile and Space Div., Space Sciences Laboratory, Valley Forge, Pa. ). of Advanced Research and Technology, Mission Analysis Div., American Institute of Aeronautics and Astronautics, Plasmadynamics Moffett Field, Calif.). Conference, Monterey, Calif., Mar. 2-4, 1966, Paper 66-183. 45 p. IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- 15 refs. TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING Members, $0.75; nonmembers, $1.50. STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, Contract No. JPL-950297. 1966. TECHNICAL PAPERS. Discussion of experimental data of high-temperature gas radiance New York, American Institute of Aeronautics and Astronautics, obtamed III several gas mixtures containing GO2, N2 and Ar. It was 1966, p. 363-369. 16 refs. found that the presence of relatively large amounts of argon (30%) Examination of some of the operational problems peculiar to a has a strong influence on the equilibrium radiative properties of the manned Mars landing mission, with particular attention to the gas. This appears as a large increase of radiance for stagnation determination of quantitative requirements for llft associated with conditions corresponding to flight velocities above 27, 000 fps. At advanced vehicles used during such missions. The aerodynamic a velocity of 30,000 fps, the gas mixture containing 30% argon ex- requirements are given for manned atmosphere capture at Mars hibits radiance which exceeds the radiance of the argon-free gas by for the current low-density atmosphere models. Aerodynamic a factor of 8. This difference diminishes at higher velocities. It requirements are also indicated for the lateral ranging required to is noted that the theoretical prediction of the radiative properties achieve certain landing sites within overall mission constraints. for the 9% CO2 - 91% N2 gas underestunates considerably the mea- Results are given for the lifting requirements on the manned landing sured radiance for this gas. At the velocity of 30, 000 fps, the mea- velucle for parachute deployment during terminal descent in the sured values are higher than calculated by a factor of approximately tenuous Martian atmosphere. It is shown that surface launch 4. It is suggested that the contribution of the CN radical may be windows may be broadened through the use of lift during the ascent larger than calculated. M. M. phase of the mission. R.A.F.

A66-25274 # A66-25235 * LAMINAR CONVECTIVE HEATING AND ABLATION IN THE MARS RADIO OCCULTATION INVESTIGATIONS OF THE ATMOSPHERE OF MARS. ATMOSPHERE. Joseph G. Marvin and Ronald B. Pope (NASA, Ames Research Arvydas Kliore and Dennis A. Tito (California Institute of Tech- Center, Moffett Field, Calif.). nology, Jet Propulsion Laboratory, Pasadena, Callf. ). IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, 1966. TECHNICAL PAPERS. 1966. TECHNICAL PAPERS. New York, American Institute of Aeronautics and Astronautics, New York, American Institute of Aeronautics and Astronautics, 1766, p. 370-382. 37 refs. 1966, p. 5-13. 9 refs. The influence of atmospheric composition on heat transfer and Description of a means for investigating the atmosphere and ablation 1s investigated. Equilibrium convective heating, includmg ionosphere of Mars by measuring the effects of their refraction on boundary-layer mass addition, is studied analytically. It is illus- the frequency, phase, and amplitude of a signal received from a trated that the gas properties at relatively low temperatures near space probe before and after occultation by the planet. Such the wall control the heating rate and that precise definition of measurements with an occultrng orbiter would yield improved deter- transport properties at the stagnation temperatures associated with minations of the shape of the planet and density profile of the lower entry IS not necessary. A correlation equation, in terms of the atmosphere, as well as the electron density profile of the ionosphere relatively low-temperature free-stream gas properties and a suitably over a large number of locations on the planet's surface, thus defined mass-addztion parameter, IS given. Heatrng rates for no providing information on diurnal, seasonal, and latitudinal variations. mass addition in representative Martian atmospheres are from 10 to Simulations of some typical 1971 orbits are discussed. R. A. F. 25% higher than those in nitrogen. Experimental heat transfer to nonablating and ablating model surfaces is presented. Data in nitrogen and argon streams compare adequately with the theory. A66-25272 # For gas mlxtures of nitrogen and carbon dioxlde and of nitrogen and SOME CONSIDERATIONS FOR MANNED MARS ENTRY AND oxygen, the heat transfer to ablating surfaces is shown to increase LANDING. as much as 25% as a result of combustion of ablation vapors. M. G. Boobai (North American Aviation, Inc. , Space and Information (Author) Systems Div. and Advanced Systems Div., Downey, Calif. ). IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING A6625275 # STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, THEORETICAL INVESTIGATION OF THE STATIC AND DYNAMIC 1966. TECHNICAL PAPERS. STABILITY OF ENTRY VEHICLES IN THE MARS ATMOSPHERE. New York, American Mstitute of Aeronautics and Astronautics, C. L. Kyriss and H. Rie (General Electric Co., Missile and Space 1966, p. 357-362. %refs. Div., Re-Entry Systems Dept., Phdadelphia, Pa.). Contract No. NAS 2-2477. IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- Consideration of certain factors involved in the entry and TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING landing phases of a manned mission to Mars. The applicability of STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, retropropulsion and aerobraking modes during these phases is 1966. TECHNICAL PAPERS. compared, and it is concluded that weight tradeoffs favor aerobraking. New York, American Institute of Aeronautics and Astronautics, The effect of present uncertainties in the atmospheric characteristics 1966, p. 383-390. 8 refs.

29 A66-25276

Inviscid equilibrium gas stability characteristics for a number spectra. Variations in the determinahon of the total carbon dioxide of pointed and spherically blunted bodies in unsteady supersonic abundance and total surface pressure between investigators are flight in the NASA Mars atmospheres have been calculated. to given. The author's preferred best-estimate of the Martian total . determine the effect of atmospheric composition on vehicle stability. surface pressure is 6 mb based on the 8700-A data of Spinrad and The computation is carried out in two parts. First, a complete Schorn and the 1.56-p data of Kuiper and Owen. A limited discussion solution of the steady state, zero angle of attack flow field in the is presented on the Mariner 4 occultation data including potential shock layer is obtalned for each model composition when treated as error sources and limitations on data applicability. Finally, a a real gas in chemical equilibrium. Then a perturbation method is comparison of the Mariner 4 and ground-based observational data li\. employed to determine the unsteady supersonic flow field. Static is made, including that of possible error sources in the data as well and dynamic stability derivatives (as a function of center of gravity as potenhal secular variations in the Martian surface pressure. location) are presented at a typical flight condition in each of the (Author) Mars model compositions and in air for several vehicle shapes. In addition, the variation of stability characteristics at discrete points along an entry trajectory is presented for a 45O pointed cone. It is shown that, in general, stability characteristics are not strongly influenced by the atmosphere composition for the vehicle geometries, A66-25292 # atmospheric compositions, and flight conditions investigated. DESIGN PROBLEMS AND EXPERIMENTS FOR MARS ATMOSPHERE (Author) PROBES. David E. Reese, Jr. (NASA, Ames Research Center, Vehicle Environment Div., Moffett Field, Calif. ) and Steven Georgiev (NASA. Ames Research Center, Moffett Field, Calif. ; Avco Corp., A66-25276 d# Research and Advanced Development Div., Wilmington, Mass. ). THE QUALITATIVE BEHAVIOR AND EFFECTS OF NONEQUILIBRIUM IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- CHEMISTRY BEHIND STRONG SHOCK WAVES IN GAS MIXTURES TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING OF CO2 AND N2. STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, Robert L. McKenzie (NASA, Ames Research Center, Moffett Field, 1966. TECHNICAL PAPERS. Calif. ). New York, American Institute of Aeronautics and Astronautics, IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- 1966, p. 542-552. 7 refs. TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING Review of experiments with a probe for the investigation of the STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, Martian atmosphere and a study of the design problems inherent in 1966. TECHNICAL PAPERS. the construction of such probes. Methods by which the structure New York, American Institute of Aeronauhcs and Astronautics, and composition of planetary atmospheres can be determined from 1966, p. 391-409. 24 refs. measurements made on board an entry vehicle are discussed; the A detailed estimate is made of the chemical system and its fundamental principle on which these methods are based is the cor- ~ reaction rates for shock conditions typical of those during entry into relation which exists between the density, pressure, and tempera- the Martian atmosphere. The results are shown to represent ture profiles for varying altitudes and vehicle deceleration meaeure- qualitatively the postshock chemical behavior and are intended to ments during the high-speed portion of the entry. Optical and mass serve as a basis for the design and analysis of related experimental spectroscopic techniques are described for measuring atmospheric investigations. They are subject, however, to substantial numerical composition. Vehicle design problems are considered in terms of adjustment as definitive experimental results become available. major vehicle subsystems including spin stabilization, instrumenta- ' The variations in the gross thermodynamic properties and individual tion, heat shield, and electrical power. D. P. F. species concentrations behind normal shock waves are Illustrated for shock speeds of 4 to 8 kmlsec and ambient densities wluch bracket the range of aerodynamic interest during atmosphere entry. The species included are CO2. N2, GO, CN, NO, 02.C, 0, and N. A system of 17 reactions is studied initially, 9 of which are shown A66-25461 to control the gross thermochemical behavior. Particular emphasis DETERMINATION OF THE LUMINANCE OF THE MARTIAN AT- MOSPHERE [DETERMINATION DE LA LUMINANCE DE L'AT- is given to the production of the strong radlant emitter, CN. Comparisons are made with some preliminary experimental results MOSPHERE DE LA PLANETE MARS]. and they demonstrate the ability of the proposed chemical system Audouin Dollfus (Paris, Observatoire, Meudon, Seine -et-Oise, model to reasonably predict the apparent production rate of CN France). behmd a normal shock wave. For most shock conditions anticlpated Acadgmie des Sciences (Paris), Comptes Rendus, Sgrie B - Sciences during entry into the Martian atmosphere, the concentration of CN Physiques, vol. 262, no. 7, Feb. 14, 1966, p. 519-522. 14 refs. is shown to rapidly overshoot its equilibrium value in the flow behind 1.n French. normal shock waves. Similar results are obtained for the shock Updating of work estimating the quantity of light diffused by the Martian atmosphere. Measurements of the variation of the polariza- layer ahead of a typical blunt Mars atmosphere probe over the major portion of most entry trajectories. (Author) tion of the light from Mars between the center and the edge of the disk give a value to the luminance of the atmosphere, in the absence of haze or clouds, of around 6.0 x 10-4 sblphot. If the low surface pressure determined spectroscopically and by Mariner 4 (9 to 20 mb) is correct, then a small amount of a fine aerosol must be permanently suspended in order to give the measured values of lumi- A66-25291 * nance . F.R.L. OUR PRESENT KNOWLEDGE OF THE MARTIAN ATMOSPHERE. D. F. Spencer (Caldornia Institute of Technology, Jet Propulsion Laboratory, Engineering Mechanics Div., Pasadena, Calif. ). IN: AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAU- A66-25834 TICS, AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING MARTIAN ATMOSPHERE - THE MARINER OCCULTATION EX- STONES TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, PERIMENT. 1966. TECHNICAL PAPERS. Joseph W. Chamberlain and Michael B. McElroy (Kitt Peak National r( New York, American Institute of Aeronautics and Astronautics, Observatory, Space Div., Tucson, Ariz. ). 1966, p. 532-541. 22 refs. Science, vol. 152, Apr. 1, 1966, p. 21-25: 35refs. Experimental data relating to the Martian surface pressure and Further analysis of data from the Mariner 4 occultation experi- surface density and the interpretation of the data required to obtain ment. It is argued that the C02 in the Martian atmosphere is not these physical properties are presented. The discussion of the strongly dissociated (as was earlier assumed) and that the main e ground-based astronomical data emphasizes the determination of ionospheric peak is analogous to the terrestrial E or perhaps F1 the Martian surface pressure from carbon dioxide absorption region. R.A.F.

30 A66-27887

A66-26031 * 866-27432 3 RADIOASTRONOMY STUDIES OF VENUS AND MARS. CONVECTIVE HEAT TRANSFER IN PLANETARY GASES. Cornel1 H. Mayer [ U. S. Naval Research Laboratory, Washington, Joseph G. Marvin and George S. Deiwert (NASA, Ames Research D. C. ). Center, Moffett Field, Calif. ). Astronautics and.Aeronautics, vol. 4, Apr. 1966, p. 13, 15, 16, 21, AIAA Journal, vol. 4, Apr. 1966, p. 727, 728. 6 refs. 23-25. Demonstration of the manner in which a versatile equation can Review of radio astronomical studies of the planet Venus. The be used to predict the heating rate in gas mixtures representative theoretical bases of such studies are outlined. Observations of of planetary atmospheres. The advantage of this equation is that Venus are recounted and the results summarized. Radio observa- the transport properties of the gas at the typically high stagnation tions of Mars, which have been less extensive and less fruitful than temperatures associated with entry velocities are eliminated and those of Venus, are briefly considered. The future prospects of replaced by those at a relatively low temperature. The equation such observations of Mars and Venus are surveyed. R. A. F can be used for ionizing monatomic gases, dissociating gases, and combinations of these. M. M.

A66-26122 ## LIMITATION ON OXYGEN CONCENTRATION IN A PRIMITIVE PLANETARY ATMOSPHERE. A66-27534 ## NATURAL OSCILLATIONS OF PLANETARY ATMOSPHERES AS L. V. Berkner and L. C. Marshall (Southwest Center for Advanced A FUNCTION OF THE PLANET'S SPEED OF ROTATION Studies, Dallas, Tex. ). [SOBSTVENNYE KOLEBANIIA PLANETNYKH ATMOSFER V Journal of the Atmospheric Sciences, vol. 23, Mar. 1966, p. 133- ZAVISIMOSTI OT SKOROSTI VRASHCHENIIA PLANETY]. 143. 25 refs. 6. S. Golitsyn and L. A. Dikii (Akademiia Nauk SSSR, Institut Research supported by the Southwest Center for Advanced Studies; Fiziki Atmosfery, Moscow, USSR). NSF Grants No. GP-768; No. GP-4708. Akademiia Nauk SSSR, Izvestiia, Fizika Atmosfery i Okeana, The absorption of ultraviolet radiation across the dissociative vol. 2, Mar. 1966, p. 225-235. 13 refs. In Russian. band (1500-2100 is computed for the three component atmospheric 1) Numerical calculation of the periods of natural oscillation system, 02. C02, HzO. for a considerable range of possible primi- and the corresponding eigenfunctions for planetary atmospheres tive atmospheres. The results illustrate clearly the limitation on as a function of the parameter y (square of the ratio of twice the photodissociation of H20 as a source of oxygen, as a consequence of linear velocity at the equator to the speed of sound). The results shadowing H20 by the oxygen produced. Thus the Urey self- of so of the numerical integration of the Laplace tidal equations are regulation of the maximum oxygenic concentration in a primitive found to correlate well with the asymptotic theories proposed by atmosphere (in the absence of appreciable photosynthetic oxygenic Hough and by Dikii, for small and large values of y. respectlvely. production) is shown as not exceeding about of the present oxy- The lower oscillation modes are calculated for the atmospheres genic concentration. The presence of excess carbon dioxide lowers of the earth and Jupiter. v. P. this lunit ,somewhat. These conclusions have important implications with respect to the limiting oxygenic content of the primitive atmosphere of any planet. (Author)

A66-27874 * A66-26132 EARTH ENTRY FLIGHT TEST OF MARS ENTRY VEHICLES. F. G. Beuf, G. D. Katz, and R. Kern (General Electric Go., THE VERTICAL TEMPERATURE DISTRIBUTION IN THE MARTIAN J. Philadelohia. Pa. ). ATMOSPHERE. I (American Institute of Aeronautics and Astronautics and NASA, George Ohring and Joseph Mariano (Geophysics Corporation of Flight Testing Conference, Huntsville. Ala., Feb. 15-17, 1965, America, Bedford, Mass. ). Paper 65-219.) Journal of the Atmospheric Sciences, vol. 23, Mar. 1966, p. 251- Journal of Spacecraft and Rockets, 255. 8 refs. vol. 3, Apr. 1966, p. 498-503. Contract No. NAS 9-3423. Review of previous calculations of the vertical temperature dis - tribution in the Martian atmosphere, based upon a convective-radiative equilibrium model. Vertical temperature distributlons computed for the Martian atmosphere indicate that the temperatures are not sensitive to variations in surface pressure and carbon dioxide com- A66-27875 # parable to present uncertainties in these parameters - a result also EARTH RE-ENTRY SIMULATION OF PLANETARY ENTRY EN- evident in the computations of Prabhakara and Hogan. Where com- VIRONMENT. parisons could be made between the present results and those of Haim Kennet (Boeing Go., Aero-Space Div., Flight Technology Prabhakara and Hogan, they indicate that the computed temperature Dept., Seattle, Wash. ) and Roy A. Taylor (Boeing Co., Aero-Space profiles are in good qualitative agreement but that the present pro- Div., Seattle, Wash. ). files are some 15 to 20°K lower above 20 km. M. F.

A66-27278 DEVELOPMENTS IN MICRO GAS CHROMATOGRAPHY. W. F. Wilhite (California Institute of Technology, Jet Propulsion Laboratory, Space Sciences Div., Pasadena. Calif. ). Journal of Gas Chromatography, vol. 4, Feb. 1966, p. 47-50. 7 refs. A micro gas chromatographic system has been developed at the A66-27887 # Jet Propulsion Laboratory to analyze the atmosphere of Mars in a few BUOYANT PROBES INTO THE VENUS ATMOSPHERE. seconds during the descent of a landing capsule. The system consists F. R. Gross (Goodyear Aerospace Gorp., Space Systems Div., of micro components, including highly efficient micro packed columns Akron, Ohio). capable of rapid separation at flow rates of less than 1 cc per minute, (AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAUTICS, a micro thermal conductivity detector with an internal volume of 0.1 UNMANNED SPACECRAFT MEETING, LOS ANGELES, CALIF., filiter and sensitivity better than 5 ppm and a sampling valve ca- MARCH 1-4. 1965 /AmPublication CP-121. p. 76-87. ) pable of injecting a 1-@litergas sample. The components, and the Journal of Spacecraft and Rockets,'vol. 3, Apr. 1966, p. 582-587. new techniques required to develop them, are described. (Author) 17 refs.

31 A66-28129

A66-28 129 heliocentric longitude reveal that the darkening wave is due to the A NEW ESTIMATE OF THE SURFACE TEMPERATURES OF VENUS. transport of both water vapor and dust from high latitudes toward William Plummer and John Strong (Johns Hopkins University, School the equator. M.M. tr of Engineering Science, Laboratory of Astrophysics and Physical Meteorology, Baltimore, Md. ). Astrophysical Journal, vol. 144, Apr, 1966, p. 422-424. 15 refs. Contract No. AF 19(628)-4334. Comments on recent measurements of the surface temperature of Venus. It is shown that the polarizatlon measurements by Clark A66-29952 # 9' and Kuz'min may be used with the radar dielectric coefficient to ROTATIONAL EFFECTS IN THE MAGNETOSPHERE OF JUPITER. estimate what part of the total microwave brightness is due to D. B. Melrose (Sussex, University, School of Mathematical and thermal radiation from the surface of Venus, as distinguished from Physical Sciences, Falmer, Brighton. England). nonthermal emission originating in the Venus atmosphere. It is COSPAR, International Space Science Symposium, 7th. Vienna, concluded that all microwave temperature measurements reported Austria, May 10-19, 1966, Paper. 11 p. 7 refs. prior to those of Clark and Kuz'min have been based upon an over- Discussion of the major formal difficulty encountered in trying simplified model which failed to provide for nonthermal emission. to construct a theoretical model magnetosphere for the planet A.B.K. Jupiter constituted by the consequences of the rapid rotation of the planet on the distribution of plasma in the magnetosphere. It is pointed out that, for the magnetosphere of Jupiter, rotational effects A66-29417 are important beyond a few radii, and, consequently, some additional UPPER ATMOSPHERE AND IONOSPHERE OF MARS. physical condition (other than interparticle collisions) must determine T. M. Donahue (Pittsburgh. University. Pittsburgh, Pa. ). the plasma distribution at such distances. It is suggested that the Science, vol. 152, May 6, 1966, p. 7631 764. 6 refs. appropriate condition is that the magnetosphere be stable against NSF-supported research, Contract No. NASr-179. fluting (interchanges of the flux tubes of the magnetic field) when It is argued that the single-layer ionosphere at 125 km discov- this can reduce the total kinetic energy of rotation of the magneto- ered rn the Mariner 4 occultation experiment is an F1 region coin- sphere. It is also suggested that the onset of the two-stream ciding with the UVphotoionization peak. The 602 density there instability causes the corotating magnetosphere to break down at must be of the order of 10l1 molecules/crn3. Such a density is con- distances well inside distances where the solar wind would give a sistent with the properties of the lower atmosphere by Mariner 4 boundary similar to'that of the magnetosphere of the earth. M. M. and the temperature model of Chamberlain and McElroy if the atmosphere is mainly CO2 below 70 km. The absence of an FZ region can be explained even If the density ratio of 0 to C02 is 100 at 230 km on the basis of the rapid conversion of Oc to O2 by C02. Thus a model with an exospheric temperature of 400°K, a modest degree A66-29958 of COz dissociation, and diffusive separation above 70 km is pos- RADIO OCCULTATION MEASUREMENT OF THE MARTIAN ATMO- sible. (Author) SPHERE OVER TWO REGIONS BY THE MARINER IV SPACE PROBE. * Arvydas Kliore, Dan L. Cain, and Gerald S. Levy (California Institute of Technology, Jet Propulsion Laboratory, Pasadena, A66-29643 Calif. 1. COSPi+R, International Space Science Symposium, 7th, Vienna, PURITY OF THE MARTIAN ATMOSPHERE [SUR LA PURETE DE Austria. May 10-19, 1966, Paper. 18 p. 12 refs. d L'ATMOSPHERE DE LA PLANETE MARS]. Durlng the July 1965 fly-by of Mars by the Mariner 4 space Audouin Dollfus and Jean Focas (Paris, Observatoire, Meudon, probe, radio occultation measurements the atmosphere were Seine -et-Oise, France). of performed over two regions above the planet's surface. Prelimi- Acadgmie des Sciences (Paris), Comptes Rendus, Sdrie B - Sciences nary analysis of the data obtained during the exit phase, which OC- Physiques, vol. 262, no. 15, Apr. 13, 1966, p. 1024-1027. In French. curred on the dark side over Mare Acidalium, mdicates that the Study of the spectral variation in the polarization of light from surface pressure there is some 3 mb higher than that over the the planet Mars, over all of the observable phase angles and for entry region (ElectrislMare Chronium). addition, analysis eight ranges of spectra covering 0.47 to 1.05 ~1,during the period In of the trajectory of the probe at the times of commencement and end Dec. 1964 to July 1965. The curves for the variation of the propor- of occultation indicates that the surface feature which interrupted tion of polarized light are plotted as a function of the phase angle the signal of the probe at commencement of occultation was at a using different filters and only retaimng data recorded in the absence radial distance of about 3384 3 km from the niass center of Mars, of observable clouds in the Martian atmosphere. The degree of * and the corresponding radial distance at exit Was about 3379 *4 km. polarization at the center of the disk for the maximum phase angle (Author ) of 39.9' is plotted as a function of the day and month of the year. It IS found that pulverized samples of limomte and goethite reproduce the characteristics of the polarized light received from Mars with close accuracy. This would appear to demonstrate that the estimate A66-29 966 # of 30 mb for the Martian atmospheric pressure is too high. D.P.F. A DISCUSSION OF THE PLANETARY QUARANTINECONSTRAINTS. J. 0. Light, C. W. Craven (Cahfornia Institute of Technology, Jet Propulsion Laboratory, Pasadena, Calif. ), W. Vishniac (Roches- A66-29951 * ter, University, Rochester, N. Y. ), and L. B. Hall (NASA, Washing- AN ANALYSIS OF MARTIAN CLOUDS AND THEIR TOPOGRAPH- ton, D. C. ). ICAL RELATIONSHIP. COSPAR, International Space Science Symposium, 7th, Vlenna, R. A. Wells (London, Universlty, University College, London, Austria, May 10-19, 1966, Paper. 16 p. England). Demonstration of the incompleteness of the current standards COSPAR, International Space Science Symposium, 7th, Vienna, for planetary quarantme because they do not consider all of the Austria, May 10-19, 1966, Paper. 59 p. 58 refs. numerous sources of potential biologlcal contamination. It is also Study of Martian clouds and of their relationships from tabulated shown that the allocation process necessary to distribute the total data representing occurrences over the past century. The frequen- probability of contamination to each of these numerous and complex cy of cloud occurrences distributed against heliocentric longitude 1s sources of contamination will be a prodigious and detailed task. * displayed in histogram form for the two chief cloud groups, white The following statement of the appropriate level of commitment is and yellow. White clouds show two peaks of maximum occurrence, recommended: the planetary quarantine policy shall require 99.9% while yellow clouds appear to show three peaks. The white cloud confidence that the unmanned exploration of Mars will not contami- histogram is a map of water vapor transfer from the polar caps to nate the planet with terrestrial organisms. A partial list and dis- the equatorial region. The yellow cloud frequency follows a general cussion of the numerous sources of contamination which must be $I increase in the amount of insolation received by the planet. Areo- considered by the set of planetary quarantine constraints is provided. graphic latitude plots of white and yellow cloud positions against M. M.

32 A66-30713

A&-30049 # made of the diurnal component of the small-scale vertical heat flux THE ATMOSPHERIC PRESSURE AT THE SURFACE OF MARS. and of the amplitude of the thermal tides that this diurnally varying Karl D. Rakos (Graz, University, Observatory, Kanzelhljhe, heat input would produce. A study is made of differential heating Austria; Lowell Observatory, Flagstaff, Ariz. ) . and general circulation at the solstices. A.B.K. COSPAR, International Space Science Symposium, 7th, Vienna, May 10-19, 1966, Paper. 4 p. NASA-supported research. Experimental results on the determination of the density of the Martian atmosphere fromphotoelectric measurements of the eclipses A6640355 * of Phobos using a newly developed photoelectric scanner, the 61-in. THE SYSTEMATIC INVESTIGATION OF THE METEOROLOGY OF reflector at Flagstaff, Ariz. in January and June 1965, and the MARS. 84-in. telescope at Kitt Peak, Ariz. in June 1965. The first useful Morris Tepper (NASA, Office of Space Science and Applications, and best observation was obtained on Jan. 11; the June observations Washington, D.C.). are not very suitable as in that month Phobos was 0.7 magnitude IN: VIRGINIA POLYTECHNIC INSTITUTE, CONFERENCE ON THE fainter than in January. The May 1967 eclipses will be more propi- EXPLORATION OF MARS AND VENUS, VIRGINIA POLYTECHNIC tious due to the fact that Phobos will be nearby two magnitudes INSTITUTE, BLACKSBURG, VA., AUGUST 23-27, 1965, PRO- brighter than in January. The surface pressure was found to be CEEDINGS. 30 mb; the observed light curve was brought into very good agree- Conference supported by the National Aeronautics and Space Ad- ment with the computed values by sucessive approximations. ministration, and the U.S. Air Force Cambrhdge Research Labora- D. P. F. tories. Blacksburg, Va., Virginia Polytechnic Institute, 1965, p. V-1 to V-14. Study of the relationship of weather conditions on Mars to Its A6630050 # planned manned exploration. It is thought that due to apparent low A THEORETICAL INVESTIGATION OF CYTHEREAN, MARTIAN atmospheric surface pressure and insignificant water pressure vapor AND JOVIAN UPPER ATMOSPHERES. most weather problems familiar to the earth excepting those related Milo Shinwm (Ochanomizu University, Dept, of physics, Tokyo, to surface winds would be eliminated. B. 8. Japan). COSPAR, International Space Science Symposium, 7th. Vienna, Austria, May 10-19, 1966, Paper. 4 p. 7 refs. Calculation of the heights of the dissociation layers on Venus, Mars, and Jupiter using the atmospheric model proposed by Kaplan, A66-30356 # Kliore. and others. The results are summarized in a table together THE POSSIBILITIES OF LIFE ON MARS. with the intensities of the GO flame airglow estimated from these Frank B. Salisbury (Colorado State University, Fort Collins, Colo. ). data. The effect of diffusion was neglected, and a technique 1s given IN: VIRGINIA POLYTECHNIC INSTITUTE, CONFERENCE ON THE for including this parameter, D. P. F. EXPLORATION OF MARS AND VENUS, VIRGINIA POLYTECHNIC INSTITUTE, BLACKSBURG, VA., AUGUST 23-27, 1965, PRO- CEEDINGS. Conference supported by the National Aeronautlcs and Space Ad- ministration, and the U.S. Air Force Cambrrdge Research Labora- 866-30352 #I tories. BALLOON-TELESCOPE OBSERVATION OF THE PLANETS. Blacksburg, Va., Virginia Polytechnic Institute, 1965, p. VI-1 to John D. Strong (Johns Hopkins University, Baltimore, Md. ). VI-16. 17 refs. IN: VIRGIKIA POLYTECHNIC INSTITUTE, CONFERENCE ON Theoretical study of the possibilities of life on Mars. The THE EXPLORATION OF MARS AND VENUS, VIRGINIA POLY- possible existence of primitive plants, thriving advanced plants, and TECHNIC INSTITUTE, BLACKSBURG, VA., AUGUST 23-27, 1965, even of intelligent lrfe on that planet are speculated upon. It IS con- PROCEEDINGS. [A66 - 30350 16- 301 cluded that cases can be made for the existence of life and perhaps Conference supported by the National Aeronautics and Space Ad- even of an advanced technology on Mars or - alternatively - for a ministration, and the U. s. Air Force Cambridge Research Labora- lifeless moonlike Mars. B.B. tones. Blacksburg, Va., Virginia Polytechnic Institute, 1965, p. 11-1 to 11-8. 18 refs. Determination of water vapor in the upper atmosphere of Venus A66-30713 # with an automatic klescope-spectrometer unit carried by a balloon. MODELS FOR THE ATMOSPHERE OF MARS BASED ON THE Certain aspects of the data-recording system are discussed, as well MARINER 4 OCCULTATION EXPERIMENT. as the method of data reduction. The results of absorption measure- Gunnar Fjeldbo, Wencke C. Fjeldbo, and Von R. Eshleman ments are interpreted in terms of water-vapor quantities on Venus. (Stanford University, Center for Radar Astronomy, Stanford, A mechanism by which the cloud temperature on the dark side of Calif. ). Venus IS prevented from falling below -4OOC is suggested. A.B.K. Journal of Geophysical Research, vol. 71, May 1, 1966, p. 2307-2316. 20 refs. Grants No. NGR-05-020-065: No. NsC-377. A66-30353 Several possible atmospheric models are investigated based on SOME ASPECTS OF THE CIRCULATION OF MARS. data from the radio occultation experiment, and one is shown to be Conway Leory (RAND Gorp., Santa Monica, Calif. ). more likely than the others. Profiles in height of the constituent IN: VIRGINIA POLYTECHNIC INSTITUTE, CONFERENCE ON number densities, electron number density, temperature, pressure, THE EXPLORATION OF MARS AND VENUS, VIRGINIA POLY- and mas5 density are derived. The analysis indicates that Mars TECHNIC INSTITUTE, BLACKSBURG, VA., AUGUST 23-27, 1965, has a tenuous carbon dioxide lower atmosphere with a temperature PROCEEDINGS. of only about 180°K near the surface, and an atomic oxygen upper Conference supported by the National Aeronautics and Space Ad- atmosphere with a temperature of only about 80°K. Frozen carbon ministration, and the U.S. Air Force Cambridge Research Labora- dioxide particles may be an almost permanent feature of the atmo- torie 5. sphere at intermediate altitudes. The main daytime ionospheric Blacksburg, Va., Virginia Polytechnic Institute, 1965, p. 111-1 to layer has its peak density at 120 km, and is most likely a Bradbury 111-10. 20 refs. (Fz)layer mth the principal ion (O+) being lost through Ot t GOz - Contract No. Nasr-Zl(7). 02t t CO. The atmospheric mass density decreases nearly ten Study of the circulation of the Martian atmosphere and of its orders of magnitude from the surface to the base of the exosphere imphcahons for terrestrial meteorology. Some of the main features at 140 km, thus remaining several orders of magnitude below the of the expected vertical temperature distribution, as given by ra- density of the earth's atmosphere at corresponding altitudes despite diative -equilibrium calculations, are reviewed. Estimates are the lower gravity. (Author)

33 A66-30889

A66-30889 # applies to atmospheric currents in the planet's temperate latitudes. PLANETARY ATMOSPHERIC DETERMINATION UTILIZING A The mean daily drift of the spot w .4056 relative to System II, SEMIPASSIVE PROBE. and -lo. 7756 relative to System I. corresponds to a mean . Frank S. Holman and Haim Kennet (Boeing Co., Aero-Space Div., rotation period of 9h49m18S. 5. A detailed study of its motion Seattle, Wash. ). disclosed a nearly sinusoidal displacement with respect to its mean (AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAUTICS, position. A period of 300 days and an amplitude of 4O in longitude UNMANNED SPACECRAFT MEETING, LOS ANGELES, CALIF., would best describe this oscillatory motion. The center of the spot MARCH 1-4, 1965. AIAA Publication CP-12, p. 236-245.) remained stationary near zenographic latitude +24O, within the prob- c Journal of Spacecraft and Rockets, vol. 3, May 1966, p. 651-658. able error of the measures. This solitary spot apparently represents 9 refs. the fifth observed outbreak of activity in the well-known but rarely observed North Temperate Current "C, " a current which has produced the shortest rotation periods ever recorded on Jupiter. There is evidence that the outbreak of rapidly 'rotating spots in this latitude A66-30925 # may be periodic, as the spots tend to appear at 12-yr intervals when THERMAL CONVECTION IN THE MARTIAN ATMOSPHERE. the North Temperate Belt lies nearest to the planet's equator. An F. M. Neubauer (Chicago, University, Dept. of Geophysical outstanding characteristic of the most recent NTBs spot was its Sciences, Chicago, Ill. ). almost complete invisibility to the visual observer, and that it could Journal of Geophysical Research, vol. 71, May 15, 1966, p. 2419- be photographically recorded only on plates taken in blue and ultra- 2426. 11 refs. violet light. (Author) Formation of dust clouds observed in the Martian atmosphere can be explained by the action of dust devils larger than 100 meters in diameter. The condition for the onset of thermal convection is A66-3301 3 the existence of an unstable temperature profile. The daily varia- AN EXPERIMENTAL STUDY OF "TAYLOR COLUMNS. " tion of the atmospheric temperature profile shows that the Martian R. Hide (Massachusetts Institute of Technology, Cambridge, Mass.) atmosphere is more favorable for the initiation of dust devils than and A. Ibbetson (Woods Hole Oceanographic Institution, Woods the earth's atmosphere. The calculations indicate that dust devils Hole, Mass.). on Mars produce wind velocities only slightly lower than those on Icarus, vol. 5, May1966, p. 279-290. 17 refs. earth. (Author) Research supported by the Royal Society of London and the Depart- ment of Scientltic and Industrlal Research; Contract No. AF 61(052)- 216; NSF Grant No. G-22390; Contract No. Nonr-2196(00). A66-31310 # Description of a theoretical and experimental investigation of THE COMMISSION ON PLANETARY SURFACES - THE PLANET Taylor columns as being likely to bear on processes occurring in Jupiter's atmosphere. Simple theoretlcal arguments suggest that JUPlTER IN 1963 [COMMISSION DES SURFACES PLANETAIRES - LA PLANETE JUPITER EN 19631. for Taylor columns to arise in a homogeneous, inviscid, incompress- r M. Marin and M. Walbaum. ible fluid that rotates uniformly about the z axis of coordinates of L' Astronomie, vol. 80, Apr. 1966, p. 151-156. In French. a Cartesian system, the ratio of the linear dimension in the z direc- Study of the surface of Jupiter, using results obtained by 29 tion of the topographical feature to that of the fluid container must observers in various parts of the world, but mamly in France. exceed a Rossby number based on the relative hydrodynamical flow The observations made it possible to follow the slow evolution of velocity, on the linear dimensions in the x and y directions of the tl atmospheric phenomena, which are described. Some comments topographical feature, and on the basic rotation rate of the system, Systematic experiments are made on the characteristics of the Red Spot. Position measure- multiplied by a number of order umty. ments of details were made, and their periods of rotation were cal- were carried out on Taylor columns produced by moving solid objects culated. F.R.L. through a liqud in a rotating cylindrical tank. They show that the theorebcal criterion is probably correct and indicate how it 1s affected by viscosity. M. M.

866-3251 7 # THE 10-MICRON LIMB DARKENING OF VENUS. A66-34149 J. A. Westphal (California Institute of Technology, Div. of Geolog- DIFFUSE REFLECTION BY AN INHOMOGENEOUS PLANETARY ical Sciences, Pasadena, Calif. ) . ATMOSPHERE. Journal of Geophysical Research, vol. 71, June 1, 1966, p. 2693- 2696. Joseph W. Chamberlain and Michael B. McElroy (Kitt Peak National Observatory, Tucson, Ariz. ). Grant No. NsG-56-60. Astrophysical Journal, vol. 144. June 1966, p. 1148-ll58. Observations of the 8- to 14-p flux from diametric scans of 8 refs. An approximate solution developed for the diffuse reflection Venus with the 200-in. Hale telescope operated in the east-arm is by an inhomogeneous atmosphere specifically one in which the Cassegrainian mode. The reduced data indicate an unexpected - albedo for single scattering, B, decreases exponentially with op- brightening near the Cytherean limb. The data show a more com- tical depth 7. The approach consists of finding a homogeneous at- plicated atmospheric structure than that postulated by published mosphere (UJ P constant) that closely mimics the intensities reflected models. Horizontal inhomogeneity of the emission complicates the by the inhomogeneous one. The solution for the diffusely reflected interpretation. W. M. R. radiation is conveniently expressed in terms of an effective Chandrasekhar H function (which is strictly defined only for a homogeneous atmosphere). This H function (which depends on UJ) thus A6633009 specifies an effective mean albedo, me, for the entire atmosphere. A RAPIDLY MOVING SPOT ON JUPITER'S NORTH TEMPERATE Then the optical depth where the local albedo is me defines, for pur- BELT. poses of this paper, an effective depth of absorption, Te. When 23(T)= Elmer J. Reese and Bradford A. Smith (New Mexico State Univer- 1 near the top of the atmosphere, which would be the case for weak sity, Observatory, University Park, N. Mex. ). absorption lines formed in a scattering atrnosphere, we find T, z Icarus, vol. 5, May 1966, p. 248-257. 6 refs. 1/2[3(1 - We)I1I2. This expression differs by a factor of 1/2 from a a Grant No. NsG-142-61. similar one relating the mean depth of absorption, (defined in an A very rapid drift in the longitude of a small dark spot on the earlier paper as the centroid of the sink hnction), to the albedo W south edge of Jupiter's North Temperate Belt (NTBs) has been of a homogeneous atmosphere. The physical distinction between these determined from measurements of 51 photographic plates taken in two concepts (mean depth and effective depth) is discussed, as is the blue and ultraviolet light at the New Mexico State University Ob- problem of defining a suitable mean depth of line formation in an in- servatory between July 7, 1964, and Apr. 1, 1965. During this homogeneous atmosphere. Numerical results from the simple ap- * interval of 268 days the NTBs spot made seven complete circuits of proximation given here compare favorably, for a wide variety of the planet relative to System 11, i. e. , the system which normally cases, with the essentially exact results obtained from a computer

34 A66-38024

program developed by Bellman et al. In the appendices a number of model and Parker's "solar wind" model (a= 3/2) shows that, in integrals involving H functions are evaluated and Bellman's derivation both cases, the asymptotic behavior at great radial distances of the basic integral equation for the inhomogeneous atmosphere is (r - -1 of the density (p), mean velocity (&), and nonradial pressure given with the more familiar notation and other conventions of components (p)s)sor pVv)are the same for the evaporative and Chandrasekhar. (Author) hydrodynamical models. In both evaporative models the radial component ( prr) of the pressure tensor is greater than the other (78)sor 9$,). This anisotropy grows with increasing radial dis- A66-34712 tances. Therefore, the assumed isotropic pressure of the ordinary ION-SPECTROMETER FOR THE TERRESTRIAL MESOSPHERE hydrodynamical models is probably too low. (Author) AND THE ATMOSPHERE OF MARS. H. Dolezalek and A. L. Oster (Avco Corp., Space Systems Div., Wilmineton.-. Mass. 1. Zeitschrift fur Geophysik, vol. 32, no. 3, 1966, p. 163-172. 17 refs. A66-37016 Contract No. DA-19-020-AMC-O058(X). THENATUREOFTHECLOUDLAYERONVENUSFROMMICRO- Description of the modifications in the design of a Gerdien- WAVE OBSERVATIONS. type chamber required for measurements of the mobility spectrum A. E. Basharinov and B. G. Kutuza (Akademiia Nauk SSSR, Institut in the layers of the terrestrial upper atmosphere and in planetary Radiotekhniki i Elektroniki, Moscow, USSR). atmospheres. Concentric rings are placed at both ends to com- JAstronomicheskii Zhurnal, vol. 43, Jan. -Feb. 1966, p. 149-153.) pensate the inner and outer edge effects; ions can only enter through Sovlet Astronomy, vol. 10, July-Aug. 1966, p. 117-120. 11 refs. a concentric slit and during certain time intervals. Both electrodes Translation. of the chamber are subdivided so as to allow a sinusoidal driving voltage to be applied, with its amplitude increasing along the axis of the chamber. Ion numbers can be elictrometrically measured for any selected mobility range. The instrument was tested in the laboratory, simulating the conditions of the lower ionosphere. A66-37017 D. P. F. SPECTROPHOTOMETRY OF THE METHANE ABSORPTION BANDS AT 0.7-1.0 p ON THE DISK OF JUPITER. V. G. Teifel' (Akademiia Nauk Kazakhskoi SSR, Astrofizicheskii A66-34896 # Institut, Alma-Ata, Kazakh SSR). THE MARINER IV MISSION TO MARS. (Astronomicheskii Zhurnal, vol. 43, Jan. -Feb. 1966, p. 154-156.) Carl Sagan (Harvard University. Harvard College Observatory; Soviet Astronomy, vol. 10, July-Aug. 1966, p. 121-123. Translation. Smithsonian Institution, Smithsonian Astrophysical Observatory. Cambridge, Mass. ). Astronomical Society of the Pacific, Leaflet, July 1966. 8 p. v Analvsis and internretation of the data obtained bv Mariner 4 A66-37035 * on the planet Mars. The significance of the lack of an appreciable SPECTRA OF JUPITER AND SATURN IN THE REGION 1 TO 2.5 magnetic field for this planet is discussed; it suggests that no mi- [SPEKTRY IUPITERA I SATURNA v OBLASTI 1 - 2.5 1. gration of iron from the mantle toward the core occurred. lt is V. I. Moroz (Gosudarstvennyi Astronomicheskii Institut, Moscow, shown that the highly diminished differentiation on Mars as com- USSR). a% pared with earth would lead to correspondingly low levels of out- Astronomicheskii Zhurnal, vol. 43, May-June 1966, p. 579-592. gassing. The analysis of the results of the radio occultation ex- 41 refs. In Russian. periment to determine the temperature at the base of the Martian Results of a study at 1 to 2.5 p of the spectra of Jupiter, Saturn, atmosphere is described - a temperature of about 100°K is indi- and the rings of Saturn, with resolutions of XIAX= 500, 150, and 20, cated, with a surface pressure in the range from 6 to 10 mb. An respectively. An "ordinary" reflection model is applied assuming analysis of the photographs indicates that there has been crater that the cloud layer boundary is optically equivalent to a solid sur- erosion. Thus the past presence of water on Mars is highly prob- face. The estimated CH4 content over Jupiter's cloud layer is less able. D. P. F. than 150 m-atm. A possible substantial contribution of the H 1-0 band to the absorption at 2p is indicated and the planet's total atmospheric pressure is estimated at 2 atm. It is believed most . A66-35799 likely that CH4 ice particles form the cloud layer of Saturn and that THE PLANET VENUS. H20 ice particles form the rings. V. z. R. Jastrow (NASA, Goddard Space Flight Center, Goddard Institute for Space Studies; Columbia University, New York, N. Y. ) and S. I. Rasool (NASA, Goddard Space Flight Center, Goddard Institute A66-38022 for Space Studies; New York University, New York, N. Y. ). MARTIAN ATMOSPHERE AND CRUST. Science Journal, vol. 2, July 1966, p. 58-62. S. myamoto (Kyoto University, Institute of Astrophysics, Kwasan The Comparison of the atmospheres of Venus and the earth. Observatory, Kyoto, Japan). high surface temperature of Venus is attributed to the exceedingly Icarus, vol. 5, July 1966, p. 360-374. 30 refs. thick and opaque atmosphere of this planet. It is shown that as a Analysis of the atmosphere and crust of the planet Mars. A result of its high C02 content, the Venusian atmosphere absorbs tentative picture of the circulation pattern in the planet's northern about 99% of the reradiated planetary heat in comparison with 90% hemisphere is proposed, based on cloud data. Mariner-4 photographs absorbed by the earth's atmosphere. An attempt is made to describe are used to analyze the crust of Mars, including the so-called the surface of Venus. It is suggested that the reason for the marked "canals. I' R.A. F. divergence in the atmospheric characteristics of the two planets may lie in the answer to the question of whether or not Venus still retains its original atmosphere. A. B. K. A66-38024 TRANSMISSION OF THE ATMOSPHERE OF MARS IN THE REGION OF 2 p. (r A66-36605 # L. D. Gray (California. University, Dept. of Engineering, Los EVAPORATIVE AND HYDRODYNAMICALATMOSPKERIC MODELS. Angeles, Calif. ). J. Lemaire (Likge, Universite: Institut d'Astrophysique, Li'ege, Icarus, vol. 5, July1966, p. 390-398. 27 refs. Belgium). NASA-sponsored research. Annales d'Astrophysique. vol. 29, May-June 1966, p. 197-203. The random Elsasser band model is used to compute the trans- 15 refs. mission of the atmospheres of earth and Mars for the 2-p bands Comparisons between (1) Chamberlain's evaporative model of carboe dioxide. This band model IS shown to give good agree- and his "solar breeze" model and (2) dpik and Singer's evaporative ment with measurements of spectral transmission for homogeneous

35 A66-39455 paths of C02 and also for nonhomogeneous paths through the earth's A66-40424 atmosphere when the Curtis -Godson approximation is used. The THE ATMOSPHERE OF MERCURY. 2-1.1 bands of C02 are strong in the atmosphere of both earth and S. I. Rasool (NASA, Goddard Space Flight Center, Goddard Institute Mars and, at a gwen temperature, their absorption is a function for Space Studies; New York University, Dept. of Meteorology and only of the product mp. Comparison of calculated values for trans - Oceanography, New York, N. Y. ), S. H. Gross (Cutler-Hammer, mission of sunllght through both atmospheres indicates that mpd, = Inc., Airborne Instruments Laboratory Div., Melville, N. Y. ). and 500 f 100 mr-atm-mb where m is the amount of C02 inone air mass W. E. McGovern (New York University, Dept. of Meteorology and and po* is the "effective" surface pressure. For mg i. 60 to 85 mr- Oceanography, New York, N. Y. ). atm, the above value of mpd leads to psb I 7.1 * 2.2 mb for the Space Science Reviews, vol. 5, Aug. 1966, p. 565-584. 43 refs. surface pressure of the Martian atmosphere. (Author ) Grant No. NsG-499. Review of information available on the temperature, composition, and surface pressure of Mercury's atmosphere and discussion of the implications of a nonsynchronous rotation of the planet on the atmosphere. Several models are constructed for the atmosphere which A66-39455 are consistent wlth the observations in an attempt to determine whether they are stable against depletion of the atmosphere by TRANSIENT TEMPERATURE RESPONSE OF A POROUS MATRIX gravitational escap;. The results arediscussed from the standpoint ENTERING A PLANETARY ATMOSPHERE. of the origin of the atmosphere. M. M. Latif M. Jiji (New York City University, Dept. of Mechamcal Engi- neering, New York, N. Y. ). Applied Scientific Research, vol. 15, no. 4-5, 1965, p. 322-330. 5 refs. Analysis of the transient temperature behanor of a transpira- A66-40469 #k tion-cooled porous matrix entering a planetary atmosphere wlth GREEN-HOUSE EFFECT IN THE ATMOSPHERE OF VENUS constant velocity and negatlve entry angle. The analysls IS based [0 TEPLlCHNOM EFFEKTE V ATMOSFERE VENERY]. on one-dimensional heat conduction in a porous plate subjected to G. M. Strelkov. a time-dependent heat flux at one side and cooled internally by mass Kosmicheskie Issledovaniia, vol. 4, July-Aug. 1966, p. 581-591. injection from a constant temperature reservoir at the opposlte side. 24 refs. In Russian. An exact closed-form solution is obtained, and temperature charts Analysis of the radiant-energy transfer below the cloud cover are given for a wide range of Fourier number and coolant flow in the Venus atmosphere, on the assumptions that the atmosphere parameters. (Author) is in a state of local thermodynamic equilibrium, the energy transfer occurs only by ab-orption and reradiation,- and that IR radiation IS fully absorbed by the cloud cover. Two cises are consiciered: (1) the atmospheric absorption coefficient is independent of frequency ("gray" atmosphere), and (2) this coefficient at wavelengths be- "r tween 8 and 12 mm 1s less appreciable than the absorption coefficient 866-39487 in the infrared. In both cases it is found that the presence of a HYDROGEN MOLECULES IN ASTRONOMY. cloud cover can not alone produce a green-house effect and that the G. B. Field, W. B. Somerville, and K. Dressler (Princeton latter must be caused by an atmosphere containing components University, New Observatory, Princeton, N. J. ). capable of IR absorption. On the assumption that carbon dipxide M IN: ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS. in the two cases constitutes 5 and 15% of the total atmospheric mass VOLUME 4. of Venus respectively, estimates are obtained of the water vapor Edited by Leo Goldberg. content which, together with the C02 content, will provlde the re- Palo Alto, Annual Reviews, Inc., 1966, p. 207-244. 155 refs. quired nontransparency in the 8-to-12-mm range. V.P. Grant No. NsG-414. Discussion of the astronomical implications of hydrogen. The structure of the hydrogen molecule and of molecular ions and polyatomic systems are discussed. Such aspects of hydrogen A66-40478 molecules in astrophysics as planetary and stellar atmospheres and MARTIAN WAVE OF DARKENING - A FROST PHENOMENON? interstellar space are considered, and the 14 discrete vibrational Joseph Otterman and Finn E. Bronner (General Electric Co. I levels associated with the electronic ground state of hydrogen are Missile and Space Div. , King of Prussia, Pa. ). mvestigated. B.B. Science, vol. 153, July 1, 1966, p. 56-60. 25 refs. Review of a new hypothesis which attributes the Martian "wave of darkening" to soil frost phenomena. It is thought that diurnal freezing and thawing of the ground, which uses moisture transported by the atmosphere from the melting polar cap, can produce various minute, frost-heaved, soil surface features which result in a A66-39558 complex, porous surface structure that causes optxcal darkening. THE ABUNDANCE AND TEMPERATURE OF CO2 IN THE MARTIAN The hypothesis is examined in terms of known properties of the ATMOSPHERE. Martian atmosphere and surface and of the availabilrty of water. Michael J. S. Belton and Donald M. Hunten (Kitt Peak National B. B. Observatory, Tucson, Ariz. ). Astrophysical Journal, vol. 145, Aug. 1966, p. 454-467. 27 refs. Spectrophotometric observations of the R-branch of the weak A66-40486 VI t 2V2 t 3V3 band of C02 at 1.05 g in the spectrum of Mars yleld MARS - NEW ABSORPTION BANDS IN THE SPECTRUM. an atmospheric abundance of 68 * 26 m-atm (STP). Taken together Janine Connes, Pierre Connes (Centre National de la Recherche with the results of Gray's analysis of the strong bands of C02 at Scientdique, Service d'ALronomie, Observatoire de Meudon, 2 I.r, this abundance indicates a su-rface pressure in the range of Meudon, Seine-et-Oise, France), and Lewis D. Kaplan (California 5-13 mb. Individual lines in the R-branch have been resolved up Institute of Technology, Jet Propulsion Laboratory, Pasadena, to J = 28, and their intensity distribution indicates a rotational Calif. ). 9 temperature of 194'K. The head region alone yields a somewhat Science, vol. 153, Aug. 12, 1966, p. 739, 740. higher temperature of 210°K. The observations were also analyzed Note on the finding of new absorption bands in the near-IR with the help of a polytropic model atmosphere. The most satisfac- spectrum of Mars by Fourier spectroscopy. They are tentatively tory fit to the data was found for a maximum air temperature at the identified in part as due to reduced gases in the Martian atmosphere. surface of 270°K and a lapse rate of 5OK km-1. The paper is con- The Mars spectra were obtained mainly to measure absorption by cluded with a brief discussion of the compatibility of the present lines in the 1.6-u CO2 bands to make it possible to estimate the sur- observations with others that are available. (Author) face pressure more precisely. B. B.

36 A66-42668

A66-4 1063 # Discussion of three classes of models for the atmosphere of STABILITY ANALYSIS OF SATURN'S RINGS WITH DIFFERENTIAL Mars which differ in identifying the main ionospheric layer measured ROTATION. by Mariner 4 as being analogous to a terrestrial F2. F1, or E layer. Shm Yabushita (Yale University, Astronomy Dept., Yale Observato- At an altitude of several hundred kilometers, the relative atmospheric ry. New Haven, COM.). mass densities for these models are approximately 1, lo2, and lo4, Royal Astronomical Society, Monthly Notices, vol. 133, no. 3, respectively, and the temperatures are roughly 100. 200, and 1966, p. 247-263. 10 refs. 4000K. Theory and observation are in best agreement for an F2 USAF-supported research. model, for which photodissociation of C02 and diffusive separation A method is presented for calculatmg the potential due to an result in an atomic-oxygen upper atmosphere, with Ot being the arbitrary thm gravitatmg rmg by making use of cylindrical func- principal ion in the isothermal topside of the ionosphere. However, tions. The equilibrium configuration of the rmg is defined in such an F1 model, mth molecular ions in a mixed and warmer upper a way that centrifugal force exactly balances the self-gravitation atmosphere, might result if photodissociation and diffusive separa- of the ring plus the gravitation due to the (spherical) planet. By tion are markedly less than would be expected from analogy with the takmg into account the differential rotation obtained in this manner earth's upper atmosphere. M. M. mathematical analysis of the stability of motion about the equilibrium configuration is carried out by making use of the equations of hydrodynamics. Frequencies of the free oscillations are shown to be A66-418 16 given as eigenvalues of a certain infinite matrut, and the eigenvalue RESOLUTION OF A CO2 "HOT BAND'' IN THE VENUS SPECTRUM. problem is then solved numerically. The upper limit to the mass Hyron Spinrad (California, University, Berkeley Astronomical of a ring which is stable against axisymmetric perturbations 1s Dept., Berkeley, Calif.). given for several model rings. If the density distribution of the Astrophysical Journal, vol. 145, Sept. 1966, p. 943-945. ring is taken as a linear combmation of the zero-order Bessel Study of very weak absorption lines observed on spectrograms functions of the first and second kmd such that the densrty vanishes of Venus in the region XX 8736-8768. These famt lmes are mainly at the mer (r = a) and outer (r = b) boundaries, the limlting mass the rotational fine structure of the excited vibrational transition of C02 designated 010-015 b2 to 5u3 t v2). The weak "hot-band" lines are best visible near X 8760, the strongest lines in the P-branch A66-41181 Charles H. McLellan and E. Brian Pritchard (NASA, Langley Re- DIRECT PHOTOGRAPHIC EVIDENCE OF A RETROGRADE ROTA- search Center, Aero-Physics Div., Mission Analysis Group, Hamp- TION OF VENUS IN FOUR DAYS [MISE EN EVIDENCE DIRECTE, ton, Va.). PAR LA PHOTOGRAPHIE, D'UNE ROTATION RETROGRADE DE VENUS EN 4 JOURS]. Charles Boyer and Pierre GuLrin (Centre National de la Recherche Scientifique, Institut d'bstrophysique, Paris; Toulouse, Universite, A66-42320 # Observatoire du Pic du Midi, Bagn'eres de Bigorre, Hautes-Pyrgnges. OSCILLATIONS OF PLANETARY ATMOSPHERES AS A FUNCTION France 1. OF THE ROTATIONAL SPEED OF THE PLANET. Acadgmie des Sciences (Paris). Comptes Rendus, Sdrie B - G. S. Golitsyn and L. A. Dilai (Akademiia Nauk SSSR, Institut Fiziki Sciences Physiques. vol. 263, no. 3, July 18, 1966, p. 253-255. Atmosfery, Moscow, USSR). In French. (Akademiia Nauk SSSR, Izvestiia, Fizika Atmosfery i Okeana, Results of a study of continuous series of high resolution vol. 2, Mar. 1966, p. 225-235.) photographs of Venus, obtained for the first tlme from the same Academy of Sciences, USSR, Izvestiya,Atmospheric and Oceatuc stahon (the Pic-du-Midi Observatory) several hours running. A Physics, vol. 2, Mar. 1966, p. 137-142. 13 refs. Translation. retrograde rotation of the whole of the cloud formations of the [For abstract see issue 14, pase 2381, Accession no. A66-275341 planet was observed with an angular velocity corresponding to one complete rotation in about four days. This period is noted to be physically incompatible with the period of 240 days obtained by A66-42667 radar. M.F. HIGH RESOLUTION SPECTRA OF PLANETARY ATMOSPHERES. Hyron Spinrad (California, University, Berkeley, Calif. ). A66-41679 IN: UNMANNED EXPLORATION OF THE SOLAR SYSTEM; AMERI- ON THE CIRCULATION OF THE ATMOSPHERES OF JUPITER CAN ASTRONAUTICAL SOCIETY, SYMPOSIUM ON UNMANNED AND SATURN. EXPLORATION OF THE SOLAR SYSTEM, DENVER, COLO.. FEB- R. Hide (Massachusetts Institute of Technology, Dept. of Geology RUARY 8-10, 1965, PROCEEDINGS. and Geophysics, and Dept. of Physics, Cambrldge, Mass.). Edited by G. W. Morgenthaler and R. G. Morra. Planetary and Space Science, vol. 14, Aug. 1966, p. 669-675, 24 Baltimore, American Astronautical Society; North Hollywood, Calif., refs. Western Periodicals Co. (Advances in the Astronautical Sciences. NSF Grant No. G-22390. Volume 19). 1965, p. 187-197. Discussion of the planetary-scale atmospherlc circulations of Some results of recent spectroscopic observations of the physi- Jupiter and Saturn in terms of basic fluid dynamics. Owing to the cal characteristics of planetary atmospheres. The significance of great size of these planets, effects of rotation are even more pro- CO2 lines in the atmospheric spectra of Mercury, Mars, and Venus nounced than in the case of the earth. There is evidence that m the is discussed. The data obtained have contributed to the understand- case of Jupiter hydromagnetic effects may have to be taken into ing of the composition, pressures, and temperatures of the atzno- account. There is direct spectroscopic evidence for the existence of spheres of some of the planets. The observational techniques used methane and ammonia in the atmospheres of Jupiter and Saturn. in the experiments and the understanding of the transfer of radiation The presumption that the main constituents of these atmospheres in these atmospheres are believed to be still rather poor. S. Z. are hydrogen and helium is based on the low mean densities of the two planets, and, in the case of Jupiter, on a measurement of the A66-42668 light variation of a star during an occultation, leading to an esti- THE ATMOSPHERE OF VENUS. mate of the mean molecular weight of the material above the cloud Patrick Thaddeus (NASA, Goddard Space Flight Center, Goddard M. F. level. Institute for Space Studies, New York, N.Y.). IN: UNMANNED EXPLORATION OF THE SOLAR SYSTEM; AMERI- CAN ASTRONAUTICAL SOCIETY, SYMPOSIUM ON UNMANNED A66-41779 EXPLORATION OF THE SOLAR SYSTEM, DENVER, COLO., FEB- ATMOSPHERE OF MARS - MARINER IV MODELS COMPARED. RUARY 8-10> 1965, PROCEEDINGS. Gunnar Fjeldbo, Wencke C. Fjeldbo, andVon R. Eshleman (Stanford Edited by G. W. Morgenthaler and R. G. Morra. University, Center for Radar Astronomy, Stanford, Cald. ). Baltimore, American Astronautical Society; North Hollywood. Calif., Science, vol. 153, Sept. 23, 1966, p. 1518-1523. 25 refs. Western Periodicals Co. (Advances in the Astronautical Sciences. Grants No. NGR-05-020-065; No. NsG-377. Volume 19), 1965, p. 201-212. 25 refs.

37 A66-42680

The observed decline in the microwave brightness temperature A67-11424 # of Venus at frequencies above 30 Gc is most easily interpreted in SYSTEMS CONSIDERATIONS FOR A PLANETARY ENTRY PROBE. terms of pressure-induced absorption in a C02-NZ atmosphere. P. A. Giragosian and M. S. Parker (Raytheon Co., Lexington, L Calculations using recent estimates of the CO2 abundance and labora- Mass. 1. tory measurements of induced absorption in model atmospheres in- International Astronautical Federation, International Astronautical dicate that the ground pressure on Venus may lie in the range of Congress, 17th, Madrid, Spain, Oct. 9-15, 1966, Paper. 8p. 100-200 atm. At such high pressures it is probable that the atmo- Design formulation of a small lightweight probe to define the sphere will have the high opacity in the range from 1-20 I( required atmospheric proportion of Mars from its dynamic response during * for the Greenhouse effect even if the C02 abundance is as low as entry. Studies of various blunt conflgurations indicate that a sphere 0.5%, and water vapor is absent. (Author) is the optimum shape for such a probe. An efficient lightweight decelerator to damp the motions of the vehicle is used to maintain a zero angle of attitude. A radiometer to measure atmospheric constituents, four pressure transducers, a temperature sensor, and a data-handling and communications system for the proposed vehicle are described. The total weight of the proposed atmospheric probe A66-42680 is 25 lb. W.A. E. USE OF ENTRY VEHICLE RESPONSES TO DEFINE THE PROPER- TIES OF THE MARS ATMOSPHERE. Alvin Seiff and David E. Reese, Jr. (NASA, Ames Research Center, Vehicle Environment Div., Moffett Field, Calif. ). IN: UNMANNED EXPLORATION OF THE SOLAR SYSTEM; AMERI- SYMPOSIUM ON UNMANNED CAN ASTRONAUTICAL SOCIETY, A67-11432 * # EXPLORATION OF THE SOLAR SYSTEM, DENVER, COM., FEB- AEROTHERMOSTRUCTURAL DESIGN OF A FLIGHT CAPSULE RUARY 8-10, 1965, PROCEEDINGS. SYSTEM ENTERING LOW DENSITY MARS ATMOSPHERE. Edited by G. W. Morgenthaler and R. G. Morra. H. Hurwicz, 0. L. Zappa, and R. M. Davis (Avco Corp., Space Baltimore, American Astronautical Society; North Hollywood, Calif., Systems Div.. Lowell, Mass.). Western Periodicals Co. (Advances in the Astronautical Sciences. International Astronautical Federation, International Astronautical Volume 19). 1965, p. 419-445. 24 refs. Development of the principles by which the atmospheric proper- Congress, 17th, Madrrd, Spain, Oct. 9-15, 1966, Paper. 25 p. 14 refs. ties of an unknown planetary atmosphere can be deduced from re- Contract No. NAS 1-5224. sponses of a probe vehicle entering the atmosphere. Experiments Discussion of the basic aerodynamic, thermodynamic, and to determine atmospheric density and pressure as functions of al- structural design aspects of a flight capsule entering a low-density titude, and to detect and determine quantities of selected gases in Mars atmosphere from orbit. The effect of change in the atmosphere the atmosphere are examined in detail. Accuracies and experiment is brought out by comparisons with a capsule designed for entry from problem areas are treated. Measurements of altitude profiles of an approach trajectory into a dense atmosphere. br atmospheric density, pressure, and temperature are discussed, The results are tabulated. An aerodynamic retardation system for rare atmospheres and the detection of chemical species in the shock layer by spectrometry is studied. M. F. is concluded to be feasible for a blunt cone entering from orbit. Aerodynamic load reduction permits significant (but not proportional) weight structural saving andlor use of conventional materials. M.M. *

A67-11436 NON-EQUILIBRIUM PROPERTIES OF MARTIAN ENTRY FLOW FIELDS. IAA Stanley Byron and Richard M. Foster (Philco Corp., Aeronutronic Div., Newport Beach, Calif.). International Astronautical Federation, International Astronautical Congress, 17th, Madrid, Spain, Oct. 9-15, 1966, Paper. 14 p. 24 refs. Brief description of the present status of three phases of work for developing a satisfactory model of the nonequilibrium properties of high-temperature COz, Nz, and Ar mixtures. Specifically, the three phases are development of a satisfactory nonequilibrium chemical model, verification of the chemical model by comparing A67-11395 # theoretical results with time-resolved radiation emission measure- MANNED SATELLITE OBSERVATIONS AND PLANETARY RE- ments behind normal shocks, and calculation of flight cases using SEARCH. the chemical model and a suitable flow-field analysis. The results D. Deirmendjian (RAND Corp., Santa Monica, Calif. ). obtained show that the chemical model satisfactorily reproduces Internationzl Astronautical Federation, International Astronautical previously published experimental measurements. In addition, Congress. 17th. Madrid, Spain, Oct. 9-15, 1966, Paper. 12 p. flight calculations show that nonequilibrium and equilibrium radiative 9 refs. heating are comparable with stagnation-point convective heating. Discussion of certain terrestrial observations from a manned M. M. geophysical satellite as training for research on other planets. The experience thus acquired is essential in solving some of the problems of the Venusian atmosphere by means of a properly Y designed fly-by mission. Observations of the natural optical phenomena produced by sunlight falling on the clouds in the atmosphere, A67- 1 1695 especially glories, can provide much information concerning the THE COMPOSITION AND SURFACE PRESSURE OF THE MARTIAN atmosphere itself. We still lack basic reliable data concerning the ATMOSPHERE - RESULTS FROM THE 1965 OPPOSITION. constitution, state, and amount of the atmosphere, and a manned Tobias Owen (Illinois Institute of Technology, Research Institute, IT fly-by mission may be a great help in resolving these uncertainties. Astro Sciences Center, Chicago, Ill. ; Arizona, University, Lunar W.A.E. and Planetary Observatory, Tucson, Ariz.).

38 A67-14088

Astrophysical Journal, vol. 146. Oct. 1966, p. 257-270. 36 refs. A67-12949 * #t Research supported by the Illinois Institute of Technology; Grant LABORATORY MEASUREMENT OF MICROWAVE ABSORPTION No. NRO-46-791. IN MODELS OF THE ATMOSPHERE OF VENUS. ‘0 Observations of the photographc spectrum of Mars obtained at W. Ho, I. A. Kaufman (Columbia University, Columbia Radiation the most recent opposition in March 1965 are presented and dis- Laboratory, New York, N. Y. ), and P. Thaddeus (NASA, Goddard cussed. The absence of any trace of the NO2 absorption at 4480 f Space Flight Center, Goddard Institute for Space Studies, New York, confirms previous upper limits set on the abundance of this gas. N. Y. 1. Observations of the weak Cqbands at 8689 and10.488H lead to a Journal of Geophysical Research, vol. 71, Nov. 1, 1966, p. 5091-5108. * derivation of 65 f 20 m-atm for the abundance of CO2 in the Martian 62 refs. atmosphere. Ths abundance is used with new ohservations of the Grant No. NsG-442; Contract No. DA-28-043-AMC-O0099(E). strong GO2 bands at 1.6 p made by Kuiper to derive a value for the Measurement of coefficients of induced absorption in model surface pressure of 9 mb. The uncertainty in this determinapon atmospheres containing C02, N2, A, and Ne, needed to calculate ranges from 5 to 20 mb, the lower values being considered most the properties of the lower atmosphere of Venus from the radio probable. A discussion of these results in the context of the origin observations on the assumption that the atmosphere is dry and and development of the Martian atmosphere suggests that, with the massive, in the temperature range 240 to 500°K to pressures as exception of water vapor, the present atmospheric composition may high as 130 atm. Since the microwave region lies on the low-frequen- be very similar to that of the primitive, outgassed terrestrial atmo- cy wing of both the translational and rotational spectrum, the micro- sphere. (Author) wave-induced absorption coefficient is proportional to the square of the frequency, and all measurements have been made at one frequency, 9260 Mc. Absorption due to small amounts of water vapor in N2 has also been studied at 9260 Mc, over a comparable pressure range, and over the temperature interval 393 to 473% The absorption coefficient in this case is found to he approximately twice that A67-11769 calculated on the basis of the Van Vleck-Weisskopf theory from all WATER VAPOR IN THE ATMOSPHERE OF VENUS. of the significant microwave and IR transitions of the water molecule. M. J. S. Belton and D. M. Hunten (Kitt Peak National Observatory, An expression for the absorption coefficient for all the atmospheres Tucson, Ariz. ). studied is given. M. F. Astrophysical Journal, vol. 146, Oct. 1966, p. 307, 308. 6 refs. Commentary on water-vapor lines detected in the spectrum of Venus. These lines were Doppler-shifted from the normal wavelengths of 8189.27 and 8193.00 A. The spectra were obtained by photoelectric scanning of the Venus spectrum formed by the 404 spectrograph of the McMath Solar Telescope. The technique used to disentangle the Venus lines from their strong telluric counter- A67-13215 * r) parts are described. W.A.E. ACOUSTIC EXPERIMENT TO DETERMINE THE COMPOSITION OF AN UNKNOWN PLANETARY ATMOSPHERE. R. A. Hanel and M. G. Strange (NASA, Goddard Space Flight Center, Greenbelt, Md. ). Acoustical Society of America, Journal, vol. 40, Oct. 1966, p. 896-905. 15 refs. * A67-11774 Measurement of the speed of sound and the acoustic impedance, WATER VAPOR ON VENUS - A CONFIRMATION. combined with a knowledge of ambient pressure and temperature, Hyron Spinrad and Stephen J. Shawl (California, University, Dept. of provide sufficient data for determrnrng the relative abundance of Astronomy, Berkeley, Calif. ). constituents rn a mlXture of nitrogen, argon, and carbon dioxide. Astrophysical Journal, vol. 146, Oct. 1966, p. 328, 329. 7 refs. Sound absorption and dispersion peld additional information for Navy-supported research. checkmg the consistency of the results. An rnstrument has been Discussion of several Doppler-displaced lines of water vapor developed to measure the acoustic properties of an unknown gas originating in the atmosphere of Venus which were observed on mixture. Laboratory results demonstrate the feasibility of deter- three coud; spectrograms. The Cytherean absorption lines were minrng the gas composition withrn a few percent. The technique quite weak, and a dispersion of 1.9 Hlmm was required to detect of velocity measurement by use of phase comparison over several them. The study is considered to confirm the detection of water on wavelengths is quite sensitive and may be useful rn other applica-(Author) Venus by balloon by Bottema et al. and recent ground-based photo- tions. electric observations by Belton and Hunten. F. R. L.

A67-14088 * # RADIATION EQUILIBRIA PERTINENT TO PLANETARY ATMO- SPHERES. P. Harteck, R. R. Reeves, Jr., B. A. Thompson, andR. W. A67-12406 # Waldron (Rensselaer Polytechnic Institute, Dept. of Chemistry, PERTURBATION TO TEMPERATURE SOUNDINGS BY BOUNDARIES Troy, N.Y.). AND ATTENUATING MEDIA. Ralph Zirkind (3rooklyn. Polytechnic Institute, Brooklyn, N. Y. 1. International Astronautical Federation, International Astronautical ConEress, 17th, Madrid, Spain, Oct. 9-15, 1966. 10 p. 5 refs. NASA-supported research. The radiometric sounding of planetary atmospheres by remote Investigation of radiation equilibria in the UV by means of a sensing techniques to obtain temperature profile data may be affected bromine lamp which gives 1017 quantalsec at 1582 and 1633 A where by boundary conditions and attenuating media. An attempt is made the latter is the most intense Br line. Since the absorption coeffi- .. .. to consider these influences as a function of wavelength. The resultr cients of 02. CO2, and 03and other gases are substantial at these indicate that at the short infrared wavelengths, surface radiation wavelengths, radiation equilibria can be obtained in times between plays a minor role whereas at the longer wavelengths it may he se- 1 hr and a few days, depending on conditions, in a 500-ml sample rious. The effect of clouds is important in the window regions of volume. Since the temperature can also be varied, the conditions the spectrum where significant portions of the total radiation are prevailing in any region of an atmosphere can be simulated. The ,s emitted. There is proposed (1) a generalized scheme for analysis irradiation of 02, CO, GOz. N2. and mixtures of these gases is of planetary atmospheres and (2) an inversion process that would discussed, together with the effects of trace amounts of water vapor employ a fictitious absorption coefficient. (Author) on the equilibria. M. M.

39 A67-14309

A67-14309 * C. A. Barth (Colorado, University. Dept. of Astro-Geophysics, and HIGH-DISPERSION SPECTROSCOPIC OBSERVATIONS OF MARS. I. Physics and Astrophysics Dept., Laboratory for Atmospheric and Hyron Spinrad, L. P. Giver (California. University, Astronomical Space Physics, Boulder, Colo. ). c Dept., Berkeley, Calif. ), Ronald A. Schorn (California Institute IN: THE MIDDLE ULTRAVIOLET: ITS SCIENCE AND TECHNOL- of Technology, Jet Propulsion Laboratory, Space Science Div., OGY. Pasadena, Calif. ), Roger Moore (RAND Gorp., Santa Monica, Calif.). Edited by A. E. S. Green. and Harlan J. Smith (Texas, University, McDonald Observatory, Fort New York, John Wiley and Sons, Inc., 1966, p. 177-218. 35 refs. Davis, Tex. ). Consideration of the phenomena that occur when a planetary 4L Astrophysical Journal, vol. 146, Nov. 1966, p. 331-338. 15 refs. atmosphere is subjected to radiation from the sun. Such radiation NASA-supported research, Grant No. Nonr(G)-00006-66. directly or indirectly subjects the upper atmosphere to charged From high-dispersion infrared McDonald and Lick Observa- particle bombardment at large geomagnetic latitudes. The phenomena tories' spectrograms of Mars we have determined a CO2 abundance producing dayglow include resonance reradiation, fluorescence, photo- of 90 f 27 (estimated error) m-atm (STP) at 200°K, chosen as a electron excitation, and chemical and ionlc reactions. The spectral representative lower-atmosphere temperature. We used the weak emissions of the aurora are produced by charged particle bombard- 5U3 C02 lines near X 8700 A. An abundance of 90 m-atm of C02 ment while the aurora itself is controlled in some way by the geo- gives a surface partial pressure of 6.6 mb. The observation and magnetic fleld. Atoms that may play a role in producing spectra In reductions are discussed. The result 1s compared to the Mariner 4 the upper atmospheres of Venus, the earth, and Mars are hydrogen, occultation data which yield P, = 5 or 6 mb if the temperature of oxygen, nitrogen, argon, and carbon. Molecules that may be impor- the lower Martian atmosphere is BOOK. The difference in surface tant in producing planetary emission spectra are nitrogen, oxygen, pressure is not substantial; the occultation results coupled with our nitric oxide, carbon monoxlde, the hydroxyl radical, the cyanogen C02 abundance suggest an almost pure C02 atmosphere for Mars. radical, and the molecular ions of nitrogen, oxygen, nitric oxide, (Author) and carbon monoxide. Planetary molecular spectra are calculated, and UV spectra of the earth are considered. F:R. L.

A67-14310 ADISCUSSION OF THE DEEP CIRCULATION OF THE ATMO- SPHERE OF VENUS. A67-14952 * * Richard M. Goody (Kitt Peak National Observatory, Tucson, Arie. ) SOME COMMENTS ON THE VENUS TEMPERATURE. and Allan R. Robinson (Harvard University, Cambridge, Mass. ). D. C. Applebaum, P. Harteck, R. R. Reeves, Jr., and B. A. Astrophysical Journal, v01. 146, Nov. 1966, p. 339-355. 19 refs. Thompson (Rensselaer Polytechnic Institute, Dept. of Chemistry, NSF Grant No. G-24903. Tioy, N.Y.). Examination of a model of the Venusiln atmosphere which 1s Journal of Geophysical Research, vol. 71, Dec. 1, 1966, p. 5541- completely opaque to both solar and planetary radiatlon, but whlch 5545. 29 refs. is m motion because of presumed differential heating between sub- NASA-supported research. solar and antisolar points, to determine whether deep penetratlon of The observed micronave emission from Venus has been solar radiation is the only possible mechanism for maintenance of widely attributed to a high surface temperature for the planet. A It 1s temperatures of -600OK at the base of the Venus cloud layer lack of realistic models to account for such a high temperature has n' argued that the geometry of the system favors moderate vertical led to a search for alternative interpretations for the emission. The mlxing coefficients (-lo4 cm21sec) and that the inflow of solar paper describes experiments in which anomalous signals have been energy is large enough to maintam an essentlally nonlinear boundary observed in the X-band region from glen discharges through C02 and The less probable case of very large layer near the cloud tops. S02. Although this type of emission may not necessarily be the turbulent coeffxlents is also consldered, and It 1s shown that the source of the micro\vave emission from Venus, the fact that it occurs interior will remain adiabatic, although the nature of the flow wlll points out the need for caution in basing conclusions about the surface differ. B. B. temperature on microwave observations. (Author)

A67-14327 A67-15557 AN IDENTIFICATION OF THE 6800-A METHANE BAND IN THE THE SPECTRA OF JUPITER AND SATURN IN THE 1.0-2.5 p SPECTRUM OF URANUS AND A DETERMINATION OF ATMO- REGION. SPHERIC TEMPERATURE. V. I. Moroz (Moskovskii Gosudarstvennyi Universltet, Astronomi- Tobias Owen (Illinois Institute of Technology, Research Institute, cheskii Jnstitut, Moscow, USSR). Chicago, Ill., Kitt Peak National Observatory, Tucson, Ariz. ). (Astronomicheskii Zhurnal, vol. 43, May-June 1966, p. 579-592. ) Astro h sical Journal, vol. 146, Nov. 1966, p. 611-613. 7 refs. Soviet Astronomy, vol. 10, Nov. -Dec. 1966, p. 457-468. 41 refs. DPesIription of the results of the identification of the 6800-b Translation. methane band in the spectrum of Uranus for the determination of [For abstract see issue 20, page 3647, Accesslon no. A66-370351 this planet's atmospheric temperature. The mean values of the wavelengths of the methane lines measured are tabulated. The relative intensities of the R-branch lines were examined as a clue to the mean temperature of the vlsible atmosphere of Uranus. The best estimate obtained on the available material was 60 f 15OK. This temperature is very close to the maximum subsolar temperature to be expected if the planet is In simple equilibrium wlth the A67-16029 # incoming solar radiation (67OK), a very different situation from VENUS - A HOT PLANET? [DIE VENUS - EIN HEISSER PLANET?]. ~ that of Jupiter. M.M. Alexander Lebedmski (Akademiia Nauk SSSR, Moscow, USSR) and W sewolod Wachnin. Weltraumfahrt Raketentechnik, vol. 17, 4th Quarter, 1966, p. 138, 139. In German. Discussion of a hypothesis according to which "global breezes" in the Venus atmosphere - which are characterized by high velocities A67-14699 and low vorticity - create conditions in which glow discharges of low THE ULTRAVIOLET SPECTROSCOPY OF PLANETS. luminous intensity can develop. Thzs being tbe case, the surface

40 A67-18311 temperature of Venus may be as little as 50 to 6OoC, while the in- evaporation if appropriate conditions are satisfied. The rates of crease in the equivalent temperature of noise radiation, caused by escape as a function of the amount of a model atmosphere under the glow discharges, can amount to 200 to 250OC. V.P. conditions of the earth and of Mars are tabulated. It is noted that the equihbnum amounts of the earth and Mars are on the same order of magnitude as the amount of the actual atmospheres of these planets. M.F.

A67- 16298 RADAR OBSERVATIONS OF VENUS AT 3.8-CM WAVELENGTH. J. V. Evans, R. P. Ingalls, L. P. Ranvllle, and R. R. Silva A67-18287 * ## (Massachusetts Institute of Technology, Lincoln Laboratory, DEFINITION OF SCIENCE SUBSYSTEMS FOR JUPITER FLYBY Lexington, Mass. ). MISSIONS. Astronomical Journal, vol. 71, Nov. 1966, p. 902-915. 32 refs. B. A. Sodek and J. C. Redmond (General Dynamics Corp., Applied During the early part of 1966 the Haystack radar ( A= 3.8 cm) Research Laboratory, Fort Worth, Tex. ). was employed to observe the planet Venus. The radar cross section American Instltute of Aeronautics and Astronautics, Aerospace observed at this wavelength was only about one-tenth as much as has Sciences Meetxng, 5th, New York, N.Y., Jan. 23-26, 1967. Paper been reported at wavelengths of 12 cm or longer. Our measurements -=67-120.-. 17. D. 29 refs. support the low value for the cross section reported by Karp et al. Members. $0.75, nonmembers, $1.50. (1964). The echo spectrum is found to be comparatively narrow, sug- Contract No. JPL-951285. gesting the solid surface as the reflecting agent. No echo power can Summary of the present state of knowledge about Jupiter, fol- be observed outside the frequency hmits expected on the basis of the lowed by a description of those features to be studied in unmanned known rotation rate and the center Doppler shift measured using a flyby missions. A general discussion of scientlfic experiments and separate A e 23 cm radar. if any energy is reflected by the atmo- instruments that can gather pertinent data, an evaluation of the rel- sphere it appears to be only a small portlon of the total. Confirmation ative priorlty of the information returned, and an indication of some that the surface is the scattering agent has been provided by near special consideratlons in their application are presented. It 1s neces- simultaneous rangmg experiments at two frequencies, which showed sary to define realistic approximations of the science payloads at that the echo delay times agreed to 5 psec - ~.e.*well within the ex- the present time, both for determining what information a Jupiter perimental accuracy. The depolarized component of the echoes was mission can provide and to examine the interface areas between the observed and found to be of the order of 14 db weaker than the ex- acquisition of scientific data and the other considerations involved pected component. An analysis of the scattering law for the planet in planrung the mission. These considerations include such items has been made, and when compared with the law observed at longer as spacecraft trajectory and orlentatlon, both m interplanetary space wavelengths indicates that about 4-6 db two-way vertical absorptron and at Jupiter; spacecraft design, including constraints on the vehicle occurs in the atmosphere of Venus. Variations in the observed cross configuratlon, weight and size, and data handling, including storage section mth time (by as much as a factor of 2) support the view that and transmission. (Author) atmospheric attenuation IS responsible at least in part for the low cross section observed. A comparison of the positions of anom- alously reflecting regions observed in these observations with the positionb reported by Carpenter (1966) during the 1964 inferior A67-18310 *# conjunction permits the Venus rotation period to be established a8 A RADIO OCCULTATION EXPERIMENT TO PROBE THE ATMO- 244 days plus or minus a few days. (Author) SPHERE OF VENUS. Arvydas Kliore, Dennis A. Tito, Dan L. Cam, and Gerald S. Levy (California Institute of Technology, Jet Propulsion Laboratory, Pasadena. Calif. ). American Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 5th, New York, N. Y., Jan. 23-26, 1967, A67- 16407 Paper 67-118. 13 p. 29 refs. THE PRESENCE OF ICE IN THE VENUS ATMOSPHERE AS Members. 50.75: nonmembers, 51.50. INFERRED FROM A HALO EFFECT. This paper describes an experiment planned for the encounter Brian T. O'Leary. of the Mariner Venus 1967 space probe. Changes in the frequency, Astrophysical Journal, vol. 146, Dec. 1966, p. 754-766. 18 refs. phase and power of the S-band radio signal introduced by its passage Discusslon of photometry of the integrated light of Venus In through the atmosphere of Venus, will be observed, and the analysis blue, violet, and red between phase angles of 153 and 165O before of these changes will lead to a profile of refractwe index. These and after the inferior conjunction of 1966. These results, combined data, together with the results of other measurements, are expected mth a study of the photometrlc, colorlmetrlc, and polarlmetrlc to yield profiles of pressure and density in the lower atmosphere, characteristics of Venus as it passes through these phase angles, and provide information on its composition. The philosophy underlying suggest a halo effect of brightness dispersions of about 0.05 mag- the design of the trajectory and high-gain antenna of the probe was nitude brighter than the background phase-curve at predicted halo based on the maximization of the information returned by thls exper- maximum and about 0.04 magnitude fainter than the background iment under the adverse effects of defocusing atte-idation and refrac- phase-curve at predicted halo minimum. The findings tentatively tive bending expected in the dense atmosphere of Venus. Finally, indicate confirmation of H20 in the Venusian atmosphere, and a the expected frequency, phase and signal strength effects computed temperature and pressure environment at the cloud tops conduclve for several models of the atmosphere of Venus are presented. to the formation of ice. B. B. (Author)

A67-18311 ** A67-18052 ## A METHOD FOR STUDYING PLANETARY ATMOSPHERES EMPLOY- A POSSIBLE FACTOR REGULATING THE AMOUNT OF THE AT- ING THE DUAL FLYBY MODE. MOSPHERE ON THE EARTH AND MARS. J. Michael Coogan (NASA, Office of Advanced Research and Tech- Makoto Komabayasl (Nagoya Universlty, Water Research Labora- nology, Mission Analysis Div., Moffett Field. Calif.). tory, Nagoya, Japan). American Institute of Aeronautics and Astronautics, Aerospace MeteoroloQical Society of Japan, Journal, vol. 44, Oct. 1966, Sciences Meeting, 5th, New York, N.Y., Jan. 23-26, 1967, p. 297-300. 10 refs. Paper 67-121. 11 p. 27 refs. Examination of a possible mechanism which can regulate the Members, $0.75; nonmembers, $1.50. total amount of a planetary atmosphere that is transparent for The major factors bearing on the theoretical and technological visible and IR radiation. It has been suspected that molecules of feasibihties of a split-trajectory dual planetary flyby mode and Its the atmospheric gas can escape from the top of the atmosphere application to absorption spectroscopy of a planetary atmosphere (exosphere) into the planetary space by either thermal or nonthermal have been examined. In this mode, a piggyback capsule IS launched

41 A67- 18429

from a conventional planetary flyby vehcle with proper timing and A67-18508 * thrust so that the capsule also flys by the planet, but on the opposite DYNAMICS OF A GUIDED PROPULSIVE SOFT LANDING PRECEDED side. If one of the flyby platforms carries a suitable light source, BY A MARTIAN ATMOSPHERIC DECELERATION. in particular a solar mirror, and the other carries a compatible Peter J. Moonan (Grumman Aircraft Engineering Gorp., Bethpage. spectrophotometer, absorption-almude profile measurements can N.Y.). be made at useful wavelengths as the line of sight between them American Institute of Aeronautics and Astronautics, Aerospace Sci- sweeps through the planetary atmosphere. From these profiles the ences Meeting, 5th, New York, N.Y., Jan. 23-26, 1967, Paper absolute density vs altitude of the absorbing conshtuents can be de- h7-170- - . I)-&-. n termined with certain qualifications. For a Mars-like 10 mbar GO2 Members, $0.79; nonmembers. $1.50. atmosphere, simulated typical measurement errors resulted in A guided propulsive solution to the problem of removing the last errors of less than 20% m the absolute density vs altitude over a several thousand feet per second of velocity from a Mars soft landing wide altitude range. These preliminary results justify further vehicle is presented. The propulsive phase of the trajectory starts study which should include the spectroscopy aspects and comparison at some point on the entry trajectory traversed by an unguided with a planetary atmosphere absorption experiment in which a star symmetrical blunt body. A gravity turn is is used as the light source and only a single flyby platform is em- ling attitude so that the the thrust vector is ployed. (Author) opposite to the velocity vector. Mass flow so that velocity is proportional to slant range to the planet surface as measured along the thrust axis. The dynamics of the trajectory are such that path angle approaches -900 and the thrust axis approaches a vertical attltude as the trajectory progresses. A67-18429 Guidance and engine ignition equations are presented and a stability * criterion for the guided soft landing trajectory is developed. THE ATOMIC AND MOLECULAR PROCESSES IN THE. UPPER The capability the system to accept large variations in the preceding ATMOSPHERES OF PLANETS. of entry trajectory resulting from atmospheric uncertainties is dem- Mlklo Shimizu (Ochanomizu Women's University, Dept. of Physics, onstrated by stimulated trajectory data. (Author) Tokyo, Japan). Report of Ionosphere and Space Research in Japan, vol. 20, no. 3, 1966, p. 271-288. 58 refs. Theoretical investigation of the atomic and molecular processes in the upper atmospherea of Venus, Mars, and Jupiter by using the atmospheric models recently proposed by JPL. The amount of A67-18645 CO molecules in the upper atmospheres Venus and Mars may be of FROST PHENOMENA ON MARS. about 2 and 0.2 cm STP respectively, provided photochemical Duwayne M. Anderson, Edward S. Gaffney, and Philip F. Low On both Venus and Mars, the effect of equilibrium takes place. (U.S. Army, Cold Regions Research and Engineerlng Laboratory, diffusion should be taken into account to determine the distribution Hanover, N.H. ). of 02 molecules, and the effect of the solar corpuscular stream on Science, vol. 155, Jan. 20, 1967, p. 319-322. 12 refs. the upper atmospheres may be pronounced because of the lack of The hypothesis that the Martian wave of darkening might be a magnetism. On Jupiter, the molecular hydrogen and the atomic frost-heaving phenomenon has been examined. Consideration of the helium are first ionized and then decomposed to produce the atomic water-vapor sorption characteristics of a silicate mineral surface hydrogen, the ionization of which may be responsible for the forma- at temperatures below freezing leads to the conclusion that, without tion of a dense Jovian ionosphere. The maximum electron density strongly deliquescent salts to attract and retain liquid water in the was found to be 1. 5 x 107/cm3, and the total amount of H atoms in the Martian soil, frost-heaving phenomena are not to be expected on Jovian upper atmosphere may be 0. 01 cm STP. A qualitative picture Mars. On the other hand frost-heaving phenomena involving the of the solar-planetary relationships based on the results of these freezing and thawing ammonia may be common in the soils of calculations 1s presented. M. F. of Jupiter. (Author)

A67-18454 *# A67-18849 * ## RADIO OCCULTATION MEASUREMENTS OF PLANETARY ATMO- LAMINAR CONVECTIVE HEATING AND ABLATION IN THE MARS SPHERES AND PLANETARY SURFACE TOPOGRAPHY. ATMOSPHERE. G. Fjeldbo (Stanford Center for Radar Astronomy, Stanford, Calif.). Joseph G. Marvin and Ronald B. Pope (NASA, Ames Research American Institute of Aeronautics and Astronautics, Aerospace Center, Moffett Field, Calif.). Sciences Meeting, 5th, New York, N.Y., Jan. 23-26. 1967, Paper (AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAUTICS, 67-119. 6p. 14 refs. AND AMERICAN ASTRONAUTICAL SOCLETY, STEPPING STONES Members, $0.75, nonmembers, $1.50. TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, 1966, Grant No. NsG-377. TECHNICAL PAPERS, p. 370-382.) The paper describes radio experiments for the study of planetary AIAA Journal, vol. 5, Feb. 1967, p. 240-248. 37 refs. atmospheres and planetary surface topography. They require mea- [For abstract see issue 13, page 2208, Accession no. A66-252741 surements of perturbatlmns to the amplitude and frequency on the radio links between a spacecraft and the earth. The spacecraft must have a trajectory that mvolves occultation of the spacecraft by the planet as seen from the earth. The changes imposed on the radio links by the planetary atmosphere are used to determlne the re- A67-18997 fractivity profile in altitude of the nondispersive {neutral)and dis- STRUCTURES OF THE TERRESTRIAL AND EXTRATERRESTRIAL persive (ionized) regions of the atmosphere. For moderately dense ATMOSPHERES. atmospheres, the radio propagation path can penetrate the atmo- Israel Katz (Northeastern University, Boston, Mass. 1. sphere tangentially all the way down to the limb, and the time of (New York Academy of Sciences, Conference on Planetolo and signal extmction and commencement can be utllized to determine %ace Mission Planning, New York, N. Y., Nov. 3, 4, 196;: Paper.) the radii of the occultmg surface features. This was the case on New York Academy of Sciences, Annals, vol. 140, Dec. 16, 1966, Mars and is also expected to apply to Mercury. The atmospheres v. 49-60. of Venus and Jupiter, on the other hand, may be too dense to permit Examination of factors - such as grawtation, solar ramation, tangential penetration all the way dovto the surface. It may, there- planetary rotation, emissivity, tidal effects, and magnetic fields - fore, be necessary to utllize the radio energy scattered from the sur- that affect atmospheric structures. First-order through eleventh- face in order to probe the lowest portion of these atmospheres. order structural features of the earth's atmosphere are described. (Author) D.H.

42 A67-2 1 2 1 3

A67-19057 * Approximate equations are used in discussing the entry trajectory ORGANIC MOLECULES AND THE COLORATION OF JUPITER. dynamics and in presenting a few of the more important entry trajec- C. E. Sagan (Harvard University, Smithsonian Institution, tory problems in future space missions. The entry of unmanned Smithsonian Astrophysical Observatory, Cambridge, Mass. ), ballistic probes into the atmosphere of Mars is considered. and a E. E. Lippincott (Maryland, University. Dept. of Chemistry, soft landing on the surface of Mars is shown to be marginal for the College Park, Md.), M. 0. Dayhoff, and R. V. Eck (National low surface pressures that are currently estimated. For ballistic Biomedical Research Foundation, Silver Spring, Md. ), entries at Venus and Jupiter, high aerodynamic deceleration forces Nature, vol. 213, Jan. 21, 1967, p. 273, 274. 7 refs. are to be expected. For the entry of manned lifting vehicles into NASA-supported research. planetary atmospheres, it is shown that a "capture" maneuver must Discussion of the simulation of the Jovlan atmosphere in which be performed to keep the vehicle from exceeding aerodynamic load a mixture of hydrogen, methane, and ammonia was supplied with limits or from skipping back out of the atmosphere. M. F. energy from a corona discharge. Such simple organic molecules were produced as hydrogen cyanide, methyl cyanide. acetylene, ethylene, and ethane. Their iliteraction products were prezicted to be brlghtly colored. With high local temperatures and quenching R67-20931 * there 14 thought to be a wde range of pressures and temperatures ANISOTROPIC NONCONSERVATIVE SCATTERING AND THE in which substituted benzene rings and polycyclic aromatic com- CLOUDS OF VENUS. pounds are formed in significant yleld. B. B. Carl Sagan (Harvard University; Smithsonian Institution, Smithsonian Astrophysical Observatory, Cambridge, Mass. ) and James B. Pollack (Smithsonian Institution, Smithsonian Astrophysical Obser - R67-19380 # vatory; Harvard University, Harvard College Observatory, Cam- THEORETICAL INVESTIGATION OF ENTRY VEHICLE STABILITY bridge, Mass. ). IN THE MARS ATMOSPHERE. Journal of Geophvsical Research, vol. 72, Jan. 15, 1967, p. 469-477. C. L. Kyriss and H. RE (General Electric Co., Missile and Space 20 refs. Div., Re-Entry Systems Dept., Theoretical Aerodynamlcs Div., Grant No. NGR-09-015-023. Philadelphia, Pa. ). Expressions have been obtained in a modified Schuster- (AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAUTICS, Schwarzschild approximation describing the monochromatic trans- AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING STONES missivity, reflectivity, and absorptivity of a cloud layer charac- TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, 1966, terized by an arbitrary single-scattering albedo and anisotropic TECHNICAL PAPERS, p. 383-390.) phase function. These analytic results for fluxes are accurate to Journal of Spacecraft and Rockets, vol. 4, Feb. 1967, p. 272-275. within a few percent when compared with a range of exact solutions 9 refs. for limiting cases, including the case of strong forward scattering [For abstract see issue 13, page 2191, Accession no. A66-252751 and large optical depth. The application of this formalism, combined with exact solutions of the Mie theory problem, to the observed visual and near-IR reflectivity of Venus permits the determination A67-20022 * of a number of properties of the Venus cloud layer, Strong's iden- VENUS - ATMOSPHERIC EVOLUTION. tification of ice as the principal constituent of the clouds is con- Margaret 0. Dayhoff, Richard V. Eck (National Biological Re- firmed. Liquid water, hydrocarbons, and dust are found to be un- search Foundatlon, Silver Spring, Md.), Ellis R. Lippincott likely principal constituents of the cloud tops. In addition, the

(Maryland, University, Dept. of Chemistry, College Park, Md. )# mean radius of cloud particles lies between 7.5 and 10 p. and the and Carl Sagan (Harvard University; Smithsonlan Institutlon, interaction optical depth of the layer is between 18 and 43 p . Smithsonian Astrophyslcal Observatory, Cambridge, Mass. ). Clouds having these properties allow a sizable fraction of the in- Science, vol. 155, Feb. 3, 1967, p. 556-558. 29 refs. cident sunlight to penetrate to the surface but are extremely opaque Grants No. NGR-21-003-002; No. NGR-21-002-059, No. NGR- to radiation thermally produced by the planet. (Author) 09-015-023. Computation of the thermodynamlc equilibrium composition of the atmosphere of Venus from the atomic composition deduced spectroscopically. It is found that there can be no free carbon, bydro- R67-21155 * carbons, formaldehyde, or any other organic molecule present in ON ENTERING AN ALIEN ATMOSPHERE. more than trace amounts. The original atomic composition of the Alvin Seiff (NASA, Ames Research Center, Vehicle Environment atmosphere must have included much larger quantities of hydrogen Div., Moffett Field, Calif.). and a carbonloxygen ratio Q 0.5. The present atomic proportions New Scientist, vol. 32, Dec. 29, 1966, p. 730-732. of the atmosphere Venus are unique that an evolutlonary mecha- of so Outline of the main problems associated with entry into the Water, nism involvsng two independent processes seems necessary. atmospheres of other planets. Because knowledge of planetary atmo- originally present in large quantities, has been photodissociated in spheres is incomplete, it is difficult to design for heating, stressing, the upper atmosphere, and the resulting atomic hydrogen has been and landing conditions of the vehicle. Furthermore, the velocity of lost in space. The resulhng excess oxygen has been very effectively entry is in some cases far above that experienced in bringing vehicles bound to the surface materials. M.F. back to earth - and this requires an extension of trihnology. For Mars and Mercury, low atmospheric densities make it difficult to slow the vehicle for a landing. F. R. L. A67-20623 * FLIGHT DYNAMICS OF PLANETARY ENTRY. Rodney 6. Wlngrove (NASA, Ames Research Center, Moffett Field, A67-21213 Calif. ). COMPARISONS OF LABORATORY AND PLANETARY SPECTRA. IV. IN: RECENT DEVELOPMENTS IN SPACE FLIGHT MECHANICS; Tobias Owen (IIT Research Institute, Chlcago, 111. , Arizona, Umver- AMERICAN ASSOCIATION FOR THE ADVANCEMENT OF SCLENCE sity, Lunar and Planetary Laboratory, Tucson, Ariz. 1. AND AMERICAN ASTRONAUTICAL SOCIETY, SPECIAL ASTRO- Icarus, vol. 6, Jan. 1967, p. 108-113. 10 refs. NAUTICS SYMPOSIUM, BERKELEY, CALIF.. DECEMBER 29, Contract No. NRO-46-791. 1965, PROCEEDINGS. Discussion of spectra of Uranus which have revealed several Symposium sponsored by the Space Flight Mechanics Committee of new absorptions in addition to the five unidentified features near the American Astronautical Society. 7500 A previously discovered by Kuiper in the spectra of Uranus Edited by P. B. Richards. and Neptune. Laboratory spectra obtained with very long optical Tarsana, Cald., American Astronautical Society (AAS Science and paths indicate that all these planetary absorptions are caused by Technology Series. Volume 9). 1966, p, 225-268. 49 refs. * methane. This result suggests that the amount of methane in the Review of both ballistic and lifting vehicle entries into the atmospheres of Uranus and Neptune 3s greater than presently planetary atmospheres of Mars, the earth, Venus, and Jupiter. accepted estimates. F. R. L.

43 A67-21215

1\67-21 215 or four agar disks 10 mm in diameter were transferred to Petri THE RELATIONSHIP BETWEEN TERRESTRIAL AND JOVIAN dishes containing a sterilized soil mix. In those species of fungi

ATMOSPHERIC CIRCULATIONS LSUR LA PARENTE DES CIRCULA- that survlved the exposure to diurnal temperature extremes but did 'I TIONS ATMOSPHERIQUES TERRESTRE ET JOVIENNE]; not grow, growth on the agar plug may have occurred but was so F. Link (eeskoslovenski Akademie Vid, Astronomickq Ustav, limited that it was not detected. Data indicated, however, that Ondiejov, Czechoslovakia). certain fungi were able to survive and produce limited mycelial -Icarus, vol. 6, Jan. 1967, p. 129-131. 5 refs. In French. growth when exposed to simulated Martian diurnal temperature ex- Comparison of terrestrial and Jovian atmospheric clrculations tremes. Although most of the hyphae and spores were probably a by study of the motion of the red spot of Jupiter between 1831 and killed after the first few cycles, resistant portions apparently suc- 1940, and of the curve of the discovery of comets, which is affected ceeded m gromng and adapting to this temperature regime. M. M. by night cloudiness. Simultaneous variations in the two circulations have been observed. It 1s considered that the common cause must be sought in solar activity. F. R. L. A67-22016 * MERCURY - NEW OBSERVATIONS OF THE INFRARED BANDS OF CARBON DIOXIDE. A67-21218 Alan B. Bmder and Dale P. Cruikshank (Arizona, University. Lunar ON THE ABUNDANCE OF ETHANE IN THE ATMOSPHERES OF and Planetary Laboratory and Dept. of Geology, Tucson, Ariz.). JUPITER AND SATURN. Science, vol. 155, Mar. 3, 1967, p. 1135. Tobias Owen (IIT Research Institute, Chicago, Ill. ). Grant No. NsG-161-61. Icarus, vol. 6, Jan. 1967, p. 138-140. 5 refs. Application of a 61-111. reflector and of an IR spectrometer to Reinvestigation of observational evidence for the existence of the study of the 1.6-p bands of CO2 in the spectrum of Mercury on Results were ethane in the atmospheres of Jupiter and Saturn. Aug. 26, 1966. From the observations made, the equivalent widths largely negative, and it is concluded that the IR observatlons are of the 1.57- and 1.61-p bands were foundto be 12.5 il.9 and 10.0 .f: consistent m revealing no trace of the presence of ethane in the 2.3 i,respectively, while for the solar comparisons the equivalent atmospheres of either planet. The upper lunit IS still rather crude widthsare12.4+ 0.7and10.5i0.8%. Thus, withmtheerror of compared wlth amounts whlch might be expected to be present as the observations, there is no evidence of a carbon dioxide atmo- F. R. a result of nonequilibrium reactions. L. sphere on Mercury. M.F.

A67-21250 A67-22235 HIGH-DISPERSION SPECTROSCOPIC OBSERVATIONS OF MARS. II. A DETERMINATION OF THE MARTIAN CO2 ABUNDANCE. Ronald A. Schorn (California Institute of Technology, Jet Propulsion Edwin S. Barker (Texas, University, Dept. of Astronomy, Austin, Laboratory, Space Sciences Div., Pasadena, Calif. ), Hyron Spinrad, Tex. ). Lawrence P. Giver (California, University, Dept. of Astronomy, L Astrophysical Journal, vol. 147, Jan. 1967, p. 379-381. Berkeley, Calif. ), Roger C. Moore (RAND Corp., Santa Monica, Account of a completely independent reduction of 1965 spectro- Calif. )*andHarlan J. Smith (Texas, Universlty, McDonald Observa- scopic data on the C02 abundance and surface pressure of Mars tory, Fort Davis, Tex. ). performed because of the partially subjective element which must Astrophysical Journal, vol. 147, Feb. 1967, p. 743-752. 17 refs. enter into the spectroscopic methods, if only from the estimation NASA-supported research; Grant No. Nonr (G)-00006-66; Contract &r of the continuum. The reductions were made on the set of plates No. AF 49(638)-1700. by Spinrad et al. The abundance reductions. using reflected Nineteen high-dispersion spectrograms of Mars taken at Fraunhofer lines to calibrate the tracmgs, were the primary McDonald and Lick Observatories during the 1964-1965 apparltion purpose of this investigation. The pressure calculations depend have been examined for Doppler-shifted rotational lines of H20 on the methods and data given by Kaplan, Munch, and Spinrad and - near h8200. The presence of H20 in the atmosphere of Mars appears 0- and 1.6-p bands, respectively, Owen and Kuiper for the saturated 2. to be confirmed, but indications are that its concentration varies These calculations contain the revision pf the self-broadening with time and location on the planet. Typical amounts of H20 are correction to the effective surface pressure that was indicated by of the order of 10-20 p preclpitable water vapor. The spectroscoplc Spinrad et al. Sources of error and causes of the discrepancies results are compared with photographic patrol studies during this found are examined. M. M. apparition. The amount of water in the vapor phase seems to depend upon the size of the Martian polar cap, Implying a physlcal connectior between the two. (Author) A67-21372 * A NOTE ON THE POSSIBLE CONTRIBUTION OF DIELECTRIC RELAXATION IN GASES TO THE MICROWAVE OPACITY OF THE CYTHEREAN ATMOSPHERE. 867-22236 * Lothar Frenkel (NASA, Electronics Research Center, Cambridge, THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES. Mass. ). Ellis R. Lippincott (Maryland, University, Dept. of Chemlstry, Planetary and Space Science, vol. 15, Jan. 1967, p. 204, 205. College Park, Md. ), Richard V. Eck, Margaret 0. Dayhoff (National 5 refs. Biomedical Research Foundation, Silver Sprmg, Md. )> and Carl Study attempting to explain the sharp rise of the absorption Sagan (Harvard University, Smithsonian Instltution, Smithsonian coefficient of the Cytherean atmosphere in the vicinity of 30 GHz Astrophysical Observatory, Cambridge, Mass. ). (1 cm'l). It is pointed out that the observed phenomenon can be Astrophysical Journal, vol. 147, Feb. 1967, p. 753-764. 35 refs. produced by an effect observed in a planetary atmosphere at moderate NASA Contract No. 21-003-002; NASA Grant No. 21-002-059; Grant pressures, namely, that in addition to their rotation spectra, No. NGR-09 -015-023. symmetrical top molecules exhibit a dielectric (Debye) relaxation The thermodynamic equilibrium composition of all possible that the absorption coefficient of such gases and their mlxtures so combinations of the elements carbon, hydrogen, oxygen, and nitrogen with nonpolar gases in the microwave region are very high. M. F. at average pressures and temperatures have been calculated for the atmospheres of Earth, Venus, Mars, and Jupiter. All reglons of Y A67-21991 * the composition diagram consistent with the observed molecular RESPONSE OF FUNGI TO DIURNAL TEMPERATURE EXTREMES. abundances are located and discussed. The constituents of the Charles R. Curtls (NASA, Ames Research Center, Exobiology terrestrial atmosphere considered as a closed system are in Div., Moffett Field, Calif.). approximate thermodynamic equilibrium in spite of the continual Nature, vol. 213, Feb. 18, 1967, p. 738, 739. 6 refs. addition of trace compounds by biological activity, lightning, radia- Description of the results of a preliminary investigation of the tion, and vulcanism. Under some circumstances, the presence of U response of various fungi to diurnal temperature extremes of -94 atmospheric organic molecules far in excess of their thermodynamic and 23 &ZoC. The fungi were grown on malt agar (BBL), and two equilibrium proportions can be an indication of indigenous biological

44 A67-24063

activity. The atmosphere of Venus seems likely to be in thermo- A67-22715 dynamic equilibrium. It then follows that the measured upper limits SELF-BROADENING EFFECTS IN THE INFRARED BANDS OF on the abundances of CH4. NH3, and CO are all inconsistent with GASES. the possibility of elemental carbon or hydrocarbons in contact wlth A. Anderson, An-Ti Chai, and Dudley Williams (Kansas State the atmosphere, either on the surface or as clouds. The evidence University of Agriculture and Applied Science, Dept. of Physics, for Mars is not inconsistent with thermodynamic equihbrmm. The Manhattan, Kan. ). computations do not indicate whether small quantities of free 02 Optical Society of America, Journal, vol. 57, Feb. 1967, p. 240-246. exist. The equilibrium abundances of all oxides of nitrogen on Mars 17 refs. are extremely low even if computed with a considerable excess of USAF-supported research. 02. For Mars and Venus there are no molecular species wlth a large Various techniques for measurement of the self-broadening of predicted equilibrium abundance and spectroscoplcally accessible spectral lines of absorbing gases as compared with the line-broaden- absorption features which have not already been identifietl. Under ing effects of nitrogen were tested and are critically compared. equilibrium conditions at low temperatures Jupiter also cannot contain Mean values of self-broadening coefficients applicable to entire ab- significant amounts of any molecule not yet observed. However, at sorption bands were redetermined with improved precision for CO, high temperatures such as would be produced by lightning discharges GO2, N20, CH4. and NH3; agreement with earlier results is good or in the Jovian thermosphere, slmple hydrocarbons and cyanides. except for NH3. Low-resolution studies of the variation of self- polycyclic aromatics, and a variety of nitrogen compounds would be broadening coefficients across absorpbon bands indicate that the expected. Some of these compounds are brightly colored, and it coefficients generally have maximum values in the spectral regions seems possible that such organic compounds contribute to the observed where absorption is greatest; however, the coefficients for individ- variable coloration of Jupiter. (Author) ual vibration-rotation lines determined at higher resolution do not, in general, show striking variations from line to line in a given band. Certain apparent anomalies in the results for NH3 are discussed. (Author)

A67-22237 A67-22768 * # ATMOSPHERE DEFINITION WITH A FREE-FALLING PROBE. MODEL ATMOSPHERES OF THE MAJOR PLANETS. Simon C. Sommer and Alfred G. Boissevam (NASA, Ames Research L. M. Trafton (Carnegie Institution of Washington and California Center, Moffett Field, Calif. ). Institute of Technology, Mount Wilson and Palomar Observatories, Astronautics and Aeronautics, vol. 5, Feb. 1967, p. 50-54. 7 refs. Pasadena, Calif.). Experimental confirmatlon of the ability of a free-falling probe Astrophysical Journal, vol. 147, Feb. 1967, p. 765-781. 39 refs. during terminal descent to draw an accurate profile of an unknown Nongray model atmospheres have been constructed for the major planetary atmosphere from onboard measurements alone. A small planets assuming and introducing first-order radiative-equilibrium instrumented capsule was carried by balloon to an altitude of corrections to account for convection. The thermal opacity was ' 130, 000 ft over White Sands Missile Range, N. Mex. During free provided by the pressure-induced absorption of H2 and also by its fall, the capsule accelerated almost to sonic velocity in a density enhancement resulting from mixing with He. The thermal opacity regime similar to that expected near the surface of Mars. Thls due to NH3 was found to be negligible in all of the major planets experiment showed that atmospheric and altitude measurements can where the effect is but minor. In constructlng the except Jupiter, be made with good accuracy. At flight velocities approaching sonic models, the He/H2 abundance ratios and effective temperatures speeds, amblent pressures and temperatures can be obtained from were considered free parameters to be determined by fitting the the acceleration history of the vehicle and from local pressure and models to the observations. IS In all the models the absorption temperature measurements, and the average molecular weight of strong enough to bring about convection in the deeper layers. In the the gas can be deduced from these measurements as well. F. R. L. case of the Jovian models, the amount of H2 lying above the convective zone is found to be approximately equal to the observed amount lying above the planet's visual cloud layer. The Jovian limb darkening in the 8-14-p region can be explained in terms of absorption due A67-22957 to H2, He, and the 10-jd band of NH3 but cannot be explained when SURFACE PRESSURES IN THE MARTIAN HIGHLANDS AND LOW- the NH3 band is excluded. Models of Jupiter for which only the LANDS. thermal opacity of H2 and NH3 are taken into account are incompatible J. Otterman (Tel-Aviv University, Institute of Planetary and Space with the observations. Adding He, however, eliminates this incom- Science, Ramat-Aviv, Israel). patibility, indicating that He is present in these atmospheres. In Nature, vol. 213, Mar. 11, 1967, p. 1000, 1001. 13 refs. the case of Jupiter, a rather large He/H2 value IS implied if there Discussion of elevation of the Martian dark areas (maria) rela- is no internal heat source. However, the observations suggest that tive to the bright areas (deserts). Various theories of Wells (1966), the value of He/H2 is less than 2 so that the existence of a small Sagan (1966), Wyarnoto (1966), Tombaugh (1966), and Fjeldbo (1966) internal heat source generating more than one-tenth of the incident are treated briefly. The lack of whitening in the maria area 1s solar flux is implied. (Author ) noted, and a hypothesis for such an observation is given. Pressure data gathered from the Mariner 4 mission are reviewed. The possibility that pressure and temperature may be higher in the highland areas than in the lowland areas is examined. R. B. S.

A67-24063 * A67-22240 * DETECTING PLANETARY LIFE FROM EARTH. ON THE LIMB DARKENING OF PLANETARY ATMOSPHERES IN Dian R. Hitchcock (United Aircraft Gorp., Hamilton Standard Div., THE THERMAL INFRARED. Biosciences Section, Windsor Locks, Conn. ), Peter Fellgett (Read- R. E. Samuelson (NASA, Goddard Space Flight Center, Greenbelt, ing, University, Dept. of Applied Physical Sciences, Reading, Md. ). Berks., England), Janine Connes (Centre National de la Recherche Astrophysical Journal, vol. 147, Feh. 1967, p. 810-815. 9 refs. Scientifique, Service d'Ae'ronomie, Observatoire de Meudon, c Demonstration of how exact solutlons to the problem of describing Meudon, Seine-et-Oise. France), Pierre Connes (Centre National the angular distribution of outgoing radiation from a slab of material de la Recherche Scientifique, Bellevue, Seine-et-Oise, France), bounded on both sides by a vacuum may be expressed in terms of Lewis D. Kaplan (California Institute of Technology, Jet Propulsion Chandrasekhar's $- and @-functions of zero order when both scat- Laboratory, Space Sciences Div., Pasadena, Calif.), J. Ring tering and temperature-gradient effects are present. Values rep- * (Hull, University, Hul1,Yorks.. England), and J. E. Lovelock. resenting the phase function for single scattering representative of Science Journal, vol. 3, Apr. 1967, p. 56-67. a flat particle-size distribution covering the range 0 5 d,< 12.73 Discussion of new techniques which make possible the detection are plotted. B.B. of extraterrestrial life from the earth's surface. The development

45 A67-24501

of such methods has led to the proposed construction of the world's A67-24843 largest telescope to investigate any possible modification of planetary * NATURE OF VENUS [PRIRODA VENERY 1. atmospheres by life. The genesis multiplex spectrometry and its of V. A. Bronshten (Vsesomznoe Ast ronomo -Geodezicheskoe application to planetary atmospheres is considered, and ways of in- Obshche stvo, USSR). terpreting the observations are outlined. The construction of a 1000 Astronomicheskii Vestnik, vol. 1, Jan. -Mar. 1967, p. 4-27. 104 refs. in. telescope is detailed, and a diagram is given which summarizes In Russian. the angular resolving power and sizes of some large radio and op- Review of the current status of our knowledge on the surface tical telescopes. B. B. and atmosphere of the planet Venus, on the basis of recent radar, radioastronomic, and IR spectroscopic observations. General data on Venus are examined, including dimenszons, mass, rotation, A67-24501 illumination, heating, magnetic field, and radiation belts. A discus- SOME COMMENTS ON MARTIAN WHITE CLOUDS. sion of the surface data includes the brightness temperature, polar- R. A. wells (London, University, Observatory, Mill Hill, Mddx., ization, radio emission, the temperature distributlou over the planet England). disk, and the physicochemlcal properties. The chemical composition Astrophysical Journal. vol. 147, Mar. 1967, p. 1181-1183. 5 refs. of the Venus atmosphere is examined, together with the equations Discussion of a scientific note and a related article to support and initial data employed III the construction of atmospheric models. P. suggestions that the mass motion of H20 m the atmosphere of Mars v. appears to be correlated with polar cap recession and growth, and possibly with the frequency of appearance of white clouds and identification of dark features on the surface. The scientific note contams A67-25204 * a correlation between the white-cloud frequency, which shows a STIMULATION OF JUPITER'S RADIO EMISSION BY IO. bimodal distribution, and the waxing and waning of the polar caps. L. Marshall (Colorado, University, Dept. of Physics, Boulder, This correlation is based on the observation that the ratio of maxi- Colo.) and W. F. Libby (California, University, Dept. of Chemistry mum mass transfer from both polar caps is equal to the ratio of the and Institute of Geophysics, Los Angeles, Calif.). two maximum cloud frequencies. The cloud frequencies were deter- Nature, vol. 214, Apr. 8, 1967, p. 126-128. 24 refs. mined from 253 observations derived from the literature, polariza- AEC -USAF-NASA-supported research. tion studies, and photographs. M.M. Discussion of variations III the decameter radio signals from Jupiter associated with the planet's five satellites. It IS seen that Io travels in the analog of the inner Van Allen radiation belt A67-24510 * surrounding Jupiter, giving rise to a plasma wake which streams ahead of it by about 130, 000 km and stimulates the radio emission TRACES OF HC1 AND HF IN THE ATMOSPHERE OF VENUS. from the Jovian atmosphere. M. F. P. Connes (Centre National de la Recherche Scientifique, Bellevue. Seine-et-Oise. France), J. Connes (Centre National de la Recherche Scientifique. Service d'A6ronomie. Observatoire de Meudon, Meudon, Seine-et-Oise, France), W. S. Benedict (Johns Hopkins University, A67-25206 * Baltimore, Md. ), and L. D. Kaplan (California Institute of Technology, MAGNETOSPHERE OF JUPITER. Jet Propulsion Laboratory, Pasadena, Calif. ). J. A. Gledhill (NASA, Goddard Space Flight Center, Laboratory for Astrophysical Journal, vol. 147, Mar. 1967, p. 1230-1237. 15 refs. Space Sciences, Planetary Ionospheres Branch, Greenbelt, Md. ). USAF-supported research. Nature, vol. 214, Apr. 8, 1967, p. 155, 156. Discussion of Venus spectra obtained with a Michelson inter- NASA -supported research. ferometer designed for high-resolution planetary infrared spectros - Determination of the maximum number density of the plasma in copy. Three atmospheric windows, corresponding to 3900 to the equatorial plane of Jupiter by equating the magnetic and rotational 5300 cm-l, 5500 to 7200 cm-1, and 7600 to 8500 cm-1 were isolated kinetic energy densities. Using an Angerami- and Thomas-type by interference filters. Narrow absorption lines are detected and method, the distribution of plasma along the line of force L is assigned to the 2-0 vibration-rotation band of HCI and the 1-0 and calculated. Numerical calculations lead to a magnetospheric model 2-0 bands of HF. The HC1 lines are consistent with 2-mm Amagat of Jupiter. It 1s noted that all four of the "sources" related to Io on of the gas in the optical path, at temperature near 240°K and pressure Jupiter appear to correlate, at least qualitatively, with the model. near 0.1 atm, in a spectral region where the effective C02 path is M. F. 1.7 x lo6 times as large. The less intensive HF data indicate about 0.02 mm Amagat of that gas. V.P.

A67-25232 * * THE VOYAGER PROGRAM. A67-24601 Edgar M. Cortright (NASA, Washington, D.C.). THE MICROWAVE SPECTRUM OF VENUS IN THE FREQUENCY American Astronautical Society, Goddard Memorial Symposium, RANGE 18-36 GCISEC. 5th, Washington, D.C., Mar. 14, 15, 1967, Paper. 37 p. P. H. Grdfith, D. D. Thornton, and W. J. Welch (California, Review of the Voyager project, coverlng goals of the Saturn- University, Space Sciences Laboratory and Radio Astronomy Labora- launched orbiterllander mission to Mars, such as planetary, atmo- tory, and Dept. of Electrical Engineering, Berkeley, Calif. ). spheric, and environmental studies. Orbital operations, capsule Icarus, vol. 6, Mar. 1967, p. 175-188. 27 refs. descent, navlgational systems, capsule description, and illustra- The microwave emission from Venus was measured at seven tions of projected goals are also treated. R.B.S. frequencies in the interval 18 to 36 Gc in July 1964 shortly after inferior conjunction. The resulting spectrum shows a fairly smooth but rapid decrease m the planet's brightness toward the hgher frequencies. The measurements are compared with the spectra of several model atmospheres which contain GO2, N2, water vapor, A67-25685 * liquid water clouds, and high dust or Ice clouds. None of the model THE ATMOSPHERE OF MARS - A DERIVATION OF PARAMETERS spectra exactly fit all the present measurements. A best fit for the FOR ENGINEERING AND DESIGN APPLICATIONS. model in which absorption is due to CO2 and N2 requires a surface George S. West, Jr. and W. T. Roberts (NASA, Marshall Space W pressure of about 200 atm. A best fit for the model which contains, Flight Center, Aero-Astrodynamics Laboratory, Aerospace En- in addition, water vapor and liquid water clouds requires ahout vironment Div., Space Environment Branch, Huntsville, Ala. ). 12 gmlcm2 of the vapor and 0.06 gm/cm2 of liquid water clouds at IN: INSTITUTE OF ENVIRONMENTAL SCIENCES, ANNUAL TECH- a temperature of 240°K. The best agreement is provided by a model NICAL MEETING, 13TH, WASHINGTON, D. C., APRIL 10-12, 1967, which contains scattering particles. For dust particles of mean PROCEEDINGS. VOLUME 1. v diameter 0.3 mm and dielectric constant 5, the required number of Mt. Prospect, Ill., Institute of Environmental Sciences, 1967, particles is 2.5 x 106Icm2. (Author) p. 121-125. 12 refs.

46 A67-263 16

Study of three models of the Martian atmosphere of differing A67-26038 * # atmospheric composition, surface pressure, and surface tempera- EXPERIMENTAL AND THEORETICAL STUDY OF MOLECULAR, ture. The molecular composition of the Martian atmosphere is dis- CONTINUUM. AND LINE RADIATION FROM PLANETARY ATMO- cussed and the atmospheric temperature is studied. A description of SPHERES. the three models - the upper density model, the mean density model, W. A. Menard, G. M. Thomas (California Institute of Technology, and the lower density model - is given. M. F. Jet Propulsion Laboratory, Pasadena, Calif. ), and T. M. Helliwell (Harvey Mudd College, Claremont, Calif. ). American Institute of Aeronautics and Astronautics, Thermophysics Specialist Conference, New Orleans, La., Apr. 17-20, 1967, Paper 67-323. 16 p. 62 refs. A67-25715 * Members, $0.75; nonmembers, $1.50. Study of the various sources of equilibrium radiation important THE MARS TRANSIT AND ENTRY ENVIRONMENT - A NEW to planetary entry problems. Shock tube measurements of the radia- PROBLEM FOR HEAT SHIELDS. tion from a mixture of 30% C02-40% N2-30% A were made over the Robert G. Nagler (California Institute of Technology, Jet Propulsion temperature range 7000-16, Several approxlmate theoretical Laboraiory. Materials Section, Pasadena, Calif. ). OOO°K. models for the molecular band structure are presented. These IN: INSTITUTE OF ENVIRONMENTAL SCIENCES, ANNUAL models are then compared with the results of spectral measurements TECHNICAL MEETING, 13TH, WASHINGTON, D. C., APRIL 10-12, of the CN violet band system. The best fit to the data is obtained 1967, PROCEEDINGS. VOLUME 2. using a CN dissociation energy of 7.7 ev. Calculations were made Mt. Prospect, Ill. , Institute of Environmental Sciences, 1967, p. 443-455. 17 refs. of the free-free and free-bound continua of singly ionized N, C. A, Consideration of the problems introduced by landing an unmanned and 0 atoms, using nonhydrogenic cross sections, and the electron 0, and C atoms, using measured vehicle on the surface of Mars, with reference to some new problems attachment continua of neutral N, cross sections. Self-absorption was accounted for in the calculation in heat shield technology. The transit and entry environments experienced by such a vehicle fromprelaunch to parachute deploy- of atomic line radiation by using a statistical model that considers ment are outhned, with discussion of the implications of the steriliza- overlapping of the individual lines. Total radiation in the region 0.3 tion, launch, interplanetary transit, and atmospheric entry environ- to 2.7 ~1 was measured at the stagnation point of a flat-faced cylinder model. Comparison of the theoretical predictions with the data ments on the selection of heat shield materials for various missions. Some of the NASA programs now in progress to screen the available suggests that an unknoim source, which was not included in the calculations, may be present. (Author) composites in these environments are also outlined. F. R. L.

A5146244 * UN THE POLARIMETRIC EVlDENCE FOR AN ATMOSPHERE 5 ON MERCURY. A67-25986 * B. T. O'Leary and D, 6. Rea (California, University, Space Sciences MICROWAVE METHOD FOR PLANETARY ATMOSPHERE RE- Laboratory, Berkeley, Calif. ). SEARCH. Astrophysical Journal, vol. 148, pt. 1, Apr. 1967, p. 249-253. 12refs. L. Frenkel (NASA, Electronics Research Center, Cambridge, Grant NO. NsG-101-61. Mass.). Review of Scientific Instruments, vol. 38, Apr. 1967, p. 557, 558. Discussion of Dollfus' conclusion of several years ago that Brief outline of the use of very high Q Fabry-Pdrot microwave Mercury has an atmosphere from observations of excess polarization cavities for the study of planetary atmospheres under ambient con- values at shorter wavelengths and at the cusps with respect to the ditions. The instrument proposed - simlar to one described by center. It 1s noted that this conclusion depended on various assump- Valkenburg and Derr, 1966 - for such a study is described. The tions regarding the polarimetric properties of Mercury and the moon. use of the instrument in a problem concerning the determination of However, in view of recent lunar and laboratory data which show the the water vapor content of an atmosphere consisting of N2 at a pres- same excess polarization both in color and location, these assum- tions are found to be incorrect or mapphcable. It follows that the sure of about 10 mm Hg is treated. R.B.S. polarization properties of Mercury can be explained by its surface only, so there IS no polarimetric evidence for an atmosphere on Mercury. The polarimetric observations suggest an upper limit of 1 mb for the surface pressure, while the simllarlty of the polarimetric and photometric properties of Mercury and the moon suggests an upper limit of mb. M.M. A67-26009 * # DETERMINATION OF MARS ATMOSPHERIC COMPOSITION BY SHOCK-LAYER RADIOMETRY DURING A PROBE EXPERIMENT. Ellis E. Whiting (NASA, Ames Research Center, Moffett Field, A67-26316 #I Calif.). SPHERICAL PARTICLE TERMINAL VELOCITIES IN THE MARTIAN DAYTIME ATMOSPHERE FROM 0 TO 50 KILOMETERS. Albert D. Anderson (Lockheed Aircraft Corp., Lockheed Missiles and Space Go., Research Laboratories, Palo Alto, Calif. ). Journal of Geophysical Research, vol. 72, Apr. 1, 1967, Examination of the feasibility and accuracy of determining atmo- p. 1951-1958. 12 refs. spheric composition by a shock-layer radiometer experiment on a Research supported by the Lockheed Independent Research Program. Mars probe. In concept, a few narrow band-pass radiometers on Presentation of the terminal velocities of spherical particles board the entry probe would view the shock layer through a small (density = 30 g/cm3). with diameters from 1 to 10,000 ~1,for three quartz window on the probe axis of symmetry and measure the radia- Martian daytime model atmospheres from 0 to 50 km, based on two tion emitted by selected atomic and molecular species in the shock different surface pressures (5.55 and 10 mb). The model atmo- layer. Various mixtures of CO2. N2. and A were used to simulate spheres are founded on results from the Mariner 4 occultation ex- * the Martian atmosphere. Experimental shock-layer spectra from periment, which gave densities in the Martian atmosphere that were ballistic-range tests show that CN(violet), Cz(Swan), C (2478 A), much lower than previous estimates. The following conclusions are and 0 (7775 A) are the most prominent features in the gas-cap spec- reached concerning the yellow (dust) clouds: (1) the vertical veloci- trum for these gas mixtures. A theoretical study of equilibrium ties required to keep yellow-cloud particles of sizes 10 e or less intensities emitted by CN(vio1et) and C2(Swan) behind a normal shock aloft are greater on Mars than on earth. (2) The minimum size of wave at Mars entry trajectory conditions shows that the relative the grains primarily responsible for the local surface yellow-cloud C02-N2-A concentrations in the ambient gas can be determined with obscurations is about 20 u. This falls within the range of estimates reasonable accuracy by this technique. (Author) in the literature (1-20 p) as to the size primarily responsible for the

47 A67-26819

surface obscurations. (3) Particles as small as 3 I could be respon- summarized, and a number of findings are cited concerning planetary sible for the rarer planet-wide obscurations lasting a month or temperatures, dissipation of planetary atmospheres, and the internal more. The above conclusions are compared with those of Ryan who structure of planets. M. M. based his analysis on a denser Martian model atmosphere (25 mb). (Author) A67-28964 A67-26819 * # DIRECT SOUNDING OF THE ATMOSPHERE OF PLANETS RADIO OCCULTATION INVESTIGATIONS OF THE ATMOSPHERE [SONDAGE DIRECT DE L'ATMOSPHERE DES PLANETES]. OF MARS. G. Israel (Centre National de la Recherche Scientifique, Service Arvydas Kliore and Dennis A. Tito (California Institute of Tech- d'Akronomie, Verribres-le-Buisson, Seine-et-Oise, France). nology, Jet Propulsion Laboratory, Systems Analysis Section, (Sociktk FranGaise d'Astronautique, Journe'e sur 1'Exploration des Pasadena, Calif. ). Planetes, Roquencourt, Seine-et-Oise, France, Dec. 1, 1966, (AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAUTICS, Expose'. ) AND AMERICAN ASTRONAUTICAL SOCIETY, STEPPING STONES Revue Franqaise d'Astronautique. Mar. 1967, p. 31-34. In French. TO MARS MEETING, BALTIMORE, MD., MARCH 28-30, 1966, Results of direct observations of the atmosphere of planets TECHNICAL PAPERS, p. 5-13. ) made by means of Manner 2. The measurement of the brightness Journal of Spacecraft and Rockets, vol. 4, May 1967, p. 578-582. temperature of the emitting regions of Venus and of its atmosphere 9 refs. is discussed. together with the direct soundlng of the Martian [For abstract see issue 13, page 2178, Accession no. A66-252351 atmosphere. Regarding the magnetic field of Mars, the measurements of Mariner 2 show the field to be only lllOOOth or 5/1O,OOOth of the earth's magnetic field, pointing to the possibllity of direct interaction with the solar wind. A67-27333 # M. M. DISTRIBUTION OF THE RADIO-BRIGHTNESS TEMPERATURE OVER THE DISK OF VENUS [O RASPREDELENII RADIOIARKOSTNOI TEMPERATURY PO DISKU VENERY]. A67-29098 * A. G. Pavel'ev and G. M. Strelkov. A DISCUSSION OF THE PLANETARY QUARANTINE CONSTRAINTS. Kosmicheskie Issledovaniia, vol. 5, Mar. -Apr. 1967, p. 265-275. J. 0. Llght, C. W. Craven (California Institute of Technology, Jet 26 refs. In Russian. Propulsion Laboratory, Pasadena, Calif. ), W. Vishnlac (Rochester, Determination of the distribution of the radio-brightness tem- University, Rochester, N. Y .), and L. B. Hall (NASA, Washmgton, perature over the disk of Venus at the wavelengths of 1.9 and 1. 35 cm D.C.). for a spherically symmetrical model of the Venus atmosphere. Thls (COSPAR, International Space Science,Symposlum, 7th, Vienna, distribution IS determmed from the results of a scanning of Venus at Austria, May 10-18, 1966, Paper.) these wavelengths by Mariner 2 during its fly-by in December 1962. IN: LIFE SCIENCES AND SPACE RESEARCH V, INTERNATIONAL The distribution of the brightness temperature averaged over the SPACE SCIENCE SYMPOSIUM, 7TH, VIENNA, AUSTRIA, MAY 10- radiation pattern of the on-board antenna of Marmer 2 IS also deter- 18, 1966, PAPERS. mined. A.B.K. Symposium sponsored by the Committee on Space Research, the International Union of Biochemlstry, the International Union of Biological Sciences, and the International Union of Physiological A67-27462 #l Sciences. DISCRETE EQUILIBRIUM TEMPERATURES OF A HYPOTHETICAL Edited by A. H. Brown and F. G. Favorlte. PLANET WITH THE ATMOSPHERE AND THE HYDROSPHERE OF Amsterdam, North-Holland Pubhshmg Go., 1967, p. 7-21. ONECOMPONENT TWO-PHASE SYSTEM UNDER CONSTANT [For abstract see issue 15, page 2441, Accesslon no. A66-299661 SOLAR RADIATION. M. Komabayasi (Nagoya University, Water Research Laboratory, Nagoya, Japan). A67-30628 Meteorological Society of Japan, Journal, vol. 45, Feb. 1967, SYSTEM DESIGN OF AN AUTOMATED LABORATORY AND ASSO- D. 137-139. l0refs. CIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORA- Qualitative consideration of the thermal equilibrium states of TION. the ocean and of the vapor atmosphere of a planet by use of a model C. E. Anderson (General Electrlc Co., Philadelphia, Pa.) and of a one-component two-phase system. The obtained result is ex- F. G. Beuf. pected to suggest the existence of a few discrete temperature levels (International Astronautlcal Federation, Internatlonal Astronautical in equilibrium on a real planet which has a vast ocean under a Congress, lbth, Athens, Greece, Sept. 13-18, 1965, Paper.) constant solar radiation. T.M. IN: SPACE CRAFT SYSTEMS, INTERNATIONAL ASTRONAUTICAL FEDERATION. INTERNATIONAL ASTRONAUTICAL CONGRESS, 16TH, ATHENS, GREECE, SEPTEMBER 13-18, 1965, PROCEEDINGS VOLUME 1. A67-27859 Congress supported by the United Nations Educational, Scientific THE GREENHOUSE EFFECT IN THE ATMOSPHERE OF VENUS. and Cultural Organization. G. M. Strelkov. Edited by MichaYLunc. (Kosmicheskie Issledovaniia, vol. 4, July-Aug. 1966, p. 581-591. ) Paris, Gauthier-Villars, Dunod, New York, Gordon and Breach, Cosmic Research, vol. 4, July-Aug. 1966, p. 514-522. 24 refs. Warsaw, Pafistwowe Wydawnictwo Naukowe, 1966, p. 147-168. Translation. Research sponsored by the General Electric Co. [For abstract see issue 22, page 3980, Accession no. A66-404691

A67-30932 A67-28959 JUPITER'S ATMOSPHERE - ITS STRUCTURE AND COMPOSITION. GENERAL SURVEY OF PLANETS [PRESENTATION D'ENSEMBLE Jack A. Greenspan and Tobias Owen (UT Research Institute, Astro DES PLANETES]. Sciences Center, Chicago, Ill.). M. Tardi. Science, vol. 156, June 16, 1967, p. 1489-1494. 23 refs. (Socie'te' Franqaise d'Astronautique. Journke sur 1'Exploration des Study of the structure and composihon of the atmosphere of Planites, Roquencourt, Seine-et-Oise, France, Dec. 1, 1966, Jupiter noting that recent laboratory and observational data support Expose'. ) the hypothesis that the composition of Jupiter's atmosphere is con- Revue Franqaise d'astronautique. Mar. 1967, p. 4-12. In French. sistent with the relative abundances of the elements found in the Summary of current knowledge concerning the solar system. sun. A model based on this assumption provides a reasonable mter- The principal characteristics of the planets of the solar system are pretation of abundances of hydrogen and other gases obtained from

48 A67 - 3 323 2

studies of various regions of the planet's spectrum. Two presently A67-33096 * unidentified absorptions may be caused by organic molecules in the THE ASHEN LIGHT AND THE MAGNETIC FIELD OF VENUS. Jovian atmosphere. P.v.T. A. J. Jeffries B British Astronomical Association, Journal, vol. 77, June 1967, p. 262, 263. A67-31487 * Discussion of the possibility of observlng auroral phenomena on Venus, by making careful observations of the so-called "ashen THE VOYAGER PROGRAMME. light." The presence of auroras on Venus would imply the presence Edgar M. Cortright (NASA, Washington, D.C.). of a magnetic field, the existence of which has not as yet been (American Astronautical Soclety, Goddard Memorial Symposium, ascertained, smce the earth's auroral phenomena occur purely as a 5th, Washington, D.C., Mar. 14, 15, 1967, Paper. ) result of the earth's magnetic field. The ashen light of Venus Space Flight, vol. 9, July 1967, p. 222-227. appears as a famt glow illummatmg the dark side of the planet. [For abstract see issue 12, page 2002, Accession no. A67-252321 An aurora might be visible from earth as part of the ashen Lght, If it were sufficiently intense and well placed for observation. P.v. T.

A67-32322 #k TWO-LAYER MODEL OF THE VENUSIAN ATMOSPHERE - MTER- 867-331 87 PRETATION OF RADAR OBSERVATIONS [DVUKHSLOINAIA RADIATIVE RELAXATION TIMES FOR MARS - A DISCUSSION OF MODEL' ATMOSFERY VENERY OB INTERPRETATSII RADIO - - MARTIAN ATMOSPHERIC DYNAMICS. LOKATSIONNYKH NABLIUDENII]. Richard Goody (Harvard University, Cambridge, Mass. ) and N. Vetukhnovskaia and A. D. Kuz'min (Akademiia Nauk SSSR, Iu. Michael J. S. Belton (Kitt Peak National Observatory, Tucson, Fizicheskii Institut, Moscow, USSR). Ariz.). Astronomicheskii Vestnik, vol. 1, Apr. -June 1967, p. 85-88. Planetary and Space Science, vol. 15, Feb. 1967, p. 247-256. 6 refs. Russian. In 17 refs. Construction of a two-layer model of the Venusian atmosphere NSF Grant No. G-24903. which satisfies the data of radioastronomic and radar self-radiation Radiative relaxation times €or temperature perturbations in measurements, includmg the 3-cm wavelength. The upper, cold C02 with small admlxtures of water vapor under conditions which (300OK) absorbmg layer defines the self-radiation spectrum, but are similar to those occurring in the Martian atmosphere have been has no mfluence on the results of radar observations, smce absorp- computed. Certain aspects of the influence of radiative transfer tion in this layer is very low even at the shortest (3.6 cm) wavelength on dynamical phenomena in the Martian atmosphere are discussed of the radar measurements. The lower, hot absorbing layer, near in terms of these radiative relaxation times. It is found that: (1) the planet surface, absorbs radio emission at centimeter wavelengths diurnal changes in the temperature profile will extend to considerably and defines the spectrum of the effective cross section of the reflec- greater heights in the Martian atmosphere than is the case on earth, ;r tion of radar signals, but hardly affects the brightness temperature the diurnal wave will propagate more by radiative transfer than by measurements, smce the temperature of this layer differs only turbulent diffusion, (2) a nonnegligible diurnal wind system exists on slightly from the surface temperature. The lower absorbmg layer Mars, (3) nonlinear interactions between the motion field and the may be the lower level of clouds with a (1 to 2) x g/cm2 dust lo3 initial state of radiative equilibrium are much smaller on Mars content. V.P. than on earth; and (4) radiative destabilization of regions wlth a negative lapse rate may be important in the upper Martian atmosphere. (Author) A67-32652 * UPPER LIMITS ON LIQUID WATER IN THE VENUS ATMOSPHERE. W. J. Welch and D. G. Rea (California, University, Space Sciences A67-33196 * Laboratory and Dept. of Astronomy, Radio Astronomy Laboratory ROTATIONAL EFFECTS ON THE DISTRIBUTION OF THERMAL and Dept. of Electrical Engineermg, Berkeley, Calif.). PLASMA IN THE MAGNETOSPHERE OF JUPITER. Astrophysical Journal, vol. 148, June 1967, pt. 2, p. L151-Ll54. D. B. Melrose (Sussex, University, School of Mathematical and 12 refs. Physical Sciences, Brighton, England; Yeshiva Universlty, Belfer NSF Grant No. GA-527; Contracts No. Nonr-222(54), No. NASr-220, Graduate School of Science, New York, N.Y.). Grant No. NsG-101-61. Planetary and Space Science, vol. 15, Feb. 1967, p. 381-393. Discussion of a consequence of the recent discovery of HC1 and 15 refs. HF in the atmosphere of Venus. The consequence is that, on ac- NASA-AEC-supported research. count of the presence of HCI, there cannot be much liquid water m The consequences of the assumption that the magnetosphere of the Venusian atmosphere. HC1 is highly soluble in water, and the Jupiter corotates with the planet are examlned, It is found convenient resulting acid has a high dc conductivity. It is pointed out that if to divide the magnetosphere mto two regions. The inner region is there were much of this acid m the Venusian atmosphere, the long- qualitatively similar to the magnetosphere of the earth provided that wavelength radar signals would be strongly attenuated, whereas the the ratio of the scale height to the radius of Jupiter IS much less radar signals appear to reach the planet's surface with little attenua- than 1/12. The outer region is dommated by rotatlonal effects. It is tion. M.M. expected to be slightly flattened, with a density falling off as Br-l. The velocity distribution of the plasma becomes increasingly anisotropic with mcreasing distance. The corotating magnetosphere breaks up as a result of electrostatic microinstabilities at 7-8 radii, well A67-32826 inside the boundary with the solar wind. (Author) MEASUREMENTS OF DISSOCIATIVE RECOMBINATION OF COzt IONS WITH ELECTRONS. Charles S. Weller and Manfred A. Biondi (Pittsburgh, University, A67-33232 Dept. of Physics, Pittsburgh, Pa.). VENUS - VOLCANIC ERUPTIONS MAY CAUSE ATMOSPHERIC OB- Physical Review Letters, vof. 19, July 10, 1967, p. 59-61. 10 refs. SCURATION. w Army-DASA-supported research. Gerald T. Davidson and Albert D. Anderson (Lockheed Aircraft Gorp., Application of the microwave-afterglow differentially pumped Lockheed Missiles and Space Co., Research Laboratories, Palo quadrupole mass-spectrometer apparatus to a quantitative determina- Alto, Calif.). tion of the dlssociative recombmation coefficient a(C02t) between Science, vol. 156, June 30, 1967, p. 1729, 1730. 12 refs. electrons and COz+ ions for models of the Martlan ionosphere. The High rates of volcanic and tectonic activities are inferred from t results suggest the need for modlfication of the Martian ionospherlc the high surface temperature of Venus. The effects of volcanlc ef- models to conform to values of a(COzt) substantially less than 10-6 fluents, gas and dust, on obscuration in the atmosphere are considered. cm3lsec. M.F. The optical extinction due to particulate matter is estimated from

49 A67-34095 assumed distributions as to particle size and altitude. As few as ten Symposium sponsored by the Committee on Space Research and the explosive eruptions per year would cause significant absorption and International Astronomical Union. scattering of visible light. (Author) Edited by A. Dollfus. Amsterdam, North-Holland Publishing Co., 1967, p. 240-245. 4 9 refs. A67-34095 Grant No. NsG-269. THE RISE OF OXYGEN IN THE EARTH'S ATMOSPHERE WITH Much new informa:itin-has_become available in_ recent years on NOTES ON THE MARTIAN ATMOSPHERE. the Martian atmosphere. Mariner 4 data have shown that the SF- L. V. Berkner and L. C. Marshall (Southwest Center for Advanced face pressure is below 10 mb, a result that is not inconsistent with Studies, Dallas, Tex.). the most recent spectroscopic studies. If the Mariner 4 ionospheric (American Geophysical Union, Western National Meeting, 5th, data are interpreted in terms of an F2 peak, the atmosphere must General Assembly, Dallas, Tex., Sept. 1965, Paper.) be very cold at all levels and the exospherlc temperature must be IN: ADVANCES IN GEOPHYSICS. VOLUME 12. near 85OK. This result is in disagreement with studies of radiative Edited by H. E. Landsberg and J. Van Mieghem. equilibrium temperatures, which indicate a relatively warm exosphere, New York. Academic Press, Inc.. 1967, p. 309-331. 42 refs. the temperature being in the vicinity of 400°K. As a consequence NSF Grants No. 768; No. 4708; Contract No. Cwb-10531. of this inconsistency and others of a slmilar nature, there is still a Discussion of oxygenic concentrations m the primitive atmo- wide range of speculation concerning the properties of the Martian sphere of the earth. The surface oxidation and photosyhthetic oxygen atmosphere. These inconsistencies will probably be resolved only production in a primitive terrestrial atmosphere are estimated from after more detailed observations have been made in planetary probes, the present atmospheric level. Conjectures are made concernmg the such as the distribution of resonance scattering of sunlight by atomic oxygenic levels m the Paleozoic and Silurian eras and in ensuing eras. oxygen. (Author) Estimates of the composition of the Martian atmosphere and surface are made, and the possibility of life on Mars is considered. A general theory of the origin of planetary atmospheres is presented and A67-34153 discussed. M.F. A STUDY OF THE GENERAL CIRCULATION OF THE MARTIAN ATMOSPHERE BASED UPON THE RESULT OF THE OCCULTATION EXPERIMENT FROM MARINER IV. A67-34149 Wen Tang (Geophysics Corporation of America, GCA Technology STUDY OF PHOTOGRAPHS OF MARS TAKEN BY MARINER 4 Div. , Bedford, Mass. ). [CONSIDERATIONS SUR LES PHOTOGRAPHIES DE MARS PRISES IN: MOON AND PLANETS; INTERNATIONAL SPACE SCIENCE PAR MARINER 41. SYMPOSIUM, 7TH, VIENNA, AUSTRIA, MAY 10-18, 1966. Glauco De Mottoni (Consiglio Nazionale delle Ricerche, Centro PAPERS. di Studio per l'Astrofislca, Osservatorlo Astronomico, Merate, Symposium sponsored by the Committee on Space Research and the Italy). International Astronomical Union. IN: MOON AND PLANETS; INTERNATIONAL SPACE SCIENCE Edited by A. Dollfus. SYMPOSIUM, 7TH, VIENNA, AUSTRIA, MAY 10-18, 1966, Amsterdam, North-Holland Publishing Co. , 1967, p. 246-252. PAPERS. 10 refs. Symposium sponsored by the Committee on Space Research and The model of the general circulation for the steady state and the International Astronomical Union. symmetrical regime based upon Charney's development is modified Edited by A. Dollfus. by including the lateral eddy viscosity. The surface stress is also Amsterdam, North-Holland Publishing Co. , 1967, p. 186-194. adjusted slightly. The resulting modified model is used to study the In French. mean zonal and meridional winds, and the type of circulation regime Analysis of enlargements of photographs of Mars transmitted on Mars during the equinoctial' seasons. With input parameters by Mariner 4, which give a new interpretation of the visible bright- based on the recent occultation experiment from Mariner 4, the ness features. Cloud observations are discussed. A series of computed mean zonal wind at an isobaric surface of one quarter of images obtained from a first graphic depiction involving the elimlna- the average surface pressure of Mars is about 36 mlsec. This tion of instrumental effects and a redu; on of transmission traces compares to a value of about 33 m/sec computed for the earth's is included. The pictures have been reproduced on a unified scale, atmosphere with the same modified model. Comparing the calculated with the outlined shape of each picture corresponding to the real magnitude of the atmospheric pole-to-equator temperature difference contours of the regions viewed on the Martian surface. F. R. L. at the middle level of the atmosphere with the observed temperature difference at the same level, as deduced from the observational indications of surface temperatures, it is concluded that the symmetrical regime cannot remain stable. Therefore, in the mean A6744151 * for the Martian year, a wave type circulation regime will prevail RADIO OCCULTATION MEASUREMENT OF THE MARTIAN ATMO- in the Martian atmosphere. (Author) SPHERE OVER TWO REGIONS BY THE MARINER IV SPACE PROBE. A. Khore, D. L. Cam, and G. S. Levy (California Institute of Technoloev,-. Jet Propulsion Laboratory, Pasadena, Calif. ). A67-34154 (COSPAR, International Space Science Symposium, 7th, Vienna, TRANSPARENCY OF THE MARTIAN ATMOSPHERE AND VISIBIL- Austria, May 10-19, 1966, Paper.) ITY OF SURFACE DETAILS IN BLUE AND ULTRAVIOLET LIGHT IN: MOON AND PLANETS, INTERNATIONAL SPACE SCIENCE [TRANSPARENCE DE L'ATMOSPHERE MARTlENNE ET VISIBILITE SYMPOSIUM, 7TH, VIENNA, AUSTRIA, MAY 10-18, 1966, PAPERS. DES DETAILS DE LA SURFACE DANS LE BLEU ET ULTRA- Symposium sponsored by the Committee on Space Research and the VIOLET]. International Astronomical Union. 3. H. Focas (Centre National de la Recherche Scientifique, Service Edited by A. Dollfus. d'bdronomie, Observatoire de Meudon, Meudon, Seine-et-Oise, France). Amsterdam, North-Holland Publishmg Co., 1967, p. 226-239. IN: MOON AND PLANETS; INTERNATIONAL SPACE SCIENCE 12 refs. SYMPOSIUM, 7TH, VIENNA, AUSTRIA, MAY 10-18, 1966, PAPERS. Symposium sponsored by the Committee on Space Research and the International Astronomical Union. A67-34152 * Edited by A. Dollfus. THE ATMOSPHERE OF MARS. Amsterdam, North-Holland Publishing Co. , 1967, p. 253-255. Francis S. Johnson (Southwest Center for Advanced Studies, In French and English. Dallas, Tex. ). The comparison of photographs taken simultaneously in red, IN: MOON AND PLANETS; INTERNATIONAL SPACE SCIENCE green, blue, and UV light shows that the intensity of semitone areas e SYMPOSIUM, 7TH. VIENNA, AUSTRIA, MAY 10-18, 1966, of the soil of Mars tends to become equal to the intensity of the PAPERS. dark areas. This provokes a deformation of the usual configurations

50 A67-3454 1 of the planet. There are very tenuous veils observed, sometimes, Description of the ground instrumentation system for the Mariner in the blue and the UV. In such cases, they provoke a rapid fading 4 occultation experiment whose ob~ectivewas the determmation of of the semitone and dark areas, while the light areas maintain a the Martian atmospheric parameters. The ObJeCtlVe was accom- higher relative intensity, giving the illusion of clouds. This does plished by measuring the Dopplet-frequency perturbations in the S- not exclude the existence of real clouds I which can easily be band telemetry link caused by the refractive index profile of the identified. Such cases are very rare. The visibility of the hght and planetary atmosphere. It was necessary to measure extremely dark areas in the blue and the UV depends on the opacity of the veils. small deviations in frequency. The ground instrumentation require- The formation and the opacity of the veils in the two hemispheres of ments are described, and the equlpment utilized is discussed, as the planet seem to follow a seasonal cycle. (Author) well as the results obtained. The earth-based receiving stations employed standard phase-lock-loop receivers. and triple-conversion open-loop receivers. A hlgh-power transmltter was used to transmit A6744156 100-kw signals to the spacecraft transponder, so that two-way Doppler SOME ASPECTS OF MARTIAN CLOUDS AND THEIR RELATION- could be obtained the instant the spacecraft emerged from occultation. SHIP TO THE TOPOGRAPHY. Various simulation tests performed with the system are discussed. R. A. Wells (London, University, Observatory, M~llH111, Mlddx., T.M. England). (COSPAR, International Space Science Symposium, 7th, Vienna, Austrla, May 10-19, 1966, Paper.) A6744536 IN: MOON AND PLANETS, INTERNATIONAL SPACE SCIENCE * RAYLEIGH SCATTERING IN AN OPTICALLY THIN ATMOSPHERE SYMPOSIUM, 7TH, VIENNA, AUSTRIA, MAY 10-18, 1966, PAPERS. Symposium sponsored by the Committee on Space Research and the AND ITS APPLICATION TO MARTIAN TOPOGRAPHY. International Astronomical Union. J. B. Pollack (Smithsonian Institution, Smithsonian Astrophysical Edited by A. Dollfus. Observatory; Harvard University, Harvard College Observatory, Amsterdam, North-Holland Publishing Co., 1967, p. 262-273. Cambridge, Mass.). 12 refs. Icarus, vol. 7, July 1967, p. 42-46. 10 refs. Research supported by the European Space Research Organization. Grant No. NGR-09-015-023. A relationship between surface pressure and atmospheric brightness is derived for an optically thin, Rayleigh scattering atmosphere. Under similar assumptions, the geometric albedo is expressed as a function of the optical depth of the atmosphere A6744158 and arbitrary reflection properties of the surface. A recent deter- A THEORETICAL INVESTIGATION OF CYTHEREAN, MARTIAN mination of the atmospheric brightness from polarization measure- AND JOVIAN UPPER ATMOSPHERES. ments implies a surface pressure of about 20 mbar over the bright Wkio Shimizu (Ochanomizu Women's University, Dept. of Physics, areas of Mars. Dust contamination is shown to be probably insuf- Tokyo, Japan). ficient to reconcile this value of surface pressure with that obtained IN: MOON AND PLANETS; INTERNATIONAL SPACE SCIENCE by the Mariner 4 occultation experiment. It is concluded that bright SYMPOSIUM, 7TH, VIENNA, AUSTRIA, MAY 10-18, 1966, areas are lowlands and that elevation differences on the order of PAPERS. 10 km exist on Mars. (Author ) Sympqsium sponsored by the Committee on Space Research and the Internahonal Astronomical Union. Edited by A. Dollfus. Amsterdam, North-Holland Publishing Go., 1967, p. 296-298. A6744540 * 7 refs. ON THE CHEMISTRY OF JUPITER'S UPPER ATMOSPHERE. Theoretical investigation of the atomic and molecular processes William C. Saslaw (California, University, Institute of Geophysics in the upper atmospheres of Venus, Mars, and Jupiter, by using and Planetary Physics, Los Angeles; California Institute of Tech- the atmospheric models recently proposed by the Jet Propulsion nology, Div. of Geological Sciences, Pasadena, Calif. ; Princeton Laboratory group. The amounts of CO molecules in the Cytherean University, New Observatory, Princeton, N. J.) and Robert L. and Martian upper atmospheres produced by the photochemical Wildey (California Institute of Technology, Div. of Geological reactions with the solar UV radiation may be about 2 and 0. 2 cm Sciences; Carnegie Institution of Washington and California Institute STP, respectively. Then, the recombinatxon of CO and 0 may cause of Technology, Mount Wilson and Palomar Observatories, Pasadena, the axrglow of the intensities 20 kR and 45 R on Venus and Mars, Calif. ; U. S. Geological Survey, Astrogeology Branch, Flagstaff, respectively. The effect of diffusion should be taken into account Ariz.). to determine the distribution of 02 molecules. The contribution of Icarus, vol. 7, July 1967, p. 85-93. 23 refs. the solar corpuscular stream to the upper atmospheric phenomena NASA-supported research. may be appreciable, due to the lack of magnetism. On Jupiter, Investigation into the ion-molecule chemistry of the upper the molecular hydrogen IS first ionized and then decomposed to Jovian atmosphere. Experimental results show that intense UV produce the atomic hydrogen whose ionization may be responsible radiation reacts with the constituents of the Jovian atmosphere to for the formation of a dense Jovian ionosphere (pe, max - 1.5 x produce C2H4 C2H6, C3H8. and higher polymers. The general The hydrogen atoms necessary for the CH4 and NH3 107/cm3). procedure for calculating both equilibrium and nonequilibrmm reactions in the lower atmosphere might be supplied by the down- abundances of these products is formulated and applied to the case ward diffusion from here. In order to study the diffusion problems, of the surface passage of a satellite shadow. A specific example the solution of a set of relevant diffusion equations by a variational is made of ethylene, for which an analytical approximation gives method has been proposed. (Author) lolo molecules in an atmospheric column of 1 cm2 cross section after a very rapid rise to equilibrium. Such a concentration of ethylene does not substantially affect the infrared radiation in the shadow. (Author) A6744498 * GROUND INSTRUMENTATION FOR MARINER IV OCCULTATION EXPERIMENT. -Gerald S. Levy (California Institute of Technology, Jet Propulsion A67-34541 Laboratory, Communication Research Section, Pasadena, Calif. ), THE EFFECTIVE BRAKING HEIGHT FOR SMALL INTERPLANE- Tom Y. Otoshi (California Institute of Technology, Jet Propulsion TARY PARTICLES IN THE MARTIAN UPPER ATMOSPHERE. Laboratory, Communications Elements Research Section, Pasadena Uri Shafrir (Tel-Aviv University, Institute of Planetary and Space Calif.), and Boris L. Seidel (Callfornla Institute of Technology, Jet Science, Ramat Aviv, Israel). Propulsion Laboratory, Telecommunications Div., Pasadena, Icarus, vol. 7, July 1967, p. 100-104. 7 refs. Calif. ). Consideration of the dynamical interaction of small interplane- IEEE Transactions on Instrumentation and Measurement, vol. IM- tary particles vnth the Martian upper atmosphere. The equation 16, June 1967, P. 100-114. 7 refs. of motion of a small particle, entering the Martian atmosphere

51 A67-34543

with cosmic velocity, is integrated numerically in a general form A67-35315 for three Martian model atmospheres. The results of the numerical VEHICULAR DESIGN FOR A PLANETARY ATMOSPHERIC MEA- integrations are compared with similar computations carried out SUREMENT PROBE. for the earth's upper atmosphere. While in the case of the earth, P. A. Giragosian and E. T. Myers (Raytheon Co., Space and the effective braking height (EBH) is around 90 km, the different Information Systems Div., Sudbury, Mass. ). Martian density profiles yield EBH of 105, 80, and 65 km for the American Astronautical Society and NewEngland Academic models suggested by Chamberlain and McElroy, Donahue, and Community, Regional Sympos Johnson, respectively. A preliminary examination of the first physics, Boston, Mass., May 25- photograph taken by Mariner 4 during its Martian flyby, whch The problem of achieving a realist reveals the existence of light-scattering particles in the Martian vehicle to measure the sensible atmospheric properties of the atmo- upper atmosphere at altitudes of over 100 km, suggests that spheres of,Mars and Venus, using present day state-of-the-art Chamberlain and McElroy's density profile is the most probable of instrumentation. is treated. Vehicle design considerations including the three. (Author) aerodynamic, thermodynamic, heat shield material selection, flight dynamics, structures and instrumentation considerations are discussed. The atmospheric properties to be measured are the density, pressure, temperature, scale height, and gas composition. A67-34543 Use is made of a small lightweight spherical ballistic entry probe VENUS - A CONTRIBUTION TO THE GREENHOUSE-IONOSPHERE to define the structure and composition of the atmospheres of Mars DEBATE. and Venus, from the dynamlc response of the probe during the entry Reginald E. Newel1 (Massachusetts Institute of Technology, Dept. portion of flight. Onboard instrumentation, including pressure, of Meteorology, Cambridge, Mass. ). and temperature sensors, spectrographs, and accelerometers are vol. 7, July 1967, p. 114-131. 106 refs. Icarus, the sources of data. (Author) The thesis that surface temperatures of 600-1000°K can be maintained by a greenhouse effect is questioned. Ionospheric models appear to have been rejected on the basis of a single measurement. It is suggested that ionospheric and microdischarge models be re- examined and that attempts to monitor the various physical phenomena on earth be made. In particular the possibility of a radio aurora A67-35442 on Venus that emits microwaves has not yet been eliminated by ter- APPLICATION OF THE HYPERSONIC ANALOG TO THE STANDING SHOCK OF MARS. restrial measurements. If such a phenomenon were demonstrated Murray Dryer and Gary R. Hec-an (ESSA, Institute for Telecom- then Venus could be undergoing an Ice Age if the albedo is close to munication Sciences and Aeronomy, Boulder, Colo. ). 0.76 or could have temperatures similar to earth if the albedo is lower. (Author) Solar Physics, vol. 2, July 1967, p. 112-124. 27 refs. A magnetospheric boundary and its associated standing-shock wave for the earth are scaled down in size to apply to Mars. A suggestion by the Mariner 4 experimenters that their magnetometer may have detected a Martian shock at 0123 UT (earth) on July 15, 1965, is accepted. The scaling procedure used pfeviously In the case A67-34796 of the Mariner 2 flyby of Venus on Dec. 14, 1962, as well as in the RADIOASTRONOMICAL RESEARCH ON VENUS AND MARS [RADIO- present case of Mars is repeated but with a different model. We ASTRONOMISCHE UNTERSUCHUNGEN VON VENUS UND MARS]. propose a magnetospheric boundary for the earth, which is based Cornel1 H. Mayer (U.S. Navy, Office of Naval Research, Naval Re- on a maximum radius of 22 earth radii suggested by Imp-1 magnetom- search Laboratory, Washington, D. C. ). eter data. We further suggest a low value (1.2) of the adiabatic (Astronautics and Aeronautics, vol. 4, Apr. 1966, p. 13-25.) exponent, y. In addition we propose the use of the interplanetary Naturwissenschaftliche Rundschau, vol. 20, May 1967, p. 192-200. magnetoacoustic Mach number, K",which is a combination of both In German. (Translation). Alfv6n and ordinary gasdynamic Mach numbers. Our choice of values Investigation of the atmosphere and surface of Venus and Mars for these parameters is not unique since many such combinations by means of radio measurements, made chiefly with the aid of the exist which will show good agreement with observation. For example, large instruments located at Arecibo and Moscow. This method has the ratio of the Martian dipole moment to that for the earth is found proven to be especially useful in studying the planet Venus, whose to be 2.1 x by our application of the hypersonic analog. This surface is permanently hidden by a thick layer of clouds. It was found value compares very closely with 3 x 10-4 deduced as an upper bound that, with Venus as well as with Mars, the main part of radio energy by the Mariner 4 investigators. The synthesis is presented as an is reflected by smooth plain regions on the surface near the center of independent calculation based on the above theoretical considerations, the disk. The manner in which reflecting power decreases toward the together with the experimenters' probable observation of a Martian limb indicates that Venus has a smoother surface than the moon. The shock wave. (Author ) steepness of its slopes is, on the average, only half as great. The exlstence of dry minerals on Venus is indicated. The radioastronomical investigation of Mars did not give as good results as obtained with Venus, mainly due to the fact that Mars is farther away from the earth and smaller than Venus and most of the time is beyond the range of modern radiotelescopes. P.v.T. A67-35829 VOLTAGEBREAKDOWNOFMONOPOLEANTENNASINTHE ATMOSPHERES OF VENUS AND MARS. J. A. Martin and J. B. Chown (Stanford Research Institute, Menlo Park, Calif. ). A67-34933 IEEE Transactions on Antennas and Propagation, vol. AP-15, RADIOPHYSICS OF JUPITER. July 1967, p. 589, 590. 11 refs. James W. Warwick (Colorado, University, Astro-Geophysics Dept., Description of data representative of the breakdown of monopole Boulder, Colo.). antennas in simulated atmospheres of Venus and Mars. The data Space Science Reviews, vol. 6, May 1967, p. 841-891. 166 refs. correspond to gas breakdown and to static conditions for antennas Brief review of observational and theoretical developments located on the planetary surfaces and on subsonic vehicles flying regarding the nonthermal emission from Jupiter smce 1963. in the lower atmosphere of the planets. It is pointed out that bounds Emphasis is placed on new data and their phenomenological inter- on the breakdown power level of antennas operating in currently pretation. It is pointed out that the principal information still needed postulated Martian and Venusian atmospheres can be predicted by IS more refined data, especially on the fast-time resolution polarim- measurement in air (upper bound) and in pure argon (lower bound). etry and spectroscopy of millisecond bursts, and that the polarization These bounds indicate that antenna systems on or near the surface diversity on these bursts, as recorded at Arecibo, needs confirma- of Mars may be limited in available radiated power because of low tion. M. M. breakdown-power levels in the thin Martian atmosphere. M. M.

52 AM-36309 Account of an attempt to obtain UV photographs of Venus at the THE MEASUREMENT OF ABUNDANCES IN PLANETARY ATMO- same time as 3.8-cm radar cross-section measurements. The UV SPHERES USING AN IMAGE INTENSIFIER AND A SOLAR SPEC- photographs were taken with the Pic-du-Midi 108-cm reflector. S TROGRAPH. The Cassegrain focal length of 15 m was extended to 40 m with the J. E. Beckman (Oxford University, Observatory, Oxford, England). help of a simple diverging lens. There was no significant range Planetary and Space Science, vol. 15, July 1967, p. 1211-1218. difference m the simultaneous 3.8 and 23-cm data taken near infe- 16 refs. rior conjunction. The major logistic problem was with the radar Research supported by the Science Research Council. system which was involved m several experiments during this pe- r+ An image intensifier tube has been used in conjunction with the riod. One important pomt brought out by the Venus photographs solar installatlon at Oxford to obtain high resolutlon spectra of Venus made during the western elongation in 1966, is that the position of and Jupiter. The spectra of Jupiter were used to obtain the equivalent the features in the W changes inan interval of a few hours. The width of the S(1) line of the quadrupole (4, 0) band of moleEular hydro- radar observations taken so far have been limited to one measure- gen in the atmosphere of Jupiter. The result is 75 km-amagat of ment per day in order to obtain a reasonable SNR. The important hydrogen above the reflecting layer. The spectra of Venus were used point in the present context is the pertinence of the UV maps, which to set apupper limit to the abundance of oxygen in its atmosphere. have been prepared from the photographs, to future radar experz- The result is 1.75 m-amagat of oxygen above the reflecting layer. ments at short wavelength. P.v.T. (Author)

A67-37400 A67-38933 JUPITER'S GREAT RED SPOT AND THREE WHITE OVALS. PHYSICS OF PLANETS [FIZIKA PLANET]. Elmer J. Reese (New Mexico State University, Observatory, Uni- V. I. Moroz. versity Park, N. Mex.). Moscow, Izdatel'stvo Nauka, 1967. 496 p. In Russian. Sky and Telescope, vol. 34, Sept. 1967, p. 185, 186. In this book an attempt 1s made to summarlze all currently available Observationsof Jupiter's Great Red Spot and three white ovals, information on the physical characteristics of the planets of the solar revealing a strong correlation between the rotational velocity of each system, as determined by high-resolution spectroscopy, radio tele- of the three white ovals and its longitudinal distance from the Red scopes, radar and IR techniques, and photometry. Partlcular attention Spot. An analysis of more than 6000 longitude determinations made is given to the most essential problems of current interest: the between October 1955 and May 1967 indicates that during that inter- Martian atmosphere, the surface temperature of Venus and the val the white ovals rotated more rapidly when near the Red Spot than structure of the Venuslan atmosphere, the nature of the radio emis- when far away. P.v.T. sion from Jupiter, and the hypothetical Mercurian atmosphere. The problems discussed in regard to Mars include: the C02 content, total pressure, and chemical composltion of the Martian atmosphere, _I A67-37479 * cloudiness, winds, and surface temperature, the transparency and THE PRESSUREAT THE CLOUD TOPANDTHEABUNDANCEOF vertical structure of the atmosphere, the polar caps, continents, and A HYDROGEN IN THE ATMOSPHERE OF JUPITER. dark regions. With respect to Venus, the problems examined include: J. E. Beckman (Calsfornia Institute of Technology, Jet Propulsion the period of revolution, albedo, phase curve, and polarization of Laboratory, Pasadena, Calif. ). Venus; the CO2 absorption bands and GO2 dissociation; the chemical Astrophysical Journal, vol. 149, Aug. 1967, pt. 1, p. 453, 454. composition of the Venusian atmosphere and cloud cover, the temper- 10 refs. ature of Venus determined from radiation in the optical region of D Exammarion of abundance determinations In the Jovian atmo - the spectrum and the radio emission and vertical atmospheric struc- sphere. Spectra which were recorded by the Struve 82-111. telescope, ture of Venus. Information on the giant planets Includes: the with a dispersion of 3.3 Almm, show clearly the narrow lines in the various phenomena observed on the disk of Jupiter, a qualitative 6190 overtone band of methane. Methane line widths between half- chemical analysis of the Jovlan atmosphere, a quantitative iuter- intensity points were found to be 0.04 with a probable error of 15%. pretation of the spectra of Jupiter (chemical composition and pres - The average was used to set a value to the total atmospheric pressure), the temperature of Jupiter and the chemlcal composition of sure of the mean reflecting layer for light of thls wavelength, and to its cloud cover, the vertical structure of the atmosphere above fix an upper limit to the hydrogen abundance above this layer. the cloud cover, the short-wave radio emisslon and the magnetlc R.B.S. field of Jupiter, and the radio emission of Jupiter at decameter wavelengths. V.P.

A67-37480 IMPROBABILITY OF NON-THERMAL RADIO EMISSION FROM A67738999 VENUS WATER CLOUDS. TAYLOR COLUMNS. F. D. Drake (Cornel1 University. Center for Radiophysics and R. Hide (Massachusetts Institute of Technology, Dept. of Geology Space Research, Ithaca, N. Y. ). and Geophysics, Cambridge, Mass.) and A. Ibbetson (Woods Hole Astrophysical Journal, vol. 149, Aug. 1967, pt. 1, p. 459-461. Oceanographic Institution, Woods Hole, Mass. ). 16 refs. IN: MAGNETISM AND THE COSMOS; NATO ADVANCED STUDY Discussion of phenomenon discovered by Dickey (1951) and INSTITUTE ON PJANETARY AND STELLAR MAGNETISM, UNI- Sartor (1963) concerning centimeter-wavelength emission from VERSITY OF NEWCASTLE -UPON-TYNE, NEWCASTLE-UPON- charged and uncharged mercury droplets (but not water droplets) TYNE, ENGLAND, APRIL 1965, PAPERS. coming in contact with a surface or another droplet, establishing Edited by W. R. Hmdmarsb, F. J. Lowes, P. H. Roberts, and the possibil?ty of nonthermal emission. Study of this phenomenon S. K. Runcorn. leads to the concluslon that electrlcal discharges involvlng droplets New York, American Elsevier Publishing Go., Inc., 1967, p. 343- m plausible atmospheres cannot contrlbute a significant nonthermal 347. 6 refs. microwave component, thereby indicating the improbabllity of Research supported by the Royal Society of London and the Depart- nonthermal radlo emission from water clouds on Venus. R. B.S. ment of Scientific and Industrial Research; NSF Grant No. G-22390; Contracts No. AF 61(052)-216; No. Nonr-21966(00). Investigation of the theoretical criterion for the occurrence of w A67-38611 Taylor columns, involving the extension of qualitative work done by ULTRAVIOLET PHOTOGRAPHS AND THE RADAR CROSS SECTION Taylor. In one experiment, a right circular cylinder is slowly OF VENUS IN 1966. moved with uniform speed along a diameter of a rotating cylindrical C. Boyer (Toulouse, Universite, Observatoire du Pic-du-Mldi. tank of liquid; in another, a flow 1s generated by a radial arm of Bagnkres-de-Bigorre. Hautes-PyrgnGes. France) andR. E. Newel1 circular cross section, which extends along a radius from the axis (Massachusetts Institute of Technology, Dept. of Meteorology, to the rim of the tank and which rotates at (Wo + 0)rad/sec about Cambridge, Mass.). the vertical axls of the tank. Typical flow patterns observed in these Astronomical Journal, vol. 72, Aug. 1967, p. 679-681. 11 refs. experiments are illustrated. B. B. A67-39000

A67-39000 A. N. Aksenov, 2. N. Grigor'eva, N. V. Priboeva, Z. G. EXPERIMENTS ON TAYLOR COLUMNS OVER HOLES. Romanenko, and V. G: Teifel' (Akademiia Nauk Kazakhskoi SSR, C. W. Titman (Newcastle-upon-Tyne, University, School of Physics, Astronomicheskii Institut, Kazakh SSR). Dept. of Geophysics and Planetary Physics. Newcastle-upon-Tyne, Astronomicheskii Vestnik, vol. 1, July-Sept. 1967, p. 173-179. a England). 5 refs. In Russian. IN: MAGNETISM AND THE COSMOS: NATO ADVANCED STUDY Values of the photometric activity factor are determined from INSTITUTE ON PLANETARY AND STELLAR MAGNETISM, UNI- photographs of Jupiter at different wavelengths obtained €or 75 VERSITY OF NE WCASTLE -UPON-TYNE , NE WCASTLE -UPON- observational nights during the period of the planet's apparition TYNE, ENGLAND, APRIL 1965, PAPERS. in 1964-1965. A cyclic change in activity having a period of about P Edited by W. R. Hindmarsh, F. J. Lowes, P. H. Roberts, and 3 months was discovered. The periodicity is best observed in the S. K. Runcorn. long-wave region of the spectrum. The northern hemisphere of New York, American Elsevier Publishing Co., Inc., 1967, p. 348- Jupiter played the principal role in the observed changes. In the 351. 6 refs. southern hemisphere the amplitude of changes in activity was con- Derivation of the conditions under whch lengthy studies of siderably smaller, and there was no evident periodicity. In the Taylor columns over both hills and hemispheric holes can be per- second half of the period, the activity fluctuatxons were damped formed. Right clrcular cylindrical obstacles about one -eighth the but the mean value remained almost the same as in the first half. depth of fluid in a tank are placed diametrlcally opposite one another: (Author) one forming a hill, the other a hole. Dye is injected midway between the base and the lid of the tank at points above the hill and the hole, and at other positions. In the case of the cylindrical obstacles the Taylor columns appear to form cylinders circumscribing the obstacles, while the Taylor column above the hole is of a smaller A67-39556 * LIFE IN THE CLOUDS OF VENUS? radius than the hole Itself. B. B. Harold Morowitz (Yale University, Dept. of Molecular Biophysics, 1\67-3900 1 New Haven, Conn. ) and Carl Sagan (Harvard University, Harvard MODELS OF JUPITER AND SATURN. College Observatory, Smithsonian Institution, Smithsonian Astro- Wendell C. DeMarcus (Kentucky, University, Lexington, Ky. ). physical Observatory, Cambridge, Mass. ). IN: MAGNETISM AND THE COSMOS; NATO ADVANCED STUDY e,vol. 215, Sept. 16, 1967, p. 1259, 1260. 14 refs. NASA-supported research. INSTITUTE ON PLANETARY AND STELLAR MAGNETISM, UNI- Speculation an indigenous biology in the clouds of Venus VERSITY OF NEWCASTLE -UPON-TYNE , NEWCASTLE -UPON- on A TYNE, ENGLAND, APRIL 1965, PAPERS. involving the stirring up of minerals from the planet's surface. postulated photosynthetic organism could reside just below the Edited by W. R. Hmdmarsh, F. J. Lowes, P. H. Roberts, and S. K. Runcorn. Venus clouds, or in the lower cloud deck. Water would be collected New York, American Elsevier Publiihmg Co., Inc., 1967, p. 352- either as rain or by contact with the droplets, and minerals blown up 364. 23 refs. from the surface could be captured on the sticky underside of the organism, and ingested by pinocytosis. B.B. Discussion of observational material bearlng on Jupiter and Saturn. An attempt is made to see how large a reduction of manifold size is achieved by the addition of each observational piece of evidence. It is pomted out that the gross structure of Jupiter and Saturn and also their hydrogen abundances seem fairly well determined by 4 those data which are easiest to interpret - namely, mass, volume, A67-40094 *# and the external potential coefficient. However, precise models A RADIO OCCULTATION EXRERIMENT TO PROBE THE ATMO- of the density and composition distributions would not seem to be SPHERE OF VENUS. attamable at the present time. The best provisional models are Arydas Kliore, Dennis A. Tito. Dan L. Cain (California Institute undoubtedly those of Peebles. Trustworthy model atmospheres are of Technology, Jet Propulsion Laboratory, Systems Analysis Re - not available at present. M.M. search Section, Pasadena, Calif.), and Gerald S. Levy (California Institute of Technology, Jet Propulsion Laboratory, Communications A67-39092 Elements Research Section, Pasadena, Calif. ). JUPITER - A WORTHY GOAL FOR SPACE RESEARCH AND AS- (American Institute of Aeronautics and Astronautics, Aerospace Sciences Meeting, 5th. New York, N.Y., Jan. 23-26, 1967, TRONAUTICS [JUPITER - EIN LOHNENDES ZIEL DER WELT- RAUMFORSCHUNC UND RAUMFLUGTECHNIK]. Paaer. .. 67 -118. ) vol. 4, Oct. 1967, p. 1339-1346. Wolfgang Kokott (BGlkow GmbH, Ottobrunn, West Germany). Journail of Spacecraft and Rockets, DGRR, Mitteilungen, vol. 20, Aug. 1967, p. 3-6. 8 refs. In 30 refs. German. [For abstract see issue 06, page 1085, Accession no. A67-183101 Review of the present state of knowledge regarding the planet Jupiter, as a basis of further research. While interplanetary investigations in the U.S. and USSR are mainly concentrated on Mars and Venus, research on the planet Jupiter is recommended for German and other continental European scientists. With an equatorial diameter of 142, 700 km, Jupiter is the largest planet of the A67-40120 # solar system. Its white bands and Great Red Spot are well known ON VENUS RADIATION SPECTRUM IN MILLIMETER RANGE [O features. The atmosphere of Jupiter is believed to contain great MILLIMETROVOM SPEKTRE IZLUCHENIIA VENERY]. quantzties of hydrogen and helium, and Its interior probably also A. P. Naumov and M. B. Kanevskii (Gor'kovskli Gosudarstvennyi contains these elements. Jupiter is the only planet other than the Universitet, Nauchno-Issledovatel' ski1 Radiofizicheskii Jnstitut, earth known to have a magnetic field and a radiation belt. Jupiter Gorki, USSR). has 12 satellites: 5 inner moons, 3 central moons, and 4 outer (Vsesoiuznaia Konferentslia PO Radioastronomii. 5th, Kharkov, moans (the latter believed to be asteroids captured by the gravita- Ukramian SSR, Oct. 18-22, 1965.) tional field of Jupiter). Many questions remain unresolved, among Radiofizika, vol. 10, no. 8, 1967, p. 1058-1069. 31 refs. In Russian. them the interior structure of Jupiter, the nature of the Great Red For a number of models of the Venus atmosphere, the bright- P.v.T. Spot, and the cosmogony of the planet and its satellites. ness temperature has been calculated in u = 48-72 Gc range in which the presence of a thin structure of the planet radiation spectrum A67-39299 +t caused by molecular oxygen may be expected. In some cases the THE ATMOSPHERIC ACTlVITY OF JUPITER IN 1964-1965 AC- brightness temperature is found to fall at the resonance frequencies by-20-900K, due to oxygen presence. It is noted that the experi- CORDING TO DATA OF PHOTOMETRIC OBSERVATIONS [AT- I MOSFERNAIA AKTIVNOST' IUPITERA V 1964-1965 gg. PO mental information of the physical conditions on the planet may be DANNYM FOTOMETRICHESKMH NABLNDENII]. obtained in the spectral region ~~48-72Gc. (Author )

54 A67-41836

A67-40140 * Discussion of the aerodynamic characteristics of a small, THE ATMOSPHERE OF MARS - A DERIVATION OF ENGINEERING lightweight probe in the form of a spherical entry vehicle which, AND DESIGN PARAMETERS. from the dynamic response of the probe durmg entry. defines the * George S. West, Jr. and W. T. Roberts (NASA, Marshall Space structure and composition of a planetary atmosphere. The following Flight Center, Aero -Astrodynamics Laboratory, Aerospace Environ- factors were considered and led to the conclusion that a spherical ment Div., Space Environment Branch, Huntsville, Ala.). shape was the optimum shape for the probe: (1) drag factors, (2) IN: AMERICAN ASTRONAUTICAL SOCIETY, SOUTHEASTERN static stability, (3) dynamic stability, (4) entry trajectory, (5) pres- SYMPOSIUM ON MISSILES AND AEROSPACE VEHICLES SCIENCES, sure distribution over a sphere, (6) shock-standoff distance and 4 HUNTSVILLE, ALA., DECEMBER 5-7, 1966, PROCEEDINGS. shape, (7) gasdynamic effects on vehicle stability, (8) flowfield VOLUME 2. properties, and (9) effect of residual and induced spin rate. Symposium sponsored by the American Astronautical Society, the University of Alabama, NASA Marshall Space Flight Center, .and R.B.S. the Missile Command of the U. S. Army. Huntsville, Ala. , American Astronautical Society, Southeast Section, A67-40799 * 1966, p. 58-1 to 58-11. 11 refs. MARTIAN IONOSPHERE - A COMPONENT DUE TO SOLAR PROTONS. Study sf the atmosphere of Mars, taking into account the Carl Sagan and Joseph Veverka (Harvard Unlversity; Smithsoman gravitational and magnetic fields, and their mteraction with the Institution, SmithsonIan Astrophysical Observatory, Cambrldge, atmosphere of the planet. Since the upper atmosphere of a planet Mass. ). is subject to diurnal, latitudinal and solar cyclic variations, three Science, vol. 158, Oct. 6, 1967, p. 110-112. 22 refs. atmospheric models (high, mean, and low density) were generated Grant No. NGR-09-015-023. with the suggestion that the mean density model be used for design, Contention that some component of the observed Martlan atmo- and that the design should be critically tested to verify its survival sphere, perhaps the subsidiary maximum at an altitude of 95 km, is in either of the other atmospheric models. It is not expected that due to penetratlon of protons from the solar wind into the Martian orbiters of the planet Mars will encounter excessive drag for the atmosphere. The proton ionization should be more nearly isotroplc lower-density model, since the atmospherlc density at 100 kin on and much more time-varlable than the electromagnetic contributlon. Mars IS about the same as that at 300 km on earth. Above this Therefore, observations at a range of local times during a Martian altitude, the atmospheric density for Mars falls off at a much faster day, and over a period including several solar events, seem indi- rate than It does on earth. This is due to the relatively low tempera- cated. Such observations cannot readily be performed by a flyby tures between LOO and 200 km. This atmosphere 1s found to vehicle, but represent a natural radio-occultation experiment for stabilize by about 1000 km because of the high temperatures en- a small Mars orbiter. The low surface magnetic-fleld strength of countered. P.v. T. Venus suggests that solar protons may also be producing ionization in the atmosphere of that planet. Forthcoming radio-occultation experiments near Venus by flyby and projected orbiter vehlcles will be useful in examining this possibility. P.v.T. , A67-40141 * ENVIRONMENT OF JUPITER. Carroll L. Hasseltine (NASA, Marshall Space Flight Center, Aero- Astrodynaniics Laboratory, Aerospace Environment Div., Space A67-40999 Environment Branch, Huntsville, Ala. ). * LIFE DETECTION BY ATMOSPHERIC ANALYSIS. AMERICAN ASTRONAUTICAL SOCIETY , SOUTHEASTERN IN. Dian R. Hitchcock (United Aircraft Gorp., Hamilton Standard Div., 1* SYMPOSIUM ON MISSILES AND AEROSPACE VEHICLES SCIENCES, Windsor Locks, Conn.) and James E. Lovelock (Californra Institute HUNTSVILLE, ALA., DECEMBER 5-7, 1966, PROCEEDINGS. of Technology, Jet Propulsion Laboratory, Bio-Science Section, VOLUME 2. Pasadena, Calif. 1. Symposium sponsored by the American Astronautical Society, the Icarus, vol. 7, Sept. 1967, p. 149-159. 16 refs. University of Alabama, NASA Marshall Space Flight Center, and Contract No. NASw-871. the Missile Command of the U.S. Army. Living systems maintain themselves in a state of relatively low Huntsville, Ala., American Astronautical Society, Southeast Section, entropy at the expense of their nonliving environments. We may 1966, p. 59-1 to 59-9. assume that this general property is common to all life m the solar Study of the planet Jupiter, Its atmosphere, and Its atmospheric system. On this assumption, evidence of large chemical free temperatures. Jupiter's huge mass gives the planet an acceleration a energy gradient between surface matter and the atmosphere in due to gravity at the poles of more than two and one half times that contact with It is evrdence of life. Furthermore, any planetary biota of the earth. Its rotation period of about 9 hr 55 mm 1s the smallest whlch interacts with its atmosphere will drive that atmosphere to a of all the planets and creates phenomena unique to Jupiter. The state of disequilibrium which, if recognized, would also constitute planet's high rotation rate causes the shape of the planet to deviate direct evidence life, provided the extent of the disequilibrium IS from a true sphere: a distinct flattening of the poles is visible. of signlficantly greater than abiological processes would permit. It Light and dark bands of clouds (zones and belts) run parallel to the is shown that the existence life on the earth can be mferred from equator. It has been confirmed that hydrogen and helium are the of knowledge of the xnaJor and trace components of the atmosphere, even dommant gases of the Jovian atmosphere. Thornton and Welch (1963) estimated the temperature of the Jovian cloud tops to be in the absence of any knowledge of the nature or extent of the dominant life forms. Knowledge of the compositlon of the Martian atmosphere 144 f 23'K based on their measurement made at 8.35 mm wave- may similarly reveal the presence of llte there. (Author) length. Temperatures are believed to mcrease with depth below the ammonia cloud tops. P.v.T.

8677-40177 A67-41836 * AEROTHERMODYNAMIC CONSIDERATIONS FOR A PLANETARY AN UPPER LIMIT FOR ATMOSPHERIC CARBON DIOXIDE ON ENTRY PROBE. MERCURY. P. A. Giragosian and E. T. Myers (Raytheon Co., Space and Jay T. Bergstralh, Harlan 3. Smith (Texas, Umversity, Dept. of Information Systems Div., Sudbury, Mass.). Astronomy, McDonald Astronomical Observatory, Fort Davis, IN: AMERICAN ASTRONAUTICAL SOCIETY, SOUTHEASTERN Tex.), and Louise D. Gray (Texas, University, Dept. of Astronomy, = SYMPOSIUM ON MISSILES AND AEROSPACE VEHICLES SCIENCES, McDonald Astronomical Observatory, Fort Davis, Tex., Californla HUNTSVILLE, ALA., DECEMBER 5-7, 1966, PROCEEDINGS. Institute of Technology, Jet Propulsion Laboratory, Pasadena, VOLUME 2. Callt.). Symposium sponsored by the American Astronautical Society, the Astrophysical Journal, vol. 149, Sept. 1967, pt. 2, p. L137-LI39. University of Alabama, NASA Marshall Space Flight Center, and 7 refs. the Missile Command of the U.S. Army. Determination of the upper limit of C02 in the atmosphere of ~ Huntsville, Ala., American Astronautical Society, Southeast Section, Mercury. It is reduced sharply due to the strength of the 12,000-A 1966, p. 96-1 to 96-12. 45 refs. C02 bands which now can be reached at high dispersion. An upper

55 A67-42325 limit of 0.58 m-atm is assigned to the abundance of C02 on Mercury during the observations, which implies an upper limit during March and April 1967 of about 0.04 mb to the surface partlal pressure of GO2. B. B. hr

A67-42325 * # PLANETARY ATMOSPHERES AND THE ORIGIN OF THE MOON. 6 A. G. W. Cameron (NASA, Goddard Space Flight Center, Goddard Institute for Space Studies, New York, N. Y. ). IN: THE EARTH-MOON SYSTEM; PROCEEDINGS OF AN INTER- NATIONAL CONFERENCE, NASA GODDARD INSTITUTE FOR SPACE STUDIES, NEW YORK, N. Y., JANUARY 20, 21, 1964. Conference sponsored by the NASA Goddard Institute for Space Studies. Edited by B. G. Marsden and A. G. W. Cameron. New York, Plenum Press, Division of Plenum Publishing Corp., 1966, p. 234-273. 32 refs. Discussion of the origin of the earth-moon system. Following a hypothetical description and analysis of the atmosphere of Venus (somewhat anachronistic at this point) and a theory concerning the origin of the earth's atmosphere, it is hypothesized that the moon was formed from terrestrial material ejected from the earth during a process of rotational instability. For the purpose of the hypothesis it is assumed that the rotational instability would be triggered by the formation of the iron core in an elongated Jacobi ellipsoid. Objec- tions are presented to this hypothesis and to other theories concerning the atmosphere of the earth and Venus, as stated by MacDonald (1964). R. B. S.

A67-42399 * #t THE EVOLUTION OF THE MARINER SPACECRAFT. J. James (California Institute of Technology, Jet Propulsion Labora- tory, Pasadena, Calif. ). International Astronautical Federation, International Astronautical Congress, 18th, Belgrade, Yugoslavia, Sept. 24-30, 1967, Paper. 15 I). Discussion of the Mariner series of space vehicles. The evolution of the Mariner designs is outlined, and the conversion of the Mariner Mars vehicle of 1964 to the Venus spacecraft of 1967 is described. It is concluded that the most significant contrzbution of the Mariner-series vehicles to future space flights has been the atmospheric density measurements made by Mariner 4 as it occulted Mars; data derived from this event have radically changed the design of future entry missions, especially those involving the survival of large instrument packages on the Martian surface. B.B.

867-42963 *# CURRENTANDFUTUREPROBLEMSINEARTHANDPLANETARY ATMOSPHERE ENTRY. Alvin Seiff (NASA, Ames Research Center, Vehicle Environment Div., Moffett Field, Calif.). American Institute of Aeronautics and Astronautics, Annual Meeting and Technical Display, 4th, Anaheim, Calif., Oct. 23-27, 1967, Paper 67-803. 11 p. 19 refs. Members, $1.00, nonmembers, $1. 50. Five problems are selected for review to indicate the present status of atmosphere entry technology. The problems selected are (1) high speed and low Reynolds number effects on aerodynamics of blunt, lifting entry vehicles, (2) radiative heatrng of blunt bodies used as planetary return vehicles, (3) problems of ablation heat shields rn tevere heating environments, (4) effects of ablation on dynamics of slender entry vehicles, and (5) transonic dynamic stability of large-angled conical bodies. This selection represents the subject area6 - aerodynamic forces, static and dynamic stability, heating, heat protection, and a phenomenon in which several of these areas interact. The effects of ablation on slender vehicle dynamics, the behavior of heat sbelds rn severe environments, and the intense radiative exposure of blunt vehicles at r manned planetary return velocities are the only problems that seem to present fundamental difficulties for future vehicles. (Author)

56 A67-809 16

1966 1967

4. AEROSPACE MEDICINE AEROSPACE MEDICINE AND BIOLOGY ABSTRACTS AND BIOLOGY ABSTRACTS

~ij6-sii45 A67-80329 TIJF GRFCNIIO1'SE FFFECT IN A GRAY FI ANETARY ATMOSPHERE. MARTIAN ATMOSPHERE AND CRUST. Hupert Wildt (Yale L'. Ohs., Nev Haven, Conn.; and Goddard Inst. for Space S Miyamoto (Kyoto U , Kwasan Obs ,Japan) Studies, New York, A. Y.) Icarus,vol. 5, Jan. 1966,~.24-33. 6 refs. Icarus, vol 5, Jul 1966, p 360-374 29 refs N Y Acad of tlopf's analyrical solution Is illustrated for several values of the green- Sa, Ore U , and Dr James Q Gant supported research house parameter, Le., the ratio of gray absorption coefficients for insolating The Martian atmosphere in its average condition IS inactive and escapfng radiation, assumed to be constant at all depths. Ps the famflllu and transparent to long-wave radiation It is activated when planetary atmospheres are nongray in the extreme, this model of the greenhouse effect does not contribute much to understanding thet temperature moisture is supplied by the evaporation of the polar cap in spring regime; but, to date, it Is the only problem in planetary radiative equilibrlum time As typical examples, the great yellow cloud in 1956. the which has been solved rigorously. Neith-Casius cloud, and the Propontis cloud are described It IS shown that we can derive some knowledge about surface relief indirectly from cloud observations In the Martian summer. energy flows from the summer hemisphere to the winter hemisphere and the prevailing wind over middle latitudes turns from spring AM-81966 westerlies to summer easterlies This prediction has been con- ON THE ABUNDANCE OF EARTH-LIKE PLANETS. firmed through the following observations a springtome polar F. J. Donahoe (Wilkes Coll., Wilkes-Barre, Pa.) front and associated dark fringe, some peculiar behavior of the Icerus.vol. 5. May 1966. p. 303-304. 5 refs polar cap shrinking, and the summertime diagonal cloud layers Earth-like planets may be more of a rarity than they were A tentative picture of the circulation pattern in the northern thought to be. The only other planet of the solar system which hemisphere IS proposed on the basis of our cloud data Crater is large enought to retain for eons gases other than hydrogen morphology revealed by the Mariner IV photographs suggests * and helium is Venus. It is hypothesized that the Earth's early that craters are one of the characteristic features of the original encounter with the Moon dispersed the gases of the proto- crust of terrestrial-type planets and that Martin deserts and maria Earth's atmosphere. Planets of approximately Earth mass correspond to the terra and maria of the Moon and the continents and oceans of our Earth, respectively Canals are interpreted as should be Venus-like rather than Earth-like unless they form tectonic lines It may be shown how wind erosion destroys most part of a double planet. of the tectonic lines but develops some of them into canals when they are properly located along the courses of vapor migration

A66-81851 EFFECTS OF ULTRA-VIOLET ALONE AND SIMULATED SOLAR ULTRA-VIOLET RADIATION ON THE LEAVES OF A6740916 HIGHER PLANTS. VENUS: ATMOSPHERIC EVOLUTION. Morris G Cline (Calif lnst of Technol, Div of Biol. Pasa- Margaret 0 Dayhoff. Richard V. Eck (Natl. Biomed Res Found, Silver Spring, Md.). Ellis R. Lippincott (Md. U, Dept. dena) and Frank B Salisbury (Utah State U . Plant Sci Dept , Logan) of Chem., College Park), and Carl Sagan (Harvard U and Smithsonian Astrophys. Obs., Cambridge. Mass.). Nature, vol 21 1. Jul 30 1966. p 484-486 12 refs Science,vol. 155, Feb 3. 1967. p 556-558. 22 refs NASA supported research NASA Contract 21-003-002. NASA Grants 21-002-059 Leaf-survival experiments involving 67 species with spe- and NGR09-015-023 cial emphasis on Xanthium pennsylvanicum, Zea mays, and Because of the high temperatures prevailing in the lower Anus nigra were conducted after ultra-violet light alone and atmosphere of Venus. its chemistry is dominated by the ten- after high-intensity simulated solar spectrum In the first dency toward thermodynamic equilibrium. From the atomic experiment. there was a wide variation in the resistance of composition deduced spectroscopically, the thermodynamic the species tested In the second experiment. the total radia- equilibrium composition of the atmosphere of Venus is com- tion levels were equivalent to those above the atmosphere of puted. and the following conclusions drawn (1) There can be Mars. Earth. and Venus (086, 2 00. and 3 82 cal /cm 2/min I no free carbon, hydrocarbons, formaldehyde. or any %her 4 respectively) Xanth/um leaves were killed after 1 8 hr of organic molecule present in more than trace amounts. (2) Venusian-level radiation but leaf-kill by Martian-level radiation The original atomic composition of the atmosphere must have required 4 5 hr Destruction of exposed leaf blades of week- included much larger quantities of hydrogen and a carbon/ old Zea plants required 8 hr of Venusian-lever radiation and oxygen ratios0.5. (This ratio is now almost precisely 0.5.) (3) 32 hr of Martian-level radiation Pinus seedlings showed no The present atomic proportions of the atmosphere of Venus serious damage until nearly 100 hr of Venusian-level radia- are so unique that an evolutionary mechanism involving two tion and 400 hr (30 days) of terrestrial-level radiation independent processes seems necessary, as follows. Water,

57 A67-80916 originally present in large quantities, has been photodissociated in the upper atmosphere, and the resulting atomic hydrogen has been lost in space. The resulting excess oxygen has been very effectively bound to the surface materials. (4) There must be some weathering process, for example, violent wind erosion, to disturb and expose a sufficient quantity of reduced surface material to react with the oxygen produced by photodissociation.

58 , ect Index

I( PLANETARY ATMOSPHERES / a continuing bibliography with indexes JULY 1968

Typical Subject Index Listing

SECTION AND ATMOSPHERIC ATTENUATION Ab7-16290

ABSORPTION SPECTRUU I URANUS AND NEPTUNE SPECTRAL ABSORPTIONS COMPARED HITH LABORATORY SPECTRA OBTAINED WITH VERY LONG OPTICAL PATHS INDICATE METHANE ROLE IN PLANETARY ABSORPTION Ab7-21213

ABSORPTION SPECTROSCOPIC DETERMINATION OF WATER VAPOR ABUNDANCE IN MARTIAN ATMOSPHERE The subject heading is a key to the subject content of the document. The Nota- Nb7-12668 tion of Content INOC). rather tRan the title of the document, is used to provide a more exact description of the subject matter When it appears. the report/ MODELS THAT ASSUME MARS ATMOSPHERE HAS ABSORPTIVE meeting paper number may provide a clue to the type of document cited (e g . RATHER THAN SCATTERING PROPERTIES. AND THAT NASA report. NASA contractor report, conference paper, translation) The ac- REDNESS OF PLANET IS DUE TO SELECTIVE ABSORPTION cession number provides a key to the location of the citation in the abstract Nb7-16808 section Under each subject heading. the Notations of Content for published literature references (A67) are listed first followed by report references lN67). MARTIAN AN0 CYTHEREAN ATMOSPHERIC COMPOSITION each set of references is arranged in ascending accession number order DETERMINATIONS USING ENTRY PROBE MEASUREMENTS OF ULTRAVIOLET AND X-RAY ATTENUATION DAC-60627 Nb7-33758

A ACC ELERAT ION ABLATION PLANETARY ATMOSPHERE STRUCTURE DETERMINED FROM MARS ATMOSPHERIC COMPOSITION AND LAMINAR ENTRY VEHICLE ONBOARD MEASUREMENTS OF PRESSURE, CONVECTIVE HEATING AND ABLATION STUDIED TO PREDICT TEMPERATURE, AND ACCELERATION .) PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING NASA-TN-0-3933 Nb7-23302 ENTRY Abb-25274 ACOUSTIC IUPEDANCE MARS ATMOSPHERIC COMPOSITION AN0 LAMINAR GASEOUS COMPOSITION OF UNKNOWN PLANETARY CONVECTIVE HEATING AN0 ABLATION STUDIED TO PREDICT ATMOSPHERE OETERMINEO. USING ACOUSTIC EXPERIMENT PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING COMBINED WITH PRESSURE AND TEMPERATURE DATA xt ENTRY Ab7-18849 Ab7-13215

ABSORPTION BANO AERODYNAMIC CHARACTERISTICS IMAGE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL SPHERICAL ENTRY VEHICLE USE0 TO DEFINE PLANETARY VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN ATMOSPHERE STRUCTURE AN0 COMPOSITION FROM DYNAMIC DISK IN NEAR IR REGION Abb-37017 RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC CHARACTER1STICS Ab7-40177 RANDOM ELSASSER BANO MOOEL TO COMPUTE ATMOSPHERIC TRANSMISSION OF EARTH AND MARS FOR 2-MICRON EXPANDABLE, TERMINAL DECELERATORS FOR MARS CARBON DIOXIDE BANDS ATMOSPHERE ENTRY JPL-TR-32-969 Abb-30024 NASA-CR-79496 Nb7-12052

NEW ABSORPTION BANDS IN NEAR IR SPECTRUM OF MARS AERODYNAHIC FORCE FOUND BY FOURIER SPECTROSCOPY VIA CARBON DIOXIDE EARTH AND PLANETARY ATMOSPHERE ENTRY PROBLEMS FOR ABSORPTION MEASUREMENTS Ab 6-4048 6 BLUNT NOSED SLENDER VEHICLES NOTING AERODYNAMICS. STABILITY, HEATING, ABLATION AND INTERACTION OF ABSORPTION LINES ON VENUS SPECTROGRAMS OF EFFECTS ROTATIONAL FINE STRUCTURE OF EXCITE0 VIBRATIONAL AIAA PAPER 67-003 Ab7-42963 TRANSITION OF CARBON DIOXIDE A66-41016 AERODYNAMIC HEATING SELF-BROADENING COEFFICIENTS OF SPECTRAL LINES AERODYNAMIC. THERMODYNAMICS HEAT SHIELD AN0 OF ABSORBING ATMOSPHERIC GASES MEASURED IN STRUCTURAL DESIGN ASPECTS OF BALLISTIC VEHICLE COMPARISON WITH LINE BROADENING EFFECTS’ OF ENTERING PLANETARY ATMOSPHERE 167-35315 NITROGEN Ab?-22715 AERONOMY ABSORPTION COEFFICIENT PHOTOCHEMISTRY OF PLANETARY GASES AN0 PLANETARY INDUCE0 ABSORPTION COEFFICIENTS IN ATMOSPHERE AERONOMY MDOEL MEASURE0 FOR CALCULATION OF VENUS LOWER NASA-CR-81262 Nb7-16515 ATHOSPHERE PROPERTIES FROM RADIO OBSERVATIONS Ab7-12949 EXPERIMENTAL AND THEORETICAL STUDIES IN PLANETARY AERONOMY DIELECTRIC RELAXATION OF GASES AN0 SHARP RISE IN NASA-CR-82937 ~67-19929 MICROWAVE ABSORPTION COEFFICIENT IN CYTHEREAN .e ATMOSPHERE ~,-1-21372 AEROSOL RADIO ASTRONOMICAL OBSERVATIONS OF VENUS - UPPER LIMITS ON LIQUID WATER CONTENT IN VENUS AEROSOL ATMOSPHERIC MODEL FOR EXPLAINING RADIO ATMOSPHERE Ab7-32652 SPECTRUM Nbb-31470

ABSORPTION CROSS SECTIDN WATER CONTENT OF VENUS ATMOSPHERE, AEROSOLSI AN0 .I RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW PRESSURE IN UPPER CLOUD LAYER, AN0 DEVIATIONS IN VALUE OF CROSS SECTION, ECHO SPECTRUM, DIRECTION OF POLARIZED LIGHT Nbb-3147 1 POLARIZATION CHARACTERISTICS, ABSORPTION CROSS AEROTHERMOOYNAMICS SUBJECT INDEX

PHOTOME TR I C ANALYSIS OF AEROSOL COMPONENT OF MARS MARTIAN ATMOSPHERE CIRCULATION MODEL FROM NARINER ATMOSPHERE N67-16810 IV OCCULTATION EXPERIMENT, STUDYING LATERAL EDDY VISCOSITY, WINOSI SURFACE TEMPERATURE AN0 STRESS DISCREPANCY BETWEEN MARS ATMOSPHERIC PRESSURE 167-34153 DATA FROM SPECTROSCOPIC MEASUREMENTS AN0 FROM PHOTOMETRIC AN0 POLARIMETRIC OBSERVATIONS JUPITER AN0 SATURN MOOELSs GIVING PLANET t N61-16811 CONSTITUTION. HEAT BALANCE AN0 ATMOSPHERIC COMPOSITION A67-39001 AEROTHERMODYNAMICS SPHERICAL ENTRY VEHICLE USE0 TO DEFINE PLANETARY ASTRONOMICAL PHOTOGRAPHY ATMOSPHERE STRUCTURE AN0 COMPOSITION FROM DYNAMIC RAPID DRIFT IN LONGITUDE OF SMALL DARK SPOT ON L RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC SOUTH EDGE OF JUPITER NORTH TEMPERATE BELT. CHARACTERISTICS A67-40177 NOTING SINUSOIDAL DISPLACEMENT CHARACTERISTICS AN0 MEASUREMENT WITH BLUE AN0 UV PHOTOGRAPHY AIR SAMPLING A66-33009 EIARTIAN ATMOSPHERE SAMPLING BY SENSORS OF PARACHUTE DROPPED CAPSULE Nb6-32064 RETROGRADE ROTATION OF CLOUD FORMATIONS OF VENUS WITH ANGULAR VELOCITY CORRESPONDING TO ONE AIRGLOW ROTATION IN FOUR DAYS ANALYZED BY HIGH RESOLUTION LUMINESCENCE FROM LOWER ATMOSPHERIC LAYERS AN0 PHOTOGRAPHY A66-41181 IONOSPHERE OBSERVED IN VENUS NIGHT AIRGLOW Nb7-16803 MARTIAN ATMOSPHERE TRANSPARENCY AN0 VISIBILITY OF SURFACE DETAILS IN BLUE AND UV LIGHT, SHOWING ALBEDO DARK AN0 SEMITONE AREAS INTENSITY, ETC CURVES OF MONOCHROMATIC ALBEDO FOR LIMB AN0 A67-34154 TERMINATOR OF VENUS N61-16806 MULTICOLOR PHOTOGRAPHIC AN0 VISUAL PATROL OF ALKANE ATMOSPHERE AN0 SURFACE OF MARTIAN NORTHERN STATISTICAL DECISION THEORY APPLIED TO MARTIAN HEMISPHERE DURING SPRING AN0 SUMMER OF 1964-1965 ATMOSPHERE ANALYSIS, LIFE DETECTION EXPERIMENTS, APPARITION AN0 GAS CHROMATOGRAM MEASUREMENTS OF N-ALKANE NASA-CR-83123 N67-21180 DISTRIBUTIONS IN MATERIALS NASA-CR-77234 N66-34667 ASTRONOMICAL PHOTOMETRY IMAGE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL AMINO ACID VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES DISK IN NEAR IR REGION A6b-37011 AND IN ORIGIN OF ORGANIC MATTER - OETERMINATION OF AMINO ACID PAIRING AN0 SEQUENCES IN PROTEINS SCATTERING ANISOTROPY EFFECT ON OPTICAL PARAMETERS NASA-CR-74559 N66-28800 OF MARTIAN ATMOSPHERE AND SURFACE - PHOTOMETRY Nbl-16620 y* ANGULAR VELOCITY RETROGRADE ROTATION OF CLOUD FORMATIONS OF VENUS ATNOSPHERIC BRIGHTNESS OF MARS DETERMINED BY WITH ANGULAR VELOCITY CORRESPONDING TO ONE POLARIMETRIC AN0 PHOTOMETRIC MEASUREMENTS ROTATION IN FOUR DAYS ANALYZED BY HIGH RESOLUTION TR-34 Nbl-24229 PHOTOGRAPHY A66-41181 ASTRONOMICAL SPECTRUM *) JUPITER GREAT REO SPOT AN0 THREE WHITE OVALS SPECTRAL STUDY OF JUPITER, SATURN AND RINGS OF SHOW CORRELATION BETWEEN OVAL ROTATIONAL VELOCITY SATURN. DETERMINING METHANE CONCENTRATION IN AND LONGITUDINAL DISTANCE FROM REO SPOT CLOUD LAYERS A66-37035 Abl-37400 ABUNDANCE AN0 TEMPERATURE OF CARBON DIOXIDE IN ANISOTROPY MARTIAN ATMOSPHERE, NOTING IMPLICATIONS. SCATTERING ANISOTROPY EFFECT ON OPTICAL PARAMETERS OBSERVATION METHODS AN0 RESULTS OF MARTIAN ATMOSPHERE AN0 SURFACE - PHOTOMETRY A6b-39558 N67-16820 NEW ABSORPTION BANDS IN NEAR IR SPECTRUM OF MARS APPROXIMATION METHOD FOUND BY FOURIER SPECTROSCOPY VIA CARBON DIOXIDE APPROXIMATION FORMULA DESCRIBING MONOCHROMATIC ABSORPTION MEASUREMENTS 166-40486 TRANSMISSION, REFLECTION. AN0 ABSORPTION OF VENUS CLOUD LAYER Nb6-31641 ABSORPTION LINES ON VENUS SPECTROGRAMS OF ROTATIONAL FINE STRUCTURE OF EXCITED VIBRATIONAL APPROXIMATION METHODS FOR SOLUTION OF EQUATION OF TRANSITION OF CARBON DIOXIDE Abb-418 16 RADIATIVE TRANSFER IN PLANETARY ATMOSPHERES Nbb-33534 PLANETARY ATMOSPHERE RESOLUTION SPECTRUM NOTING CARBON DIOXIDE LINES, RADIATION TRANSFER. INVARIANT IMBEDDING EQUATIONS FOR DETERMINING COMPOSITION, TEMPERATURES, PRESSURES, ETC VERTICAL STRATIFICATION OF TERRESTRIAL AN0 A66-42667 PLANETARY ATMOSPHERES ON BhSIS OF SATELLITE OBSERVATIONS VENUS ATMOSPHERE NOTING PRESSURE INDUCE0 RM-5229-PR Nb7-32463 ABSORPTION IN CARBON DIOXIDE-NITROGEN ATMOSPHERE AS INDICATED IN DECLINE OF MICROWAVE BRIGHTNESS ARGON TEMPERATURE Ab6-42668 GASEOUS BREAKDOWN OF SIMULATED PLANETARY ATMOSPHERES AN0 ILLUSTRATION OF GREENHOUSE WATER VAPOR LINES IN SPECTRUM OF VENUS OBTAINED EFFECT, THERMAL RADIATION FROM IONIZED ARGON, BY PHOTOELECTRIC SCqNNING OF SPECTRUM LIQUID MAGNETOHYDRODYNAMIC POWER CONVERSION A67-11769 Nb7-23655 MEAN VALUES OF METHANE WAVELENGTHS IN URANUS ASTRONOMICAL COORDINATE SPECTRUM MEASURED FOR OETERMINATION OF ATMOSPHERIC Ih LATITUDE AN0 LONGITUDE OF JUPITER RED SPOT TEMPERATURE A67-14327 MEASURED FROM PHOTOGRAPHS OBTAINED DURING 1965 AN0 1966 SPECTRAL STUDY OF JUPITER, SATURN AN0 RINGS OF NASA-CR-85560 N67-31108 SATURN. DETERMINING METHANE CONCENTRATION IN CLOUD LAYERS A61-15557 ASTRONOMICAL MODEL M DISCRETE EQUILIBRIUM TEMPERATURES OF HYPOTHETICAL PHOTOMETRY OF INTEGRATED LIGHT OF VENUS. PLANET WITH ATMOSPHERE AN0 HYDROSPHERE OF ONE- INFERRING PRESENCE OF ICE IN ATMOSPHERE FROM HALO COMPONENT TWO-PHASE SYSTEM UNDER CONSTANT SOLAR EFFECT OF BRIGHTNESS DISPERSION RADIATION Abl-21462 A67-16407

1-2 SUBJECT INDEX ATMOSPHERE MODEL

URANUS AN0 NEPTUNE SPECTRAL ABSORPTIONS COMPARED RADAR, RADIO ASTRONOMIC AN0 IR SPECTROSCOPIC WITH LABORATORY SPECTRA OBTAINED WITH VERY LONG OBSERVATIONS OF VENUS SURFACE AND ATMOSPHERE, OPTICAL PATHS INDICATE METHANE ROLE IN PLANETARY EXAMINING GENERAL AN0 SURFACE DATA, CHEMICAL ABSORPTION Ab7-2 1213 COMPOSITION AN0 ATMOSPHERIC MODEL CONSTRUCTION 667-24843 d CARBON DIOXIDE STUDY IN MERCURY ATMOSPHERE YIELDS NEGATIVE RESULTS FROM OBSERVATIONS MADE WITH IR MAGNETOSPHERIC MODEL OF JUPITER FROM NUMERICAL SPECTROMETER AN0 61 INCH REFLECTOR CALCULATION OF MAXIMUM NUMBER DENSITY OF PLASMA Ab7-22016 Ab7-25206

ASTRONOMICAL TELESCOPE MARTIAN ATMOSPHERE MODELS WITH DIFFERENT BALLOON-CARRIED AUTOMATIC TELESCOPE-SPECTROMETER COMPOSITION, PRESSURE AND TEMPERATURE OBSERVATION OF VENUS UPPER ATMOSPHERE AN0 Ab7-25685 DETERMINATION OF WATER VAPOR CONTENT A6630352 MARTIAN DAYTIME ATMOSPHERE FROM ZERO TO 50 KM PRESENTING SPHERICAL PARTICLE TERMINAL VELOCITIES LUNAR AN0 PLANETARY STUDIES DEALING WITH COUDE AN0 POSSIBLE SIZES FOR OBSCURATIONSt USING FACILITY WITH 24-INCH TELESCOPE, OICKE-TYPE MARINER IV OCCULTATION Ab7-26316 RADIOMETER TO MEASURE EMISSION FROM VENUS. AND EMISSION SPECTRA OF SILICATES Nb7-23660 TWO-LAYER MODEL OF VENUSIAN ATMOSPHERE SATISFYING RADIDASTRONOMIC AN0 RADAR SELF-RADIATION ASTROPHYSICS MEASUREMENTS Ab7-32322 ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS FROM MARINER I1 RADIOMETER DATA, AN0 CARBON DIOXIDE IONS WITH ELECTRONS DISSOCIATIVE THERMODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES RECOMBINATION MEASUREMENTS WITH MICROWAVE- NASA-CR-7 6106 Nbb-31639 AFTERGLOW DIFFERENTIALLY PUMPED QUAORUPOLE MASS- SPECTROMETER APPARATUS, NOTING MARTIAN ATMOSPHERE RESEARCH IN CELESTIAL MECHANICS, ASTROPHYSICS, MODEL RADIO PHYSICS, PLANETARY ATMOSPHERES. SOLAR SRCC-55 Ab7-32826 PHYSICS, AN0 OTHER AREAS OF SPACE SCIENCES NASA-TM-X-57737 Nbb-32006 MODEL FOR DISTRIBUTION OF THERMAL PLASMA IN MAGNETOSPHERE OF JUPITER UNDER ASSUMPTION OF RESEARCH ON PLANETARY ATMOSPHERES. VENUS DARK COROTATION WITH PLANET Ab7-33196 SIDE EMISSION, OZONE CONCENTRATION. CLOUD AN0 AEROSOL SCATTERING* ATMOSPHERIC RADIATION ATOMIC AN0 MOLECULAR PROCESSES IN CYTHEREAN, SCATTERING. AN0 EARTH HEAT BUDGET AND ALBEDO MARTIAN AN0 JOVIAN UPPER ATMOSPHERES NASA-CR-77048 Nbb-33437 Ab7-34158

ASTRONOMY. ASTROPHYSICS. CELESTIAL MECHANICS. EFFECTIVE BRAKING HEIGHT / EBH/ FOR SMALL GEODESY, SOLAR PHYSICS, IONOSPHERE AND RADIO' INTERPLANETARY PARTICLES OF COSMIC VELOCITY PHYSICS, FIELDS AND PARTICLESI AN0 PLANETARY ENTERING MARTIAN UPPER ATMOSPHERE ATMOSPHERES Ab7-34541 NASA-TM-X-57969 Nbb-37946 VENUS RADIATION SPECTRUM IN MM RANGE FROM VENUS ATLAS AGGENA LAUNGH VEHICLE ATMOSPHERE MODELS Ab7-40120 x MARINER VENUS PROJECT DESIGN CHANGES FOR FLYBY MISSION AN0 SENSING OF VENUS ATMOSPHERE ATMOSPHERE OF MARS STUDIED USING THREE MODELS Nbj-25094 GENERATED TO SHOW HIGH, MEAN AND LOW DENSITY COMPDSITIONS TO ACCOUNT FOR GRAVITATIONAL AND ATLAS CENTAUR LAUNCH VEHICLE MAGNETIC FIELDS Ab7-40140 MARINER MARS 1969 PROJECT AN0 SPACECRAFT DESIGN MODIFICATIONS FOR FLYBY MISSIONS IDNOSPHERE MODEL TO EXPLAIN SPECTRUM OF BRIGHTNESS Nb7-25095 TEMPERATURES FOUND IN RADIO EMISSION FROM VENUS ATMOSPHERE Nb7-16804 ATMOSPHERE MODEL ATMOSPHERIC MOOELSI COMPARING CHAMBERLAIN ATMOSPHERIC MODEL COMPARED WITH ASTRONOMICAL EVAPORATIVE AND SOLAR BREEZE MODELS, OPIK AND OBSERVATIONS TO DETERMINE EFFECT OF CLOUD COVER SINGER EVAPORATIVE MODEL AN0 PARKER SOLAR AN0 RESULTING HIGH EFFECTIVE TEMPERATURE OF WINO MODEL Abb-36605 RADIO EMISSION FROM VENUS IN CENTIMETER RANGE Nb7-16805 MARINER IV MODELS OF THREE MARS ATMOSPHERIC LAYERS ANALOGOUS TO TERRESTRIAL E. F-1 AN0 F-2 MODELS THAT ASSUME MARS ATMOSPHERE HAS ABSORPTIVE LAYERS, CONSIDERING RELATIVE MASS DENSITIES, RATHER THAN SCATTERING PROPERTIES, AN0 THAT TEMPERATURES, CARBON DIOXIDE PHOTODISSOCIATION AN0 REDNESS OF PLANET IS DUE TO SELECTIVE ASSORPTION IONIZATION PROFILE Abb-41779 Nb7-1bB08

METEOROLOGY OF MARS AND VENUS MODEL FOR MARTIAN ATMOSPHERE AN0 PLANETARY NASA-CR-75315 Nbb-27238 SURFACE ASSUMING ATMOSPHERIC SPECTRUM WITH PURELY SCATTERING PROPERTIES AN0 SURFACE MARS ATMOSPHERE MODELS AT THREE DENSITY LEVELS COVERED WITH LIMONITE DUST Nb7-lb809 NASA-TM-X-53484 Nbb-31944 ATMOSPHERE OF MERCURY COMPARING ATMOSPHERE MODELS OF MARS BASED ON NASA-TM-X-57322 Nb7-18273 MARINER IV OCCULATIOM DATA NASA-CR-78134 Nbb-37214 MARTIAN ATMOSPHERE MODEL DEDUCED FROM MARINER IV IONOSPHERE ELECTRON DENSITY MEASUREMENTS INDUCED ABSORPTION COEFFICIENTS IN ATMOSPHERE NASA-CR-84825 Nb7-28785 MODEL MEASURED FOR CALCULATION OF VENUS LOWER ATMOSPHERE PROPERTIES FROM RADIO OBSERVATIONS DERIVATION OF ATMOSPHERIC PARAMETERS FOR d Ab7-12949 GREENHOUSE MODEL OF VENUS ATMOSPHERE NASA-TM-X-53497 Nb7-29983 ATOMIC AND MOLECULAR PROCESSES IN UPPER ATMOSPHERES OF VENUS, MARS AND JUPITER MODEL COMPUTATIONS OF TEMPERATURE VARIATIONS AN0 INVESTIGATED BY ATMOSPHERIC MODELS, PRESENTING WIND CIRCULATIONS IN MARTIAN ATMOSPHERE c SOLAR-PLANCTARY RELATIONSHIP Ab7-18429 NASA-CR-855 69 Nb7-30624

MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF ' TWO-LAYER ATMOSPHERE MODEL OF VENUS VENUS COMPARED WITH SEVERAL MODEL ATMOSPHERES NASA-CR-88980 Nb7-38348 Ab7-24601

1-3 ATMOSPHERIC ABSORPTION SUBJECT INDEX

ATMOSPHERIC ABSORPTION OSCILLATIONS OF SATURN RINGS AN0 ESTIMATION OF VENUS ATMOSPHERE NOTING PRESSURE INDUCED UPPER LIMIT TO MASS OF RING IF MOTION IS STABLE ABSORPTION IN CARBON DIOXIDE-NITROGEN ATMOSPHERE AGAINST AXISYMMETRIC PERTURBATIONS AS INDICATED IN DECLINE OF MICROWAVE BRIGHTNESS Abb-41063 TEMPERATURE Abb-42668 THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES PLANETARY ATMOSPHERIC ABSORPTION SPECTROSCOPY AN0 IN ORIGIN OF ORGANIC MATTER - DETERMINATION EMPLOYING SPLIT-TRAJECTORY DUAL FLYBY MODE OF AMINO ACID PAIRING AN0 SEQUENCES IN PROTEINS AIAA PAPER 67-121 Ab7-18311 NASA-CR-74559 Nbb-28800

ATMOSPHERIC ATTENUATION CALCULATION OF THERMODYNAMIC EQUILIBRIUM * BOUNDARIES AN0 ATTENUATING MEDIA EFFECT ON COMPOSITION OF EARTH, VENUS, MARS AN0 RADIOMETRIC SOUNDING OF PLANETARY ATMOSPHERES BY JUPITER ATMOSPHERES Nbb-28801 REMOTE SENSING TECHNIQUES Ab7-12406 PRESSURE. COHPOSITION~ AN0 PARTICLE CONTENT OF RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW MARTIAN ATMOSPHERE - POLARIZATIONI SPECTRAL VALUE OF CROSS SECTION, ECHO SPECTRUM, BRIGHTNESS. AN0 TEMPERATURE OF MARTIAN SURFACE POLARIZATION CHARACTERISTICS, ABSORPTION CROSS Nbb-31472 SECTION AN0 ATMOSPHERIC ATTENUATION Ab7-16298 SPECTROSCOPIC MEASUREMENT OF CARBON DIOXIDE IN MARS ATMOSPHERE FOR SURFACE PRESSURE AN0 ATMOSPHERIC CHEMISTRY ATMOSPHERIC COMPOSITION Nbb-31473 ATOMIC AN0 MOLECULAR PROCESSES IN UPPER ATMOSPHERES OF VENUS. MARS AN0 JUPITER SPECTROSCOPTIC MEASUREMENTS OF WATER VAPOR AN0 INVESTIGATED BY ATMOSPHERIC MODELS. PRESENTING CARBON DIOXIDE CONTENTS IN MARS ATMOSPHERE SOLAR-PLANETARY RELATIONSHIP Ab7-18429 Nbb-31474

ION-MOLECULE CHEMISTRY OF JUPITER UPPER EARTH AN0 PLANETARY OCEAN AN0 ATMOSPHERIC ORIGIN, ATMOSPHERE. STUDYING EQUILIBRIUM AN0 EVOLUTION, AN0 COMPOSITION Nbb-37965 NONEQUILI8RIUM ABUNOANCES OF HYDROCARBON PRODUCTS DUE TO UV RADIATION REACTION Ab7-34540 GASEOUS COMPOSITION OF UNKNOWN PLANETARY ATMOSPHERE DETERMINED, USING ACOUSTIC EXPERIMENT THERMODYNAMIC EQUILIBRIUM IN PREBIOLOGICAL COMBINED WITH PRESSURE AN0 TEMPERATURE DATA ATMOSPHERES. AN0 INORGANIC ORIGIN OF ORGANIC Ab7-13215 COMPOUNDS NASA-SP-3040 Nb7-27295 RADIATION EQUILIBRIA IN UV LIGHT ON AIR, OXYGEN, CARBON OIOXIOE~ETC, ANALYZED BY BROMINE LAMP IN ATMOSPHERlC CIRCULATION CONNECTION WITH STUDIES OF PLANETARY ATMOSPHERES MARS ATMOSPHERIC CIRCULATIONI DIURNAL HEATING, Ab?-14088 THERMAL TIDES AND EFFECTS ON EARTH ATMOSPHERE Abb-30353 PHOTOMETRY OF INTEGRATED LIGHT OF VENUS, INFERRING PRESENCE OF ICE IN ATMOSPHERE FROM HALO PLANETARY SCALE ATMOSPHERIC CIRCULATIONS OF EFFECT OF BRIGHTNESS DISPERSION JUPITER AN0 SATURN USING FLUID DYNAMICS, NOTING Ab7-16407 ROTATION EFFECTS Abb-41679 THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS *i MARTIAN ATMOSPHERIC CIRCULATION - VERTICAL ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION TEMPERATURE OISTRIBUTION, DIURNAL HEATING AN0 DEDUCE0 SPECTROSCOPICALLY Ab7-20022 TIDES, AND DIFFERENTIAL HEATING AN0 GENERAL CIRCULATION AT SOLSTICES Nbb-31489 SELF-BROADENING COEFFICIENTS OF SPECTRAL LINES OF ABSORBING ATMOSPHERIC GASES MEASURE0 IN DEEP CIRCULATION IN VENUSIAN ATMOSPHERE MODEL COMPARISON WITH LINE BROADENING EFFECTS OF OPAQUE TO SOLAR AN0 PLANETARY RADIATION BUT WITH NITROGEN Ab7-22715 DIFFERENTIAL HEATING Ab?-14310 VENUS ATMOSPHERE SPECTRA OBTbINEO BY MICHELSON RELATIONSHIP BETWEEN TERRESTRIAL AN0 JOVIAN INTERFEROMETER, FINDING H CL LINES CONSISTENT ATMOSPHERIC CIRCULATIONS DUE TO SOLAR ACTIVITY WITH 2-MM AMAGAT OF GAS Ab7-21215 JPL-TR-32-1106 Ab7-24510

PHOTOMETRIC OBSERVATION DATA ON JUPITER RADAR, RADIO ASTRONOMIC AN0 IR SPECTROSCOPIC ATMOSPHERIC ACTIVITY /19b4-1965/ NOTING THREE- OBSERVATIONS OF VENUS SURFACE AN0 ATMOSPHERE, MONTH PERIODIC CHANGE Ab7-39299 EXAMINING GENERAL AN0 SURFACE DATA, CHEMICAL COMPOSITION AN0 ATMOSPHERIC MODEL CONSTRUCTION NUMERICAL MODEL FOR SIMULATING GENERAL CIRCULATION Ab7-24843 OF ATMOSPHERE OF MARS NASA-CR-81146 N67-15280 MARTIAN ATMOSPHERE MODELS WITH DIFFERENT COMPOSITION. PRESSURE AN0 TEMPERATURE ATMOSPHERIC COMPOSITION Ab7-25685 RADIO ASTRONOMY STUDIES OF VENUS AN0 MARS NOTING SURFACE PROPERTIES, ATMOSPHERIC STRUCTURE, PLANETARY ATMOSPHERIC COMPOSITION STUDY UNDER ETC Abb-2 bo3 1 AMBIENT CONDITIONS USING INSTRUMENT INVOLVING VERY HIGH Q FABRY- PEROT MICROWAVE CAVITIES LIMITATION ON OXYGEN CONCENTRATION IN POSSIBLE Ab7-2598 b PRIMITIVE ATMOSPHERES EXAMINED VIA PHYSICAL AN0 PHOTOCHEMICAL FACTORS Abb-26122 MARS ATMOSPHERIC COMPOSITION DETERMINATION BY SHOCK LAYER RADIOMETRY TECHNIQUE DURING PROBE MARS UPPER ATMOSPHERE AN0 SINGLE-LAYER IONOSPHERE EXPERIMENT UV PHOTOIONIZATION, TEMPERATURE PROFILE AN0 AIAA PAPER 67-293 Ab7-26009 CHEMICAL COMPOSITION 166-29417 B STRUCTURE AN0 COMPOSITION OF JUPITER ATMOSPHERE, MARS ATMOSPHERE MODELS BASED ON MARINER IV NOTING LABORATORY AN0 OBSERVATIONAL DATA OCCULTATION DERIVING ELECTRON NUMBER DENSITY. SUPPORTING HYPOTHESIS OF CONSISTENCY WITH SOLAR TEMPERATURE, PRESSURE. MASS DENSITY, ETC, NOTING ELEMENTS ABUNDANCE Ab7-30932 CARBON DIOXIDE PRESENCE Abb-30713 UPPER LIMITS ON LIQUID WATER CONTENT IN VENUS u VENUS ATMOSPHERE. SURFACE TEMPERATURE AN0 ATMOSPHERE Ab7-32652 RADIATION CHARACTERISTICS Abb-35799 OXYGENIC CONCENTRATIONS IN PRIMITIVE EARTH CYLINDRICAL FUNCTIONS FOR CALCULATING FREE ATMOSPHERE, DISCUSSING MARTIAN ATMOSPHERE

1-4 SUBJECT INDEX ATMOSPHERIC PRESSURE

COMPOS1TI ON Ab7-34095 PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS LANDING MISSION, DISCUSSING USE OF LIFTING JUPITER AND SATURN MODELS, GIVING PLANET VEHICLES Abb-25273 CONSTITUTION* HEAT BALANCE AND ATMOSPHERIC COMPOSITION Ab7-39001 MARS ATMOSPHERIC COMPOSITION AND LAMINAR I CONVECTIVE HEATING AND ABLATION STUDIED TO PREDICT SPHERICAL ENTRY VEHICLE USED TO DEFINE PLANETARY PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING ATMOSPHERE STRUCTURE AND COMPOSITION FROM DYNAMIC ENTRY Abb-25274 RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC CHARACTERISTICS Ab7-40177 INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS FOR POINTED AND SPHERICALLY BLUNT BODIES IN 5 MARTIAN ATMOSPHERE COMPONENT DUE TO PROTON UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE PENETRATION INTO ATMOSPHERE FROM SOLAR WINO, Ab6- 2527 5 SUGGESTING RADIO OCCULTATION BY MARS ORBITER Ab7-40799 PROGRESS AND PROBLEMS IN ATMOSPHERIC ENTRY FOR MANNED AND UNMANNED PLANETARY PROBES - REENTRY EXTRATERRESTRIAL LIFE DETECTION STUDIED FROM PHYSICS KNOWLEDGE OF MAJOR AND TRACE COMPONENTS OF NASA-TM-X-56855 Nbb-29405 ATMOSPHERES Ab740999 MANNED MARS EXCURSION VEHICLE FOR THIN MARS UPPER LIMIT OF CARBON DIOXIDE ABUNDANCE IN ATMOSPHERE MERCURY ATMOSPHERE Ab7-41836 NASA-TM-X-53475 Nbb-30788

EVOLUTION OF ATMOSPHERIC COMPONENTS OF VENUS DYNAMIC MODEL STUDY TO DETERMINE LOW SUBSONIC Ab7-80916 SPEED STABILITY AN0 DRAG CHARACTERISTICS DURING VERTICAL DESCENT OF ENTRY CONFIGURATIONS SIMULATION FACILITY FOR ATMOSPHERIC COMPOSITION. CONSIDERED FOR PROBES OF PLANETARY ATMOSPHERES PRESSURE, AN0 DAILY VARIATIONS OF MARS AND NASA-TN-0-3499 Nbb-31351 OTHER PLANETS NASA-TT-F-11062 Nb7-27533 AERODYNAMIC, THERMODYNAMIC AND STRUCTURAL DESIGN ASPECTS OF FLIGHT CAPSULE ENTERING LOW DENSITY MARTIAN AN0 CYTHEREAN ATMOSPHERIC COMPOSITION MARS ATMOSPHERE FROM ORBIT Ab7- 1143 2 DETERMINATIONS USING ENTRY PROBE MEASUREMENTS OF ULTRAVIOLET AND X-RAY ATTENUATION MARS ATMOSPHERIC COMPOSITION AND LAMINAR DAC-60627 Nbl-33758 CONVECTIVE HEATING AN0 ABLATION STUDIED TO PREDICT PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING ATMOSPHERIC DENSITY ENTRY Abl-18849 MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS DETERMINING SHAPE, ATMOSPHERE DENSITY PROFILE, FOR POINTED AN0 SPHERICALLY BLUNT BDOIES IN DIURNAL VARIATIONS, ETC Abb-25235 UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE Ab7-19380 MARS ATMOSPHERIC DENSITY DETERMINED FROM PHOTOELECTRIC MEASUREMENTS OF ECLIPSES OF PHOBOS FLIGHT DYNAMICS OF BALLISTIC AN0 LIFTING VEHICLE Abb-30049 ENTRIES INTO PLANETARY ATMOSPHERES OF MARS. EARTH. VENUS AN0 JUPITER Ab7-20623 i$ MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, ENERGY DISSIPATION AN0 OTHER PROBLEMS FOR ALIEN DETERMINING SHAPE, ATMOSPHERE DENSITY PROFILE, PLANETARY ATMOSPHERIC ENTRY AT HIGH SPEEDS OF DIURNAL VARIATtONS, ETC INTERPLANETARY FLIGHT Ab7-21155 JPL-TR-32-1157 Ab7-26819 FREE FALLING PROBE TEST DURING TERMINAL DESCENT ATMOSPHERE OF MARS STUDIED USING THREE MODELS FOR DETERMINING UNKNOWN PLANETARY ATMOSPHERE GENERATED TO SHOW HIGH, MEAN AND LOW DENSITY PROFILE FROM ONBOARO MEASUREMENTS ALONE COMPOSITIONS TO ACCOUNT FOR GRAVITATIONAL AND Ab7-22168 MAGNETIC FIELDS Ab7-40140 AERODYNAMIC, THERMOOYNAMICP HEAT SHIELD AN0 MARINER SPACE VEHICLES DESIGN EVOLUTION NOTING STRUCTURAL DESIGN ASPECTS OF BALLISTIC VEHICLE CONTRIBUTION TO FUTURE SPACE FLIGHTS THROUGH ENTERING PLANETARY ATMOSPHERE Ab7-35315 MEASUREMENT OF ATMOSPHERIC DENSITY OF MARS Ab7-42399 EARTH AND PLANETARY ATMOSPHERE ENTRY PROBLEMS FOR BLUNT NOSE0 SLENDER VEHICLES NOTING AERODYNAMICS, ATMOSPHERIC DIFFUSION STABILITY. HEATING. ABLATION AND INTERACTION OF LIGHT DIFFUSION OF MARTIAN ATMOSPHERE MEASURE0 BY EFFECTS SPECTROSCOPIC EVALUATION OF POLARIZATION VARIATION AIAA PAPER 67-803 Ab7-42963 FROM DISK CENTER TO EDGE Abb-25461 AERODYNAMIC LIFT IN FUTURE SPACE VEHICLE DESIGN- WATER CONTENT AN0 DIFFUSION IN MARTIAN ATMOSPHERE DURING VARIOUS FLIGHT REGIMES IN ATMOSPHERES OF AND PROPERTIES OF LIGHT AND DARK SIDES OF EARTH AND PLANETS MARTIAN SOIL Nbb-3 148 1 P-3559 Nb7-285 13

ATMOSPHERIC EMISSION CHEMICAL KINETICS OF CARBON DIOXIDE FOR MARTIAN POLARIZATION STUDIES OF RADIO EMISSION FROM UPPER ATMOSPHERIC ENTRY APPLICATIONS LAYER AND SURFACE COVERING OF PLANETS ARL-67-0113 Nb7-3945% Nb7-1b817 ATMOSPHERIC HEAT BUDGET VENUS TWILIGHT SKY INVESTIGATED FOR DISCREPANCIES MECHANISM REGULATING TOTAL AMOUNT OF EARTH AND BETWEEN PREDICTED AND OBSERVED SHAPE AN0 MARS ATMOSPHERE TRANSPARENT TO VISIBLE AND IR PERIODIC APPEARANCE OF PLANET RADIATION Ab7-18052 4 RM-5386-PR Nb7-37243 ATMOSPHERIC IMPURITY ATMOSPHERIC ENTRY VOLCANIC AND TECTONIC ACTIVITY ON VENUS INFERRED HIGH-TEMPERATURE GAS RADIANCE IN SIMULATED FROM HIGH SURFACE TEMPERATURE, CONSIDERING PLANETARY PTMDSPHERE AT VARIOUS ENTRY VELOCITIES POSSIBLE EFFECT ON ATMOSPHERE OBSCURATION AIAA PAPER 66-163 166-25169 Ab7-33232 r MANNED MARS ENTRY AND LANDING, DISCUSSING ATMOSPHERIC PRESSURE AEROBRAKING AS FEASIBLE ENTRY MODE SPHERICAL SEMIPASSIVE PROBE FOR OENSITY/ATTITUOE Abb-25272 AND PRESSURE/ALTITUDE PROFILE OF PLANETARY

1-5 ATMOSPHERIC RADIATION - SUBJECT INDEX

ATMOSPHERES, NOTABLY MARS AN0 VENUS ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION Ab6-30089 DEDUCED SPECTROSCOPICALLY 167-20022

MARTIAN ATMOSPHERIC SURFACE PRESSURE BETWEEN AURORAL ACTIVITY OCCULTATION LEVELS AT ELECTRICS AN0 MARE ASHEN LIGHT AND MAGNETIC FIELD OF VENUS AC IOAL IUM Ab7-33096 NASA-CR-75816 N6b-29298 AURORAL EMISSION CARBON DIOXIDE ABUNDANCE AND SURFACE PRESSURE OF SOLAR RADIATION EFFECT ON PLANETARY ATMOSPHERE MARTIAN ATMOSPHERE, NOTING SELF-BROADENING NOTING CHARGED PARTICLE BOMBARDMENT, DAYGLOW CORRECTION A67-21250 PHENOMENA, AURORAL EMISSION. ETC Ab7-14699 ATMOSPHERIC PRESSURE AT CLOUD TOP AN0 HYDROGEN ABUNDANCE IN JUPITER ATMOSPHERE OETERMINEO BY ANALYZING METHANE SPECTRAL LINE WIDTHS B A67-37479 BACILLUS SIMULATED MARTIAN ATMOSPHERIC AN0 ECOLOGICAL PHOTOMETRIC ANALYSIS OF AEROSOL COMPONENT OF MARS EFFECTS ON BACILLUS CEREUS SPORE GERMINATION ATMOSPHERE Nb7-16810 NASA-CR-74969 Nbb-26263

DISCREPANCY BETWEEN MARS ATMOSPHERIC PRESSURE BALLISTIC VEHICLE DATA FROM SPECTROSCOPIC MEASUREMENTS AN0 FROM AERODYNAMIC. THERMODYNAMIC, HEAT SHIELD AN0 PHOTOMETRIC AN0 POLARIMETRIC OBSERVATIONS STRUCTURAL DESIGN ASPECTS OF BALLISTIC VEHICLE N67-16011 ENTERING PLANETARY ATMOSPHERE A67-353 15

INFRARED SPECTROSCOPY TO DETERMINE TEMPERATURE, BALLOON PRESSUREt AN0 CHEMICAL COMPOSITION OF MARTIAN VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE ATMOSPHERE Nb7-16813 INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AN0 OF STATIC EQUILIBRIUM WITHIN KAPLAN ATMOSPHERE ATMOSPHERIC RADIATION A66-27887 RANDOM ELSASSER BAND MODEL TO COMPUTE ATMOSPHERIC TRANSMISSION OF EARTH AN0 MARS FOR 2-MICRON BALLOON FLIGHT CARBON DIOXIDE BANDS DETERMINATION OF ICE CLOUDS AND WATER VAPOR IN JPL-TR-32-969 166-38024 VENUS ATMOSPHERE FROM BALLOON OBSERVATIONS Nbb-31463 MOLECUCARI CONTINUUM AND LINE RADIATION OF PLANETARY ATMOSPHERES, COMPARING MOLECULAR BAN0 DATA RECORDING AN0 REDUCTION OF WATER VAPOR STRUCTURE MODELS WITH SPECTRAL MEASUREMENTS OF CN CONTENT IN UPPER ATMOSPHERE OF VENUS AS VIOLET BAND DETERMINED BY BALLOON CARRIED AUTOMATIC AIAA PAPER 67-323 A67-26038 TELESCOPE-SPECTROMETER UNIT N66-31468

EQUILIBRIUM RADIATION IN AIR AN0 GAS MIXTURES BALLOON SOUNDING ASSUMED TO REPRESENT NEAR PLANET ATMOSPHERES BALLOON-CARRIED AUTOMATIC TELESCOPE-SPECTROMETER NASA-CR-81315 Nb7-16722 OBSERVATION OF VENUS UPPER ATMOSPHERE AN0 DETERMINATION OF WATER VAPOR CONTENT ATMOSPHERIC SCATTERING 866-30352 DIFFUSE REFLECTION BY PLANETARY INHOMOGENEOUS ATMOSPHERE WITH ALBEDO FOR SINGLE SCATTERING BIBLIOGRAPHY DECREASES EXPONENTIALLY WITH OPTICAL OEPTH ANNOTATED BIBLIOGRAPHY ON PLANETARY ATMOSPHERES A66-34149 NASA-SP-7017/01/ Nb6-36 130

RESEARCH ON PLANETARY ATMOSPHERESI VENUS DARK BIBLIOGRAPHY AN0 AUTHOR ON MERCURY SURFACE. SIDE EMISSIONI OZONE CONCENTRATION, CLOUD AN0 ATMOSPHERE, ROTATION, TEMPERATURE. AND TERRAIN AEROSOL SCATTERING, ATMOSPHERIC RADIATION NASA-CR-84113 Nb7-26454 SCATTERING, AND EARTH HEAT BUDGET AN0 ALBEDO NASA-CR-77048 N6b-33437 BIOCHEMISTRY THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES ANISOTROPIC NONCONSERVATIVE SCATTERING IN MODIFIED AN0 IN ORIGIN OF ORGANIC MATTER - DETERMINATION SCHUSTER- SCHWARZSCHILO APPROXIMATION AN0 VENUS OF AMINO ACID PAIRING AND SEQUENCES IN PROTEINS CLOUD LAYER A67-20931 NASA-CR-74559 Nbb-26800

RELATION BETWEEN SURFACE PRESSURE AN0 ATMOSPHERIC BIOLOGICAL EFFECT BRIGHTNESS IN OPTICALLY THIN RAYLEIGH SCATTERING PLANETARY QUARANTINE CONSTRAINTS, NOTING ATMOSPHERE, CONSIDERING APPLICATION TO MARS PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION A67-34536 A6b-29966

TWILIGHT CUSP EXTENSIONS OF VENUS AN0 PLANETARY QUARANTINE CONSTRAINTS, NOTING APPLICATION TO DERIVING HEIGHTS OF SCATTERING PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION ATMOSPHERE A67-29098 P-3621 Nb7-35341 BIOSIMULATION ATMOSPHERIC STRATIFICATION RESPONSE OF FUNGI TO DIURNAL TEMPERATURE EXTREMES, INVARIANT IMBEOOING EQUATIONS FOR DETERMINING DESCRIBING SOIL, SIMULATED MARTIAN TEMPERATURE VERTICAL STRATIFICATION OF TERRESTRIAL AN0 REGIME AND FUNGI GROWTH Ab7-21991 PLANETARY ATMOSPHERES ON BASIS OF SATELLITE OBSERVATIONS BOUNDARY LAYER RM-5229-PR Nb7-32463 NUMERICAL SOLUTION OF TRANSPORT AN0 ENERGY EQUATIONS IN PLANETARY BOUNDARY LAYER ATMOSPHERIC TEMPERATURE ECOM-6020 Nbb-33271 MEAN VALUES OF METHANE WAVELENGTHS IN URANUS SPECTRUM MEASURE0 FOR DETERMINATION OF ATMOSPHERIC BOUNDARY LAYER STABILITY TEMPERATURE Ab7-14327 SPATIAL AND TEMPORAL DISTRIBUTION OF GRADIENT RICHARDSON NUMBER IN SURFACE AN0 PLANETARY JUPITER ENVIRONMENTS EFFECTS OF HUGE MASS, HIGH BOUNDARY LAYERS ROTATION RATE. TEMPERATURE AN0 DOMINANT H AND HE ECOM-5123 Nb7-35919 ATMOSPHERE A67-40141 BRIGHTNESS ATOMIC STRUCTURE SUPERCOOLEO WATER OROPLETS HYPOTHESIZED IN VENUS THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS CLOUD LAYER, BASE0 ON RADIOMETRIC OBSERVATION IN

1-6 SUBJECT INDEX CHEMICAL COMPOSITION

SHF RANGE 666-37016 SPECTROSCOPTIC MEASUREMENTS OF WATER VAPOR AND CARBON DIOXIDE CONTENTS IN MARS ATMOSPHERE BRIGHTNESS DISTRIBUTION OF MARTIAN DISK USED TO Nbb-31474 DETERMINE OPTICAL PARAMETERS OF ITS ATMOSPHERE " AND SURFACE FROM ABSOLUTE PHOTOMETRIC DATA CARBON DIOXIDE ABUNDANCE AND SURFACE PRESSURE OF Nbb-33533 MARTIAN ATMOSPHERE Nbb-31475

MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF MOOEL OF NONEPUILIBRIUM PROPERTIES OF HIGH VENUS COMPARED WITH SEVERAL MOOEL ATMOSPHERES TEMPERATURE CARBON DIOXIDE AND OTHER GAS MIXTURES Ab7-24601 IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING P MARTIAN ATMOSPHERE Ab7-11436 DISTRIBUTION OF RADIO BRIGHTNESS TEMPERATURE OVER DISK OF VENUS Ab7-27333 CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS VISIBLE BRIGHTNESS FEATURES IN MARINER IV OF MARS Ab?-14309 PHOTOGRAPHS OF MARS INTERPRETED AS CLOUDS Ab?-34149 CARBON DIOXIDE ABUNDANCE AN0 SURFACE PRESSURE OF MARTIAN ATMOSPHERE, NOTING SELF-BROADENING IONOSPHERE MOOEL TO EXPLAIN SPECTRUM OF BRIGHTNESS CORRECTION Ab7-21250 TEMPERATURES FOUNO IN RADIO EMISSION FROM VENUS ATMOSPHERE N67-16804 CARBON DIOXIDE STUDY IN MERCURY ATMOSPHERE YIELDS NEGATIVE RESULTS FROM OBSERVATIONS MAOE WITH IR ATMOSPHERIC BRIGHTNESS OF MARS DETERMINED BY SPECTROMETER AND 61 INCH REFLECTOR POLARIMETRIC AND PHOTOMETRIC MEASUREMENTS Ab7-220Lb TR-34 Nb7-24229 MARTIAN TRANSIENT PHENOMENA CORRELATIONS AMONG BRIGHTNESS DISCRIMINATION MASS MOTION OF WATER IN ATMOSPHERE. POLAR CAP PHOTOMETRY OF INTEGRATED LIGHT OF VENUS, GROWTH AN0 WHITE CLOUD APPEARANCE FREQUENCY INFERRING PRESENCE OF ICE IN ATMOSPHERE FROM HALO Ab7-24501 EFFECT OF BRIGHTNESS DISPERSION Ab7-16407 CARBON OIOXIDE IONS WITH ELECTRONS OISSOCIATIVE RECOMBINATION MEASUREMENTS WITH MICROWAVE- TWO-LAYER MODEL OF VENUSIAN ATMOSPHERE SATISFYING AFTERGLOW DIFFERENTIALLY PUMPED QUADRUPOLE MASS- RADIOASTRDNOMIC AND RADAR SELF-RADIATION SPECTROMETER APPARATUS, NOTING MARTIAN ATMOSPHERE MEASUREMENTS Ab7-32322 MOOEL SRCC-55 Ab7-32826

C UPPER LIMIT OF CARBON DIOXIDE ABUNDANCE IN CAPSULE MERCURY ATMOSPHERE Ab7-41836 '$ ON-BOARD TRACKING SYSTEM OF TWO-WAY COHERENT OOPPLER BETWEEN ENTRY CAPSULE AND ORBITING BUS FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTIAN FOR DETERMINING ORBIT OF ENTRY CAPSULE AN0 ATMOSPHERE FOR DETERMINATION OF PROFILES OF ESTIMATING ATMOSPHERIC PARAMETERS CARBON OIOXIDE, PARTICULATE MATTER AND WATER Nb7-15904 VAPOR NASA-TN-D-4115 Nb7-34884 a4 CARBON DIOXIDE CHEMICAL SYSTEM AND REACTION RATES BEHIND SWONG CHEMICAL KINETICS OF CARBON DIOXIDE FOR MARTIAN SHOCK WAVES IN MIXTURES OF CARBON DIOXIDE AN0 ATMOSPHERIC ENTRY APPLICATIONS NITROGEN USE0 TO STUDY ENTRY CONOITIONS INTO MARS ARL-67-0113 Nb7-39458 ATMOSPHERE 166-25276 CARBON MONOXIDE VERTICAL TEMPERATURE DISTRIBUTION IN MARTIAN OISSOCIATION LAYER HEIGHTS ON VENUS, MARS AND ATMOSPHERE, NOTING INSENSITIVITY TO SURFACE JUPITER, NOTING CO FLAME AIRGLOW INTENSITIES PRESSURE AN0 CARBON DIOXIDE VARIATIONS Abb-30050 166-26132 CHEMICAL REACTIONS BETWEEN SOLAR HYDROGEN AN0 MARS ATMOSPHERE MOOELS BASED ON MARINER IV CARBON MONOXIDE IN VENUS ATMOSPHERE OCCULTATION DERIVING ELECTRON NUMBER DENSITY. NASA-CR-82960 Nb7-19904 TEMPERATURE, PRESSURE. MASS DENSITY, ETC, NOTING CARBON DIOXIDE PRESENCE Abb-30713 CELESTIAL MECHANICS RESEARCH IN CELESTIAL MECHANICS. ASTROPHYSICSi RANDOM ELSASSER BAND MODEL TO COMPUTE ATMOSPHERIC RADIO PHYSICS. PLANETARY ATMOSPHERES. SOLAR TRANSMISSION OF EARTH AND MARS FOR 2-MICRON PHYSICS, AN0 OTHER AREAS OF SPACE SCIENCES CARBON OIOXIDE BANDS NASA-TM-X-57737 Nbb-32006 JPL-TR-32-969 Abb-30024 CELESTIAL OBSERVATION ABUNDANCE AND TEMPERATURE OF CARBON DIOXIDE IN ASHEN LIGHT AN0 MAGNETIC FIELD OF VENUS MARTIAN ATMOSPHERE, NOTING IMPLICATIONS, Ab7-33096 OBSERVATION METHODS AND RESULTS Abb-39558 CHANDRASEKHAR EQUATION INITIAL VALUE APPROACH TO CHANDRASEKHAR PLANETARY ABSORPTION LINES ON VENUS SPECTROGRAMS OF PROBLEM TO ESTIMATE PLANETARY PROPERTIES AND ROTATIONAL FINE STRUCTURE OF EXCITED VIBRATIONAL ATMOSPHERIC COVERS TRANSITION OF CARBON DIOXIOE Abb-4181b RM-4991-PR Nbb-29959

PLANETARY ATMOSPHERE RESOLUTION SPECTRUM NOTING INVARIANT IMBEDDING EQUATIONS FOR DETERMINING CARBON OIOXIOE LINES, RADIATION TRANSFER. VERTICAL STRATIFICATION OF TERRESTRIAL AN0 COMPOSITION, TEMPERATURES, PRESSURES, ETC PLANETARY ATMOSPHERES ON BASIS OF SATELLITE b Abb-42667 OBSERVATIONS RM-5229-PR Nb7-32463 VENUS ATMOSPHERE NOTING PRESSURE INDUCE0 ABSORPTION IN CARBON DIOXIDE-NITROGEN ATMOSPHERE CHARGED PARTICLE AS INDICATED IN OECLINE OF MICROWAVE BRIGHTNESS SOLAR RADIATION EFFECT ON PLANETARY ATMOSPHERE TEMPERATURE Abb-42668 NOTING CHARGE0 PARTICLE BOMBARDMENT. DAYGLOW )* PHENOMENA. AURORAL EMISSION. ETC SPECTROSCOPIC MEASUREMENT OF CARBON DIOXIDE IN 867-14699 MARS ATMOSPHERE FOR SURFACE PRESSURE AN0 ATMOSPHERIC COMPOSITION Nbb-31473 CHEMICAL COMPOSITION INFRARED SPECTROSCOPY TO DETERMINE TEMPERATURE,

1-7 CHEUICAL KINETICS SUBJECT INDEX

PRESSURE. AN0 CHEMICAL COMPOSITION OF MARTIAN COLOR PHOTOGRAPHY ATMOSPHERE ~67-16813 MULTICOLOR PHOTOGRAPHIC AND VISUAL PATROL OF ATMOSPHERE AN0 SURFACE OF MARTIAN NORTHERN CHEUICAL KINETICS HEMISPHERE DURING SPRING AN0 SUMMER OF 1964-1965 CHEMICAL SYSTEM AN0 REACTION RATES BEHIND STRONG APPARITION SHOCK WAVES IN MIXTURES OF CARBON DIOXIDE AN0 NASA-CR-83123 N67-21160 e NITROGEN USE0 TO STUDY ENTRY CONDITIONS INTO MARS ATMOSPHERE 166-25276 COLUMN GAS CHROMATOGRAPHY COLUUN PACKED WITH POROUS CHEMICAL KINETICS OF CARBON OIOXIOE FOR MARTIAN POLYMER BEADS FOR USE UITH MASS SPECTROMETER FOR ATMOSPHERIC ENTRY APPLICATIONS RESOLVING MARTIAN ATMOSPHERE COMPONENTS s ARL-67-0113 N67-39458 ~6r-12128

CHEMICAL REACTION COMBUSTION TEMPERATURE CHEMICAL REACTIONS BETWEEN SOLAR HYDROGEN AN0 IGNITION TEMPERATURES OF POWDERED METALS IN CARBON MONOXIOE IN VENUS ATMOSPHERE SIMULATED MARS AN0 VENUS ATMOSPHERES NASA-CR-82960 N67-19904 NASA-CR-62878 N67-20169

CLOUD COUET MARTIAN CLOUD ANALYSIS AN0 TOPOGRAPHICAL SPECTROPHOTOMETRY AN0 POLARIMETRY OF LUNAR RELATIONSHIPS REGIONS, OPTICAL PROPERTIES OF ATMOSPHERE AN0 ESRO-SN-54 N66-31187 SURFACE OF MARS. AN0 COMETARY TAILS NASA-TT-F-362 N66-33526 ANISOTROPIC NONCONSERVATIVE SCATTERING IN MODIFIED SCHUSTER- SCHWARZSCHILO APPROXIMATION AN0 VENUS COMPUTER PROGRAM CLOUD LAYER A67-20931 I BM 7094 COMPUTER PROGRAM FOR THEORETICAL CALCULATION OF OUTGOING INFRARED RADIANCES FROM CLOUD COVER ATMOSPHERES OF EARTH AN0 MARS AS AI0 IN RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN SATELLITE MEASUREMENT INTERPRETATIONS VENUS ATMOSPHERE. NOTING GREENHOUSE EFFECT NASA-TN-0-4045 N67-32936 CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE OF IR ABSORPTION A66-40469 COMPUTER SIMULATION RADIATIVE-CONVECTIVE EQUILIBRI'UM CALCULATIONS FOR WATER CONTENT OF VENUS ATMOSPHERE, AEROSOLSP AN0 TWO-LAYER MARTIAN ATMOSPHERE PRESSURE IN UPPER CLOUD LAYER. AN0 DEVIATIONS IN NASA-CR-75633 N66-29732 DIRECTION OF POLARIZED LIGHT N66-31471 CONFERENCE RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN OBSERVATIONS OF MOON, VENUS, MARS, AN0 VENUS ATMOSPHERE. NOTING GREENHOUSE EFFECT JUPITER - SURFACE FEATURES AND ATMOSPHERIC CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE CHARACTERISTICS - RADIO, RADAR, TELESCOPIC, AN0 OF IR ABSORPTION A67-27859 SPECTROSCOPIC OBSERVATIONS NASA-CR-76142 N66-31446 ATMOSPHERIC MODEL COMPARED WITH ASTRONOMICAL OBSERVATIONS TO DETERMINE EFFECT OF CLOUD COVER PLANETARY PHYSICS SEMINAR - POLARIZATION. AN0 RESULTING HIGH EFFECTIVE TEMPERATURE OF SPECTROMETRIC, AN0 RADIO SIGNAL TECHNIQUES FOR RADIO EMISSION FROM VENUS IN CENTIMETER RANGE MEASURING MARTIAN SURFACE AN0 ATMOSPHERIC a N67-16805 PARAMETERS N67-12664

ATMOSPHERE, TEMPERATURE, AN0 CLOUD COVER OF VENUS CONTAHINATION NASA-CR-86635 N67-32308 PLANETARY CONTAHINATION BY VIABLE TERRESTRIAL MICROORGANISMS TRANSPORTED ON SPACECRAFT CLOUO PHOTOGRAPHY AD-648864 N67-27042 MARTIAN ATMOSPHERE AN0 CRUST ANALYZED, BASED ON MARINER IV CLOUD PHOTOGRAPHS A66-36022 CONTROL SYSTEM OPTIMAL CONTROL THEORY AN0 INFORMATION CLOUO PHYSICS SYSTEMS DEVELOPMENTS ~6r-33596 MARTIAN CLOUDS ANALYSIS AN0 TOPOGRAPHICAL RELATIONSHIPS, DISCUSSING WHITE AN0 YELLOW CONVECTIVE HEAT TRANSFER CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES HEATING RATES IN GAS MIXTURES OF PLANETARY A66- 2995 1 ATMOSPHERES PREDICTED BY EQUATION USING TRANSPORT PROPERTIES OF GASES AT LOWER TEMPERATURES PROBLEMS IN DETECTING ICE AN0 WATER CLOUDS ON A66-27432 VENUS N66-31464 CONVECTIVE AN0 RADIATIVE HEAT TRANSFER TO METHOD FOR CALCULATING PROPERTIES OF MONOCHROMATIC SPACE VEHICLES ENTERING PLANETARY ATMOSPHERES RADIATION THROUGH LAYER OF DISPERSED PARTICLES AT SUPERORBITAL VELOCITIES AN0 ITS APPLICATION TO VENUS CLOUDS NASA-CR-584 N66-37027 N66-31445 CORONA DISCHARGE ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM FROM MARINER I1 RADIOMETER DATA. AN0 CORONA OISCHARGEt PRODUCING SIMPLE ORGANIC THERMODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES MOLECULES A67-19057 NASA-CR-76106 N66-31639 COSUOLOGY APPROXIMATION FORMULA DESCRIBING MONOCHROMATIC PLANET JUPITER RESEARCH, NOTING UNRESOLVED TRANSMISSION, REFLECTION. AN0 ABSORPTION OF QUESTIONS OF COSMOLOGY. INTERIOR STRUCTURE AN0 VENUS CLOUO LAYER N66-31641 GREAT REO SPOT A67-39092 MARTIAN CLOUDS ANALYSIS AN0 TOPOGRAPHICAL CYTOLOGY * RELATIONSHIPS, DISCUSSING WHITE AN0 YELLOW INDIGENOUS BIOLOGY IN VENUS CLOUDS, PROPOSING CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES ISOPYCNIC FLOAT BLADDER MACROORGANISM INGESTING A67-34156 WATER AN0 MINERALS BLOWN UP FROM SURFACE BY L PINOCYTOSIS A67-39556 COHERENT RADAR ON-BOARD TRACKING SYSTEM OF TWO-WAY COHERENT u DOPPLER BETWEEN ENTRY CAPSULE AND ORBITING BUS D FOR DETERMINING ORBIT OF ENTRY CAPSULE AN0 DATA ANALYSIS ESTIMATING ATMOSPHERIC PARAMETERS STRUCTURE AN0 COMPOSITION OF JUPITER ATMOSPHERE, N67-15904 NOTING LABORATORY AN0 OBSERVATIONAL DATA

1-6 SUBJECT INDEX EARTH-MOON SYSTEM

SUPPORTING HYPOTHESIS OF CONSISTENCY WITH SOLAR DYNAMIC STAB1LITY ELEMENTS ABUNDANCE Ab7-30932 INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS FOR POINTED AND SPHERICALLY BLUNT BODIES IN DATA RECORDING UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE DATA RECORDING AN0 REDUCTION OF WATER VAPOR Abb-25275 4 CONTENT IN UPPER ATMOSPHERE OF VENUS AS DETERMINED BY BALLOON CARRIED AUTOMATIC INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS TELESCOPE-SPECTROMETER UNIT Nbb-31408 FOR POINTED AN0 SPHERICALLY BLUNT BODIES IN UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE DATA TRANSMISSION Ab7-19380 c PROPERTIES OF MARS ATMOSPHERE ANALYZED BY EJECTED CAPSULE FROM SPACECRAFT, NOTING EARTH AN0 PLANETARY ATMOSPHERE ENTRY PROBLEMS FOR COMMUNICATIONS SYSTEM A6b-30556 BLUNT NOSED SLENDER VEHICLES NOTING AERODYNAMICS, STABILITY, HEATING, ABLATION AND INTERACTION OF DECELERATOR EFFECTS EXPANDABLE, TERMINAL DECELERATORS FOR MARS AIAA PAPER 67-003 Ab7-42963 ATMOSPHERE ENTRY NASA-CR-79496 Nb7-12052 E DECISION THEORY EARTH DECISION THEORY BIOLOGICAL SEARCH STRATEGIES AN0 ABUNDANCE OF EARTH-LIKE PLANET-CONSIDERATIONS OF PLANETARY QUARANTINE ASPECTS OF MARS EARTH AN0 VENUS ATMOSPHERES Abb-01966 EXPLORATORY MISSIONS NASA-CR-89772 Nb7-40462 ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS FROM MARINER I1 RADIOMETER DATA, AND DEEP SPACE THERMODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES N ASA SPACE EXPLORATION PROGRAMS DESIGN NASA-CR-76106 Nbb-31639 MODIFICATIONS AN0 INSTRUMENTATION DEVELOPMENTS NASA-CR-83745 Nb7-25092 THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS ON CARBON, HYDROGEN, OXYGEN, AN0 NITROGEN IN DENSITY DISTRIBUTION EARTH? VENUS, MARS, AN0 JUPITER ATMOSPHERES SPHERICAL SEMIPASSIVE PROBE FOR OENSITY/ATTITUOE Nbb-31642 AND PRESSURE/ALTITUDE PROFILE OF PLANETARY ATMOSPHERES, NOTABLY MARS AN0 VENUS COMPARISON OF SURFACE AN0 ATMOSPHERIC Abb-30089 CHARACTERISTICS OF EARTH AN0 VENUS NASA-TM-X-57351 Nb7-18435 MARS ATMOSPHERE MODELS AT THREE DENSITY LEVELS NASA-TM-X-53404 Nbb-31944 EARTH ALBEDO RESEARCH ON PLANETARY ATMOSPHERES, VENUS DARK *t. *t. DIELECTRIC CONSTANT SIDE EMISSION. OZONE CONCENTRATION. CLOUD AN0 INDUCED ABSORPTION COEFFICIENTS IN ATMOSPHERE AEROSOL SCATTERING, ATMOSPHERIC RADIATION MODEL MEASURED FOR CALCULATION OF VENUS LOWER ..ATTERING, AN0 EARTH HEAT BUDGET AN0 ALBEDO ATMOSPHERE PROPERTIES FROM RADIO OBSERVATIONS NASA-CR-77048 Nbb-33437 Ab7-12949 EARTH ATMOSPHERE b DIELECTRIC RELAXATION OF GASES AN0 SHARP RISE IN CALCULATION OF THERMODYNAMIC EQUILIBRIUM MICROWAVE ABSORPTION COEFFICIENT IN CYTHEREAN COMPOSITION OF EARTH. VENUS, MARS AN0 ATMOSPHERE Ab7-21372 JUPITER ATMOSPHERES Nbb-28001

DIGITAL COMPUTER ORIGIN OF ATMOSPHERES OF VENUS AND EARTH THEORY AN0 NUMERICAL PROCEDURE FOR DIGITAL Nbb-32034 COMPUTER APPLICATION OF GREENHOUSE EFFECT FOR PLANETARY ATMOSPHERE OF FINITE DEPTH EARTH AN0 PLANETARY OCEAN AN0 ATMOSPHERIC ORIGIN. RM-5076-PR Nb7-22562 EVOLUTIONI AN0 COMPOSITION Nbb-37965

DIURNAL VARIATION MECHANISM REGULATING TOTAL AMOUNT OF EARTH AND MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY MARS ATMOSPHERE TRANSPARENT TO VISIBLE AN0 IR MEASURING EFFECT ON RADIO OCCULTATION OF PLANET. RADIATION Ab7-18052 DETERMINING SHAPE. ATMOSPHERE DENSITY PROFILE, DIURNAL VARIATIONS. ETC Abb-25235 STRUCTURES OF TERRESTRIAL AN0 EXTRATERRESTRIAL ATMOSPHERES Ab7-10997 MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, RELATIONSHIP BETWEEN TERRESTRIAL AND JOVIAN DETERMINING SHAPE. ATMOSPHERE DENSITY PROFILE. ATMOSPHERIC CIRCULATIONS DUE TO SOLAR ACTIVITY DIURNAL VARIATIONS. ETC Ab7-21215 JPL-TR-32-1157 Ab7-26819 OXYGENIC CONCENTRATIONS IN PRIMITIVE EARTH DUST ATMOSPHERE, DISCUSSING MARTIAN ATMOSPHERE OUST CLOUD FORMATION BY THERMAL CONVECTION IN COMPOSITION Ab7-34095 MARTIAN ATMOSPHERE Abb-30925 ATMOSPHERIC DATA FOR EARTH, MARS, AND VENUS SPHERICAL OUST PARTICLE TERMINAL VELOCITIES IN Nb7-19026 MODEL VENUS ATMOSPHERE LMSC-6-77-67-16 Nb7-34596 EARTH ATMOSPHERIC RADIATION SPECTRAL INFLUENCES ON INFRARED MEASUREMENTS OF PLANETARY ATMOSPHERES OYNAUIC MODEL NASA-CR-84157 Nb7-26507 DYNAMIC MODEL STUDY TO DETERMINE LOW SUBSONIC SPEED STABILITY AN0 DRAG CHARACTERISTICS DURING I BH 7094 COMPUTER PROGRAM FOR THEORETICAL I VERTICAL DESCENT OF ENTRY CONFIGURATIONS CALCULATION OF OUTGOING INFRARED RADIANCES FROM CONSIDERED FOR PROBES OF PLANETARY ATMOSPHERES ATMOSPHERES OF EARTH AN0 MARS AS AI0 IN NASA-TN-0-3499 N6b-31351 SATELLITE MEASUREMENT INTERPRETATIONS NASA-TN-0-4045 Nb7-32936 DYNAMIC RESPONSE SPHERICAL ENTRY VEHICLE USE0 TO DEFINE PLANETARY EARTH-NOON SYSTEM Y ATMOSPHERE STRUCTURE AN0 COMPOSITION FROM DYNAMIC EARTH-MOON SYSTEM ORIGIN ASSUMING MOON WAS FORMED RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC FROM TERRESTRIAL MATERIAL EJECTED FROM EARTH CHARACTER1STICS Ab7-40177 DURING ROTATIONAL INSTABILITY Ab7-42325

1-9 ECLIPSE SUBJECT INDEX

EC LIPSE ENERGY EQUATION MARS ATMOSPHERIC DENSITY DETERMINED FROM NUMERICAL SOLUTION OF TRANSPORT AN0 ENERGY PHOTOELECTRIC MEASUREMENTS OF ECLIPSES OF PHOBOS EQUATIONS IN PLANETARY BOUNDARY LAYER Abb-30049 ECOM-6020 Nbb-33271

'g ECOLOGY ENERGY LEVEL SIMULATED MARTIAN ATMOSPHERIC AND ECOLOGICAL DATA REPRESENTING MONOPOLE ANTENNA VOLTAGE EFFECTS ON BACILLUS CEREUS SPORE GERMINATION BREAKOWON IN SIMULATED MARS AN0 VENUS NASA-CR-74969 Nbb-26263 ATMOSPHERES Ab7-35829

EIGENFUNCTION ENERGY TRANSFER NUMERICAL CALCULATION OF PERIOOS OF NATURAL RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE ROTATIONAL SPEED A6b-27534 OF IR ABSORPTION A6b-40469

NUMERICAL CALCULATION OF PERIOOS OF NATURAL RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE ROTATIONAL SPEED Abb-42320 OF IR ABSORPTION Ab7-27859

ELECTRIC DISCHARGE ENGINEERING DEVELOPMENT NONTHERMAL RADIO EMISSION FROM ELECTRIC DISCHARGES OPTIMAL CONTROL THEORY AND INFORMATION WITHIN VENUS WATER CLOUDS A67-37480 SYSTEMS DEVELOPMENTS Nb7-33596

ELECTRON BEAM ENTROPY ION SOURCES WITH MAGNETICALLY ALIGNED ELECTRON EXTRATERRESTRIAL LIFE DETECTION STUDIED FROM BEAM AND COMPATIBILITY WITH QUADRUPOLE MASS KNOWLEDGE OF MAJOR AN0 TRACE COMPONENTS OF SPECTROMETER FOR PLANETARY ATMOSPHERIC ANALYSIS ATMOSPHERES 167-40999 NASA-CR-774 Nb7-25054 ENVIRONMENT MODEL ELECTRON DENSITY ATMOSPHERE OF MARS STUDIED USING THREE MODELS MARS ATMOSPHERE MODELS BASED ON MARINER IV GENERATE0 TO SHOW HIGH, MEAN AN0 LOW DENSITY OCCULTATION DERIVING ELECTRON NUMBER DENSITY, COMPOSITIONS TO ACCOUNT FOR GRAVITATIONAL AN0 TEMPERATURES PRESSURE, MASS OENSITYI ETCI NOTING MAGNETIC FIELDS Ab7-40140 CARBON DIOXIDE PRESENCE Abb-30713 ENVIRONMENT SIMULATION ELECTRON FLUX DATA REPRESENTING MONOPOLE ANTENNA VOLTAGE SPACE RECEIVER OBSERVATIONS OF JOVIAN DECAMETER BREAKOWON IN SIMULATED MARS AN0 VENUS FLUX ATMOSPHERES Ab7-35829 *e NASA-CR-82654 Nb7-19113 SIMULATION FACILITY FOR ATMOSPHERIC COMPOSITION, ELECTRON-ION RECOMBINATION PRESSURE, AN0 DAILY VARIATIONS OF MARS AN0 CARBON DIOXIDE IONS WITH ELECTRONS DISSOCIATIVE OTHER PLANETS RECOMBINATION MEASUREMENTS WITH MICROWAVE- NASA-TT-F-11062 Nb7-27533 AFTERGLOW DIFFERENTIALLY PUMPED QUADRUPOLE MASS- 4, SPECTROMETER APPARATUS. NOTING MARTIAN ATMOSPHERE EQUILIBRIUM MODEL RADIATIVE-CONVECTIVE EQUILIBRIUM CALCULATIONS FOR SRCC-55 Ab7-32826 TWO-LAYER MARTIAN ATMOSPHERE NASA-CR-75633 Nbb-29732 ELECTRONIC EQUIPMENT OPTICAL AN0 ELECTRONIC COMPONENTS FOR ULTRAVIOLET TOTAL EQUILIBRIUM SHOCK LAYER RADIATIVE HEAT ROCKET SPECTROPHOTOMETRY IN PLANETARY ATMOSPHERE TRANSFER FOR ENTRY BODY CONFIGURATIONS IN NASA-CR-78485 N6b-38722 SIMULATED MARS ATMOSPHERE Nb7-12109

ELEMENT ABUNDANCE EQUILIBRIUM FLOW COMPOSITION AND SURFACE PRESSURE OF MARTIAN THERMODYNAMIC PROPERTIES OF THREE MARTIAN MODEL ATMOSPHERE DETERMINED FROM PHOTOGRAPHIC SPECTRUM ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOW OF MARS OBTAINED AT MARCH 1965 OPPOSITION FIELDS FOR REAL GASES - TABLES A67-11695 ATOM-66-1 Nb7-34135

THERMODYNAMIC EQUILIBRIUM COMPOSITION OF ALL ERROR COMBINATIONS OF C, H. 0 AN0 N AT AVERAGE SINGLE AN0 DOUBLE GAS NUMBER-DENSITY EQUATIONS FOR PRESSURE AN0 TEMPERATURE CALCULATED FOR DETERMINING TEMPERATURE-ALTITUDE PROFILE, HIGH ATMOSPHERES OF EARTH, VENUS, MARS AN0 JUPITER AN0 LOW SOLAR ACTIVITY ATMOSPHERIC MODELS. AN0 Ab7-22236 ERROR ANALYSIS NASA-CR-79525 Nb7-13018 STRUCTURE AN0 COMPOSITION OF JUPITER ATMOSPHERE. NOTING LABORATORY AND OBSERVATIONAL DATA ETHANE SUPPORTING HYPOTHESIS OF CONSISTENCY WITH SOLAR I R OBSERVATIONS FOR PRESENCE OF ETHANE IN ELEMENTS ABUNDANCE Ab7-30932 ATMOSPHERES OF JUPITER AN0 SATURN REANALYZED AND FOUND CONSISTENT WITH PREVIOUS RESULTS ATMOSPHERIC PRESSURE AT CLOUD TOP AN0 HYDROGEN Ab7-21218 ABUNDANCE IN JUPITER ATMOSPHERE DETERMINED BY ANALYZING METHANE SPECTRAL LINE WIDTHS EVOLUTION Ab7-37479 EVOLUTION OF ATMOSPHERIC COMPONENTS OF VENUS Ab7-80916 UPPER LIMIT OF CARBON DIOXIDE ABUNDANCE IN MERCURY ATMOSPHERE Ab7-41836 EXPERIMENT DESIGN 1 EXPERIMENTAL METHOD FOR STUDYING TAYLOR COLUMNS EMISSION SPECTRUM OVER HILLS AND HOLES IN JUPITER ATMOSPHERE SPECTRAL VARIATION IN LIGHT POLARIZATION OF Ab7-39000 MARTIAN ATMOSPHERE FOR ALL OBSERVABLE PHASE ANGLES Abb-29643 EXTRATERRESTRIAL ENVIRONMENT ANNOTATED BIBLIOGRAPHY ON PLANETARY ATMOSPHERES w, ENERGY DISSIPATION NASA-SP-7017/01/ Nbb-36130 ENERGY DISSIPATION AN0 OTHER PROBLEMS FOR ALIEN PLANETARY ATMOSPHERIC ENTRY AT HIGH SPEEDS OF STRUCTURES OF TERRESTRIAL AN0 EXTRATERRESTRIAL INTERPLANETARY FLIGHT Ab7-21155 ATMOSPHERES Ab7-18997

1-10 SUBJECT INDEX GEOMAGNETIC MICROPULSATION

STRUCTURE AN0 COMPOSITION OF JUPITER ATMOSPHEREI FREE OSCILLATION NOTING LABORATORY AND OBSERVATIONAL DATA CYLINDRICAL FUNCTIONS FOR CALCULATING FREE SUPPORTING HYPOTHESIS OF CONSISTENCY WITH SOLAR OSCILLATIONS OF SATURN RINGS AN0 ESTIMATION OF ELEMENTS ABUNDANCE 167-30932 UPPER LIMIT TO MASS OF RING IF MOTION IS STABLE AGAINST AXISYMMETRIC PERTURBATIONS EXTRATERRESTRIAL LIFE Abb-41063 DETECTING PLANETARY LIFE FROM EARTH Ab7-24063 FREEZING FROST PHENOMENA ON MARS EXAMINED ON BASIS OF VOYAGER PROJECT GOALS, ORBITAL OPERATIONSt CAPSULE MARTIAN WAVE OF DARKENING, NOTING NECESSITY OF DESCENT, NAVIGATIONAL SYSTEMS, ETC DELIQUESCENT SALTS TO ATTRACT AN0 RETAIN WATER ON Ab7-25232 SURFACE Ab7-18645

VOYAGER PROJECT GOALS, ORBITAL OPERATIONS, CAPSULE FROST DESCENT, NAVIGATIONAL SYSTEMS. ETC MARTIAN WAVE OF DARKENING ATTRIBUTE0 TO SOIL FROST Ab7-31487 PHENOMENA Ab 6-40478

INDIGENOUS BIOLOGY IN VENUS CLOUDS, PROPOSING FUNGUS ISOPYCNIC FLOAT BLADDER MACROORGANISM INGESTING RESPONSE OF FUNGI TO DIURNAL TEMPERATURE EXTREMES, WATER AND MINERALS BLOWN UP FROM SURFACE BY DESCRIBING SOIL, SIMULATED MARTIAN TEMPERATURE PINOCYTOSIS Ab7-39556 REGIME AND FUNGI GROWTH Ab7-21991

EXTRATERRESTRIAL LIFE DETECTION STUDIED FROM KNOWLEDGE OF MAJOR AN0 TRACE COMPONENTS OF G ATMOSPHERES 167-40999 6AMHA RADIATION MARTIAN SURFACE AND ATMOSPHERIC PARAMETER MEASUREMENTS BY MEANS OF GAMMA RAY SPECTROMETRIC F INSTRUMENTATION ABOARD VOYAGER MISSION FLAME IONIZATION Nb7-12667 DISSOCIATION LAYER HEIGHTS ON VENUS, MARS AND JUPITER, NOTING CO FLAME AIRGLOW INTENSITIES GAS CHROMATOGRAPHY Abb-30050 MICRO GAS CHROMATOGRAPHIC SYSTEM FOR MARS ATMOSPHERE ANALYSIS DURING CAPSULE DESCENT FLIGHT SIMULATION Abb-2727 B SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE. STATISTICAL DECISION THEORY APPLIED TO MARTIAN TRACKING, COST AND SCHEDULE ATMOSPHERE ANALYSIS, LIFE DETECTION EXPERIMENTS, AIAA PAPER 65-219 Abb-27874 AN0 GAS CHROMATOGRAM MEASUREMENTS OF N-ALKANE DISTRIBUTIONS IN MATERIALS FLOW PATTERN NASA-CR-77234 Nbb-34667 TAYLOR COLUMNS OCCURRENCE CRITERION IN JUPITER ATMOSPHERE INVESTIGATED EXPERIMENTALLY, GIVING GAa CHROMATOGRAPHY COLUMN PACKED WITH POROUS FLOW PATTERNS Ab7-38999 POLYMER BEADS FOR USE WITH MASS SPECTROMETER FOR RESOLVING MARTIAN ATMOSPHERE COMPONENTS FLUID MECHANICS Nb7-12128 TAYLOR COLUMNS OCCURRENCE CRITERION IN JUPITER ATMOSPHERE INVESTIGATED EXPERIMENTALLY, GIVING GAS HIXTURE FLOW PATTERNS Ab f-38999 DIRECT CALCULATION AN0 TABLES OF SPECIFIC HEATS AND RELATED THERMODYNAMIC PROPERTIES OF EXPERIMENTAL METHOD FOR STUDYING TAYLOR COLUMNS ARBITRARY GAS MIXTURES - MARS ATMOSPHERE MODEL OVER HILLS AND HOLES IN JUPITER ATMOSPHERE NASA-TN-0-3540 Nbb-34373 Ab7-39000 MODEL OF NONEQUILIBRIUM PROPERTIES OF HIGH FLUX DENSITY TEMPERATURE CARBON DIOXIDE AND OTHER GAS MIXTURES LIMB DARKENING MEASUREMENTS OF VENUS AT 8-14 IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING MICRONS WITH 200 INCH HALE TELESCOPE MARTIAN ATMOSPHERE Ab7-11436 Abb-32517 GASEOUS COMPOSITION OF UNKNOWN PLANETARY FLYBY HISSION ATMOSPHERE DETERMINED, USING ACOUSTIC EXPERIMENT IONDSOUNOER TECHNIQUES AN0 THEORY TO INVESTIGATE COMBINED WITH PRESSURE AN0 TEMPERATURE DATA PLANETARY ATMOSPHERES FROM FLYBY OR ORBITAL Ab7-13215 MISS IONS NASA-CR-493 Nbb-28011 EQUILIBRIUH RADIATION IN AIR AN0 GAS MIXTURES ASSUMED TO REPRESENT NEAR PLANET ATMOSPHERES SCIENCE SUBSYSTEMS FOR JUPITER FLYBY MISSIONSI NASA-CR-81315 Nb7-16722 DISCUSSING EQUIPMENT SELECTION, MISSION'PLANNINGi SPACECRAFT DESIGN AN0 TRAJECTORY AN0 CONSTRAINTS 6AS SPECTROSCOPY ON VEHICLE CONFIGURATION HIGH-TEMPERATURE GAS RADIANCE IN SIMULATED AIAA PAPER 67-120 167-18287 PLANETARY ATMOSPHERE AT VARIOUS ENTRY VELOCITIES AIAA PAPER 66-183 166-25169 MARINER VENUS PROJECT DESIGN CHANGES FOR FLYBY MISSION AN0 SENSING OF VENUS ATMOSPHERE DIELECTRIC RELAXATION OF GASES AN0 SHARP RISE IN Nb7-25094 MICROWAVE ABSORPTION COEFFICIENT IN CYTHEREAN ATMOSPHERE Ab7-21372 MARINER MARS 1969 PROJECT AN0 SPACECRAFT DESIGN MODIFICATIONS FOR FLYBY MISSIONS GASEOUS DIFFUSION Nb7-25095 GASEOUS BREAKDOWN OF SIMULATED PLANETARY ATMOSPHERES AN0 ILLUSTRATION OF GREENHOUSE FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTIAN EFFECT, THERMAL RADIATION FROM IONIZED ARGON. ATMOSPHERE FOR DETERMINATION OF PROFILES OF LIQUID MAGNETOHYDRODYNAMIC POWER CONVERSION CARBON DIOXIOEI PARTICULATE MATTER AN0 WATER Nb7-23655 VAPOR NASA-TN-0-4115 Nb7-34884 6EOASTROPHYSICS GEOASTROPHYSICS RESEARCH PERTAINING TO PLANETARY FREE FLIGHT TEST APPARATUS ATMOSPHERES AN0 GEOMAGNETIC PULSATION FREE FALLING PROBE TEST DURING TERMINAL DESCENT Nb7-2b461 FOR DETERMINING UNKNOWN PLANETARY ATMOSPHERE PROFILE FROM ONBOARD MEASUREMENTS ALONE GEOMAGNETIC HICROPULSATION Ab7-22768 GEOASTROPHYSICS RESEARCH PERTAINING TO PLANETARY

1-11 GEOPHYSICAL SATELLITE SUBJECT INDEX

ATMOSPHERES AND GEOMAGNETIC PULSATION GREENHOUSE MODEL OF VENUS ATMOSPHERE N67-26461 NASA-TM-X-53497 ~67-29983

GEOPHYSICAL SATELLITE GROUND SUPPORT SYSTEH TERRESTRIAL OBSERVATIONS FROM MANNED GEOPHYSICAL GROUND INSTRUMENTATION SYSTEM FOR MARINER 1’4 SATELLITE APPLIED TO PLANETARY ATMDSPHERIC OCCULTATION EXPERIMENT7 USING DOPPLER FREQUENCY PHENOMENA - VENUS PROBES PERTURBATION METHOD FOR MARS ATMOSPHERIC P-3418 N66-39579 PARAMETERS DETERHINATION Ab7-34498

GEOPHYSICS GUIDANCE STABILITY RESEARCH ON PLANETARY ATMOSPHERES, VENUS DARK GUIDED PROPULSIVE SOLUTION TO MARS ATMLXPHERE- SIDE EMISSION, OZONE CONCENTRATION, CLOUD AND AEROSOL SCATTERING, ATMOSPHERIC RADIATION AIAA PAPER 67-170 A67-18508 SCATTERING, AN0 EARTH HEAT BUDGET AN0 ALBEDO NASA-CR-77048 N66-33437 H MANNED GEOPHYSICAL OBSERVATIONS FROM SATELLITES AS HEAT BALANCE TRAINING GROUND FOR PLANETARY RESEARCH, ESPECIALLY JUPITER AND SATURN MODELS, GIVING PLANET VENUS ATMOSPHERE A67- 11395 CONSTITUTION. HEAT BALANCE AND ATMOSPHERIC COMPOSITION Abl-39001 GERDIEN CONDENSER GERDIEN TYPE CHAMBER FOR MEASUREMENTS OF ION HEAT BALANCE. PRESSURIZATION9 AND MINIMUM WEIGHT MOBILITY SPECTRUM IN TERRESTRIAL MESOSPHERE AND DESIGN CRITERIA FOR INFLATABLE STRUCTURES IN MARS ATMOSPHERE Ab6-34712 NEAR-PLANETARY ATMOSPHERE NASA-CR-84829 N67-28789 GERMINATION SIMULATED MARTIAN ATMOSPHERIC AND ECOLOGICAL ESTIMATES OF VERTICAL TEMPERATURE STRUCTURE. HEAT EFFECTS ON BACILLUS CEREUS SPORE GERMINATION BALANCE, SOLSTICE CIRCULATION. AND THERMALLY NASA-CR-74969 Nb6-26263 DRIVEN TIDES ON MARS IN COMPARISON WITH LIKE CONDITIONS ON EARTH GLOW DISCHARGE NASA-CR-86912 Nb7-32494 UPPER ATMOSPHERE GLOW DISCHARGES STUDIED IN CONNECTION WITH THERMAL RADIO NOISE EMISSION HEAT BUDGET FROM VENUS SURFACE N66-38994 COMPARING ATMOSPHERE MODELS OF MARS BASED ON I MARINER IV OCCULATION DATA INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS NASA-CR-78134 N b6-372 14 THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS HAVE BEEN OBSERVED IN X-BAND FROM GLOH DISCHARGES HEAT SHIELD Ab7-14952 INTERPLANETARY TRANSIT AND ATMOSPHERIC ENTRY OF *) UNMANNED VEHICLE LANDING ON MARS SURFACE7 WITH GRAVITATIONAL EFFECT REFERENCE TO HEAT SHIELD TECHNOLOGY ATMOSPHERE OF MARS STUDIED USING THREE MODELS JPL-TR-32-1145 A67-25715 GENERATED TO SHOW HIGH, MEAN AND LOW DENSITY COMPOSITIONS TO ACCOUNT FOR GRAVITATIONAL AND AERODYkANICr THERMODYNAMIC, HEAT SHIELD AND MAGNETIC FIELDS 167-40140 STRUCTURAL DESIGN ASPECTS OF BALLISTIC VEHICLE ENTERING PLANETARY ATMOSPHERE A67-35315 ’ GRAVITY MARTIAN ATMOSPHERIC SURFACE PRESSURE BETWEEN HELIOCENTRICITY OCCULTATION LEVELS AT ELECTRICS AND MARE BLUE CLEARINGS OF MARS ATMOSPHERE AS FUNCTION OF ACIDALIUM NUMBER OF METEOR SHOWERS INTERSECTING MARS NASA-CR-75816 N6b-29298 ORBIT AT INTERVALS OF HELIOCENTRIC LONGITUDE NASA-CR-59938 N66-33414 GREENHOUSE EFFECT RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN HIGH TEHPERATURE AIR VENUS ATMOSPHERE7 NOTING GREENHOUSE EFFECT EQUILIBRIUM RADIATION IN AIR.AND GAS MIXTURES CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE ASSUMED TO REPRESENT NEAR PLANET ATMOSPHERES OF IR ABSORPTION Abb-40469 NASA-CR-81315 N67-16722

GREENHOUSE EFFECT IN GRAY PLANETARY ATMOSPHERE HUH IO1TY A6b-81145 DOPPLER-DISPLACED LINES OF WATER VAPOR ORIGINATING IN ATMOSPHERE OF VENUS OBSERVED ON THREE COUDE NONGRAY MODEL ATMOSPHERES OF JOVIAN PLANETS SPECTROGRAMS A67-11774 CONSTRUCTED FOR DIFFERENT RELATIVE CONCENTRATIONS OF HELIUM AND DIATOMIC HYDROGEN AND VARIOUS LIKELY HYDROCARBON EFFECTIVE TEMPERATURES AS CHIEF SOURCES OF THERMAL ION-MOLECULE CHEMISTRY OF JUPITER UPPER OPACITY Ab7-22237 ATMOSPHERE, STUDYING EQUILIBRIUM AND NONEQUILIBRIUM ABUNDANCES OF HYDROCARBON PRODUCTS RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN DUE TO UV RADIATION REACTION A67-34540 VENUS ATMOSPHERE. NOTING GREENHOUSE EFFECT CAUSE0 BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE HYDROCHLORIC ACID OF IR ABSORPTION Ab7-27859 UPPER LIMITS ON LIQUID WATER CONTENT IN VENUS ATMOSPHERE Ab7-3265 2 VENUS SURFACE TEMPERATURE AND MICROWAVE EMISSIONS DISCUSSING IONOSPHERIC MODEL, GREENHOUSE EFFECT, HYDRODYNAMICS MICROOISCHARGE MODEL. RADIO AURORA. ETC EXPERIMENTAL ANALYSIS OF TAYLOR COLUMNS LIKELY TO A67-34543 BEAR ON PROCESSES OCCURRING IN JUPITER ATMOSPHERE A66-33013 THEORY AN0 NUMERICAL PROCEDURE FOR DIGITAL * COMPUTER APPLICATION OF GREENHOUSE EFFECT FOR PLANETARY SCALE ATMOSPHERIC CIRCULATIONS OF PLANETARY ATMOSPHERE OF FINITE DEPTH JUPITER AN0 SATURN USING FLUID DYNAMICS, NOTING RM-5076-PR Nb7-22562 ROTATION EFFECTS Ab6-41619

GASEOUS BREAKDOWN OF SIMULATE0 PLANETARY HYDROGEN ATMOSPHERES AN0 ILLUSTRATION OF GREENHOUSE MOLECULAR HYDROGEN STRUCTUREt CONSIDERING ‘I EFFECT7 THERMAL RADIATION FROM IONIZED ARGON. PLANETARY AND STELLAR ATMOSPHERES AND INTERSTELLAR LIQUID MAGNETOHYDRODYNAMIC POWER CONVERSION SPACE A6b-39487 Nb7-23655 ATMOSPHERIC PRESSURE AT CLOUD TOP AND HYDROGEN DERIVATION OF ATMOSPHERIC PARAMETERS FOR ABUNDANCE IN JUPITER ATMOSPHERE DETERMINED BY

1-12 SUBJECT INDEX Ir4STRUMENTAL ANALYSIS

ANALYZING METHANE SPECTRAL LINE WIDTHS NASA-CR-04157 Nb7-26507 Ab7-37479 INFRARED RADIATION CHEMICAL REACTIONS BETWEEN SOLAR HYDROGEN AND RAOIANT ENERGY TRANSFER BELOW CLOUD COVER IN * CARBON MONOXIDE IN VENUS ATMOSPHERE VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT NASA-CR-82960 N67-19904 CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE OF IR ABSORPTION Abb-40469 HYDROGEN CHLORIDE VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON MECHANISM REGULATING TOTAL AMOUNT OF EARTH AN0 INTERFEROMETER7 FINDING H CL LINES CONSISTENT MARS ATMOSPHERE TRANSPARENT TO VISIBLE AND IR L WITH 2-MM AMAGAT OF GAS RAD1AT1 ON Ab7-10052 JPL-TR-32-1106 Ab7-24510 RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN UPPER LIMITS ON LIPUID WATER IN VENUS ATMOSPHERE VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT DUE TO PRESENCE OF HYDROGEN CHLORIDE CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE NASA-CR-84601 Nb7-20001 OF IR ABSORPTION Ab7-27059

HYDROSPHERE LIMB DARKENING OF PLANETARY ATMOSPHERES IN THERMAL DISCRETE EPUILIBRIUM TEMPERATURES OF HYPOTHETICAL INFRARED PLANET WITH ATMOSPHERE AN0 HYDROSPHERE OF ONE- NASA-TM-X-57359 Nb7-18200 COMPONENT TWO-PHASE SYSTEM UNDER CONSTANT SOLAR RADIATION Ab7-27462 METHOD FOR CALCULATING INFRARED RADIATION FROM PLANETARY ATMOSPHERES HYPERSONIC FLOW BMWF-FB-W-67-02 N67-30793 MODEL OF NDNEQUILIBRIUM PROPERTIES OF HIGH TEMPERATURE CARBON DIOXIDE AN0 OTHER GAS MIXTURES INVERSE PROBLEM OF RADIATIVE TRANSFER AS APPLIED IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING TO REMOTE MEASUREMENTS OF INFRARED RADIATION MARTIAN ATMOSPHERE A67- 1143 6 FROM PLANETARY ATMOSPHERES NASA-TM-X-55057 Nb7-32049 MAGNETOSPHERIC BOUNDARY AN0 STANDING SHOCK WAVE FOR EARTH SCALED DOWN TO APPLY TO MARS I BM 7094 COMPUTER PROGRAM FOR THEORETICAL Ab7-35442 CALCULATION OF OUTGOING INFRARED RADIANCES FROM ATMOSPHERES OF EARTH AND MARS AS AI0 IN HYPERSONIC REENTRY SATELLITE MEASUREMENT INTERPRETATIONS HYPERSONIC ENTRY VEHICLE MEASUREMENT OF MARS NASA-TN-0-4045 Nb7-32936 ATMOSPHERIC DENSITY, PRESSURE7 COMPOSITION, TEMPERATURE AND DETECTION SPECTROMETRY OF CHEMICAL INFRARED SPECTROMETER SPECIES IN SHOCK LAYER Abb-42600 VIBRATION AND THERMAL RADIATION EFFECTS ON FILTER WEDGE INFRARED SPECTROMETER USED IN SPACECRAFT &+ STUDIES OF PLANETARY ATMOSPHERES I NASA-CR-85797 Nb7-31336 ICE DETERMINATION OF ICE CLOUDS AND WATER VAPOR IN INFRARED SPECTROSCOPY VENUS ATMOSPHERE FROM BALLOON OBSERVATIONS CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K Nbb-31463 DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS c OF MARS 867-14309 PROBLEMS IN DETECTING ICE AND WATER CLOUDS ON VENUS Nbg-31464 RAOAR.-RADIO ASTRONOMIC AND IR SPECTROSCOPIC OBSERVATIONS OF VENUS SURFACE AND ATMOSPHERE7 ICE FORMATION EXAMINING GENERAL AND SURFACE DATA, CHEMICAL PHOTOMETRY OF INTEGRATED LIGHT OF VENUSI COMPOSITION AND ATMOSPHERIC MODEL CONSTRUCTION INFERRING PRESENCE OF ICE IN ATMOSPHERE FROM HALO ~67-24843 EFFECT OF BRIGHTNESS DISPERSION Ab7-16407 INFRARED SPECTROSCOPY TO DETERMLNE TEMPERATURE, PRESSURE, AN0 CHEMICAL COMPOSITION OF MARTIAN FROST PHENOMENA ON MARS EXAMINED ON BASIS OF ATMOSPHERE Nb7-16813 MARTIAN WAVE OF DARKENING, NOTING NECESSITY OF DELIQUESCENT SALTS TO ATTRACT AND RETAIN WATER ON FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTTAN SURFACE Ab7-10645 ATMOSPHERE FOR DETERHINATION OF PROFILES OF CARBON DIOXIDE. PARTICULATE MATTER AND WATER IMAGE INTENSIFIER VAPOR HIGH RESOLUTION SPECTRA OF VENUS AN0 JUPITER NASA-TN-0-4115 Nb7-34084 USING IMAGE INTENSIFIER AN0 SOLAR SPECTROGRAPH, MEASURING ABUNDANCES IN PLANETARY ATMOSPHERES INFRARED SPECTRUM Ab7-36309 NEW ABSORPTION BANDS IN NEAR IR SPECTRUM OF MARS FOUND BY FOURIER SPECTROSCOPY VIA CARBON DIOXIDE INFLATABLE STRUCTURE ABSORPTION MEASUREMENTS Abb-40486 HEAT BALANCE, PRESSURIZATION7 AN0 MINIMUM WEIGHT DESIGN CRITERIA FOR INFLATABLE STRUCTURES IN I R OBSERVATIONS FOR PRESENCE OF ETHANE IN NEAR-PLANETARY ATMOSPHERE ATMOSPHERES OF JUPITER AN0 SATURN REANALYZED AND NASA-CR-B 4829 Nb7-28709 FOUND CONSISTENT WITH PREVIOUS RESULTS Ab7-21210 INFORMATION THEORY OPTIMAL CONTROL THEORY AND INFORMATION INITIAL VALUE PROBLEM SYSTEMS DEVELOPMENTS Nb7-33596 INITIAL VALUE APPROACH TO CHANDRASEKHAR PLANETARY PROBLEM TO ESTIMATE PLANETARY PROPERTIES AN0 INFRARED ASTRONOMY ATMOSPHERIC COVERS CARBON OIOXIDE STUDY IN MERCURY ATMOSPHERE YIELDS RM-4991-PR N6b-29959 c NEGATIVE RESULTS FROM OBSERVATIONS MADE WITH IR SPECTROMETER AN0 61 INCH REFLECTOR INSTRUMENT PACKAGE Ab7-22016 MARTIAN ATMOSPHERE SAMPLING BY SENSORS OF PARACHUTE DROPPED CAPSULE Nbb-32064 SOLUTION OF ANGULAR DISTRIBUTION OF OUTGOING v THERMAL RADIATION FROM PLANETARY ATMOSPHERE. USING INSTRUMENTAL ANALYSIS CHANDRASEKHAR DIFFUSE SCATTERING AN0 TRANSMISSION GAS CHROMATOGRAPHY COLUMN PACKED WITH POROUS FUNCTIONS . Ab7-22240 PDLYMER BEADS FOR USE WITH MASS SPECTROMETER FOR RESOLVING MARTIAN ATMOSPHERE COMPONENTS EARTH ATMOSPHERIC RADIATION SPECTRAL INFLUENCES ON Nb7-12128 INFRARED MEASUREMENTS OF’ PLANETARY ATMOSPHERES

1-13 INSTRUMENTATION SUBJECT INDEX

INSTRUMENTATION NASA-CR-84412 N67-27370 OPTICAL RADIOMETER FEASIBILITY STUDY FOR DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM IONOSPHERIC CO~POSlTIOlv SHOCK LAYER RADIATION DURING ENTRY - IONOSOUNDER TECHNIQUES AND THEORY TO INVESTIGATE INSTRUMENTATION PLANETARY ATMOSPHERES FROM FLYBY OR ORBITAL * NASA-03-73027 Nbb-35663 MISSIONS NASA-CR-493 N66-28011 SURFACE AND ATMOSPHERIC PARAMETER MEASUREMENTS BY USE OF POLARIZATION INSTRUMENTATION ABOARD IONOSPHERIC ELECTRON DENSITY MARINER ORBITER SPACE PROBE N67-12666 MARTIAN ATMOSPHERE AND IONOSPHERE ELECTRON DENSITY AND REFRACTIVITY PROFILES DETERMINED BY TWO .( INTEGRAL EQUATION FREQUENCY BEAT OCCULTATION TECHNIQUE USE0 BY REDUCTION OF INTEGRAL EQUATIONS OF RADIATIVE MARINER IV SPACE PROBE Nb7-12665 TRANSFER FOR PLANETARY ATMOSPHERE WITH RAYLEIGH SCATTERING FREQUENCY, PHASE, AN0 AMPLITUDE CHANGES OF RM-5056-PR Nbb-35579 MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AN0 IDNOSPHERE OF MARS OBSERVED BEFORE AN0 AFTER INTERPLANETARY OUST PLANETARY OCCULATATION Nb7-12754 CONDITIONS OF ENCOUNTER BETWEEN INTERPLANETARY OUST PARTICLES AN0 PLANETS MARTIAN ATMOSPHERE MODEL DEDUCED FROM MARINER IV NASA-TM-X-57009 Nbb-35309 IDNOSPHERE ELECTRON DENSITY MEASUREMENTS NASA-CR-84825 Nb7-28785 EFFECTIVE BRAKING HEIGHT / EBH/ FOR SMALL INTERPLANETARY PARTICLES OF COSMIC VELOCITY IONOSPHERIC REFLECTION ENTERING MARTIAN UPPER ATMOSPHERE LUMINESCENCE FROM LOWER ATMOSPHERIC LAYERS AN0 Ab7-34541 IDNOSPHERE OBSERVED IN VENUS NIGHT AIRGLOW Nb7-16803 INTERPLANETARY FLIGHT ENERGY DISSIPATION AN0 OTHER PROBLEMS FOR ALIEN JONOSPHERIC SOUNDING PLANETARY ATMOSPHERIC ENTRY AT HIGH SPEEDS OF FEASIBILITY OF USING RADIO SOUNDING TECHNIQUES TO INTERPLANETARY FLIGHT Ab7-21155 INVESTIGATE IONOSPHERIC PROPERTIES OF PLANETS NASA-CR-689 Nb7-28368 INTERPLANETARY PROPULSION CONFIGURATION GUIDE0 PROPULSIVE SOLUTION TO MARS ATMOSPHERE- DECELERATED SOFT LANDING VEHICLE TRAJECTORY J AIAA PAPER 67-170 Ab7-18508 JUPITER /PLANET/ JUPITER PLANETARY SURFACE OBSERVATIONS SHOW SLOW INTERPLANETARY SPACE EVOLUTION OF ATMOSPHERIC PHENOMENA SPACE RECEIVER OBSERVATIONS OF JOVIAN DECAMETER A6b-3 1310 FLUX NASA-CR-82654 Nb7-19113 lBSERVATIDNS OF MOON, VENUS, MARS. AND JUPITER - SURFACE FEATURES AN0 ATflOSPHERIC INTERSTELLAR GAS CHARACTERISTICS - RADIO. RADAR, TELESCOPIC, AN0 MOLECULAR HYDROGEN STRUCTUREt CONSIDERING SPECTROSCOPIC OBSERVATIONS PLANETARY AND STELLAR ATMOSPHERES AN0 INTERSTELLAR NASA-CR-76142 Nbb-31446 SPACE Abb-39487 9 ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS INVARIANT IMBEDDING FROM MARINER I1 RADIOMETER DATA, AND INVARIANT IMBEDDING EQUATIONS FOR DETERMINING THERHODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES VERTICAL STRATIFICATION OF TERRESTRIAL AND NASA-CR-76106 Nbb-31639 PLANETARY ATMOSPHERES ON BASIS OF SATELLITE OBSERVATIONS JUPITER GREAT REO SPOT AN0 THREE WHITE OVALS RM-5229-PR Nb7-32463 SHOW CORRELATION BETWEEN OVAL ROTATIONAL VELOCITY AND LONGITUDINAL DISTANCE FROM RED SPOT INVERSI ON Ab7-37400 INVERSE PROBLEM OF RADIATIVE TRANSFER AS APPLIED TO REMOTE MEASUREMENTS OF INFRARED RADIATION SOVIET BOOK ON PLANETARY PHYSICS COVERING FROM PLANETARY ATMOSPHERES MARTIAN, VENUSIAN AN0 MERCURIAN ATMOSPHERES, NASA-TM-X-55857 Nb7-32849 VENUSIAN SURFACE TEMPERATURE AN0 JOVIAN RADIO EMISSION Ab7-30933 ION ION SOURCES WITH MAGNETICALLY ALIGNED ELECTRON JUPITER AND SATURN MOOELSI GIVING PLANET BEAM AN0 COMPATIBILITY WITH QUADRUPOLE MASS CONSTITUTION, HEAT BALANCE AND ATMOSPHERIC SPECTROMETER FOR PLANETARY ATMOSPHERIC ANALYSIS COMPOSITION Ab7-39001 NASA-CR-774 Nb7-25054 JUPITER ATMOSPHERE ION MOBILITY JOVIAN ROTATIONAL EFFECTS ON MAGNETOSPHERIC MODEL GEROIEN TYPE CHAMBER FOR MEASUREMENTS OF ION AN0 CONDITIONS OF FLUTING AND TWO-STREAM MOBILITY SPECTRUM IN TERRESTRIAL MESOSPHERE AN0 INSTABILITY Abb-29952 MARS ATMOSPHERE A6b-34712 RAPID DRIFT IN LONGITUDE OF SMALL DARK SPOT ON IONOSPHERE SOUTH EDGE OF JUPITER NORTH TENPERATE BELT, MARINER IV MODELS OF THREE MARS ATMOSPHERIC NOTING SINUSOIDAL DISPLACEMENT CHARACTfRISTICS LAYERS ANALOGOUS TO TERRESTRIAL E, F-1 AN0 F-2 AND MEASUREMENT WITH BLUE AND UV PHOTOGRAPHY LAYERS, CONSIDERING RELATIVE MASS DENSITIES, Abb-33009 TEMPERATURES, CARBON DIOXIDE PHOTODISSOCIATION AN0 IONIZATION PROFILE Abb-41779 EXPERIMENTAL ANALYSIS OF TAYLOR COLUMNS LIKELY TO BEAR ON PROCESSES OCCURRING IN JUPITER ATMOSPHERE EFFECTS OF MARINER IV IONOSPHERIC DATA ON Abb-33013 MARS ATMOSPHERE COMPOSITION PREDICTIONS NASA-CR-76666 Nb6-32302 IMAGE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN ASTRONOMY, ASTROPHYSICS, CELESTIAL MECHANICS. DISK IN NEAR IR REGION Ab6-37017 GEODESY, SOLAR PHYSICS. IONOSPHERE AN0 RADIO PHYSICSt FIELDS AND PARTICLES, AND PLANETARY SPECTRAL STUDY OF JUPITER, SATURN AND RINGS OF ATMOSPHERES SATURN, DETERMINING METHANE CONCENTRATION IN NASA-TM-X-57969 Nbb-37946 CLOUD LAYERS Abb-37035 COMPONENT OF MARS IONOSPHERE DUE TO SOLAR PROTONS PLANETARY SCALE ATMOSPHERIC CIRCULATIONS OF

1-14 SUBJECT INDEX LIGHT SCATTERING

JUPITER AN0 SATURN USING FLUID DYNAMICS, NOTING JUPITER ENVIRONMENT? EFFECTS OF HUGE MASS. HIGH ROTATION EFFECTS Abb-41679 ROTATION RATE, TEMPERATURE AND DOMINANT H AND HE ATMOSPHERE Abl-40141 PROPERTIES OF ATMOSPHERES OF MARS, JUPITER AN0 VENUS Nbb-32039 SPACE RECEIVER OBSERVATIONS OF JOVIAN DECAMETER b FLUX SPECTRAL STUDY OF JUPITER, SATURN AND RINGS OF NASA-CR-82654 Nbl-19113 SATURN? DETERMINING METHANE CONCENTRATION IN CLOUO LAYERS Abl-15557 LATITUDE AN0 LONGITUDE OF JUPITER REO SPOT MEASURED FROM PHOTOGRAPHS OBTAINED DURING 1965 +. SCIENCE SUBSYSTEMS FOR JUPITER FLYBY MISSIONS? AN0 1966 DISCUSSING EQUIPMENT SELECTION, MISSION PLANNING, NASA-CR-85560 Nbl-31108 SPACECRAFT DESIGN AN0 TRAJECTORY AN0 CONSTRAINTS ON VEHICLE CONFIGURATION SPECTRAL REFLECTANCE OF SILICATE ROCK POWDERS, AIAA PAPER 61-120 Ab7-18281 JUPITER ATMOSPHERE MEASUREMENTS, AN0 VISIBLE AN0 NEAR-INFRAREO SPECTRUM DATA FOR ANALYZING JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM LUNAR SURFACE N67-34175 CORONA DISCHARGE, PRODUCING SIMPLE ORGANIC MOLECULES Abl-19051 K RELATIONSHIP BETWEEN TERRESTRIAL AN0 JOVIAN KINETIC ENERGY ATMOSPHERIC CIRCULATIONS DUE TO SOLAR ACTIVITY MAGNETOSPHERIC MOOEL OF JUPITER FROM NUMERICAL Abl-21215 CALCULATION OF MAXIMUM NUMBER DENSITY OF PLASMA 161-25206 I R OBSERVATIONS FOR PRESENCE OF ETHANE IN ATMOSPHERES OF JUPITER AN0 SATURN REANALYZED AN0 FOUND CONSISTENT WITH PREVIOUS RESULTS L Ab7-21218 LAMINAR HEAT TRANSFER MARS ATMOSPHERIC COMPOSITION AN0 LAMINAR STIMULATION OF JUPITER RADIO EMISSION BY IO CONVECTIVE HEATING AND ABLATION STUDIED TO PREDICT A61-25204 PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING ENTRY Abb-25274 MAGNETOSPHERIC MOOEL OF JUPITER FROM NUMERICAL CALCULATION OF MAXIMUM NUMBER DENSITY OF PLASMA MARS ATMOSPHERIC COMPOSITION AN0 LAMINAR 667-25206 CONVECTIVE HEATING AN0 ABLATION STUDIED TO PREDICT PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING STRUCTURE AN0 COMPOSITION OF JUPITER ATMOSPHERE, ENTRY Abl-18849 NOTING LABORATORY AN0 OBSERVATIONAL DATA SUPPORTING HYPOTHESIS OF CONSISTENCY WITH SOLAR LANDING noDuLE GUIDE0 PROPULSIVE SOLUTION TO MARS ATMOSPHERE- b- ELEMENTS ABUNDANCE Abl-30932 DECELERATED SOFT LANDING VEHICLE TRAJECTORY MOOEL FOR DISTRIBUTION OF THERMAL PLASMA IN AIAA PAPER 61-170 Ab7-18508 MAGNETOSPHERE OF JUPITER UNDER ASSUMPTION OF COROTATION WITH PLANET Ab7-33196 LENTICULAR BODY MARTIAN CLOUOS ANALYSIS AN0 TOPOGRAPHICAL

I8 ATOMIC AN0 MOLECULAR PROCESSES IN CYTHEREAN? RELATIONSHIPS. DISCUSSING WHITE AN0 YELLOW MARTIAN AN0 JOVIAN UPPER ATMOSPHERES CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES 667-34158 Abb-29951

ION-MOLECULE CHEMISTRY OF JUPITER UPPER MARTIAN CLOUDS ANALYSIS AN0 TOPOGRAPHICAL ATMOSPHERE? STUDYING EQUILIBRIUM AN0 RELATIONSHIPS. DISCUSSING WHITE AN0 YELLOW NONEQUILIBRIUM ABUNOANCES OF HYDROCARBON PRODUCTS CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES DUE TO UV RADIATION REACTION Ab7-34540 Abl-34156

NONTHERMAL RADIO EMISSION FROM JUPITER LIFE ATMOSPHERE, STUDYING IO MOOULATIDN EFFECT PLANETARY ATMOSPHERES AN0 POSSIBILITY OF LIFE IN Ab7-34933 SOLAR SYSTEM P-3669 Nb7-39518 HIGH RESOLUTION SPECTRA OF VENUS AN0 JUPITER USING IMAGE INTENSIFIER AN0 SOLAR SPECTROGRAPH, LIFE DETECTOR MEASURING ABUNOANCES IN PLANETARY ATMOSPHERES STATISTICAL DECISION THEORY APPLIED TO MARTIAN Abl-36309 ATMOSPHERE ANALYSIS, LIFE DETECTION EXPERIMENTS? AN0 GAS CHROMATOGRAM MEASUREMENTS OF N-ALKANE JUPITER GREAT RED SPOT AN0 THREE WHITE OVALS DISTRIBUTIONS IN MATERIALS SHOW CORRELATION BETWEEN OVAL ROTATIONAL VELOCITY NASA-CR-71234 Nb6-34667 AN0 LONGITUDINAL DISTANCE FROM REO SPOT Abl-31400 DETECTING PLANETARY LIFE FROM EARTH Ab7-24063 ATMOSPHERIC PRESSURE AT CLOUO TOP AN0 HYDROGEN ABUNDANCE IN JUPITER ATMOSPHERE DETERMINED BY LIFT ANALYZING METHANE SPECTRAL LINE WIDTHS PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS Abl-31479 LANDING MISSION, DISCUSSING USE OF LIFTING VEHICLES Abb-25273 TAYLOR COLUMNS OCCURRENCE CRITERION IN JUPITER ATMOSPHERE INVESTIGATED EXPERIMENTALLY, GIVING AERODYNAMIC LIFT IN FUTURE SPACE VEHICLE DESIGN FLOW PATTERNS Ab7-38999 DURING VARIOUS FLIGHT REGIMES IN ATMOSPHERES OF EARTH AN0 PLANETS EXPERIMENTAL METHOD FOR STUDYING TAYLOR COLUMNS P-3559 Nbl-28513 r OVER HILLS AN0 HOLES IN JUPITER ATMOSPHERE 161-39000 LIGHT ABSORPTION DIFFUSE REFLECTION BY PLANETARY INHOMOGENEOUS PLANET JUPITER RESEARCH, NOTING UNRESOLVED ATMOSPHERE WITH ALBEOO FOR SINGLE SCATTERING QUESTIONS OF COSMOLOGYt INTERIOR STRUCTURE AN0 DECREASES EXPONENTIALLY WITH OPTICAL DEPTH GREAT REO SPOT Abl-39092 Abb-34149 e PHOTOMETRIC OBSERVATION DATA ON JUPITER LIGHT SCATTERING ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- LIGHT DIFFUSION OF MARTIAN ATMOSPHERE MEASURED BY MONTH PERIODIC CHANGE Abl-39299 SPECTROSCOPIC EVALUATION OF POLARIZATION VARIATION FROM DISK CENTER TO EDGE A6b-25461

3-15 LIGHT TRANSMISSION SUBJECT INDEX

COMPUTED EFFECTS OF SPECULAR REFLECTION ON MAGNETIC FIELDS Ab7-4014P SCATTERING OF LIGHT BY RAYLEIGH PLANETARY ATMOSPHERE ION SOURCES WITH MAGNETICALLY ALIGNED ELECTRON NASA-CR-76122 Nbb-30187 BEAM AN0 COMPATIBILITY WITH QUADRUPOLE MASS SPECTROMETER FOR PLANETARY ATMOSPHERIC ANALYSIS *t ANISOTROPIC NONCONSERVATIVE SCATTERING IN MODIFIED NASA-CR-774 Nb7-25054 SCHUSTER- SCHWARZSCHILD APPROXIMATION AND VENUS CLOUD LAYER Ab7-20931 UAGNETOHYDRODYNAMIE GENERATOR GASEOUS BREAKDOWN OF SIMULATED PLANETARY MODEL FOR MARTIAN ATMOSPHERE AN0 PLANETARY ATMOSPHERES AN0 ILLUSTRATION OF GREENHOUSE SURFACE ASSUMING ATMOSPHERIC SPECTRUM WITH EFFECT, THERMAL RADIATION FROM IONIZED ARGON, PURELY SCATTERING PROPERTIES AND SURFACE LIQUID MAGNETOHYDROOYNAXIC POWER CONVERSION COVERED WITH LIMONITE DUST Nb7-lb809 Nbl-23655

SCATTERING ANISOTROPY EFFECT ON OPTICAL PARAMETERS MAGNETOHYDRODYNAMICS OF MARTIAN ATMOSPHERE AND SURFACE - PHOTOMETRY PLANETARY SCALE ATMOSPHERIC CIRCULATIONS OF Nb7-16820 JUPITER AND SATURN USING FLUID DYNAMICS, NOTING ROTATION EFFECTS Abb-41 b19 SCATTERING OF LIGHT IN PLANETARY ATMOSPHERES AN0 DIFFUSE REFLECTION OF LIGHT BY TURBID MEDIUM MAGNETOSPHERE Nb7-23425 JOVIAN ROTATIONAL EFFECTS ON MAGNETOSPHERIC MODEL AND CONDITIONS OF FLUTING AND TWO-STREAM LIGHT TRANSMISSION INSTABILITY Abb-29952 CALCULATION OF TOTAL RADIATION EMERGING FROM PLANETARY ATMOSPHERES OPTICALLY THICKER THAN MOOEL FOR DISTRIBUTION OF THERMAL PLASMA IN THOSE OF EARTH MAGNETOSPHERE OF JUPITER UNOER.ASSUMPTION OF RM-5343-PR Nb7-32966 COROTATION WITH PLANET Ab7-33196

LIMB MAGNETOSPHERIC BOUNDARY AND STANDING SHOCK WAVE LIMB-DARKENING OBSERVATIONS OF VENUS BY MARINER FOR EARTH SCALED DOWN TO APPLY TO MARS I1 SPACECRAFT MICROWAVE RADIOMETERS Ab7-35442 Nb6-3 1640 MAGNETOSPHERIC ELECTRON DENSITY CURVES OF MONOCHROMATIC ALBEDO FOR LIMB AND MAGNETOSPHERIC MODEL OF JUPITER FROM NUMERICAL TERMINATOR OF VENUS Nb7-16806 CALCULATION OF MAXIMUM NUMBER DENSITY OF PLASMA Ab7-25206 LOW SPEED STABILITY DYNAMIC MODEL STUDY TO DETERMINE LOW SUBSONIC MANNED SPACE FLIGHT SPEED STABILITY AND DRAG CHARACTERISTICS DURING N ASA METEOROLOGICAL FLIGHT PROGRAM PLANS, VERTICAL DESCENT OF ENTRY CONFIGURATIONS PROCEDURES FOR PARTICIPATION IN SPACE FLIGHT -% CONSIDERED FOR PROBES OF PLANETARY ATMOSPHERES PROGRAMS. AN0 REQUIREMENTS FOR METEOROLOGICAL NASA-TN-0-3499 Nbb-3 1351 RESEARCH ON MARS Nb7-24309

LOWER ATMOSPHERE MANNED SPACECRAFT ESTIMATES AN0 DEFINITIONS ON CHARACTERISTICS OF MANNED MARS EXCURSION VEHICLE FOR THIN MARS VENUS LOWER ATMOSPHERE ATMOSPHERE B P-3513 Nb7-22577 NASA-TM-X-53475 Nbb-30788

LUMINESCENCE TERRESTRIAL OBSERVATIONS FROM MANNED GEOPHYSICAL SPECTROSCOPIC AND PHOTOMETRIC ANALYSIS OF VENUS SATELLITE APPLIED TO PLANETARY ATMOSPHERIC AN0 MARS ATMOSPHERES TO DETERMINE LUMINESCENCE PHENOMENA - VENUS PROBES AND OTHER PROPERTIES P-3418 11166-39519 NASA-TT-F-394 N67-16801 MANNED GEOPHYSICAL OBSERVATIONS FROM SATELLITES AS LUMINESCENCE FROM LOWER ATMOSPHERIC LAYERS AN0 TRAINING GROUND FOR PLANETARY RESEARCH. ESPECIALLY IONOSPHERE OBSERVED IN VENUS NIGHT AIRGLOW VENUS ATMOSPHERE Abl-11395 Nb7-16803 MARINER 11 SPACE PROBE LUNAR ORBITER ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS NASA PROGRAMS RELATED TO SURVEYOR. MARINER, FROM MARINER I1 RADIOMETER DATA, AN0 PIONEER, VENUS PROBE, AN0 SIMILAR PROJECTS THERMODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES Nb7-25097 NASA-CR-7b10b Nbb-31639

LUNAR SURFACE LIMB-DARKENING OBSERVATIONS OF VENUS BY MARINER SPECTROSCOPIC 08SERVATION AN0 SPECTRAL ANALYSIS OF 11 SPACECRAFT MICROWAVE RADIOMETERS ASTRONOMICAL DATA ON PLANETARY ATMOSPHERE, LUNAR Nbb-31640 SURFACE AN0 RADIO EMISSION NASA-TT-F-8881 Nbb-29398 VENUS BRIGHTNESS TEMPERATURE AN0 ATMOSPHERE AN0 MARS ATMOSPHERE SOUNOED BY MARINER I1 SPACE SPECTROPHOTOMETRY AN0 POLARIMETRY OF LUNAR PROBE, NOTING DATA ON MARS MAGNETIC FIELD REGIONS, OPTICAL PROPERTIES OF ATMOSPHERE AND 867-28964 SURFACE OF MARS, AND COMETARY TAILS NASA-TT-F-382 Nbb-33 52b MARINER VENUS PROJECT DESIGN CHANGES FOR FLYBY MISSION AND SENSING OF VENUS ATMOSPHERE SPECTRAL REFLECTANCE OF SILICATE ROCK POWDERS. Nb7-25094 JUPITER ATMOSPHERE XEASUREMENTS, AN0 VISIBLE AND NEAR-INFRARED SPECTRUM DATA FOR ANALYZING MARINER IV SPACE PROBE LUNAR SURFACE Nb7-34775 MARINER IV OCCULTATION EXPERIMENT CONCERNING CARBON OIOXIDE AN0 IONOSPHERIC PEAKS IN MARTIAN Y M ATMOSPHERE Abb-25834 MAGNETIC FIELD RADIO OCCULTATION MEASUREMENT OF MARTIAN PLANET JUPITER RESEARCH, NOTING UNRESOLVED ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE QUESTIONS OF COSMOLOGY. INTERIOR STRUCTURE AND PROBE Abb-29958 GREAT REO SPOT Ab7-39092 y1 MARS ATMOSPHERE MODELS BASE0 ON MARINER IV ATMOSPHERE OF MARS STUDIED USING THREE MODELS OCCULTATION DERIVING ELECTRON NUMBER DENSITY, GENERATED TO SHOW HIGH, MEAN AN0 LOW DENSITY TEMPERATURE. PRESSURE. MASS DENSITY, ETC, NOTING COMPOSITIONS TO ACCOUNT FOR GRAVITATIONAL AN0 CARBON DIOXIDE PRESENCE Abb-30713

1-16 SUBJECT INDEX MARS ATMOSPHERE

MARINER IV MARS OBSERVATION DATA ANALYSIS AN0 Abb-25272 INTERPRETATION Abb-34896 PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS MARINER IV MODELS OF THREE MARS ATMOSPHERIC LANDING MISSION, DISCUSSING USE OF LIFTING Q LAYERS ANALOGOUS TO TERRESTRIAL E, F-1 AND F-2 VEHICLES Abb-25273 LAYERS, CONSIDERING RELATIVE MASS DENSITIESw TEMPERATURES, CARBON DIOXIDE PHOTODISSOCIATION AN0 OBSERVATIONS OF MOON, VENUS, MARS, AN0 IONIZATION PROFILE Abb-41779 JUPITER - SURFACE FEATURES AN0 ATMOSPHERIC CHARACTERISTICS - RADIO, RADAR, TELESCOPICI AN0 MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS SPECTROSCOPIC OBSERVATIONS Nb6-31446 ATMOSPHERE Nbb-31477 NASA-CR-76142

MARINER IV RADIO OCCULTATION MEASUREMENTS OF ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS MARS UPPER ATMOSPHERE Nbb-31478 FROM MARINER I1 RADIOMETER DATA, AN0 THERMODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES EFFECTS OF MARINER IV IONOSPHERIC DATA ON NASA-CR-76106 Nbb-31639 MARS ATMOSPHERE COMPOSITION PREDICTIONS NASA-CR-7bbbb Nbb-32302 THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS ON CARBON. HYDROGEN, OXYGEN, AND NITROGEN IN MARTIAN DAYTIME ATMOSPHERE FROM ZERO TO 50 KM EARTH, VENUS. MARS, AN0 JUPITER ATMOSPHERESN6b-31642 PRESENTING SPHERICAL PARTICLE TERMINAL VELOCITIES AN0 POSSIBLE SIZES FOR OBSCURATIONS9 USING MARINER IV OCCULTATION Ab7-263 16 POLARIMETRIC STUDY OF PLANET MARS Nbb-36942 AFCRL-66-492 VISIBLE BRIGHTNESS FEATURES IN MARINER IV PHOTOGRAPHS OF MARS INTERPRETED AS CLOUDS VENUS BRIGHTNESS TEMPERATURE AN0 ATMOSPHERE AN0 Ab7-34149 MARS ATMOSPHERE SOUNDED BY MARINER I1 SPACE PROBE, NOTING DATA ON MARS MAGNETIC FIELD RADIO OCCULTATION MEASUREMENT OF MARTIAN Ab7-26964 ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE PROBE Ab7-3415 1 ATMOSPHERIC BRIGHTNESS OF MARS DETERMINED BY POLARIMETRIC AN0 PHOTOMETRIC MEASUREMENTS GROUND INSTRUMENTATION SYSTEM FOR MARINER IV TR-34 Nb7-24229 OCCULTATION EXPERIMENT* USING DOPPLER FREQUENCY PERTURBATION METHOD FOR MARS ATMOSPHERIC MARS ATMOSPHERE PARAMETERS DETERMINATION Ab7-34498 MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, FREQUENCY, PHASE, AN0 AMPLITUDE CHANGES OF DETERMINING SHAPE, ATMOSPHERE DENSITY PROFILE, MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AND DIURNAL VARIATIONS, ETC Abb-25235 9 IONOSPHERE OF MARS OBSERVED BEFORE AN0 AFTER PLANETARY OCCULATATION Nb7-12754 MANNED MARS ENTRY AN0 LANDING, DISCUSSING AEROBRAKING AS FEASIBLE ENTRY MODE MARTIAN ATMOSPHERE MODEL DEDUCE0 FROM MARINER IV Abb-25272 IDNOSPHERE ELECTRON DENSITY MEASUREMENTS NASA-CR-84825 Nb7-28785 PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS 0 LANDING MISSION. DISCUSSING USE OF LIFTING MARINER PROGRAM VEHICLES Abb-25273 MARINER/ VENUS SPACE PROBE EXPERIMENT PROPOSED TO MEASURE ECLIPSE OF SOLAR X-RAYS BY VENUSIAN MARS ATMOSPHERIC COMPOSITION AN0 LAMINAR ATMOSPHERE Nbb-27957 CONVECTIVE HEATING AN0 ABLATION STUDIED TO PREDICT PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING MARINER SPACE VEHICLES DESIGN EVOLUTION NOTING ENTRY Abb-25274 CONTRIBUTION TO FUTURE SPACE FLIGHTS THROUGH MEASUREMENT OF ATMOSPHERIC DENSITY OF MARS INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS Ab7-42399 FOR POINTED AND SPHERICALLY BLUNT BODIES IN UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE N ASA SPACE EXPLORATION PROGRAMS DESIGN Abb-25275 MODIFICATIONS AN0 INSTRUMENTATION DEVELOPMENTS NASA-CR-83745 Nb7-25092 CHEMICAL SYSTEM AND REACTION RATES BEHIND STRONG SHOCK HAVES IN MIXTURES OF CARBON DIOXIDE AND MARINER MARS 1969 PROJECT AN0 SPACECRAFT DESIGN NITROGEN USE0 TO STUDY ENTRY CONDITIONS INTO MARS MODIFICATIONS FOR FLYBY MISSIONS ATMOSPHERE Abb-2527 b Nb7-25095 MARTIAN SURFACE PRESSURE AN0 SURFACE DENSITY FROM NASA PROGRAMS RELATED TO SURVEYOR. MARINER, INTERPRETATION OF OBSERVATIONAL DATA PIONEER, VENUS PROBE, AN0 SIMILAR PROJECTS Abb-25291 Nb7-25097 DESIGN AN0 FEASIBILITY STUDIES OF MARS ATMOSPHERE MARINER SPACE PROBE PROBE VEHICLE Abb-25292 MARINER VENUS 1967 SPACE PROBE. OBTAINING ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX LIGHT DIFFUSION OF MARTIAN ATMOSPHERE MEASURE0 BY FROM RADIO SIGNAL FREQUENCY, INTENSITY AND PHASE SPECTROSCOPIC EVALUATION OF POLARIZATION VARIATION CHANGES FROM DISK CENTER TO EDGE Abb-25461 AIAA PAPER 67-118 Ab7-18310 MARINER IV OCCULTATION EXPERIMENT CONCERNING MARINER VENUS 1967 SPACE PROBE, OBTAINING CARBON DIOXIDE AND IONOSPHERIC PEAKS IN MARTIAN ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX ATMOSPHERE 666-25834 FROM RADIO SIGNAL FREQUENCY. INTENSITY AND PHASE c CHANGES VERTICAL TEMPERATURE DISTRIBUTION IN MARTIAN AIAA PAPER 67-116 Ab7-40094 ATMOSPHEREI NOTING INSENSITIVITY TO SURFACE PRESSURE AN0 CARBON DIOXIDE VARIATIONS MARINER SPACE VEHICLES DESIGN EVOLUTION NOTING Abb-26132 CONTRIBUTION TO FUTURE SPACE FLIGHTS THROUGH w MEASUREMENT OF ATMOSPHERIC DENSITY OF MARS MICRO GAS CHROMATOGRAPHIC SYSTEM FOR MARS Ab7-42399 ATMOSPHERE ANALYSIS DURING CAPSULE DESCENT Abb-27278 MARS /PLANET/ MANNED MARS ENTRY AN0 LANDING, DISCUSSING SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST AEROBRAKING AS FEASIBLE ENTRY MODE PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE,

1-17 MARS ATMOSPHERE CONTD SUBJECT INDEX

TRACKING, COST AN0 SCHEDULE METEOROLOGY OF MARS,ANO VENUS AIAA PAPER 65-219 Abb-27874 NASA-CR-75315 Nbb-27238

EARTH REENTRY SIMULATION OF PLANETARY ENTRY SPECTROSCOPIC STUDY OF SOLAR AN0 PLANETARY ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF MARS ATMOSPHERES - OBSERVATIONS OF VENUS AN0 JUPITER, * AND VENUS TYPE AN0 ANALYSIS OF SIMULATED MARTIAN ATMOSPHERE AIAA PAPER b5-218 Abb-27 87 5 IN VISIBLE AN0 INFRARED REGIONS NASA-CR-75488 Nbb-27755 MARS UPPER ATMOSPHERE AN0 SINGLE-LAYER IONOSPHERE UV PHOTOIONIZATION. TEMPERATURE PROFILE AN0 MARTIAN ATMOSPHERIC SURFACE PRESSURE BETWEEN CHEMICAL COMPOSITION Abb-29417 OCCULTATION LEVELS AT ELECTRICS AN0 MARE AC IOALIUM SPECTRAL VARIATION IN LIGHT POLARIZATION OF NASA-CR-75816 Nbb-29298 MARTIAN ATMOSPHERE FOR ALL OBSERVABLE PHASE ANGLES Abb-29643 RADIATIVE-CONVECTIVE EQUILIBRIUM CALCULATIONS FOR TWO-LAYER MARTIAN ATMOSPHERE MARTIAN CLOUDS ANALYSIS AND TOPOGRAPHICAL NASh-CR-75633 Nbb-29732 RELATIONSHIPS, DISCUSSING WHITE AN0 YELLOW CLASSIFICATION AND FREQUENCY OF OCCURRENCES MARTIAN CLOUD ANALYSIS AN0 TOPOGRAPHICAL Abb-29951 RELATIONSHIPS ESRO-SN-54 Nbb-31187 RADIO OCCULTATION MEASUREMENT OF MARTIAN ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE PRESSUREt COMPOSITION. AN0 PARTICLE CONTENT OF PROBE Ab629958 MARTIAN ATMOSPHERE - POLARIZATIONI SPECTRAL BRIGHTNESS, AND TEMPERATURE OF MARTIAN SURFACE PLANETARY QUARANTINE CONSTRAINTS. NOTING Nbb-31472 PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION Abb-29966 SPECTROSCOPIC MEASUREMENT OF CARBON OIOXIOE IN MARS ATMOSPHERE FOR SURFACE PRESSURE AND MARS ATMOSPHERIC DENSITY DETERMINED FROM ATMOSPHERIC COMPOSITION Nbb-31473 PHOTOELECTRIC MEASUREMENTS OF ECLIPSES OF PHOBOS Abb-30049 SPECTROSCOPTIC MEASUREMENTS OF WATER VAPOR AN0 CARBON OIOXIOE CONTENTS IN MARS ATMOSPHERE MARS ATMOSPHERIC CIRCULATIONI DIURNAL HEATING. N6b-31474 THERMAL TIDES AND EFFECTS ON EARTH ATMOSPHERE Abb-30353 CARBON DIOXIDE ABUNDANCE AND SURFACE PRESSURE OF MARTIAN ATMOSPHERE Nbb-3147 5 WEATHER CONDITIONS ON MARS AND RELATION TO PROJECTED MANNED EXPLORATION Abb-30355 MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS ATMOSPHERE Nbb-31477 Q PROPERTIES OF MARS ATMOSPHERE ANALYZED BY EJECTED CAPSULE FROM SPACECRAFT, NOTING MARINER IV RADIO OCCULTATION MEASUREMENTS OF COMMUNICATIONS SYSTEM A6b-30556 MARS UPPER ATMOSPHERE Nbb-31478

MARS ATMOSPHERE MODELS BASEO ON MARINER IV WATER CONTENT AN0 DIFFUSION IN MARTIAN ATMOSPHERE OCCULTATION DERIVING ELECTRON NUMBER DENSITY, AN0 PROPERTIES OF LIGHT AND DARK SIDES OF TEMPERATURE, PRESSURE, MASS DENSITY. ETCt NOTING MARTIAN SDIL Nbb-3148 1 CARBON DIOXIDE PRESENCE Abb-307 13 MARTIAN ATMOSPHERIC CIRCULATION - VERTICAL OUST CLOUD FORMATION BY THERMAL CONVECTION IN TEMPERATURE DISTRIBUTIONt DIURNAL HEATING AND MARTIAN ATMOSPHERE Abb-30925 TIDES, AND DIFFERENTIAL HEATING AN0 GENERAL CIRCULATION AT SOLSTICES Nbb-31489 GERDIEN TYPE CHAMBER FOR MEASUREMENTS OF ION MOBILITY SPECTRUM IN TERRESTRIAL MESOSPHERE AN0 WEATHER FORECASTING FOR MANNED MARS LANDING BY MARS ATMOSPHERE Abb-34712 USE Of METEOROLOGICAL SATELLITE Nb6-3 149 1 MARINER IV MARS OBSERVATION DATA ANALYSIS AND INTERPRETATION Abb-34896 MAGNETIC-SECTOR MASS SPECTROMETER FOR MARS ATMOSPHERE ANALYSIS MARTIAN ATMOSPHERE AN0 CRUST ANALYZED, BASEO ON NASA-CR-76498 Nbb-31926 MARINER IV CLOUD PHOTOGRAPHS Abb-38022 MARS ATMOSPHERE MODELS AT THREE DENSITY LEVELS RANDOM ELSASSER BAN0 MODEL TO COMPUTE ATMOSPHERIC NASA-TM-X-53484 Nbb-31944 TRANSMISSION OF EARTH AND MARS FOR 2-MICRON CARBON DIOXIDE BANDS PROPERTIES OF ATMOSPHERES OF MARS, JUPITER AND JPL-TR-32-969 166-38024 VENUS 166-32039

ABUNDANCE AND TEMPERATURE OF CARBON DIOXIDE IN MARTIAN ATMOSPHERE SAMPLING BY SENSORS OF MARTIAN ATMOSPHERE, NOTING IMPLICATIONS. PARACHUTE DROPPED CAPSULE Nbb-32064 OBSERVATION METHODS AN0 RESULTS Abb-39558 EFFECTS OF MARINER IV IONOSPHERIC DATA ON MARS ATMOSPHERE COMPOSITION PREDICTIONS MARTIAN WAVE OF DARKENING ATTRIBUTED TO SOIL FROST NASA-CR-76666 Nbb-32302 PHENOMENA Abb-40478 BLUE CLEARINGS OF MARS ATMOSPHERE AS FUNCTION OF NEW ABSORPTION BANDS IN NEAR IR SPECTRUM OF MARS NUMBER OF METEOR SHOWERS INTERSECTING MARS FOUND BY FOURIER SPECTROSCOPY VIA CARBON DIOXIDE ORBIT AT INTERVALS OF HELJOCENTRIC LONGITUDE ABSORPTION MEASUREMENTS Abb-40486 NASA-CR-59938 Nbb-33414

MARINER IV MODELS OF THREE MARS ATMOSPHERIC SPECTROPHOTOMETRY AN0 POLARIMETRY OF LUNAR LAYERS ANALOGOUS TO TERRESTRIAL E. F-1 AND F-2 REGIONS, DPTICAL PROPERTIES OF ATMOSPHERE AN0 LAYERS. CONSIDERING RELATIVE MASS DENSITIESI SURFACE OF MARS, AN0 COMETARY TAILS TEMPERATURES, CARBON DIOXIDE PHOTOOISSOCIATION AND NASA-TT-F-382 N6b-33526 IONIZATION PROFILE Abb-41779 v OPTICAL PROPERTIES OF ATMOSPHERE AND SURFACE OF HYPERSONIC ENTRY VEHICLE MEASUREMENT OF MARS MARS Nbb-33530 ATMOSPHERIC DENSfTY. PRESSURE, COMPOSITION^ TEMPERATURE AN0 DETECTION SPECTROMETRY OF CHEMICAL BRIGHTNESS DISTRIBUTION OF MARTIAN DISK USE0 TO SPECIES IN SHOCK LAYER Abb-42 680 DETERMINE OPTICAL PARAMETERS OF ITS ATMOSPHERE

1-18 SUBJECT INDEX MARS ATMOSPHERE CDNTD

AN0 SURFACE FROM ABSOLUTE PHOTOMETRIC DATA MASS MOTION OF WATER IN ATMOSPHERE, POLAR CAP Nbb-33533 GROWTH AN0 WHITE CLOUD APPEARANCE FREQUENCY Ab7-24501 DIRECT CALCULATION AND TABLES OF SPECIFIC HEATS * AND RELATED THERMODYNAMIC PROPERTIES OF VOYAGER PROJECT GOALS. ORBITAL OPERATIONS. CAPSULE ARBITRARY GAS MIXTURES - MARS ATMOSPHERE MODEL DESCENT, NAVIGATIONAL SYSTEMS, ETC NASA-TN-0-3540 166-34373 Ab7-25232

STATISTICAL DECISION THEORY APPLIED TO MARTIAN MARTIAN ATMOSPHERE MODELS HITH DIFFERENT ATMOSPHERE ANALYSIS. LIFE DETECTION EXPERIMENTS. COMPOSITION. PRESSURE AN0 TEMPERATURE L AND GAS CHROMATOGRAM MEASUREMENTS OF N-ALKANE Ab7-25b85 DISTRIBUTIONS IN MATERIALS NASA-CR-77234 Nbb-34667 MARS ATMOSPHERIC COMPOSITION OETERMINATION BY SHOCK LAYER RADIOMETRY TECHNIQUE DURING PROBE OPTICAL RADIOMETER FEASIBILITY STUDY FOR EXPERIMENT DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM AIAA PAPER 67-293 Ab7-26009 SHOCK LAYER RADIATION DURING ENTRY - INSTRUMENTATION flARTIAN DAYTIME ATMOSPHERE FROM ZERO TO 50 KM NASA-CR-73027 Nbb-35663 PRESENTING SPHERICAL PARTICLE TERMINAL VELOCITIES AND POSSIBLE SIZES FOR OBSCURATIONS, USING TERMINAL VELOCITY CALCULATIONS FOR SPHERICAL MARINER IV OCCULTATION Ab7-2631 b PARTICLES IN MARTIAN DAYTIME MODEL ATMOSPHERES LMSC-6-76-66-21 Nbb-37122 MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, COMPARING ATMOSPHERE MODELS OF MARS BASE0 ON DETERMINING SHAPE. ATMOSPHERE DENSITY PROFILE. MARINER IV OCCULATION DATA DIURNAL VARIATIONS, ETC NASA-CR-76134 Nbb-37214 JPL-TR-32-1157 Ab7-26819

MARS ATMOSPHERE ENTRY PROBE CONFIGURATION, PLANETARY QUARANTINE CONSTRAINTS, NOTING AERODYNAMIC CHARACTERISTICS. FLOW FIELD. PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION STABILITY AUGMENTATION. INSTRUMENTATION, Ab7-29098 THERMAL SHIELDING, DATA HANDLING AND COMMUNICATIONS Ab?-1 1424 SYSTEM DESIGN OF AUTOMATED LABORATORY AND ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN AERODYNAMIC, THERMODYNAMIC AND STRUCTURAL DESIGN EXPLORATION Ab?-30628 ASPECTS OF FLIGHT CAPSULE ENTERING LOW DENSITY MARS ATMOSPHERE FROM ORBIT Ab7-11432 VOYAGER PROJECT GOALS. ORBITAL OPERATIONS. CAPSULE DESCENT, NAVIGATIONAL SYSTEMS. ETC MODEL OF NONEQUILIBRIUM PROPERTIES OF HIGH Ab7-31487 c TEMPERATURE CARBON DIOXIDE AND OTHER GAS MIXTURES IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING CARBON DIOXIDE IONS WITH ELECTRONS OISSOCIATIVE MARTIAN ATMOSPHERE Ab7-11436 RECOMBINATION MEASUREMENTS WITH MICROWAVE- AFTERGLOW DIFFERENTIALLY PUMPED QUADRUPOLE MASS- COMPOSITION AN0 SURFACE PRESSURE OF MARTIAN SPECTROMETER APPARATUS, NOTING MARTIAN ATMOSPHERE ATMOSPHERE DETERMINED FROM PHOTOGRAPHIC SPECTRUM MODEL u OF MARS OBTAINED AT MARCH 1965 OPPOSITION SRCC-55 867-32826 Ab%-11695 RADIATIVE RELAXATION TIMES FOR TEMPERATURE CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K PERTURBATIONS IN CO 2 WITH SMALL WATER VAPOR DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS ADMIXTURE UNDER CONDITIONS SIMILAR TO MARTIAN OF MARS Ab7-14309 ATMOSPHERE, DISCUSSING DYNAMICAL PHENOMENA Ab7-33187 MECHANISM REGULATING TOTAL AMOUNT OF EARTH AN0 MARS ATMOSPHERE TRANSPARENT TO VISIBLE AN0 IR RADIO OCCULTATION MEASUREMENT OF MARTIAN RAD1AT1 ON 167-18052 ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE PROBE Ab7-34151 GUIDED PROPULSIVE SOLUTION TO MARS ATMOSPHERE- DECELERATED SOFT LANDING VEHICLE TRAJECTORY MARS ATMOSPHERE SURFACE PRESSURE, RADIATIVE AIAA PAPER 67-170 Ab7-18508 EQUILIBRIUM TEMPERATURES, SUNLIGHT RESONANCE SCATTERING DISTRIBUTION, ETC 867-34152 MARS ATMOSPHERIC COMPOSITION AN0 LAMINAR CONVECTIVE HEATING AND ABLATION STUDIED TO PREDICT MARTIAN ATMOSPHERE CIRCULATION MODEL FROM MARINER PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING IV OCCULTATION EXPERIMENT. STUDYING LATERAL EDDY ENTRY Ab7-18849 VISCOSITYI WINDS, SURFACE TEMPERATURE AND STRESS Ab7-34153 INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS FOR POINTED AN0 SPHERICALLY BLUNT BODIES IN MARTIAN ATMOSPHERE TRANSPARENCY AN0 VISIBILITY OF UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE SURFACE DETAILS IN BLUE AN0 UV LIGHT, SHOWING Ab?-19380 DARK AN0 SEMITONE AREAS INTENSITYI ETC Ab7-34154 CARBON DIOXIDE ABUNDANCE AN0 SURFACE PRESSURE OF MARTIAN ATMOSPHERE* NOTING SELF-BROADENING MARTIAN CLOUDS ANALYSIS AND TOPOGRAPHICAL CORRECTION Ab7-21250 RELATIONSHIPS, DISCUSSING WHITE AN0 YELLOW CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES RESPONSE OF FUNGI TO DIURNAL TEMPERATURE EXTREMES, Ab7-34156 DESCRIBING SOIL, SIMULATED MARTIAN TEMPERATURE REGIME AND FUNGI GROWTH Ab7-21991 ATOMIC AND MOLECULAR PROCESSES IN CYTHEREAN. MARTIAN AN0 JOVIAN UPPER ATMOSPHERES m HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR Ab7-34158 WATER VAPOR PRESENCE, RESULTS INDICATE AMOUNT DEPENDS ON SIZE OF POLAR CAP GROUND INSTRUMENTATION SYSTEM FOR MARINER IV JPL-TR-32-1048 Ab7-22235 OCCULTATION EXPERIMENT, USING DOPPLER FREQUENCY PERTURBATION METHOD FOR MARS ATMOSPHERIC ELEVATION DIFFERENCES BETWEEN MARTIAN DARK AREAS PARAMETERS OETERMINATION Ab7-34498 /MARIA/ AND BRIGHT AREAS /DESERTS/, DISCUSSING SURFACE PRESSURE AN0 TEMPERATURE EFFECTIVE BRAKING HEIGHT / EBH/ FOR SMALL Ab7-22957 INTERPLANETARY PARTICLES OF COSMIC VELOCITY ENTERING MARTIAN UPPER ATMOSPHERE MARTIAN TRANSIENT PHENOMENA CORRELATIONS AMONG Ab7-34541

1-19 MARS ATMOSPHERE CONTD SUBJECT INDEX

VENUS AN0 MARS ATMOSPHERE AND SURFACE STUDIED BY MODELS THAT ASSUME MARS ATMOSPHERE HAS ABSORPTIVE RADIO ASTRONOMY Ab7-34796 RATHER THAN SCATTERING PROPERTIES. AND THAT REDNESS OF PLANET IS DUE TO SELECTIVE ABSORPTION MAGNETOSPHERIC BOUNDARY AND STANDING SHOCK WAVE Nb7-16808 FOR EARTH SCALED DOWN TO APPLY TO MARS .6h Ab7-35442 MODEL FOR MARTIAN ATMOSPHERE AND PLANETARY SURFACE ASSUMING ATMOSPHERIC SPECTRUM WITH SOVIET BOOK ON PLANETARY PHYSICS COVERING PURELY SCATTERING PROPERTIES AND SURFACE MARTIAN, VENUSIAN AN0 MERCURIAN ATMOSPHERES, COVERED WITH LIMONITE DUST Nb7- 16809 VENUSIAN SURFACE TEMPERATURE AND JOVIAN RADIO EMISSION Ab7-38933 PHOTOMETRIC ANALYSIS OF AEROSOL COMPONENT OF MARS I* ATMOSPHERE Nb7-16810 ATMOSPHERE OF MARS STUDIED USING THREE MODELS GENERATED TO SHOW HIGH, MEAN AND LOW DENSITY UISCREPANCY BETWEEN MARS ATMOSPHERIC PRESSURE COMPOSITIONS TO ACCOUNT FOR GRAVITATIONAL AND DATA FROM SPECTROSCOPIC MEASUREMENTS AND FROM MAGNETIC FIELDS Ab7-40140 PHOTOMETRIC AND POLARIMETRIC OBSERVATIONS Nb7-16861 SPHERICAL ENTRY VEHICLE USED TO DEFINE PLANETARY ATMOSPHERE STRUCTURE AND COMPOSITION FROM DYNAMIC INFRARED SPECTROSCOPY TO DETERMINE TEMPERATURE, RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC PRESSURE, AND CHEMICAL COMPOSITION OF MARTIAN CHARACTERISTICS Ab7-40177 ATMOSPHERE Nb7-1b813

MARTIAN ATMOSPHERE COMPONENT DUE TO PROTON SHOCK LAYER RADIATION PREDICTIONS FROM MOLECULAR PENETRATION INTO ATMOSPHERE FROM SOLAR WINO, BAND SYSTEMS IN MARTIAN AND VENUSIAN SUGGESTING RAOIO OCCULTATION BY MARS ORBITER ATMOSPHERES Ab7-40799 NASA-TN-D-3850 Nb7-17629

ANALYSIS OF MARTIAN ATMOSPHERE AND CRUST FROM THERMAL STRUCTURE OF UPPER MARS ATMOSPHERE VISUAL OBSERVATION Ab7-80329 NASA-TM-X-57327 Nb7-18652

EXPANDABLE, TERMINAL DECELERATORS FOR MARS ATMOSPHERIC DATA FOR EARTH9 MARS, AN0 VENUS ATMOSPHERE ENTRY Nb7-19026 NASA-CR-79496 Nb7-12052 IGNITION TEMPERATURES OF POWDERED METALS IN TOTAL EQUILIBRIUM SHOCK LAYER RADIATIVE HEAT SIMULATED MARS AN0 VENUS ATMOSPHERES TRANSFER FOR ENTRY BODY CONFIGURATIONS IN NASA-CR-82878 Nb7-20169 SIMULATED MARS ATMOSPHERE N67-12109 MULTICOLOR PHOTOGRAPHIC AN0 VISUAL PATROL OF GAS CHROMATOGRAPHY COLUMN PACKED WITH POROUS ATMOSPHERE AN0 SURFACE OF MARTIAN NORTHERN POLYMER BEADS FOR USE WITH MASS SPECTROMETER FOR HEMISPHERE DURING SPRING AN0 SUMMER OF 1964-1965 9 RESOLVING MARTIAN ATMOSPHERE COMPONENTS APPARITION Nb7-12128 NASA-CR-83123 Nb7-21180

PLANETARY PHYSICS SEMINAR - POLARIZATION, N ASA METEOROLOGICAL FLIGHT PROGRAM PLANS, SPECTROMETRIC, AN0 RAOIO SIGNAL TECHNIQUES FOR PROCEDURES FOR PARTICIPATION IN SPACE FLIGHT s MEASURING MARTIAN SURFACE AN0 ATMOSPHERIC PROGRAMS, AN0 REQUIREMENTS FOR METEOROLOGICAL PARAMETERS Nb7-12664 RESEARCH ON MARS Nb7-24309

MARTIAN ATMOSPHERE AN0 IONOSPHERE ELECTRON DENSITY MARINER MARS 1969 PROJECT AN0 SPACECRAFT DESIGN AN0 REFRACTIVITY PROFILES DETERMINED BY TWO MDDIFICATIONS FOR FLYBY MISSIONS FREQUENCY BEAT OCCULTATION TECHNIQUE USE0 BY Nb7-25095 MARINER IV SPACE PROBE Nb7-12665 NASA PROGRAMS RELATED TO SURVEYORI MARINER, SURFACE AN0 ATMOSPHERIC PARAMETER MEASUREMENTS BY PIONEER, VENUS PROBE, AND SIMILAR PROJECTS USE OF POLARIZATION INSTRUMENTATION ABOARD Nb7-25097 MARINER ORBITER SPACE PROBE Nb7-12666 COMPONENT OF MARS IONOSPHERE DUE TO SOLAR PROTONS MARTIAN SURFACE AN0 ATMOSPHERIC PARAMETER NASA-CR-84411 Nb7-27370 MEASUREMENTS BY MEANS OF GAMMA RAY SPECTROMETRIC INSTRUMENTATION ABOARD VOYAGER MISSION MARTIAN ATMOSPHERE MODEL DEDUCED FROM MARINER IV Nb7-12667 IONOSPHERE ELECTRON DENSITY MEASUREMENTS NASA-CR-84825 Nb7-28785 ABSORPTION SPECTROSCOPIC DETERMINATION OF WATER VAPOR ABUNDANCE IN MARTIAN ATMOSPHERE MODEL COMPUTATIONS OF TEMPERATURE VARIATIONS AN0 Nb7-12668 WIND CIRCULATIONS IN MARTIAN ATMOSPHERE NASA-CR-85569 Nb7-30624 FREQUENCY. PHASE, AN0 AMPLITUDE CHANGES OF MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AN0 ESTIMATES OF VERTICAL TEMPERATURE STRUCTURE, HEAT IONOSPHERE OF MARS OBSERVED BEFORE AN0 AFTER BALANCE, SOLSTICE CIRCULATION, AND THERMALLY PLANETARY OCCULATATION Nb7-12754 DRIVEN TIDES ON MARS IN COMPARISON WITH LIKE CONDITIONS ON EARTH NUMERICAL MODEL FOR SIMULATING GENERAL CIRCULATION NASA-CR-869 12 Nb7-32494 OF ATMOSPHERE OF MARS NASA-CR-81146 Nb7-15280 I BM 7094 COMPUTER PROGRAM FOR THEORETICAL CALCULATION OF OUTGOING INFRARED RADIANCES FROM ON-BOARD TRACKING SYSTEM OF TWO-WAY COHERENT ATMOSPHERES OF EARTH AND MARS AS AID IN DOPPLER BETWEEN ENTRY CAPSULE AND ORBITING BUS SATELLITE MEASUREMENT INTERPRETATIONS FOR DETERMINING ORBIT OF ENTRY CAPSULE AN0 NASA-TN-D-4045 Nb7-32936 ra ESTIMATING ATMOSPHERIC PARAMETERS Nb7-15904 MARTIAN AN0 CYTHEREAN kTMOSPHERIC COMPOSITION DETERMINATIONS USING ENTRY PROBE MEASUREMENTS OF SPECTROSCOPIC AN0 PHOTOMETRIC ANALYSIS OF VENUS ULTRAVIOLET AND X-RAY ATTENUATION AN0 MARS ATMOSPHERES TO DETERMINE LUMINESCENCE OAt-60627 Nb7-33758 AN0 OTHER PROPERTIES r NASA-TT-F-394 Nb7-1680 1 THERMODYNAMIC PROPERTIES OF THREE MARTIAN MODEL ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOW OPTICAL THICKNESS OF MARS ATMOSPHERE DETERMINED FIELDS FOR REAL GASES - TABLES BY PHOTOMETRIC OBSERVATIONS Nb7-16807 ATOM-66-1 N67-34135

1-20 SUBJECT INDEX METEOROLOGICAL PROBE

FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTIAN Ab7-34536 ,ATMOSPHERE FOR DETERMINATION OF PROFILES OF CARBON DIOXIDE, PARTICULATE MATTER AND WATER VENUS AND MARS ATMOSPHERE AN0 SURFACE STUDIED BY VAPOR RADIO ASTRONOMY Ab7-34796 NASA-TN-D-4115 Nb7-34884 ANALYSIS OF MARTIAN ATMOSPHERE AND CRUST FROM CHEMICAL KINETICS OF CARBON DIOXIDE FOR MARTIAN VISUAL OBSERVATION Ab7-80329 ATMOSPHERIC ENTRY APPLICATIONS ARL-67-0113 Nb7-39458 SCATTERING ANISOTROPY EFFECT ON OPTICAL PARAMETERS OF MARTIAN ATMOSPHERE AND SURFACE - PHOTOMETRY DUST DEVILS IN RELATION TO MARTIAN YELLOW CLOUDS Nb7-16820 NASA-CR-89578 Nb7-40004 MASS SPECTROMETER MARS ENVIRONMENT MAGNETIC-SECTOR MASS SPECTROMETER FOR MARS SIMULATED MARTIAN ATMOSPHERIC AND ECOLOGICAL ATMOSPHERE ANALYSIS EFFECTS ON BACILLUS CEREUS SPORE GERMINATION NASA-CR-76498 Nbb-31926 NASA-CR-74969 Nbb-26263 CARBON DIDXIDE IONS WITH ELECTRONS DISSOCIATIVE DECISION THEORY BIOLOGICAL SEARCH STRATEGIES AND RECOMBINATION MEASUREMENTS WITH MICROWAVE- PLANETARY QUARANTINE ASPECTS OF MARS AFTERGLOW DIFFERENTIALLY PUMPED QUADRUPOLE MASS- EXPLORATORY MISSIONS SPECTROMETER APPARATUS, NOTING MARTIAN ATMOSPHERE NASA-CR-89772 Nb7-40462 MODEL SRCC-55 Ab7-32826 MARS PROBE MICRO GAS CHROMATOGRAPHIC SYSTEM FOR MARS GAS CHROMATOGRAPHY COLUMN PACKED WITH POROUS ATMOSPHERE ANALYSIS DURING CAPSULE DESCENT POLYMER BEADS FOR USE WITH MASS SPECTROMETER FOR Abb-27278 RESOLVING MARTIAN ATMOSPHERE COMPONENTS Nb7-12128 PROPERTIES OF MARS ATMOSPHERE ANALYZED BY EJECTED CAPSULE FROM SPACECRAFT, NOTING ION SDURCES HITH MAGNETICALLY ALIGNED ELECTRON COMMUNICATIONS SYSTEM Abb-30556 BEAM AN0 COMPATIBILITY WITH QUADRUPOLE MASS SPECTROMETER FOR PLANETARY ATMOSPHERIC ANALYSIS MARINER IV MARS OBSERVATION DATA ANALYSIS AND NASA-CR-774 Nb7-25054 INTERPRETATION Abb-34896 MATHEMATICAL MODEL SYSTEM DESIGN FOR NONSURVIVABLE MARS PROBE NUMERICAL MDOEL FOR SIMULATING GENERAL CIRCULATION DEPLOYED FROM ORBITING SPACECRAFT TO PERFORM OF ATMOSPHERE OF MARS ENGINEERING EXPERIMENTS FOR ATMOSPHERIC AND NASA-CR-81146 Nb7-15280 TERRAIN PROPERTY OETERMINATION NASA-CR-66131 Nbb-31819 MATRIX ALGEBRA MATRIX ALGEBRAIC REDUCTION OF EQUATIONS OF MARS ATMOSPHERE ENTRY PROBE CONFIGURATION, RADIATIVE HEAT TRANSFER FOR PLANETARY ATMOSPHERE AERODYNAMIC CHARACTERISTICS. FLOW FIELD. RM-4951-PRv PT. I Nbb-34876 STABILITY AUGMENTATION, INSTRUMENTATION, THERMAL SHIELDING. DATA HANOLING AN0 MEASURING APPARATUS COMMUNICATIONS Ab7-11424 INSTRUMENTS FOR MEASURING ALTITUDE DEPENDENT PHYSICAL PROPERTIES OF VENUS ATMOSPHERE FROM MARS PROBE DESIGN AND SUBSYSTEM PERFORMANCE ENTRY CAPSULE Nb7-15764 CHARACTERISTICS FOR INVESTIGATING MARTIAN ATMOSPHERE MERCURY /PLANET/ NASA-CR-530 Nb7-32719 MERCURY ATMOSPHERIC TEMPERATURE, COMPOSITION AND SURFACE PRESSURE AN0 EFFECT OF NONSYNCHRONOUS MARS SPACECRAFT ROTATION Abb-40424 MANNED MARS EXCURSION VEHICLE FOR THIN MARS ATMOSPHERE POLARIZATION PROPERTIES OF MERCURY EXPLAINED BY NASA-TM-X-53475 Nbb-30788 SURFACE ONLY, SO THERE IS NO POLARIMETRIC EVIDENCE FOR ATMOSPHERE ON MERCURY Ab7-26244 INTERPLANETARY TRANSIT AND ATMOSPHERIC ENTRY OF UNMANNED VEHICLE LANDING ON MARS SURFACE, WITH SOVIET BOOK ON PLANETARY PHYSICS COVERING REFERENCE TO HEAT SHIELD TECHNOLOGY MARTIAN. VENUSIAN AND MERCURIAN ATMOSPHERES. JPL-TR-32-1145 Ab7-25715 VENUSIAN SURFACE TEMPERATURE AND JOVIAN RADIO EM1SS ION Ab7-38933 MARS SURFACE RADIO ASTRONOMY STUDIES OF VENUS AND MARS UPPER LIMIT OF CARBON DIOXIDE ABUNDANCE IN NOTING SURFACE PROPERTIES, ATMOSPHERIC STRUCTURE, MERCURY ATMOSPHERE Ab7-41836 ETC Abb-26031 ATMOSPHERE OF MERCURY FROST PHENOMENA ON MARS EXAMINE0 ON BASIS OF NASA-TM-X-57322 Nb7-18273 MARTIAN WAVE OF DARKENING, NOTING NECESSITY OF DELIQUESCENT SALTS TO ATTRACT AND RETAIN WATER ON BIBLIOGRAPHY AND AUTHOR ON MERCURY SURFACEI SURFACE Ab7-18645 ATMOSPHERE, ROTATION. TEMPERATURE, AN0 TERRAIN NASA-CR-84113 Nb7-26454 MARTIAN TRANSIENT PHENOMENA CORRELATIONS AMONG MASS MOTION OF WATER IN ATMOSPHERE. POLAR CAP MESOSPHERE GROWTH AND WHITE CLOUD APPEARANCE FREQUENCY GERDIEN TYPE CHAMBER FOR MEASUREMENTS OF ION 167-24501 MOBILITY SPECTRUM IN TERRESTRIAL MESOSPHERE AN0 MARS ATMOSPHERE Abb-34712 VISIBLE BRIGHTNESS FEATURES IN MARINER IV PHOTOGRAPHS OF MARS INTERPRETED AS CLOUDS METEOR SHOWER Ab7-34149 BLUE CLEARINGS OF MARS ATMOSPHERE AS FUNCTION OF NUMBER OF METEOR SHDHERS INTERSECTING MARS MARTIAN ATMOSPHERE TRANSPARENCY AN0 VISIBILITY OF ORBIT AT INTERVALS OF HELIOCENTRIC LONGITUDE SURFACE DETAILS IN BLUE AND UV LIGHT, SHOWING NASA-CR-59938 Nbb-33414 DARK AND SEMITONE AREAS INTENSITY. ETC Ab7-34154 METEOROLOGICAL PROBE PLANETARY ATMOSPHERE STRUCTURE DETERMINED FROM RELATION BETWEEN SURFACE PRESSURE AN0 ATMOSPHERIC ENTRY VEHICLE ONBOARD MEASUREMENTS OF PRESSURE, BRIGHTNESS IN OPTICALLY THIN RAYLEIGH SCATTERING TEMPERATURE, AND ACCELERATION ATMOSPHERE, CONSIDERING APPLICATION TO MARS NAS A-TN-D-3933 N67-23302

1721 METEOROLOGICAL SATELLITE SUBJECT INDEX

METEOROLOGICAL SATELLITE MICROWAVE RADIOMETER WEATHER FORECASTING FOR MANNED MARS LANDING BY LIMB-DARKENING OBSERVATIONS OF VENUS BY MARINER USE OF METEOROLOGICAL SATELLITE I1 SPACECRAFT MICROWAVE RADIOMETERS Nbb-3 1491 Nbb-31640

N ASA METEOROLOGICAL FLIGHT PROGRAM PLANS. MICROWAVE SPECTRUM * PROCEDURES FOR PARTICIPATIDN IN SPACE FLIGHT MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF PROGRAMS. AN0 REQUIREMENTS FOR METEOROLOGICAL VENUS COMPARE0 WITH SEVERAL MODEL ATMOSPHERES RESEARCH ON MARS Nb7-24309 A67-24601

METEOROLOGICAL STATION MOLECULAR DISSOCIATION ro SPACE RECEIVER OBSERVATIONS OF JOVIAN DECAMETER CARBON DIOXIDE IONS WITH ELECTRONS DISSOCIATIVE FLUX RECOMBINATION MEASUREMENTS WITH MICROWAVE- NASA-CR-82654 Nb7-19113 AFTERGLOW DIFFERENTIALLY PUMPED QUAORUPOLE MASS- SPECTROMETER APPARATUS, NOTING MARTIAN ATMOSPHERE METEOROLOGY MODEL MARS ATMOSPHERIC CIRCULATION. DIURNAL HEATING. SRCC-55 Ab7-32826 THERMAL TIDES AND EFFECTS ON EARTH ATMOSPHERE Abb-30353 MOLECULAR GAS MOLECULAR HYDROGEN STRUCTURE. CONSIDERING WEATHER CONDITIONS ON MARS AN0 RELATION TO PLANETARY AND STELLAR ATMOSPHERES AND INTERSTELLAR PROJECTED MANNED EXPLORATION Abb-30355 SPACE Abb-39487

METEOROLOGY OF MARS AND VENUS MOLECULAR INTERACTION NASA-CR-75315 Nbb-27238 JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM CORONA DISCHARGE. PRODUCING SIMPLE ORGANIC METHANE MOLECULES Ab7-19057 SPECTRAL STUDY OF JUPITER, SATURN AND RINGS OF SATURN, DETERMINING METHANE CONCENTRATION IN ATOMIC AND MOLECULAR PROCESSES IN CYTHEREAN, CLDUO LAYERS Ab6-3703 5 MARTIAN AND JOVIAN UPPER ATMOSPHERES Ab7-34158 MEAN VALUES OF METHANE WAVELENGTHS IN URANUS SPECTRUM MEASURED FOR DETERMINATION OF ATMOSPHERIC MOLECULAR SPECTRUM TEMPERATURE 867-14327 SELF-BROADENING COEFFICIENTS OF SPECTRAL LINES OF ABSORBING ATMOSPHERIC GASES MEASURE0 IN SPECTRAL STUDY OF JUPITER, SATURN AN0 RINGS OF COMPARISON WITH LINE BROADENING EFFECTS OF SATURN, DETERMINING METHANE CONCENTRATION IN NITROGEN Ab7-22715 CLOUD LAYERS Ab7-15557 SHOCK LAYER RADIATION PREDICTIONS FROM MOLECULAR URANUS AND NEPTUNE SPECTRAL ABSORPTIONS COMPARED BAN0 SYSTEMS IN MARTIAN AN0 VENUSIAN * WITH LABORATORY SPECTRA OBTAINED WITH VERY LONG ATMOSPHERES OPTICAL PATHS INDICATE METHANE ROLE IN PLANETARY NASA-TN-0-3850 Nb7-17629 ABSORPTION Ab7-21213 MOLECULAR STRUCTURE MICHELSON INTERFEROMETER MOLECULAR HYDROGEN STRUCTURE, CONSIDERING VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON PLANETARY AND STELLAR ATMOSPHERES AND INTERSTELLAR =s INTERFEROMETERI FINDING H CL LINES CONSISTENT SPACE Abb-39487 WITH 2-MM AMAGAT OF GAS JPL-TR-32-1106 Ab?-2451 0 MONATOMIC GAS HEATING RATES IN GAS MIXTURES OF PLANETARY MICROORGANISM ATMOSPHERES PREDICTED BY EQUATION USING TRANSPORT PLANETARY CONTAMINATION BY VIABLE TERRESTRIAL PROPERTIES OF GASES AT LOWER TEMPERATURES MICROORGANISMS TRANSPORTED ON SPACECRAFT 166-27432 AD-648864 Nb7-27042 MONOCHROMATIC RADIATION MICROWAVE APPARATUS METHOD FOR CALCULATING PROPERTIES OF MONOCHROMATIC PLANETARY ATMOSPHERIC COMPOSITION STUDY UNDER RADIATION THROUGH LAYER DF DISPERSED PARTICLES AMBIENT CONDITIONS USING INSTRUMENT INVOLVING VERY AND ITS APPLICATION TO VENUS CLOUDS HIGH Q FABRY- PEROT MICROWAVE CAVITIES Nbb-31465 Ab7-25986 CURVES OF MONOCHROMATIC ALBEDO FOR LIMB AN0 CARBON DIOXIDE IONS WITH ELECTRONS DISSOCIATIVE TERMINATOR OF VENUS Nb7-16806 RECOMBINATION MEASUREMENTS WITH MICRDWAVE- AFTERGLOW DIFFERENTIALLY PUMPED QUADRUPOLE MASS- MONOPOLE ANTENNA SYSTEM SPECTROMETER APPARATUS, NOTING MARTIAN ATMOSPHERE DATA REPRESENTING MONOPOLE ANTENNA VOLTAGE MOOEL BREAKDWON IN SIMULATED MARS AND VENUS SRCC-55 867-32826 ATMOSPHERES Ab7-35829

MICROWAVE ATTENUATION MOON DIELECTRIC RELAXATION OF GASES AND SHARP RISE IN OBSERVATIONS OF MOON. VENUS, MARS, AND MICROWAVE ABSORPTION COEFFICIENT IN CYTHEREAN JUPITER - SURFACE FEATURES AND ATMOSPHERIC ATMOSPHERE Ab7-21372 CHARACTERISTICS - RADIO, RADAR, TELESCOPICt AND SPECTROSCOPIC OBSERVATIONS MICROWAVE PROBE NASA-CR-76142 Nbb-31446 VENUS ATMOSPHERE NOTING PRESSURE INDUCED ABSORPTION IN CARBON DIOXIDE-NITROGEN ATMOSPHERE MOTION EQUATION AS INDICATED IN DECLINE OF MICROWAVE BRIGHTNESS EFFECTIVE BRAKING HEIGHT / EBH/ FOR SMALL TEMPERATURE Abb-42668 INTERPLANETARY PARTICLES OF COSMIC VELOCITY ENTERING MARTIAN UPPER ATMOSPHERE rp MICROWAVE RADIATION Ab7-34541 INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS HAVE BEEN OBSERVED IN X-BAN0 FROM GLOW DISCHARGES N Ab7-14952 NASA PROGRAM N ASA METEOROLOGICAL FLIGHT PROGRAM PLANS, u VENUS SURFACE TEMPERATURE AND MICROWAVE EMISSION. PROCEDURES FOR PARTICIPATION IN SPACE FLIGHT DISCUSSING IONOSPHERIC MODEL, GREENHOUSE EFFECT, PROGRAMSI AN0 REQUIREMENTS FOR METEOROLOGICAL MICROOISCHARGE MODEL. RADIO AURORA. ETC RESEARCH ON MARS Nb7-24309 Ab7-34543

1-22 SUBJECT INDEX OPTICAL THICKNESS

N ASA SPACE EXPLORATION PROGRAMS DESIGN DETERMINING SHAPE. ATMOSPHERE DENSITY PROFILE, MODIFICATIONS AND INSTRUMENTATION DEVELOPMENTS DIURNAL VARIATIONSI ETC Abb-25235 NASA-CR-83745 Nb7-25092 MARS ATMOSPHERE MODELS BASED ON MARINER IV NATURAL SATELLITE OCCULTATION DERIVING ELECTRON NUMBER DENSITY, MARS ATMOSPHERIC DENSITY DETERMINED FROM TEMPERATURES PRESSURE, MASS DENSITY, ETCt NOTING PHOTOELECTRIC MEASUREMENTS OF ECLIPSES OF PHOBOS CARBON OIOXIDE PRESENCE Abb-307 13 Abb-30049 MARTIAN ATMOSPHERIC SURFACE PRESSURE BETWEEN STIMULATION OF JUPITER RADIO EMISSION BY IO OCCULTATION LEVELS AT ELECTRICS AND MARE Ab7-25204 ACIDALIUM NASA-CR-75816 Nbb-29298 NONTHERMAL RADIO EMISSION FROM JUPITER ATMOSPHERE, STUDYING 10 MODULATION EFFECT MARINER IV RAOIO OCCULTATION MEASUREMENT OF MARS Abl-34933 ATMOSPHERE Nbb-31477

NEAR INFRARED MARINER IV RADIO OCCULTATION MEASUREMENTS OF IMAGE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL MARS UPPER ATMOSPHERE Nbb-31478 VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN DISK IN NEAR IR REGION Abb-37017 MARS ATMOSPHERE AND IONOSPHERE ANALYZED BY MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, NEPTUNE DETERMINING SHAPE, ATMOSPHERE DENSITY PROFILE. URANUS AND NEPTUNE SPECTRAL ABSORPTIONS COMPARED DIURNAL VARIATIONS. ETC WITH LABORATORY SPECTRA OBTAINED WITH VERY LONG JPL-TR-32-1157 Ab7-26819 OPTICAL PATHS INDICATE METHANE ROLE IN PLANETARY ABSORPTION Ab7-21213 GROUND INSTRUMENTATION SYSTEM FOR MARINER IV OCCULTATION EXPERIMENT, USING DOPPLER FREQUENCY NITROGEN PERTURBATION METHOD FOR MARS ATMOSPHERIC CHEMICAL SYSTEM AN0 REACTION RATES BEHIND STRONG PARAMETERS DETERMINATION Ab7-34498 SHOCK WAVES IN MIXTURES OF CARBON DIOXIDE AND NITROGEN USED TO STUDY ENTRY CONDITIONS INTO MARS MARTIAN ATMOSPHERE AND IONOSPHERE ELECTRON DENSITY ATMOSPHERE Abb-25276 AN0 REFRACTIVITY PROFILES DETERMINED BY TWO FREQUENCY BEAT OCCULTATION TECHNIQUE USED BY SPECTROSCOPIC INVESTIGATION OF VENUS ATMOSPHERE MARINER IV SPACE PROBE Nb7-12665 TO DETERMINE NITROGEN, OXYGEN, CARBON DIOXIDE, WATER VAPORt AN0 OTHER COMPONENTS FREQUENCY, PHASE, AN0 AMPLITUDE CHANGES OF Nb7-16802 MARINER IV RAOIO SIGNAL THROUGH ATMOSPHERE AN0 IONOSPHERE OF MARS OBSERVED BEFORE AND AFTER NITROGEN OXIDE PLANETARY OCCULATATION Nb7-12754 SPECTROSCOPIC STUDY OF SOLAR AND PLANETARY ATMOSPHERES - OBSERVATIONS OF VENUS AND JUPITER. OCEAN AND ANALYSIS OF SIMULATED MARTIAN ATMOSPHERE EARTH AND PLANETARY OCEAN AND ATMOSPHERIC ORIGIN. IN VISIBLE AND INFRARED REGIONS EVOLUTION, AN0 COMPOSITION Nbb-37965 NASA-CR-75488 Nbb-27755 OPTICAL INSTRUMENT NONEQUILIBRIUM FLOW OPTICAL INSTRUMENTS FOR ULTRAVIOLET MEASUREMENTS MODEL OF NONEQUILIBRIUM PROPERTIES OF HIGH IN PLANETARY ATMOSPHERES Nb7-17793 TEMPERATURE CARBON DIOXIDE AND OTHER GAS MIXTURES IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING OPTICAL MEASUREMENT MARTIAN ATMOSPHERE Ab7-11436 SCATTERING ANISOTROPY EFFECT ON OPTICAL PARAMETERS OF MARTIAN ATMOSPHERE AND SURFACE - PHOTOMETRY NONEPUILIBRIUM RADIATION Nb7-16820 HIGH-TEMPERATURE GAS RADIANCE IN SIMULATED PLANETARY ATMOSPHERE AT VARIOUS ENTRY VELOCITIES OPTICAL POLARIZATION AIAA PAPER 66-183 Abb-25169 LIGHT DIFFUSION OF MARTIAN ATMOSPHERE MEASURED BY SPECTROSCOPIC EVALUATION OF POLARIZATION VARIATION NONGRAY ATMOSPHERE FROM DISK CENTER TO EDGE Abb-25461 NONGRAY MODEL ATMOSPHERES OF JOVIAN PLANETS CONSTRUCTED FOR DIFFERENT RELATIVE CONCENTRATIONS SPECTRAL VARIATION IN LIGHT POLARIZATION OF OF HELIUM AND DIATOMIC HYDROGEN AND VARIOUS LIKELY MARTIAN ATMOSPHERE FOR ALL OBSERVABLE PHASE EFFECTIVE TEMPERATURES AS CHIEF SOURCES OF THERMAL ANGLES Abb-29643 OPACITY Ab7-22237 OPTICAL PROPERTY NUMERICAL ANALYSIS SPECTROPHOTOMETRY AND POLARIMETRY OF LUNAR NUMERICAL SOLUTION OF TRANSPORT AND ENERGY REGIONS. OPTICAL PROPERTIES OF ATMOSPHERE AND EQUATIONS IN PLANETARY BOUNDARY LAYER SURFACE OF MARS, AND COMETARY TAILS ECOM-6020 Nbb-33271 NASA-TT-F-382 Nbb-33526

THEORY AND NUMERICAL PROCEDURE FOR DIGITAL OPTICAL PROPERTIES OF ATMOSPHERE AN0 SURFACE OF COMPUTER APPLICATION OF GREENHOUSE EFFECT FOR MARS Nbb-33530 PLANETARY ATMOSPHERE OF FINITE DEPTH RM-5076-PR Nb7-22562 BRIGHTNESS DISTRIBUTION OF MARTIAN DISK USE0 TO DETERMINE OPTICAL PARAMETERS OF ITS ATMOSPHERE NUMERICAL INTEGRATION AND SURFACE FROM ABSOLUTE PHOTOMETRIC DATA NUMERICAL CALCULATION OF PERIODS OF NATURAL Nbb-33533 OSCILLATIONS AND CORRESPONDING EIGENFUNCTIONS OF PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS CALCULATION OF TOTAL RADIATION EMERGING FROM ROTATIONAL SPEED Abb-27534 PLANETARY ATMOSPHERES OPTICALLY THICKER THAN THOSE OF EARTH NUMERICAL CALCULATION OF PERIODS OF NATURAL RM-5343-PR Nb7-32966 OSCILLATIONS AND CORRESPONDING EIGENFUNCTIONS OF PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS OPTICAL SPECTRUM ROTATIONAL SPEED Abb-42320 OPTICAL AN0 ELECTRONIC COMPONENTS FOR ULTRAVIOLET ROCKET SPECTROPHOTOMETRY IN PLANETARY ATMOSPHERE 0 NASA-CR-78485 Nb6-38722 OCCULTATION OPTICAL THICKNESS MARS ATMOSPHERE AND IONOSPHERE ANALYZED BY OPTICAL THICKNESS OF MARS ATMOSPHERE DETERMINED MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, BY PHOTOMETRIC OBSERVATIONS N67-1b807

1-23 ORBIT CALCULATION SUBJECT INDEX

ORBIT CALCULATION PERIOOICITY ON-BOARD TRACKING SYSTEM OF TWO-WAY COHERENT PHOTOMETRIC OBSERVATION DATA ON JUPITER DOPPLER BETWEEN ENTRY CAPSULE AN0 ORBITING BUS ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- FOR DETERMINING ORBIT OF ENTRY CAPSULE AN0 MONTH PERIODIC CHANGE A67-39299 ESTIMATING ATMOSPHERIC PARAMETERS N67-15904 PHOTOCHEUISTRY PHOTOCHEMISTRY OF PLANETARY GASES AND PLANETARY ORBITAL LAUNCH AERONOMY SYSTEM DESIGN FOR NONSURVIVABLE MARS PROBE NASA-CR-81262 N67-16515 DEPLOYED FROM ORBITING SPACECRAFT TO PERFORM ENGINEERING EXPERIMENTS FOR ATMOSPHERIC AN0 PHOTODISSOCIATION TERRAIN PROPERTY DETERMINATION LIMITATION ON OXYGEN CONCENTRATION IN POSSIBLE NASA-CR-66131 N66-31819 PRIMITIVE ATMOSPHERES EXAMINED VIA PHYSICAL AND PHOTOCHEMICAL FACTORS A66-26122 ORBITAL VELOCITY CONVECTIVE AN0 RADIATIVE HEAT TRANSFER TO PHOTOELECTRIC PHOTDUETRY SPACE VEHICLES ENTERING PLANETARY ATMOSPHERES WATER VAPOR LINES IN SPECTRUM OF VENUS OBTAINED AT SUPERORBITAL VELOCITIES BY PHOTOELECTRIC SCANNING OF SPECTRUM NASA-CR-584 N66-37021 A67-11769

ORGANIC COMPOUND PHOTOMETRY OF INTEGRATED LIGHT OF VENUS, THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES INFERRING PRESENCE OF ICE IN ATMOSPHERE FROM HALO AN0 IN ORIGIN OF ORGANIC MATTER - DETERMINATION EFFECT OF BRIGHTNESS DISPERSION OF AMINO ACID PAIRING AND SEQUENCES IN PROTEINS A67-16407 NASA-CR-74559 N66-28800 PHOTOGRAPH INTERPRETAFION JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM VISIBLE BRIGHTNESS FEATURES IN MARINER IV CORONA DISCHARGE. PRODUCING SIMPLE ORGANIC PHOTOGRAPHS OF MARS INTERPRETED AS CLOUDS MOLECULES A67-19057 A67-34149

THERMODYNAMIC EQUILIBRIUM IN PREBIOLOGICAL PHOTOGRAPHIC UEASUREMENT ATMOSPHERES, AN0 INORGANIC ORIGIN OF ORGANIC RAPID DRIFT IN LONGITUDE OF SMALL DARK SPOT ON COMPOUNDS SOUTH EDGE OF JUPITER NORTH TEMPERATE BELT, NASA-SP-3040 N67-27295 NOTING SINUSOIDAL DISPLACEMENT CHARACTERISTICS AN0 MEASUREMENT WITH BLUE AN0 UV PHOTOGRAPHY OXYGEN A66-33009 OXYGENIC CONCENTRATIONS IN PRIMITIVE EARTH ATMOSPHERE, DISCUSSING MARTIAN ATMOSPHERE PHOTOGRAPHIC RECORDING COMPOSITION A67-34095 SIMULTANEOUS UV PHOTOGRAPHS AN0 RADAR CROSS SECTION MEASUREMENTS OF VENUS, DISCUSSING OXYGEN PRODUCTION ATMOSPHERIC MOTION AN0 ROTATION LIMITATION ON OXYGEN CONCENTRATION IN POSSIBLE A61-38611 PRIMITIVE ATMOSPHERES EXAMINED VIA PHYSICAL AND PHOTOCHEMICAL FACTORS A66-26122 PHOTOIONIZATION MARS UPPER ATMOSPHERE AND SINGLE-LAYER IONOSPHERE UV PHOTOIONIZATION, TEMPERATURE PROFILE AN0 CHEMICAL COMPOSITION A66-29417 PARTICLE SPHERICAL DUST PARTICLE TERMINAL VELOCITIES IN PHOTOUETRY HOOEL VENUS ATMOSPHERE PHOTOMETRIC OBSERVATION DATA ON JUPITER LMSC-6-77-67-18 N67-34596 ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- MONTH PERIODIC CHANGE A67-39299 PARTICLE CLOUD TERMINAL VELOCITY CALCULATIONS FOR SPHERICAL SPECTROSCOPIC AN0 PHOTOMETRIC ANALYSIS OF VENUS PARTICLES IN MARTIAN DAYTIME MODEL ATMOSPHERES AN0 MARS ATMOSPHERES TO DETERMINE LUMINESCENCE LMSC-6-76-66-21 N66-37122 AN0 OTHER PROPERTIES NASA-TT-F-394 N67-16801 PARTICLE FLUX CONDITIONS OF ENCOUNTER BETWEEN INTERPLANETARY OPTICAL THICKNESS OF MARS ATMOSPHERE DETERMINED OUST PARTICLES AN0 PLANETS BY PHOTOMETRIC OBSERVATIONS N67-16807 NASA-TM-X-57009 N66-35309 PHOTOMETRlC ANALYSIS OF AEROSOL COMPONENT OF MARS PARTICLE MOTION ATMOSPHERE N67-16810 MARTIAN DAYTIME ATMOSPHERE FROM ZERO TO 50 KM PRESENTING SPHERICAL PARTICLE TERMINAL VELOCITIES DISCREPANCY BETWEEN MARS ATMOSPHERIC PRESSURE AN0 POSSIBLE SIZES FOR OBSCURATIONS, USING DATA FROM SPECTROSCOPIC NEASUREMENTS AN0 FROM MARINER IV OCCULTATION A67-26316 PHOTOMETRIC AND POLARIMETRIC OBSERVATIONS N67-16811 EFFECTIVE BRAKING HEIGHT / EBH/ FOR SMALL INTERPLANETARY PARTICLES OF COSMIC VELOCITY PHOTOSYNTHESIS ENTERING MARTIAN UPPER ATMOSPHERE INDIGENOUS BIOLOGY IN VENUS CLOUDS, PROPOSING A67-34541 ISOPYCNIC FLOAT BLADDER MACROORGANISM INGESTING WATER AN0 MINERALS BLOWN UP FROM SURFACE BY PARTICLE SIZE PINOCYTOSIS ~6r-39556 MARTIAN DAYTIME ATMOSPHERE FROM ZERO TO 50 KM PRESENTING SPHERICAL PARTICLE TERMINAL VELOCITIES PHYSICAL PROPERTY AN0 POSSIBLE SIZES FOR OBSCURATIONS, USING INSTRUMENTS FOR MEASURING ALTITUDE DEPENDENT MARINER IV OCCULTATION A67-26316 PHYSICAL PROPERTIES OF VENUS ATMOSPHERE FROM ENTRY CAPSULE N67-15164 PERIODIC OSCILLATION NUMERICAL CALCULATION OF PERIODS OF NATURAL PIONEER SPACE PROBE OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF NASA PROGRAMS RELATED TO SURVEYOR, MARINER, PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS PIONEER, VENUS PROBE, AND SIMILAR PROJECTS ROTATIONAL SPEED A66-27534 N67-25097

NUMERICAL CALCULATION OF PERIODS OF NATURAL PLANETARY CONFIGURATION OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF MARTIAN ATMOSPHERE TRANSPARENCY AND VISIBILITY OF PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS SURFACE DETAILS IN BLUE AN0 UV LIGHT, SHOWING ROTATIONAL SPEED A66-42320 DARK AN0 SEMITONE AREAS INTENSITY, ETC

1-24 SUBJECT INDEX PLANETARY RAOIATION

A67-34154 COMPOSITION A67-34095

PLANETARY CONSTITUTION EARTH-MOON SYSTEM ORIGIN ASSUMING MOON WAS FORMED JUPITER AND SATURN MODELS, GIVING PLANET FROM TERRESTRIAL MATERIAL EJECTED FROM EARTH CONSTITUTION, HEAT BALANCE AND ATMOSPHERIC DURING ROTATIONAL INSTABILITY A67-4232 5 a COMPOSITION A67-39001 PLANETARY EXPLORATION PLANETARY DISU DESIGN AND FEASIBILITY STUDIES OF MARS ATMOSPHERE BRIGHTNESS DISTRIBUTION OF MARTIAN DISK USEO TO PROBE VEHICLE A66-25292 DETERMINE OPTICAL PARAMETERS OF ITS ATMOSPHERE * AND SURFACE FROM ABSOLUTE PHOTOMETRIC DATA WEATHER CONDITIONS ON MARS AND RELATION TO N66-33533 PROJECTED MANNED EXPLORATION A66-30355

PLANETARY ENTRY MANNED GEOPHYSICAL OBSERVATIONS FROM SATELLITES AS SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST TRAINING GROUND FOR PLANETARY RESEARCH. ESPECIALLY PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE, VENUS ATMOSPHERE A61-11395 TRACKING, COST AND SCHEDULE AIAA PAPER 65-219 A66-27874 SCIENCE SUBSYSTEMS FOR JUPITER FLYBY MISSIONS, DISCUSSING EQUIPMENT SELECTION, MISSION PLANNING. EARTH REENTRY SIMULATION OF PLANETARY ENTRY SPACECRAFT DESIGN AN0 TRAJECTORY AN0 CONSTRAINTS ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF MARS ON VEHICLE CONFIGURATION AND VENUS TYPE AIAA PAPER 67-120 Ab7-1B287 AIAA PAPER 65-216 A66-27875 PLANETARY ATMOSPHERIC ABSORPTION SPECTROSCOPY VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE EMPLOYING SPLIT-TRAJECTORY DUAL FLYBY MODE INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AN0 OF AIAA PAPER 67-121 A67-18311 STATIC EQUILIBRIUM WITHIN KAPLAN ATMOSPHERE A66-27887 VOYAGER PROJECT GOALS, ORBITAL OPERATIONS* CAPSULE DESCENT. NAVIGATIONAL SYSTEMS. ETC HYPERSONIC ENTRY VEHICLE MEASUREMENT OF MARS A67-25232 ATMOSPHERIC DENSITY, PRESSURE, COMPOSITION, TEMPERATURE AND DETECTION SPECTROMETRY OF CHEMICAL SYSTEM DESIGN OF AUTOMATED LABORATORY AN0 SPECIES IN SHOCK LAYER A66-42680 ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORATION Ab7-30628 MARS ATMOSPHERE ENTRY PROBE CONFIGURATION. AERODYNAMIC CHARACTERISTICS. FLOW FIELD, VOYAGER PROJECT GOALS, ORBITAL OPERATIONSI CAPSULE STABILITY AUGMENTATION, INSTRUMENTATION, DESCENT, NAVIGATIONAL SYSTEMS. ETC THERMAL SHIELDING9 DATA HANDLING AND A67-31481 COMMUNICATIONS A67-11424 PLANETARY LANDING MODEL OF NONEQUILIBRIUM PROPERTIES OF HIGH MANNED MARS ENTRY AN0 LANDING, DISCUSSING TEMPERATURE CARBON DIOXIDE AND OTHER GAS MIXTURES AERDBRAKING AS FEASIBLE ENTRY MODE IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING A66-25272 MARTIAN ATMOSPHERE A67-11436 PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS 'gl FLIGHT DYNAMICS OF BALLISTIC AND LIFTING VEHICLE LANDING MISSION. DISCUSSING USE OF LIFTING ENTRIES INTO PLANETARY ATMOSPHERES OF MARS,. VEHICLES A66-25273 EARTH. VENUS AND JUPITER 167-20623 GUIDED PROPULSIVE SOLUTION TO MARS ATMOSPHERE- MOLECULAR, CONTINUUM AND LINE RADIATION OF DECELERATED SOFT LANDING VEHICLE TRAJECTORY PLANETARY ATMOSPHERES, COMPARING MOLECULAR BAND AIAA PAPER 67-170 A67-18508 STRUCTURE MODELS WITH SPECTRAL MEASUREMENTS OF CN VIOLET BAND EXPANDABLE, TERMINAL DECELERATORS FOR MARS AIAA PAPER 67-323 A67-26036 ATMOSPHERE ENTRY NASA-CR-79496 N67- 1205 2 SPHERICAL ENTRY VEHICLE USEO TO DEFINE PLANETARY ATMOSPHERE STRUCTURE AND COMPOSITION FROM DYNAMIC PLANETARY LONGITUDE RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC LATITUDE AND LONGITUDE OF JUPITER REO SPOT CHARACTERISTICS A6740177 MEASURED FROM PHOTOGRAPHS OBTAINED DURING 1965 AN0 1966 PLANETARY ENVIRONMENT NASA-CR-85560 N67-31108 PLANETARY QUARANTINE CONSTRAINTS, NOTING PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION PLANETARY MAGNETIC FIELD A66-29966 ASHEN LIGHT AND MAGNETIC FIELO OF VENUS A67-33096 INTERPLANETARY TRANSIT AN0 ATMOSPHERIC ENTRY OF UNMANNED VEHICLE LANDING ON MARS SURFACE, WITH PLANETARY MASS REFERENCE TO HEAT SHIELD TECHNOLOGY JUPITER ENVIRONMENT, EFFECTS OF HUGE MASS9 HIGH J PL-TR-32-1145 A67-25715 ROTATION RATE, TEMPERATURE AN0 DOMINANT H AN0 HE ATMOSPHERE A67-40141 SOLAR SYSTEM PLANETS CHARACTERISTICS, TEMPERATURES9 ATMOSPHERES AND INTERNAL PLANETARY MOTION STRUCTURE A67-28959 JOVIAN ROTATIONAL EFFECTS ON MAGNETOSPHERIC MODEL AN0 CONDITIONS OF FLUTING AN0 TWO-STREAM PLANETARY QUARANTINE CONSTRAINTS. NOTING INSTABILITY A66-29952 PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION A67-29098 PLANETARY RADIATION VENUS ATMOSPHERE, SURFACE TEMPERATURE AN0 I JUPITER ENVIRONMENT, EFFECTS OF HUGE MASS, HIGH RADIATION CHARACTERISTICS A66-35799 ROTATION RATE, TEMPERATURE AND DOMINANT H AND HE ATMOSPHERE Ab7-40141 MEAN VALUES OF METHANE WAVELENGTHS IN URANUS SPECTRUM MEASURED FOR DETERMINATION OF ATMOSPHERIC PLANETARY EVOLUTION TEMPERATURE A67-14327 JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM u CORONA DISCHARGE, PRODUCING SIMPLE ORGANIC RELATION BETWEEN SURFACE PRESSURE AN0 ATMOSPHERIC MOLECULES A67-19057 BRIGHTNESS IN OPTICALLY THIN RAYLEIGH SCATTERING ATMOSPHERE. CONSIDERING APPLICATION TO MARS OXYGENIC CONCENTRATIONS IN PRIMITIVE EARTH A67-34536 ATMOSPHERE, DISCUSSING MARTIAN ATMOSPHERE

1-25 PLANETARY SURFACE SUBJECT INDEX

SOVIET BOOK ON PLANETARY PHYSICS COVERING INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS MARTIAN. VENUSIAN AND MERCURIAN ATMOSPHERES, THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS VENUSIAN SURFACE TEMPERATURE AND JOVIAN RADIO HAVE BEEN OBSERVED IN X-BAND FROM GLOW DISCHARGES EMISSION Ab7-38933 A67-14952 81 VENUS RADIATION SPECTRUM IN MM RANGE FROM VENUS SURFACE TEMPERATURE OF VENUS A67-16029 ATMOSPHERE MODELS A67-40120 SOLAR SYSTEM PLANETS CHARACTERISTICS, EQUILIBRIUM RADIATION IN AIR AND GAS MIXTURES TEMPERATURES, ATMOSPHERES AND INTERNAL ASSUMED TO REPRESENT NEAR PLANET ATMOSPHERES STRUCTURE Ab7-28959 NASA-CR-81315 N67-16722 a RADIATIVE RELAXATION TIMES FOR TEMPERATURE PLANETARY SURFACE PERTURBATIONS IN CO 2 WITH SMALL WATER VAPOR JUPITER PLANETARY SURFACE OBSERVATIONS SHOW SLOW ADMIXTURE UNDER CONDITIONS SIMILAR TO MARTIAN EVOLUTION OF ATMOSPHERIC PHENOMENA ATMOSPHERE. DISCUSSING DYNAMICAL PHENOMENA A66-31310 A67-33187

PRESSURE, COMPDSITIONI AND PARTICLE CONTENT OF VOLCANIC AN0 TECTONIC ACTIVITY ON VENUS INFERRED MARTIAN ATMOSPHERE - POLARIZATION, SPECTRAL FROM HIGH SURFACE TEMPERATURE. CONSIDERING BRIGHTNESS. AND TEMPERATURE OF MARTIAN SURFACE POSSIBLE EFFECT ON ATMOSPHERE OBSCURATION Nbb-31472 A67-33232

CARBON DIOXIDE ABUNDANCE AND SURFACE PRESSURE OF VENUS SURFACE TEMPERATURE AND MICROWAVE EMISSION, MARTIAN ATMOSPHERE N66-31475 DISCUSSING IONOSPHERIC MODEL, GREENHOUSE EFFECT. MICROOISCHARGE MODEL, RADIO AURORA. ETC SPECTROPHOTOMETRY AN0 POLARIMETRY OF LUNAR 167-34543 REGIONS, OPTICAL PROPERTIES OF ATMOSPHERE AN0 SURFACE OF MARS, AN0 COMETARY TAILS MODEL COMPUTATIONS OF TEMPERATURE VARIATIONS AN0 NASA-TT-F-382 Nb6-33526 WIND CIRCULATIONS IN MARTIAN ATMOSPHERE NASA-CR-65569 N67-30624 OPTICAL PROPERTIES OF ATMOSPHERE AND SURFACE OF MARS N66-33530 ATMOSPHERE, TEMPERATURE. AND CLOUD COVER OF VENUS NASA-CR-86635 ~6r-3230~ RADIO OCCULTATION TECHNIQUES FOR ANALYSIS OF PLANETARY ATMOSPHERES AND SURFACE TOPOGRAPHY BY ESTIMATES OF VERTICAL TEMPERATURE STRUCTURE. HEAT MEASURING PERTURBATIONS TO AMPLITUDE AN0 FREQUENCY BALANCE. SOLSTICE CIRCULATION, AND THERMALLY ON RADIO LINKS DRIVEN TIDES ON MARS IN COMPARISON WITH LIKE AIAA PAPER 67-119 167-18454 CONOITIDNS ON EARTH NASA-CR-66912 N67-32494 PLANETARY PHYSICS SEMINAR - POLARIZATION. 4 SPECTROMETRIC. AND RADIO SIGNAL TECHNIQUES FOR PLANT /BIOL/ MEASURING MARTIAN SURFACE AND ATMOSPHERIC LEAF-KILL OF BLADES AN0 PINE NEEDLES BY SIMULATED PARAMETERS Nb7-12664 MARS, EARTH, AND VENUS SOLAR RADIATION A66-61851 SURFACE AND ATMOSPHERIC PARAMETER MEASUREMENTS BY w USE OF POLARIZATION INSTRUMENTATION ABOARD PLASMA DENSITY MARINER ORBITER SPACE PROBE N67-12666 MAGNETOSPHERIC MODEL OF JUPITER FROM NUMERICAL CALCULATION OF MAXIMUM NUMBER DENSITY OF PLASMA MARTIAN SURFACE AN0 ATMOSPHERIC PARAMETER A67-25206 MEASUREMENTS BY MEANS OF GAMMA RAY SPECTROMETRIC INSTRUMENTATION ABOARD VOYAGER MISSION PLASMA TURBULENCE ~67-12667 STIMULATION OF JUPITER RADIO EMISSION BY IO A67-25204 MODELS THAT ASSUME MARS ATMOSPHERE HAS ABSORPTIVE RATHER THAN SCATTERING PROPERTIES, AN0 THAT POLAR CAP REDNESS OF PLANET IS DUE TO SELECTIVE ABSORPTION HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR N67-16808 WATER VAPOR PRESENCE, RESULTS INDICATE AMOUNT DEPENDS ON SIZE OF POLAR CAP MODEL FOR MARTIAN ATMOSPHERE AN0 PLANETARY JPL-TR-32-1048 A67-22235 SURFACE ASSUMING ATMOSPHERIC SPECTRUM WITH PURELY SCATTERING PROPERTIES AN0 SURFACE MARTIAN TRANSIENT PHENOMENA CORRELATIONS AMONG COVERED WITH LIMONITE OUST Nb7-16609 MASS MOTION OF WATER IN ATMOSPHERE, POLAR CAP GROWTH AND WHITE CLOUD APPEARANCE FREQUENCY POLARIZATION STUDIES OF RADIO EMISSION FROM UPPER A67-24501 LAYER AN0 SURFACE COVERING OF PLANETS ~6r-16817 POLARIMETRY SPECTROPHOTOMETRY AND POLARIMETRY OF LUNAR MULTICOLOR PHOTOGRAPHIC AN0 VISUAL PATROL OF REGIONS. OPTICAL PROPERTIES OF ATMOSPHERE AND ATMOSPHERE AND SURFACE OF MARTIAN NORTHERN SURFACE OF MARS, AN0 COMETARY TAILS HEMISPHERE DURING SPRING AN0 SUMMER OF 1964-1965 NASA-TT-F-382 N66-33526 APPARITION NASA-CR-83123 N67-21180 POLARIMETRIC STUDY OF PLANET MARS AFCRL-66-492 N66-36942 PLANETARY TEMPERATURE VENUS SURFACE TEMPERATURE FROM MICROWAVE POLARIZATION PROPERTIES OF MERCURY EXPLAINED BY MEASUREMENTSI NOTING THERMAL AND NONTHERMAL SURFACE ONLY, SO THERE IS NO POLARIMETRIC EVIDENCE RAOI ATION A6628129 FOR ATMOSPHERE ON MERCURY A67-26244

MARS UPPER ATMOSPHERE AN0 SINGLE-LAYER IONOSPHERE DISCREPANCY BETWEEN MARS ATMOSPHERIC PRESSURE % UV PHOTOIONIZATION, TEMPERATURE PROFILE AND DATA FROM SPECTROSCOPIC MEASUREMENTS AND FROM CHEMICAL COMPOSITION A66-29417 PHOTOMETRIC AN0 POLARIMETRIC OBSERVATIONS Nb7-16811 VENUS ATMOSPHERE, SURFACE TEMPERATURE AND RADIATION CHARACTERISTICS A66-35799 ATMOSPHERIC BRIGHTNESS OF MARS DETERMINED BY POLARIMETRIC AND PHOTOMETRIC MEASUREMENTS BOUNDARIES AND ATTENUATING MEOIA EFFECT ON TR-34 Nb7-24229 RADIOMETRIC SOUNDING OF PLANETARY ATMOSPHERES BY REMOTE SENSING TECHNIQUES A67-12406 POLARIZATION PRESSURE. COMPOSITION. AND PARTICLE CONTENT OF

1-26 SUBJECT INDEX RADIATION TRANSFER

MARTIAN ATMOSPHERE - POLARIZATION, SPECTRAL MEASUREMENTS Ab7-32322 BRIGHTNESS, AND TEMPERATURE OF MARTIAN SURFACE Nbb-31472 TWO-LAYER ATMOSPHERE MODEL OF VENUS NASA-CR-88980 Nb7-38348 RADIO AN0 X-RAY ASTRONOMY RESEARCH ON X-RAY POLARIZATION, X-RAY TELESCOPE AN0 PLANETARY RADAR ATTENUATION ATMOSPHERE Nb7-2bb20 UPPER LIMITS ON LIQUID WATER CONTENT IN VENUS ATMOSPHERE Ab7-32652 POLARIZATION CHARACTERISTICS RADAR OBSERVATIONS OF VENUS AT 3-8 CM NOTING LOW RADAR CROSS SECTION VALUE OF CROSS SECTION, ECHO SPECTRUM, SIMULTANEOUS UV PHOTOGRAPHS AN0 RADAR CROSS POLARIZATION CHARACTERISTICS, ABSORPTION CROSS SECTION MEASUREMENTS OF VENUS. DISCUSSING SECTION AND ATMOSPHERIC ATTENUATION ATMOSPHERIC MOTION AND ROTATION Ab7-16298 Ab7-38611

POLARIZATION PROPERTIES OF MERCURY EXPLAINED BY RADAR ECHO SURFACE ONLY, SO THERE IS NO POLARIMETRIC EVIDENCE RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW FOR ATMOSPHERE ON MERCURY Ab7-26244 VALUE OF CROSS SECTION. ECHO SPECTRUM. POLARIZATION CHARACTERISTICS, ABSORPTION CROSS POLARIZATION STUDIES OF RADIO EMISSION FROM UPPER SECTION AND ATMOSPHERIC ATTENUATION LAYER AN0 SURFACE COVERING OF PLANETS Ab?-16298 Nb7-16817 RADIANT ENERGY POLARIZED LIGHT RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN WATER CONTENT OF VENUS ATMOSPHERE, AEROSOLS, AN0 VENUS ATMOSPHEREt NOTING GREENHOUSE EFFECT PRESSURE IN UPPER CLOUD LAYER, AND DEVIATIONS IN CAUSE0 BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE DIRECTION OF POLARIZED LIGHT N bb-3 1471 OF IR ABSORPTION 166-40469

SURFACE AN0 ATMOSPHERIC PARAMETER MEASUREMENTS BY RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN USE OF POLARIZATION INSTRUMENTATION ABOARD VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT MARINER ORBITER SPACE PROBE Nb7-12666 CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE OF IR ABSORPTION Ab7-27859 POROUS PLATE TRANSIENT TEMPERATURE RESPONSE OF TRANSPIRATION- RADIATION COOLED POROUS MATRIX ENTERING PLANETARY ATMDSPHERE OPTICAL RADIOMETER FEASIBILITY STUDY FOR WITH CONSTANT VELOCITY AN0 NEGATIVE ENTRY ANGLE DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM Abb-39455 SHOCK LAYER RADIATION DURING ENTRY - INSTRUMENTATION POWDERED METAL NASA-CR-73027 Nbb-35 663 IGNITION TEMPERATURES OF POWDEREO METALS IN SIMULATED MARS AN0 VENUS ATMOSPHERES RADIATION BELT NASA-CR-82878 Nb7-20169 PLANET JUPITER RESEARCH, NOTING UNRESOLVED QUESTIONS OF COSMOLOGY, INTERIOR STRUCTURE AND POWER CONVERSION GREAT RED SPOT Ab7-39092 GASEOUS BREAKDOWN OF SIMULATED PLANETARY ATMOSPHERES AND ILLUSTRATION OF GREENHOUSE RADIATION CONTROL EFFECT, THERMAL RADIATION FROM IONIZED ARGON, RADIATION EQUILIBRIA IN UV LIGHT ON AIR. OXYGEN, LIQUID MAGNETOHYDROOYNAMIC POWER CONVERSION CARBON DIOXIDE, ETC, ANALYZED BY BROMINE LAMP IN Nb7-23655 CONNECTION WITH STUDIES OF PLANETARY ATMOSPHERES A67- 1408 B PRESSURE EFFECT VENUS ATMOSPHERE NOTING PRESSURE INDUCED RADIATION DISTRIBUTION ABSORPTION IN CARBON DIOXIDE-NITROGEN ATMOSPHERE SOLUTION OF ANGULAR DISTRIBUTION OF OUTGOING AS INDICATED IN DECLINE OF MICROWAVE BRIGHTNESS THERMAL RADIATION FROM PLANETARY ATMOSPHERE, USING TEMPERATURE Abb-42668 CHANDRASEKHAR DIFFUSE SCATTERING AN0 TRANSMISSION FUNCTIONS Ab7-22240 CONDITIONS OF ENCOUNTER BETWEEN INTERPLANETARY OUST PARTICLES AND PLANETS RADIATION EFFECT NASA-TM-X-57009 Nbb-35309 RADIATIVE-CONVECTIVE EQUILIBRIUM CALCULATIONS FOR TWO-LAYER MARTIAN ATMOSPHERE PRESSURE MEASUREMENT NASA-CR-75633 Nbb-29732 ELEVATION DIFFERENCES BETWEEN MARTIAN DARK AREAS /MARIA/ AND BRIGHT AREAS /DESERTS/, DISCUSSING RADIATION SPECTRUM SURFACE PRESSURE AN0 TEMPERATURE VENUS RADIATION SPECTRUM IN MM RANGE FROM VENUS Ab7-22957 ATMOSPHERE MODELS Ab7-40120

PLANETARY ATMOSPHERE STRUCTURE DETERMINED FROM EARTH ATMOSPHERIC RADIATION SPECTRAL INFLUENCES ON ENTRY VEHICLE ONBOARO MEASUREMENTS OF PRESSURE. INFRARED MEASUREMENTS OF PLANETARY ATMOSPHERES TEMPERATURE, AN0 ACCELERATION NASA-CR-84157 Nb7-26507 NASA-TN-D-3933 Nb7-23302 METHOD FOR CALCULATING INFRARED RADIATION FROM PROTEIN PLANETARY ATMOSPHERES THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES BMWF-FB-W-67-02 Nb7-30793 AND IN ORIGIN OF ORGANIC MATTER - DETERMINATION OF AMINO ACID PAIRING AN0 SEQUENCES IN PROTEINS RADIATION TRANSFER NASA-CR-74559 Nbb-28800 PLANETARY ATMOSPHERE RESOLUTION SPECTRUM NOTING CARBON DIOXIDE LINES, RADIATION TRANSFER, COMPOSITIONI TEMPERATURES* PRESSURES, ETC Q 166-42 667 QUANTITATIVE ANALYSIS ABSORPTION SPECTROSCOPIC DETERMINATION OF WATER APPROXIMATION METHODS FOR SOLUTION OF EQUATION OF VAPOR ABUNDANCE IN MARTIAN ATMOSPHERE RADIATIVE TRANSFER IN PLANETARY ATMOSPHERES Nb7-12668 Nbb-33534

INVERSE PROBLEM OF RADIATIVE TRANSFER AS APPLIED R TO REMOTE MEASUREMENTS OF INFRAREO RADIATION RADAR ASTRONOMY FROM PLANETARY ATMOSPHERES TWO-LAYER MODEL OF VENUSIAN ATMOSPHERE SATISFYING NASA-TM-X-55857 Nb7-32849 RADIOASTRONOMIC AN0 RADAR SELF-RAOIATION

1-27 RADIATIVE HEAT TRANSFER SUBJECT INDEX

RADIATIVE HEAT TRANSFER ~67-ita05 MATRIX ALGEBRAIC REDUCTION OF EQUATIONS OF RADIATIVE HEAT TRANSFER FOR PLANETARY ATMOSPHERE POLARIZATION STUDIES OF RADIO EMISSION FROM UPPER RM-4951-PRp PT. I N66-34876 LAYER AND SURFACE COVERING OF PLANETS N67-16817 n REDUCTION OF INTEGRAL EQUATIONS OF RADIATIVE TRANSFER FOR PLANETARY ATMOSPHERE WITH RAYLEIGH LUNAR AND PLANETARY STUDIES DEALING WITH COUDE SCATTERING FACILITY WITH 24-INCH TELESCOPE, OICKE-TYPE RM-5056-PR N66-35579 RADIOMETER TO MEASURE EMISSION FROM VENUS, AND

EMISSION SPECTRA OF SILICATES ~6r-23660 ~ CONVECTIVE AN0 RADIATIVE HEAT TRANSFER TO SPACE VEHICLES ENTERING PLANETARY ATMOSPHERES RADIO NOISE AT SUPERORBITAL VELOCITIES UPPER ATMOSPHERE GLOW DISCHARGES STUDIED IN NASA-CR-584 N66-37027 CONNECTION WITH THERMAL RADIO NOISE EMISSION FROM VENUS SURFACE N66-38994 RADIATIVE RELAXATION TIMES FOR TEMPERATURE PERTURBATIONS IN CO 2 WITH SMALL WATER VAPOR RADIO OBSERVATION ADMIXTURE UNDER CONDITIONS SIMILAR TO MARTIAN MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY ATMOSPHERE. DISCUSSING OYNAMICAL PHENOMENA MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, ~67-33187 DETERMINING SHAPE, ATMOSPHERE DENSITY PROFILE, DIURNAL VARIATIDNSs ETC A66-25235 TOTAL EQUILIBRIUM SHOCK LAYER RADIATIVE HEAT TRANSFER FOR ENTRY BODY CONFIGURATIONS IN MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS SIMULATED MARS ATMOSPHERE N67- 12109 ATMOSPHERE N66-31477

RADIO ASTRONOMY MARINER IV RADIO OCCULTATION MEISUREMENTS OF RADIO ASTRONOMY STUDIES OF VENUS AN0 MARS MARS UPPER ATMOSPHERE ~66-31478 NOTING SURFACE PROPERTIES. ATMOSPHERIC STRUCTURE. ETC A66-26031 INDUCED ABSORPTION COEFFICIENTS IN ATMOSPHERE MODEL MEASURED FOR CALCULATION OF VENUS LOWER RADIO ASTRONOMICAL OBSERVATIONS OF VENUS - ATMOSPHERE PROPERTIES FROM RADIO OBSERVATIONS AEROSOL ATMOSPHERIC MODEL FOR EXPLAINING RADIO A67-12949 SPECTRUM N66-31470 RADIO OCCULTATION TECHNIQUES FOR ANALYSIS OF MARINER VENUS 1967 SPACE PROBE, OBTAINING PLANETARY ATMOSPHERES AND SURFACE TOPOGRAPHY BY ATMOSPHERIC PRESSURE DENSITY AND REFRACTIVE INDEX MEASURING PERTURBATIONS TO AMPLITUOE AN0 FREPUENCY FROM RADIO SIGNAL FREQUENCY, INTENSITY AND PHASE ON RADIO LINKS CHANGES AIAA PAPER 67-119 A67-18454 AIAA PAPER 67-118 A67-18310 MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY a RADAR, RADIO ASTRONOMIC AN0 IR SPECTROSCOPIC MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, OBSERVATIONS OF VENUS SURFACE AND ATMOSPHERE, DETERMINING SHAPE. ATMOSPHERE DENSITY PROFILE, EXAMINING GENERAL AN0 SURFACE DATA, CHEMICAL OIURNAL VARIATIONS, ETC COMPOSITION AN0 ATMOSPHERIC MODEL CONSTRUCTION JPL-TR-32-1157 A67-26819 A67-24843 RADIO PROPAGATION # VENUS AND MARS ATMOSPHERE AN0 SURFACE STUDIED BY RADIO OCCULTATION TECHNIQUES FOR ANALYSIS OF RADIO ASTRONOMY A67-34796 PLANETARY ATMOSPHERES AND SURFACE TOPOGRAPHY BY MEASURING PERTURBATIONS TO AMPLITUDE AND FREQUENCY MARINER VENUS 1967 SPACE PROBE, OBTAINING ON RADIO LINKS ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX AIAA PAPER 67-119 167-18454 FROM RADIO SIGNAL FREQUENCY. INTENSITY AN0 PHASE CHANGES RADIO SIGNAL AIAA PAPER 67-118 A67-40094 RADIO OCCULTATION MEASUREMENT OF MARTIAN ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE RADIO AN0 X-RAY ASTRONOMY RESEARCH ON X-RAY PROBE A66-29958 POLARIZATION, X-RAY TELESCOPE AN0 PLANETARY ATMOSPHERE N67-26620 RADIO OCCULTATION MEASUREMENT OF MARTIAN ATMOSPHERE OVER THO REGIONS BY MARINER IV RADIO AURORA SPACE PROBE A67-34151 VENUS SURFACE TEMPERATURE AN0 MICROWAVE EMISSION, DISCUSSING IONOSPHERIC MODEL, GREENHOUSE EFFECT, FREPUENCY, PHASE, AN0 AMPLITUOE CHANGES OF MICRODISCHARGE MODEL, RADIO AURORA, ETC MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AN0 A67-34543 IONOSPHERE OF MARS OBSERVED BEFORE AND AFTER PLANETARY OCCULATATION N67-12754 RADIO EMISSION SPECTROSCOPIC OBSERVATION AN0 SPECTRAL ANALYSIS OF RADIO WAVE ASTRONOMICAL DATA ON PLANETARY ATMOSPHERE, LUNAR DISTRIBUTION OF RADIO BRIGHTNESS TEMPERATURE OVER SURFACE AN0 RADIO EMISSION DISK OF VENUS A67-27333 NASA-TT-F-8881 N66-29398 RADIOMETER STIMULATION OF JUPITER RADIO EMISSION BY 10 OPTICAL RAOIOMETER FEASIBILITY STUDY FOR A67-25204 DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM SHOCK LAYER RADIATION DURING ENTRY - NONTHERMAL RADIO EMISSION FROM JUPITER INSTRUMENTATION ATMOSPHERE, STUDYING IO MODULATION EFFECT NASA-CR-73027 N66-35663 A67-34933 RADIOMETRY NONTHERMAL RADIO EMISSION FROM ELECTRIC DISCHARGES MARS ATMOSPHERIC COMPOSITION DETERMINATION BY WITHIN VENUS WATER CLOUDS A67-37480 SHOCK LAYER RADIOMETRY TECHNIPUE DURING PROBE EXPERIMENT IONOSPHERE MDDEL TO EXPLAIN SPECTRUM OF BRIGHTNESS AIAA PAPER 67-293 A67-26009 TEMPERATURES FOUND IN RADIO EMISSION FROM VENUS ATMOSPHERE N67-16804 RADIOPHYSICS c NONTHERMAL RADIO EMISSION FROM JUPITER ATMOSPHERIC MOOEL COMPARED WITH ASTRONOMICAL ATMOSPHERE, STUDYING IO MODULATION EFFECT OBSERVATIONS TO DETERMINE EFFECT OF CLOUD COVER A67-34933 AN0 RESULTING HIGH EFFECTIVE TEMPERATURE OF RADIO EMISSION FROM VENUS IN CENTIMETER RANGE

1-26 SUBJECT INDEX SATELLITE OBSERVATION

RADIOSONDE ECOM-5123 N67-35919 BOUNDARIES AN0 ATTENUATING MEDIA EFFECT ON RADIOMETRIC SOUNDING OF PLANETARY ATMOSPHERES BY ROCK REMOTE SENSING TECHNIQUES A67-12406 SPECTRAL REFLECTANCE OF SILICATE ROCK POWDERS, JUPITER ATMOSPHERE MEASUREMENTS, AN0 VISIBLE RAYLEIGH DISTRIBUTION AN0 NEAR-INFRARED SPECTRUM DATA FOR ANALYZING COMPUTED EFFECTS OF SPECULAR REFLECTION ON LUNAR SURFACE N67-34775 SCATTERING OF LIGHT BY RAYLEIGH PLANETARY ATMOSPHERE ROCKET INSTRUMENTATION NASA-CR-76122 N66-30187 OPTICAL AN0 ELECTRONIC COMPONENTS FOR ULTRAVIOLET ROCKET SPECTROPHOTOMETRY IN PLANETARY ATMOSPHERE RAYLEIGH SCATTERING NASA-CR-78485 N66-38722 REDUCTION OF INTEGRAL EQUATIONS OF RADIATIVE TRANSFER FOR PLANETARY ATMOSPHERE WITH RAYLEIGH ROTARY STABILITY SCATTERING EARTH-MOON SYSTEM ORIGIN ASSUMING MOON WAS FORMED RM-5056-PR N66-35579 FROM TERRESTRIAL MATERIAL EJECTED FROM EARTH DURING ROTATIONAL INSTABILITY A67-42325 RELATION BETWEEN SURFACE PRESSURE AN0 ATMOSPHERIC BRIGHTNESS IN OPTICALLY THIN RAYLEIGH SCATTERING ROTATING ENVIRONMENT ATMOSPHERE. CONSIDERING APPLICATION TO MARS NUMERICAL CALCULATION OF PERIODS OF NATURAL 167-34536 OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF PLANETARY ATROSPHERES AS FUNCTION OF PLANETS REAL GAS ROTATIONAL SPEED A66-27534 THERMODYNAMIC PROPERTIES OF THREE MARTIAN MODEL ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOH RETROGRADE ROTATION OF CLOUD FORMATIONS OF VENUS FIELDS FOR REAL GASES - TABLES WITH ANGULAR VELOCITY CORRESPONDING TO ONE ATOM-66-1 N67-34135 ROTATION IN FOUR DAYS ANALYZED BY HIGH RESOLUTION PHOTOGRAPHY A66-41181 REENTRY PHYSICS PROGRESS AN0 PROBLEMS IN ATMOSPHERIC ENTRY FOR NUMERICAL CALCULATION OF PERIODS OF NATURAL MANNED AN0 UNMANNED PLANETARY PROBES - REENTRY OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF PHYSICS PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS NASA-TM-X-56855 Nb6-29405 ROTATIONAL SPEED A6b-42320

FLIGHT DYNAMICS OF BALLISTIC AN0 LIFTING VEHICLE JUPITER ENVIRONMENT. EFFECTS OF HUGE MASS. HIGH ENTRIES INTO PLANETARY ATMOSPHERES OF MARS, ROTATION RATE, TEMPERATURE AND DOMINANT H AN0 HE EARTH, VENUS AN0 JUPITER A67-2062 3 ATMOSPHERE A67-40141

REENTRY VEHICLE ROTATING PLASMA HYPERSONIC ENTRY VEHICLE MEASUREMENT OF MARS MODEL FOR DISTRIBUTION OF THERMAL PLASMA IN ATMOSPHERIC DENSITY. PRESSURE* COMPOSITION* MAGNETOSPHERE OF JUPITER UNDER ASSUMPTION OF TEMPERATURE AN0 DETECTION SPECTROMETRY OF CHEMICAL COROTATION WITH PLANET A67-33196 SPECIES IN SHOCK LAYER A66-42680

CONVECTIVE AN0 RADIATIVE HEAT TRANSFER TO S SPACE VEHICLES ENTERING PLANETARY ATMOSPHERES SATELLITE COMMUNICATION AT SUPERORBITAL VELOCITIES PROPERTIES OF MARS ATMOSPHERE ANALYZED BY NASA-CR-584 N66-37027 EJECTED CAPSULE FROM SPACECRAFT. NOTING COMMUNICATIONS SYSTEM 866-30556 REFRACTIVE INDEX MARINER VENUS 1961 SPACE PROBE, OBTAINING SATELLITE MEASUREMENT ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX RADIO OCCULTATION TECHNIQUES FOR ANALYSIS OF FROM RADIO SIGNAL FREQUENCY. INTENSITY AN0 PHASE PLANETARY ATMOSPHERES AN0 SURFACE TOPOGRAPHY BY CHANGES MEASURING PERTURBATIONS TO AMPLITUDE AN0 FREQUENCY AIAA PAPER 67-118 A61-18310 ON RADIO LINKS AIAA PAPER 67-119 A67-18454 MARINER VENUS 1967 SPACE PROBE, OBTAINING ATMOSPHERIC PRESSURE DENSITY AND REFRACTIVE INDEX SATELLITE OBSERVATION FROM RAOiO SIGNAL FREQUENCY, INTENSITY AN0 PHASE MANNED GEOPHYSICAL OBSERVATIONS FROM SATELLITES AS CHANGES TRAINING GROUND FOR PLANETARY RESEARCH, ESPECIALLY AIAA PAPER 67-118 A67-40094 VENUS ATMOSPHERE A67-11395

REFRACTIVITY VENUS BRIGHTNESS TEMPERATURE AN0 ATMOSPHERE AN0 MARTIAN ATMOSPHERE AN0 IONOSPHERE ELECTRON DENSITY MARS ATMOSPHERE SOUNDED BY MARINER I1 SPACE AND REFRACTIVITY PROFILES DETERMINED BY TWO PROBE, NOTING DATA ON MARS MAGNETIC FIELD FREQUENCY BEAT OCCULTATION TECHNIQUE USE0 BY A67-20964 MARINER IV SPACE PROBE Nbl-12665 MARTIAN ATMOSPHERE CIRCULATION MOOEL FROM MARINER RELAXATION IV OCCULTATION EXPERIMENT, STUDYING LATERAL EDDY DIELECTRIC RELAXATION OF GASES AN0 SHARP RISE IN VISCOSITY, WINOS, SURFACE TEMPERATURE AN0 STRESS MICROWAVE ABSORPTION COEFFICIENT IN CYTHEREAN A67-34153 ATMOSPHERE Ab7-2 1372 GROUND INSTRUMENTATION SYSTEM FOR MARINER IV RELAXATION TIME OCCULTATION EXPERIMENT. USING DOPPLER FREQUENCY RADIATIVE RELAXATION TIMES FOR TEMPERATURE PERTURBATION METHOD FOR MARS ATMOSPHERIC PERTURBATIONS IN CO 2 WITH SMALL WATER VAPOR PARAMETERS DETERMINATION 167-34498 ADMIXTURE UNDER CONDITIONS SIMILAR TO MARTIAN ATMOSPHERE. DISCUSSING OYNAMICAL PHENOMENA MARTIAN ATMOSPHERE COMPONENT DUE TO PROTON A67-33187 PENETRATION INTO ATMOSPHERE FROM SOLAR WINO, SUGGESTING RADIO OCCULTATION BY MARS ORBITER RESEARCH PROJECT A67-40799 GEOASTROPHYSICS RESEARCH PERTAINING TO PLANETARY ATMOSPHERES AN0 GEOMAGNETIC PULSATION INVARIANT IM8EDDING EQUATIONS FOR DETERMINING N61-26461 VERTICAL STRATIFICATION OF TERRESTRIAL AN0 PLANETARY ATMOSPHERES ON BASIS OF SATELLITE RICHARDSON NUMBER OBSERVATIONS SPATIAL AN0 TEMPORAL DISTRIBUTION OF GRADIENT RM-5229-PR N67-32463 RICHARDSON NUMBER IN SURFACE AN0 PLANETARY BOUNDARY LAYERS

1-29 SATELLITE PHOTOGRAPHY SUBJECT INDEX

SATELLITE PHOTOGRAPHY MARS, EARTH, AN0 VENUS SOLAR RADIATION VISIBLE BRIGHTNESS FEATURES IN MARINER IV A6b-81851 PHOTOGRAPHS OF MARS INTERPRETED AS CLOUOS A67-34149 SLENDER BODY EARTH AND PLANETARY ATMOSPHERE ENTRY PROBLEMS FOR SATURN /PLANET/ BLUNT NOSED SLENDER VEHICLES NOTING AERODYNAMICS, SPECTRAL STUDY OF JUPITER, SATURN AN0 RINGS OF STABILITY, HEATING, ABLATION AN0 INTERACTION OF SATURN, DETERMINING METHANE CONCENTRATION IN EFFECTS CLOUD LAYERS 166-37035 AIAA PAPER 67-803 A67-42963

CYLINDRICAL FUNCTIONS FOR CALCULATING FREE SOFT LANDING t OSCILLATIONS OF SATURN RINGS AN0 ESTIMATION OF GUIDE0 PROPULSIVE SOLUTION TO MARS ATHOSPHERE- UPPER LIMIT TO MASS OF RING IF MOTION IS STABLE DECELERATED SOFT LANDING VEHICLE TRAJECTORY AGAINST AXISYMMETRIC PERTURBATIONS AIAA PAPER 67-170 A67-18508 166-41063 SOIL PLANETARY SCALE ATMOSPHERIC CIRCULATIONS OF MARTIAN WAVE OF DARKENING ATTRIBUTED TO SOIL FROST JUPITER AN0 SATURN USING FLUID DYNAMICS, NOTING PHENOMENA A66-40478 ROTATION EFFECTS A66-41679 WATER CONTENT AN0 DIFFUSION IN MARTIAN ATMOSPHERE SPECTRAL STUDY OF JUPITER. SATURN AN0 RINGS OF AN0 PROPERTIES OF LIGHT AND DARK SIDES OF SATURN, DETERMINING METHANE CONCENTRATION IN MARTIAN SOIL N66-31481 CLOUD LAYERS A67-15557 RESPONSE OF FUNGI TO DIURNAL TEMPERATURE EXTREMES, I R OBSERVATIONS FOR PRESENCE OF ETHANE IN DESCRIBING SOIL, SIMULATED MARTIAN TEMPERATURE ATMOSPHERES OF JUPITER AN0 SATURN REANALYZED AN0 REGIME AND FUNGI GROWTH Ab7-21991 FOUND CONSISTENT WITH PREVIOUS RESULTS Ab7-21218 SOLAR ACTIVITY RELATIONSHIP BETWEEN TERRESTRIAL AN0 JOVIAN JUPITER AN0 SATURN MOOELSi GIVING PLANET ATMOSPHERIC CIRCULATIONS DUE TO SOLAR ACTIVITY CONSTITUTION, HEAT BALANCE AN0 ATMOSPHERIC A67-21215 COMPOSITION A67-39001 SINGLE AN0 DOUBLE GAS NUMBER-DENSITY EQUATIONS FOR SEASONAL VARIATION DETERMINING TEMPERATURE-ALTITUDE PROFILES HIGH PHOTOMETRIC OBSERVATION DATA ON JUPITER AN0 LOW SOLAR ACTIVITY ATMOSPHERIC MODELS, AN0 ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- ERROR ANALYSIS MONTH PERIODIC CHANGE A67-39299 NASA-CR-79525 N67-13018

MULTICOLOR PHOTOGRAPHIC AN0 VISUAL PATROL OF SOLAR ATMOSPHERE ATMOSPHERE AN0 SURFACE OF MARTIAN NORTHERN SPECTROSCOPIC STUDY OF SOLAR AND PLANETARY t- HEMISPHERE DURING SPRING AN0 SUMMER OF 1964-1965 ATMOSPHERES - OBSERVATIONS OF VENUS AN0 JUPITER, APPARITION AN0 ANALYSIS OF SIMULATED MARTIAN ATMOSPHERE NASA-CR-83123 Nb7-21180 IN VISIBLE AND INFRARED REGIONS NASA-CR-75488 N6b-27755 SHOCK LAYER OPTICAL RADIOMETER FEASIBILITY STUDY FOR SOLAR PHYSICS * DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM RESEARCH IN CELESTIAL MECHANICS, ASTROPHYSICS, SHOCK LAYER RADIATION DURING ENTRY - RADIO PHYSICS, PLANETARY ATMOSPHERES* SOLAR INSTRUMENTATION PHYSICS, AN0 OTHER AREAS OF SPACE SCIENCES NASA-CR-73027 N66-35663 NASA-TM-X-57737 N66-32006

MARS ATMOSPHERIC COMPOSITION DETERMINATION BY SOLAR PROTON SHOCK LAYER RADIOMETRY TECHNIQUE DURING PROBE MARTIAN ATMOSPHERE COMPONENT DUE TO PROTON EXPERIMENT PENETRATION INTO ATMOSPHERE FROM SOLAR WINO, AIAA PAPER 67-293 A67-26009 SUGGESTING RADIO 0CCULTATION.BY MARS ORBITER A67-40799 TOTAL EQUILIBRIUM SHOCK LAYER RADIATIVE HEAT TRANSFER FOR ENTRY BODY CONFIGURATIONS IN COMPONENT OF MARS IONOSPHERE DUE TO SOLAR PROTONS SIMULATED MARS ATMOSPHERE N67-12109 NASA-CR-84411 N67-27370

SHOCK LAYER RADIATION PREDICTIONS FROM MOLECULAR SOLAR RADIATION BAND SYSTEMS IN MARTIAN AN0 VENUSIAN LEAF-KILL OF BLADES AN0 PINE NEEDLES BY SIMULATED ATMOSPHERES MARS, EARTH, AN0 VENUS SOLAR RADIATION NASA-TN-0-3850 Nb7-17629 A66-81851

SHOCK WAVE CONDITIONS OF ENCOUNTER BETWEEN INTERPLANETARY CHEMICAL SYSTEM AN0 REACTION RATES BEHIND STRONG DUST PARTICLES AN0 PLANETS SHOCK WAVES IN MIXTURES OF CARBON DIOXIDE AN0 NASA-TM-X-57009 N66-35309 NITROGEN USE0 TO STUDY ENTRY CONDITIONS INTO MARS ATMOSPHERE Ab6-25276 SOLAR RADIATION EFFECT ON PLANETARY ATMOSPHERE NOTING CHARGED PARTICLE BOMBARDMENTI DAYGLOW MAGNETOSPHERIC BOUNDARY AN0 STANDING SHOCK WAVE PHENOMENA, AURORAL EMISSION. ETC FOR EARTH SCALE0 DOWN TO APPLY TO MARS A67-14699 A67-35442 DISCRETE EQUILIBRIUM TEMPERATURES OF HYPOTHETICAL SILICATE PLANET WITH ATMOSPHERE AN0 HYDROSPHERE OF ONE- LUNAR AN0 PLANETARY STUDIES DEALING WITH COUDE COMPONENT TWO-PHASE SYSTEM UNDER CONSTANT SOLAR

FACILITY WITH 24-INCH TELESCOPE, OICKE-TYPE RAD1AT1 ON Ab7-27462 ~ RADIOMETER TO MEASURE EMISSION FROM VENUS, AN0 EMISSION SPECTRA OF SILICATES N67-23660 SOLAR SPECTROGRAPH HIGH RESOLUTION SPECTRA OF VENUS AN0 JUPITER SIMILARITY HYPOTHESIS USING IMAGE INTENSIFIER AN0 SOLAR SPECTROGRAPH, SPATIAL AN0 TEMPORAL OISTRIBUTION OF GRADIENT MEASURING ABUNDANCES IN PLANETARY ATMOSPHERES RICHARDSON NUMBER IN SURFACE AN0 PLANETARY A67-36309 BOUNDARY LAYERS ECOM-5123 N67-35919 SOLAR SYSTEM ENERGY DISSIPATION AN0 OTHER PROBLEMS FOR ALIEN SIMULATION PLANETARY ATMOSPHERIC ENTRY AT HIGH SPEEDS OF LEAF-KILL OF BLADES AN0 PINE NEEDLES BY SIMULATED INTERPLANETARY FLIGHT A67-21155

1-30 SUBJECT INDEX SPECTRAL BAN0

VOYAGER PROJECT GOALS, ORBITAL DPERATIONSs CAPSULE PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION DESCENT, NAVIGATIONAL SYSTEMSI ETC Abb-29966 Ab7-25232 PLANETARY QUARANTINE CONSTRAINTS, NOTING SOLAR SYSTEM PLANETS CHARACTERISTICS. PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION TEMPERATURES, ATMOSPHERES AND INTERNAL 167-29098 STRUCTURE Abl-28959 SPACECRAFT DESIGN VOYAGER PROJECT GOALS, ORBITAL OPERATIONS, CAPSULE DESIGN AN0 FEASIBILITY STUDIES OF MARS ATMOSPHERE DESCENT, NAVIGATIONAL SYSTEMS, ETC PROBE VEHICLE Abb-25292 rb Ab7-31487 SYSTEM DESIGN OF AUTOMATED LABORATORY AN0 PLANETARY ATMOSPHERES AND POSSIBILITY OF LIFE IN ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN SOLAR SYSTEM EXPLORATION Ab7-30628 P-3669 Nb7-39518 MARINER SPACE VEHICLES DESIGN EVOLUTION NOTING SOLAR WINO CONTRIBUTION TO FUTURE SPACE FLIGHTS THROUGH ATMOSPHERIC MODELS, COMPARING CHAMBERLAIN MEASUREMENT OF ATMOSPHERIC DENSITY OF MARS EVAPORATIVE AND SOLAR BREEZE MODELS, OPIK AND Ab7-42399 SINGER EVAPORATIVE MOOEL AND PARKER SOLAR WIND MODEL Abb-36605 MARS PROBE DESIGN AN0 SUBSYSTEM PERFORMANCE CHARACTERISTICS FOR INVESTIGATING MARTIAN MAGNETOSPHERIC BOUNDARY AND STANDING SHOCK WAVE ATMOSPHERE FOR EARTH SCALED DOWN TO APPLY TO MARS NASA-CR-530 Nb7-32719 Ab7-35442 SPACECRAFT ENVIRONMENT SOLAR X-RAY INTERPLANETARY TRANSIT AN0 ATMOSPHERIC ENTRY OF MARINER/ VENUS SPACE PROBE EXPERIMENT PROPOSED TO UNMANNED VEHICLE LANDING ON MARS SURFACE, WITH MEASURE ECLIPSE OF SOLAR X-RAYS BY VENUSIAN REFERENCE TO HEAT SHIELD TECHNOLOGY ATMOSPHERE Nbb-27957 JPL-TR-32-1145 Ab7-25715

SPACE BUS SPACECRAFT INSTRUMENTATION ON-BOARD TRACKING SYSTEM OF TWO-WAY COHERENT SCIENCE SUBSYSTEMS FOR JUPITER FLYBY MISSIONSI DOPPLER BETWEEN ENTRY CAPSULE AND ORBITING BUS DISCUSSING EQUIPMENT SELECTION, MISSION PLANNING. FOR DETERMINING ORBIT OF ENTRY CAPSULE AND SPACECRAFT DESIGN AN0 TRAJECTORY AND CONSTRAINTS ESTIMATING ATMOSPHERIC PARAMETERS ON VEHICLE CONFIGURATION Nb7-15904 AIAA PAPER 67-120 Ab7-18287

SPACE EXPLORATION INSTRUMENTS FOR MEASURING ALTITUDE DEPENDENT * N ASA SPACE EXPLORATION PROGRAMS DESIGN PHYSICAL PROPERTIES OF VENUS ATMOSPHERE FROM MODIFICATIONS AND INSTRUMENTATION OEVECDPMENTS ENTRY CAPSULE Nb7-15764 NASA-CR-83745 Nb7-25092 VIBRATION AN0 THERMAL RADIATION EFFECTS ON FILTER SPACE FLIGHT WEDGE INFRARED SPECTROMETER USED IN SPACECRAFT MARINER SPACE VEHICLES DESIGN EVOLUTION NOTING STUDIES OF PLANETARY ATMOSPHERES w CONTRIBUTION TO FUTURE SPACE FLIGHTS THROUGH NASA-CR-85797 Nb7-31336 MEASUREMENT OF ATMOSPHERIC DENSITY OF MARS. Ab7-42399 SPACECRAFT PERFORMANCE AERODYNAMIC LIFT IN FUTURE SPACE VEHICLE DESIGN SPACE PROBE DURING VARIOUS FLIGHT REGIMES IN ATMOSPHERES OF SPHERICAL SEMIPASSIVE PROBE FOR DENSITY/ATTITUDE EARTH AN0 PLANETS AND PRESSURE/ALTITUDE PROFILE OF PLANETARY P-3559 Nb7-28513 ATMOSPHERES, NOTABLY MARS AND VENUS Abb-30889 SPACECRAFT SHIELDING AERODYNAMIC, THERMODYNAMIC AND STRUCTURAL DESIGN MARINER/ VENUS SPACE PROBE EXPERIMENT PROPOSED TO ASPECTS OF FLIGHT CAPSULE ENTERING LOW DENSITY MEASURE ECLIPSE OF SOLAR X-RAYS BY VENUSIAN MARS ATMOSPHERE FROM ORBIT Ab7-11432 ATMOSPHERE Nbb-27957 INTERPLANETARY TRANSIT AND ATMOSPHERIC ENTRY OF DYNAMIC MODEL STUDY TO DETERMINE LOW SUBSONIC UNMANNED VEHICLE LANDING ON MARS SURFACE. WITH SPEED STABILITY AND DRAG CHARACTERISTICS DURING REFERENCE TO HEAT SHIELD TECHNOLOGY VERTICAL DESCENT OF ENTRY CONFIGURATIONS J PL-TR- 32- 1145 Ab7-25715 CONSIDERED FOR PROBES OF PLANETARY ATMOSPHERES NASA-TN-0-3499 Nbb-31351 SPECIFIC HEAT DIRECT CALCULATION AND TABLES OF SPECIFIC HEATS TWILIGHT INVESTIGATIONS OF PLANETARY ATMOSPHERES AND RELATED THERMODYNAMIC PROPERTIES OF FROM SPACE PROBES ARBITRARY GAS MIXTURES - MARS ATMOSPHERE MODEL FTD-MT-65-400 Nb7-19543 NASA-TN-0-3540 Nbb-34373

SPACE SCIENCE SPECTRAL ANALYSIS SOVIET BOOK ON PLANETARY PHYSICS COVERING SPECTROSCOPIC STUDY OF SOLAR AND PLANETARY MARTIAN, VENUSIAN AND MERCURIAN ATMOSPHERES, ATMOSPHERES - OBSERVATIONS OF VENUS AND JUPITER, VENUSIAN SURFACE TEMPERATURE AND JOVIAN RADIO AND ANALYSIS OF SIMULATED MARTIAN ATMOSPHERE EMISSION Ab7-38933 IN VISIBLE AND INFRARED REGIONS NASA-CR-75488 Nb6-277 5 5 PLANET JUPITER RESEARCH, NOTING UNRESOLVED QUESTIONS OF COSMOLOGY. INTERIOR STRUCTURE AND SPECTROSCOPIC OBSERVATION AND SPECTRAL ANALYSIS OF GREAT RED SPOT Ab7-39092 ASTRONOMICAL DATA ON PLANETARY ATMOSPHERE, LUNAR 9 SURFACE AND RADIO EMISSION HIGHLIGHTS OF SPACE SCIENCE ACHIEVEMENTS IN 1965 NASA-TT-F-8881 Nbb-29398 NASA-SP-136 Nb7-19022 HIGH RESOLUTION SPECTRA OF VENUS AN0 JUPITER SPACECRAFT CONFIGURATION USING IMAGE INTENSIFIER AND SOLAR SPECTROGRAPH, TOTAL EQUILIBRIUM SHOCK LAYER RADIATIVE HEAT MEASURING ABUNDANCES IN PLANETARY ATMOSPHERES u TRANSFER FOR ENTRY BODY CONFIGURATIONS IN Ab7-36309 SIMULATED MARS ATMOSPHERE N67-12109 SPECTRAL BAND SPACECRAFT CONTAHINATIDN RANDOM ELSASSER BAND MODEL TO COMPUTE ATMOSPHERIC PLANETARY QUARANTINE CONSTRAINTS* NOTING TRANSMISSION OF EARTH AN0 MARS FOR 2-MICRON

1-31 SPECTRAL LINE SUBJECT INDEX

CARBON DIOXIDE BANDS SPECTROMETRIC. AN0 RADIO SIGNAL TECHNIQUES FOR JPL-TR-32-969 A66-38024 MEASURING MARTIAN SURFACE AND ATMOSPHERIC PARAMETERS N67-126b4 MOLECULAR, CONTINUUM AN0 LINE RADIATION OF PLANETARY ATMOSPHERES, COMPARING MOLECULAR BAND SPECTROSCOPIC AN0 PHOTOMETRIC ANALYSIS OF VENUS a STRUCTURE MODELS WITH SPECTRAL MEASUREMENTS OF CN AN0 MARS ATMOSPHERES TO DETERMINE LUMINESCENCE VIOLET BAN0 AN0 OTHER PROPERTIES AIAA PAPER 67-323 A67-26038 NASA-TT-F-394 N67-16801

SPECTRAL LINE SPECTROSCOPIC INVESTIGATION OF VENUS ATMOSPHERE VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON TO DETERMINE NITROGEN, OXYGEN, CARBON DIOXIDE, 4* INTERFEROMETER. FINDING H CL LINES CONSISTENT WATER VAPOR, AN0 OTHER COMPONENTS WITH 2-MM AMAGAT OF GAS N67-16802 JPL-TR-32- 1106 Ab7-24510 DISCREPANCY BETWEEN MARS ATMOSPHERIC PRESSURE SPECTRAL LINE WIDTH DATA FROM SPECTROSCOPIC MEASUREMENTS AN0 FROM SELF-BROADENING COEFFICIENTS OF SPECTRAL LINES PHOTOMETRIC AN0 POLARIMETRIC OBSERVATIONS OF ABSORBING ATMOSPHERIC GASES MEASURE0 IN N67-16811 COMPARISON WITH LINE BROADENING EFFECTS OF NITROGEN A67-22715 SPECULAR REFLECTION COMPUTED EFFECTS OF SPECULAR REFLECTION ON ATMOSPHERIC PRESSURE AT CLOUD TOP AN0 HYDROGEN SCATTERING OF LIGHT BY RAYLEIGH PLANETARY ABUNDANCE IN JUPITER ATMOSPHERE DETERMINED BY ATMOSPHERE ANALYZING METHANE SPECTRAL LINE WIDTHS NASA-CR-76122 N66-30187 A67-37479 SPORE SPECTRAL REFLECTANCE SIMULATED MARTIAN ATMOSPHERIC AND ECOLOGICAL SPECTRAL REFLECTANCE OF SILICATE ROCK POWDERS, EFFECTS ON BACILLUS CEREUS SPORE GERMINATION JUPITER ATMOSPHERE MEASUREMENTS. AN0 VISIBLE NASA-CR-74969 N66-26263 AN0 NEAR-INFRARED SPECTRUM DATA FOR ANALYZING LUNAR SURFACE N67-34775 STAGNATION TEMPERATURE HEATING RATES IN GAS MIXTURES OF PLANETARY SPECTRAL RESOLUTION ATMOSPHERES PREDICTED BY EQUAT'ION USING TRANSPORT PLANETARY ATMOSPHERE RESOLUTION SPECTRUM NOTING PROPERTIES OF GASES AT LOWER TEMPERATURES CARBON DIOXIDE LINES, RADIATION TRANSFER. A66-27432 COMPOSITIONI TEMPERATURES. PRESSURES. ETC A66-42667 STANDING WAVE MAGNETOSPHERIC BOUNDARY AN0 STANDING SHOCK UAVE SPECTROGRAM FOR EARTH SCALED DOWN TO APPLY TO MARS HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR A67-35442 WATER V4POR PRESENCE, RESULTS INDICATE AMOUNT DEPENDS ON SIZE OF POLAR CAP STATIC STABILITY JPL-TR-32-1048 A67-22235 INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS FOR POINTED AND SPHERICALLY BLUNT BODIES IN SPECTROMETER UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE BALLOON-CARRIED AUTOMATIC TELESCOPE-SPECTROMETER A66-25275 OBSERVATION OF VENUS UPPER ATMOSPHERE AND DETERMINATION OF HATER VAPOR CONTENT INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS A66-30352 FOR POINTED AND SPHERICALLY BLUNT BODIES IN UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE GEROIEN TYPE CHAMBER FOR MEASUREMENTS OF ION A67-19380 MOBILITY SPECTRUM IN TERRESTRIAL MESOSPHERE AN0 MARS ATMOSPHERE A66-34712 EARTH AN0 PLANETARY ATMOSPHERE ENTRY PROBLEMS FOR BLUNT NOSED SLENDER VEHICLES NOTING AERODYNAMICS. DATA RECORDING AND REDUCTION OF WATER VAPOR STABILITY, HEATING. ABLATION.AND INTERACTION OF CONTENT IN UPPER ATMOSPHERE OF VENUS AS EFFECTS DETERMINED BY BALLOON CARRIED AUTOMATIC AIAA PAPER 67-803 A67-42963 TELESCOPE-SPECTROMETER UNIT N66-3 1488 STATISTICAL OECISION THEORY SPECTROMETRY STATISTICAL DECISION THEORY APPLIED TO MARTIAN MARTIAN SURFACE AN0 ATMOSPHERIC PARAMETER ATMOSPHERE ANALYSIS, LIFE DETECTION EXPERIMENTS. MEASUREMENTS BY MEANS OF GAMMA RAY SPECTROMETRIC AND GAS CHROMATOGRAM MEASUREMENTS OF N-ALKANE INSTRUMENTATION ABOARD VOYAGER MISSION DISTRIBUTIONS IN MATERIALS N67-12667 NASA-CR-77234 N66-34667

SPECTROPHOTOMETRY STEFAN-BOLTZMINN LAW SPECTROPHOTOMETRY AND POLARIMETRY OF LUNAR NONGRAY MODEL ATMOSPHERES OF JOVIAN PLANETS REGIONS, OPTICAL PROPERTIES OF ATMOSPHERE AN0 CONSTRUCTED FOR DIFFERENT RELATIVE CONCENTRATIONS SURFACE OF MARS, AN0 COMETARY TAILS OF HELIUM AND DIATOMIC HYDROGEN AN0 VARIOUS LIKELY NASA-TT-F-382 N66-33526 EFFECTIVE TEMPERATURES AS CHIEF SOURCES OF THERMAL OPACITY A67-22237 SPECTROSCOPIC TELESCOPE DETECTING PLANETARY LIFE FROM EARTH STELLAR ATMOSPHERE A67-24063 ATMOSPHERIC MODELS, COMPARING CHAMBERLAIN EVAPORATIVE AND SOLAR BREEZE MODELS. OPIK AND SPECTROSCOPY SINGER EVAPORATIVE MODEL AND PARKER SOLAR SPECTROSCOPIC MEASUREMENT OF CARBON DIOXIDE IN WIND MODEL A66-36605 MARS ATMOSPHERE FOR SURFACE PRESSURE AN0 ATMOSPHERIC COMPOSITION N66-3 1473 MOLECULAR HYDROGEN STRUCTURE, CONSIDERING * PLANETARY AN0 STELLAR ATMOSPHERES AND INTERSTfLLAR SPECTROSCOPTIC MEASUREMENTS OF WATER VAPOR AND SPACE A66-39487 CARBON DIOXIDE CONTENTS IN MARS ATMOSPHERE N66-31474 STERILIZATION DECISION THEORY BIOLOGICAL SEARCH STRATEGIES AN0 .r THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS PLANETARY QUARANTINE ASPECTS OF MARS ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION EXPLORATORY MISSIONS DEDUCED SPECTROSCOPICALLY A67-20022 NASA-CR-89772 N67-40462 PLANETARY PHYSICS SEMINAR - POLARIZATION.

1-32 SUBJECT INDEX TEMPERATURE MEASUREMENT

STIMULATED EMISSION IV OCCULTATION EXPERIMENT, STUDYING LATERAL EDDY STIMULATION OF JUPITER RADIO EMISSION BY 10 VISCOSITY, WINDS, SURFACE TEMPERATURE AN0 STRESS Ab7-25204 Ab7-34153

STORM SURVEYOR PROJECT DUST DEVILS IN RELATION TO MARTIAN YELLOW CLOUDS N ASA SPACE EXPLORATION PROGRAMS DESIGN NASA-CR-89578 Nb7-40004 MODIFICATIONS AN0 INSTRUMENTATION DEVELOPMENTS NASA-CR-83745 Nb7-25092 STRUCTURAL DESIGN AERODYNAMICr THERMODYNAMIC AND STRUCTURAL DESIGN NASA PROGRAMS RELATED TO SURVEYOR. MAR ASPECTS OF FLIGHT CAPSULE ENTERING LOW DENSITY PIONEER, VENUS PROBE, AND SIMILAR PRDJ MARS ATMOSPHERE FROM ORBIT Ab7-1 1432 Nb7-25097

AERODYNAMIC, THERMODYNAMIC, HEAT SHIELD AND SYSTEMS DESIGN STRUCTURAL DESIGN ASPECTS OF BALLISTIC VEHICLE SYSTEM DESIGN FOR NONSURVIVABLE MARS PROBE ENTERING PLANETARY ATMOSPHERE Ab7-35315 DEPLOYED FROM ORBITING SPACECRAFT TO PERFORM ENGINEERING EXPERIMENTS FOR ATMOSPHERIC AND SURFACE LAYER TERRAIN PROPERTY DETERMINATION SPATIAL AN0 TEMPORAL DISTRIBUTION OF GRADIENT NASA-CR-66131 Nbb-31819 RICHARDSON NUMBER IN SURFACE AN0 PLANETARY BOUNDARY LAYERS SYSTEM DESIGN OF AUTOMATED LABORATORY AN0 ECOM-5123 Nb7-35919 ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORATION Ab7-30628 SURFACE PRESSURE MARTIAN SURFACE PRESSURE AND SURFACE DENSITY FROM INTERPRETATION OF OBSERVATIONAL DATA T Abb-25291 TABLE DIRECT CALCULATION AND TABLES OF SPECIFIC HEATS VERTICAL TEMPERATURE DISTRIBUTION IN MARTIAN AND RELATED THERMODYNAMIC PROPERTIES OF ATMDSPHEREI NOTING INSENSITIVITY TO SURFACE ARBITRARY GAS MIXTURES - MARS ATMOSPHERE MODEL PRESSURE AND CARBON DIOXIDE VARIATIONS NASA-TN-0-3540 Nbb-34373 Ab6-26132 THERMODYNAMIC PROPERTIES OF THREE MARTIAN MODEL MARTIAN ATMOSPHERIC SURFACE PRESSURE BETWEEN ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOW OCCULTATION LEVELS AT ELECTRICS AN0 MARE FIELDS FOR REAL GASES - TABLES ACIDALIUM ATOM-66-1 N67-34135 NASA-CR-75816 Nbb-29298 TAYLOR THEOREM CARBON DIOXIDE ABUNDANCE AND SURFACE PRESSURE OF EXPERIMENTAL ANALYSIS OF TAYLOR COLUMNS LIKELY TO MARTIAN ATMOSPHERE Nbb-31475 BEAR ON PROCESSES OCCURRING IN JUPITER ATMOSPHERE Abb-33013 ELEVATION DIFFERENCES BETWEEN MARTIAN DARK AREAS /HARIA/ AND BRIGHT AREAS /DESERTS/, DISCUSSING TAYLOR COLUMNS OCCURRENCE CRITERION IN JUPITER SURFACE PRESSURE AND TEMPERATURE ATMOSPHERE INVESTIGATED EXPERIMENTALLY* GIVING Ab?-22957 FLOW PATTERNS Ab7-38999

MARTIAN ATMOSPHERE MODELS WITH DIFFERENT EXPERIMENTAL METHOD FOR STUDYING TAYLOR COLUMNS COMPOSITION. PRESSURE AND TEMPERATURE OVER HILLS AN0 HOLES IN JUPITER ATMOSPHERE Ab7-25 68 5 Ab7-39000

MARS ATMOSPHERE SURFACE PRESSURE* RADIATIVE TEMPERATURE DISTRIBUTION EQUILIBRIUM TEMPERATURES. SUNLIGHT RESONANCE MARTIAN ATMOSPHERIC CIRCULATION - VERTICAL SCATTERING DISTRIBUTION, ETC Ab7-34152 TEMPERATURE DISTRIBUTION. DIURNAL HEATING AN0 TIDES, AND DIFFERENTIAL HEATING AND GENERAL RELATION BETWEEN SURFACE PRESSURE AN0 ATMOSPHERIC CIRCULATION AT SOLSTICES Nbb-31489 BRIGHTNESS IN OPTICALLY THIN RAYLEIGH SCATTERING ATMOSPHERE, CONSIDERING APPLICATION TO MARS DISTRIBUTION OF RAOIO'BRIGHTNESS TEMPERATURE OVER Ab7-34536 DISK OF VENUS Ab7-27333

SURFACE PROPERTY ESTIMATES OF VERTICAL TEMPERATURE STRUCTURE, HEAT PRESSURE. COMPOSITION. AN0 PARTICLE CONTENT OF BALANCE, SOLSTICE CIRCULATION. AND THERMALLY MARTIAN ATMOSPHERE - POLARIZATION. SPECTRAL DRIVEN TIDES ON MARS IN COMPARISON WITH LIKE BRIGHTNESSI AND TEMPERATURE OF MARTIAN SURFACE CONDITIONS ON EARTH Nbb-31472 NASA-CR-66912 Nb7-32494

COMPARISON OF SURFACE AND ATMOSPHERIC TEMPERATURE EFFECT CHARACTERISTICS OF EARTH AND VENUS TRANSIENT TEMPERATURE RESPONSE OF TRANSPIRATION- NASA-TM-X-57351 Nb7-18435 COOLED POROUS MATRIX ENTERING PLANETARY ATMOSPHERE WITH CONSTANT VELOCITY AND NEGATIVE ENTRY ANGLE SURFACE TEMPERATURE Abb-39455 VENUS SURFACE TEMPERATURE FROM MICROWAVE MEASUREMENTS, NOTING THERMAL AN0 NONTHERMAL RESPONSE OF FUNGI TO DIURNAL TEMPERATURE EXTREMES, RAD1AT1 ON Abb-28129 DESCRIBING SOIL, SIMULATED MARTIAN TEMPERATURE REGIME AND FUNGI GROWTH Ab7-21991 VENUS ATMOSPHERE, SURFACE TEMPERATURE AND RADIATION CHARACTERISTICS Abb-35799 TEMPERATURE GRADIENT MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF SURFACE TEMPERATURE OF VENUS Ab7-1b029 VENUS COMPARED WITH SEVERAL MODEL ATMOSPHERES Ab7-24601 MARTIAN ATMOSPHERE MODELS WITH DIFFERENT COMPOSITIONI PRESSURE AND TEMPERATURE TEMPERATURE MEASUREMENT Ab7-25685 ABUNDANCE AND TEMPERATURE OF CARBON DIOXIDE IN MARTIAN ATMOSPHERE, NOTING IMPLICATIONSI VOLCANIC AN0 TECTONIC ACTIVITY ON VENUS INFERRED OBSERVATION METHODS AND RESULTS FROM HIGH SURFACE TEMPERATURE, CONSIDERING Abb-39558 POSSIBLE EFFECT ON ATMOSPHERE OBSCURATION Ab7-33232 MEAN VALUES OF METHANE WAVELENGTHS IN URANUS SPECTRUM MEASURE0 FOR DETERMINATION OF ATMOSPHERIC MARTIAN ATMOSPHERE CIRCULATION MODEL FROM MARINER TEMPERATURE Ab7-14327

1-33 TEMPERATURE PROFILE SUBJECT INDEX

MARS ATMOSPHERE SURFACE PRESSURE, RADIATIVE JUPITER ATMOSPHERES Nb6-28801 EQUILIBRIUM TEMPERATURES, SUNLIGHT RESONANCE SCATTERING DISTRIBUTIONI ETC Ab7-34152 ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS FROM MARINER I1 RADIOMETER DATA, AN0 PLANETARY ATMOSPHERE STRUCTURE DETERMINED FROM THERMODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES ip ENTRY VEHICLE DNBOARO MEASUREMENTS OF PRESSURE, NASA-CR-7b10b Nbb-31639 TEMPERATURE, AND ACCELERATION NASA-TN-0-3933 Nb7-23302 THERHODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS ON CARBON, HYDROGENI OXYGEN, AN0 NITROGEN IN TEMPERATURE PROFILE EARTH, VENUS. MARS, AND JUPITER ATMOSPHERES VERTICAL TEMPERATURE DISTRIBUTION IN MARTIAN Nb6-31642 ATMOSPHERE. NOTING INSENSITIVITY TO SURFACE PRESSURE AND CARBON DIOXIDE VARIATIONS THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS Abb-26132 ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION DEDUCED SPECTROSCOPICALLY Ab7-20022 BOUNDARIES AN0 ATTENUATING MEDIA EFFECT ON RADIOMETRIC SOUNDING OF PLANETARY ATMOSPHERES BY THERMODYNAMIC EQUILIBRIUM COMPOSITION OF ALL REMOTE SENSING TECHNIQUES Ab7- 12406 COMBINATIONS OF C, H, 0 AN0 N AT AVERAGE PRESSURE AN0 TEMPERATURE CALCULATED FOR SINGLE AND DOUBLE GAS NUMBER-DENSITY EQUATIONS FOR ATMOSPHERES OF EARTH, VENUS, MARS AND JUPITER DETERMINING TEMPERATURE-ALTITUOE PROFILE. HIGH Abl-22236 AN0 LOW SOLAR ACTIVITY ATMOSPHERIC MODELS, AND ERROR ANALYSIS THERMODYNAMIC EQUILIBRIUM IN PREBIOLOGICAL NASA-CR-79525 Nb7-13018 ATMOSPHERES. AN0 INORGANIC ORIGIN OF ORGANIC COMPOUNDS IONOSPHERE MODEL TO EXPLAIN SPECTRUM OF BRIGHTNESS NASA-SP-3040 Nb7-27295 TEMPERATURES FOUND IN RADIO EMISSION FROM VENUS ATMOSPHERE Nb7-16804 THERMODYNAMIC PROPERTY DIRECT CALCULATION AND TABLES OF SPECIFIC HEATS TEST PROGRAM AN0 RELATED THERMODYNAMIC PROPERTIES OF SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST ARBITRARY GAS MIXTURES - MARS ATMOSPHERE MODEL PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE, NASA-TN-0-3540 Nbb-34373 TRACKING, COST AND SCHEDULE AIAA PAPER 65-219 Abb-27874 THERHODYNAMIC PROPERTIES OF THREE MARTIAN MODEL ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOW THERMAL CONVECTION FIELDS FOR REAL GASES - TABLES DUST CLOUD FORMATION BY THERMAL CONVECTION IN ATOM-66-1 Nb7-34135 MARTIAN ATMOSPHERE Abb-30925 THERMOSTABILITY THERMAL PLASMA DISCRETE EQUILIBRIUM TEMPERATURES OF HYPOTHETICAL 9 MODEL FOR DISTRIBUTION OF THERMAL PLASMA IN PLANET WITH ATMOSPHERE AND HYDROSPHERE OF DNE- MAGNETOSPHERE OF JUPITER UNDER ASSUMPTION OF COMPONENT TWO-PHASE SYSTEM UNDER CONSTANT SOLAR COROTATION WITH PLANET Ab7-33196 RAD1ATION A67-27462

THERMAL PROPERTY TIDAL OSCILLATION THERMAL STRUCTURE OF UPPER MARS ATMOSPHERE NUMERICAL CALCULATION OF PERIODS OF NATURAL * NASA-TM-X-57327 Nb7-18652 OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS THERMAL PROTECTION ROTATIONAL SPEED Abb-27534 EARTH AN0 PLANETARY ATMOSPHERE ENTRY PROBLEMS FOR BLUNT NOSE0 SLENDER VEHICLES NOTING AERODYNAMICS. NUMERICAL CALCULATION OF PERIODS OF NATURAL STABILITY. HEATING, ABLATION AN0 INTERACTION OF OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF EFFECTS PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS AIAA PAPER 67-803 Ab7-42963 ROTATIONAL SPEED Abb-42320

THERMAL RADIATION TIDE NONGRAY MOOEL ATMOSPHERES OF JOVIAN PLANETS MARTIAN ATMOSPHERIC CIRCULATION - VERTICAL CONSTRUCTED FOR DIFFERENT RELATIVE CONCENTRATIONS TEMPERATURE DISTRIBUTION. DIURNAL HEATING AND OF HELIUM AND DIATOMIC HYDROGEN AN0 VARIOUS LIKELY TIDES, AN0 DIFFERENTIAL HEATING AND GENERAL EFFECTIVE TEMPERATURES AS CHIEF SOURCES OF THERMAL CIRCULATION AT SOLSTICES Nbb-31489 OPACITY Ab7-22237 TOPOGRAPHY SOLUTION OF ANGULAR OISTRIBUTION OF OUTGOING MARTIAN CLOUDS ANALYSIS AND TOPOGRAPHICAL THERMAL RADIATION FROM PLANETARY ATMOSPHERE, USING RELATIONSHIPS, DISCUSSING WHITE AND YELLOW CHANORASEKHAR DIFFUSE SCATTERING AND TRANSMISSION CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES FUNCTIONS Ab7-22240 666-29951

LIMB DARKENING OF PLANETARY ATMOSPHERES IN THERMAL MARTIAN CLOUD ANALYSIS AND TOPOGRAPHICAL INFR ARE0 RELATIONSHIPS NASA-TM-X-57359 Nb7-18280 ESRD-SN-54 Nbb-31187

VIBRATION AN0 THERMAL RADIATION EFFECTS ON FILTER MARTIAN CLOUDS ANALYSIS AND TOPOGRAPHICAL WEDGE INFRARED SPECTROMETER USE0 IN SPACECRAFT RELATIONSHIPS, DISCUSSING WHITE AN0 YELLOW STUDIES OF PLANETARY ATMOSPHERES CLASSIFICATION AND FREQUENCY OF OCCURRENCES NASA-CR-85797 Nb7-3 1336 Ab7-34156

THERMAL RADIO EMISSION TRACE CONTAMINANT UPPER ATMOSPHERE GLOW DISCHARGES STUDIED IN EXTRATERRESTRIAL LIFE DETECTION STUDIED FROM CONNECTION WITH THERMAL RADIO NOISE EMISSION KNOWLEDGE OF MAJOR AN0 TRACE CDMPON€NTS OF -f4 FROM VENUS SURFACE Nbb-38994 ATMOSPHERES Ab7-40999

THERMODYNAMIC EQUILIBRIUM TRACKING SYSTEM THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES ON-BOARD TRACKING SYSTEM OF TWO-WAY COHERENT AND IN ORIGIN OF ORGANIC MATTER - DETERMINATION DOPPLER BETWEEN ENTRY CAPSULE AND ORBITING BUS OF AMINO ACID PAIRING AND SEQUENCES IN PROTEINS FOR DETERMINING ORBIT OF ENTRY CAPSULE AN0 c NASA-CR-74559 Nbb-28800 ESTIMATING ATMOSPHERIC PARAMETERS Nb7-15904 CALCULATION OF THERMODYNAMIC EQUILIBRIUM COMPOSITION OF EARTH, VENUS, MARS AN0

1-34 SUBJECT INDEX VENUS

TRAJECTORY ANALYSIS MARTIAN AND CYTHEREAN ATMOSPHERIC COMPOSITION SCIENCE SUBSYSTEMS FOR JUPITER FLYBY MISSIONS, DETERMINATIONS USING ENTRY PROBE MEASUREMENTS OF DISCUSSING EQUIPMENT SELECTION. MISSION PLANNING. ULTRAVIOLET AND X-RAY ATTENUATION SPACECRAFT DESIGN AND TRAJECTORY AND CONSTRAINTS DAC-60627 Nb7-33758 * ON VEHICLE CONFIGURATION AIAA PAPER 67-120 167-18267 ULTRAVIOLET SPECTROMETER OPTICAL INSTRUMENTS FOR ULTRAVIOLET MEASUREMENTS TRANSIENT RESPONSE IN PLANETARY ATMOSPHERES Nb7-17793 TRANSIENT TEMPERATURE RESPONSE OF TRANSPIRATION- COOLED POROUS MATRIX ENTERING PLANETARY ATMOSPHERE ULTRAVIOLET SPECTROPHOTOMETRY .L WITH CONSTANT VELOCITY AND NEGATIVE ENTRY ANGLE OPTICAL AND ELECTRONIC COMPONENTS FOR ULTRAVIOLET Abb-39455 ROCKET SPECTROPHOTOMETRY IN PLANETARY ATMOSPHERE NASA-CR-78465 Nbb-38722 TRANSPARENCY MECHANISM REGULATING TOTAL AMOUNT OF EARTH AND ULTRAVIOLET SPECTRUM MARS ATMOSPHERE TRANSPARENT TO VISIBLE AND IR SOLAR RAOIATION EFFECT ON PLANETARY ATMOSPHERE RAD1AT1 ON Ab7-18052 NOTING CHARGE0 PARTICLE BDMBARDMENT, DAYGLOW PHENOMENA, AURORAL EMISSION, ETC TRANSPIRATION COOLING Ab7-14699 TRANSIENT TEMPERATURE RESPONSE OF TRANSPIRATION- COOLED POROUS MATRIX ENTERING PLANETARY ATMOSPHERE MRANNEO SPACECRAFT WITH CONSTANT VELOCITY AND NEGATIVE ENTRY ANGLE SYSTEM DESIGN OF AUTOMATED LABORATORY AN0 Abb-39455 ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORATION 167-30628 TRANSPORT EQUATION NUMERICAL SOLUTION OF TRANSPORT AND ENERGY UPPER ATMOSPHERE EQUATIONS IN PLANETARY BOUNDARY LAYER MARINER IV RADIO OCCULTATION MEASUREMENTS OF ECOM-6020 Nbb-33271 MARS UPPER ATMOSPHERE Nb6-31478

TRANSPORT PROPERTY UPPER ATMOSPHERE GLOW DISCHARGES STUDIED IN MATRIX ALGEBRAIC REDUCTION OF EQUATIONS OF CONNECTION WITH THERMAL RADIO NOISE EMISSION RADIATIVE HEAT TRANSFER FOR PLANETARY ATMOSPHERE FROM VENUS SURFACE Nbb-38994 RM-4951-PR. PT. I Nbb-34876 ATOMIC AN0 MOLECULAR PROCESSES IN UPPER TURBULENT HEAT TRANSFER ATMOSPHERES OF VENUS, MARS AND JUPITER RADIATIVE-CONVECTIVE EQUILIBRIUM CALCULATIONS FOR INVESTIGATED BY ATMOSPHERIC MODELS, PRESENTING TWO-LAYER MARTIAN ATMOSPHERE SOLAR-PLANETARY RELATIONSHIP Ab7-18429 NASA-CR-75633 N6b-29732 UPPER IONOSPHERE o TWILIGHT ION-MOLECULE CHEMISTRY OF JUPITER UPPER TWILIGHT INVESTIGATIONS OF PLANETARY ATMOSPHERES ATMOSPHERE, STUDYING EQUILIBRIUM AND FROM SPACE PROBES NONEQUILIBRIUM ABUNDANCES OF HYDROCARBON PRODUCTS FTD-MT-65-400 Nb7-19543 DUE TO UV RADIATION REACTION Ab7-34540

TWILIGHT CUSP EXTENSIONS OF VENUS AND URANUS (Y APPLICATION TO OERIVING HEIGHTS OF SCATTERING MEAN VALUES OF METHANE WAVELENGTHS IN URANUS ATMOSPHERE SPECTRUM MEASURED FOR DETERMINATION OF ATMOSPHERIC P-3621 N67-35341 TEMPERATURE 167-14327

VENUS TWILIGHT SKY INVESTIGATED FOR DISCREPANCIES URANUS AND NEPTUNE SPECTRAL ABSORPTIONS COMPARED BETYEEN PREDICTED AND OBSERVED SHAPE AND WITH LABORATORY SPECTRA OBTAINED WITH VERY LONG PERIODIC APPEARANCE OF PLANET OPTICAL PATHS INDICATE METHANE ROLE IN PLANETARY RM-5386-PR Nb7-37243 ABSORPTION 167-21213 U Y ULTRAVIOLET LIGHT VAN ALLEN BELT MARTIAN ATMOSPHERE TRANSPARENCY AND VISIBILITY OF STIMULATION OF JUPITER RADIO EMISSION BY IO SURFACE DETAILS IN BLUE AND UV LIGHT, SHOWING Ab7-25204 DARK AN0 SEMITONE AREAS INTENSITY, ETC Ab7-34154 VELOCITY DISTRIBUTION TERMINAL VELOCITY CALCULATIONS FOR SPHERICAL SIMULTANEOUS UV PHOTOGRAPHS AND RADAR CROSS PARTICLES IN MARTIAN DAYTIME MOOEL ATMOSPHERES SECTION MEASUREMENTS OF VENUS, DISCUSSING LMSC-b-7666-21 Nbb-37 122 ATMOSPHERIC MOTION AND ROTATION Ab7-38611 VELOCITY MEASUREMENT SPHERICAL OUST PARTICLE TERMINAL VELOCITIES IN ULTRAVIOLET PHOTOMETRY MODEL VENUS ATMOSPHERE RAP10 DRIFT IN LONGITUDE OF SMALL DARK SPOT ON LMSC-677-67-18 Nb7-34596 SOUTH EDGE OF JUPITER NORTH TEMPERATE BELT, NOTING SINUSOIDAL DISPLACEMENT CHARACTERISTICS VELOCITY PROFILE AND MEASUREMENT WITH BLUE AN0 UV PHOTOGRAPHY SPACE RECEIVER OBSERVATIONS OF JOVIAN DECAMETER Abb-33009 FLUX NASA-CR-82654 Nb7-19113 ULTRAVIOLET RADIATION MARS UPPER ATMOSPHERE AND SINGLE-LAYER IONOSPHERE VENUS UV PHOTOIONIZATIONI TEMPERATURE PROFILE AND ABUNDANCE OF EARTH-LIKE PLANET-CONSIDERATIONS OF CHEMICAL COMPOSITION Abb-29417 EARTH AND VENUS ATMOSPHERES Abb-61966 F RADIATION EQUILIBRIA IN UV LIGHT ON AIR, OXYGEN, OBSERVATIONS OF MOON. VENUS, MARS, AND CARBON DIOXIDE. ETC, ANALYZED BY BROMINE LAMP IN JUPITER - SURFACE FEATURES AND ATMOSPHERIC CONNECTION WITH STUDIES OF PLANETARY ATMOSPHERES CHARACTERISTICS - RADIO. RADAR, TELESCOPICI AND Ab7-14088 SPECTROSCOPIC OBSERVATIONS NASA-CR-76142 Nbb-31446 Y ION-MOLECULE CHEMISTRY OF JUPITER UPPER ATMOSPHERE. STUDYING EQUILIBRIUM AN0 ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS NONEQUILIBRIUM ABUNDANCES OF HYDROCARBON PRODUCTS FROM MARINER I1 RADIOMETER DATA, AND DUE TO UV RADIATION REACTION 167-34540 THERMOOYNAMIC ANALYSES OF PLANETARY ATMOSPHERES NASA-CR-76106 Nbb-31639

1-35 VENUS ATMOSPHERE SUBJECT INDEX

THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS METHOD FOR CALCULATING PROPERTIES OF MONO CHROMA TI^ ON CARBON, HYDROGEN, OXYGEN, AN0 NITROGEN IN RADIATION THROUGH LAYER OF DISPERSE0 PARTICLES EARTH, VENUS, MARS. AN0 JUPITER ATMOSPHERES AND ITS APPLICATION TO VENUS CLOUDS Nb6-31642 N6b-31465 4 VENUS BRIGHTNESS TEMPERATURE AND ATMOSPHERE AN0 RADIO ASTRONOMICAL OBSERVATIONS OF VENUS - MARS ATMOSPHERE SOUNDED BY MARINER I1 SPACE AEROSOL ATMOSPHERIC MODEL FOR EXPLAINING RADIO PROBE, NOTING DATA ON MARS MAGNETIC FIELD SPECTRUM Nbb-31470 A67-28964 WATER CONTENT OF VENUS ATMOSPHERE, AEROSOLS, AN0 ir COMPARISON OF SURFACE AN0 ATMOSPHERIC PRESSURE IN UPPER CLOUD LAYER. AND DEVIATIONS IN CHARACTERISTICS OF EARTH AND VENUS DIRECTION OF POLARIZED LIGHT Nbb-3147 1 NASA-TM-X-57351 N67-18435 DATA RECORDING AN0 REDUCTION OF WATER VAPOR ESTIMATES AND OEFINITIONS ON CHARACTERISTICS OF CONTENT IN UPPER ATMOSPHERE OF VENUS AS VENUS LOWER ATMOSPHERE OETERHINEO BY BALLOON CARRIE0 AUTOMATIC P-3513 Nb7-22577 TELESCOPE-SPECTROHETER UNIT Nb6-31488

VENUS ATMOSPHERE LIMB-DARKENING OBSERVATIONS OF VENUS BY MARINER RADIO ASTRONOMY STUDIES OF VENUS AN0 MARS I1 SPACECRAFT MICROWAVE RADIOMETERS NOTING SURFACE PROPERTIES, ATMOSPHERIC STRUCTURE. Nbb-31640 ETC Abb-26031 APPROXIMATION FORMULA DESCRIBING MONOCHROMATIC EARTH REENTRY SIMULATION OF PLANETARY ENTRY TRANSMISSION, REFLECTION, AN0 ABSORPTION OF ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF MARS VENUS CLOUD LAYER Nbb-31b41 AND VENUS TYPE AIAA PAPER 65-218 Abb-27875 ORIGIN OF ATMOSPHERES OF VENUS AND EARTH Nbb-32034 VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AND OF PROPERTIES OF ATMOSPHERES OF MARS, JUPITER AND STATIC EQUILIBRIUM WITHIN KAPLAN ATMOSPHERE VENUS Nb6-32039 Abb-27887 UPPER ATMOSPHERE GLOW DISCHARGES STUOIEO IN VENUS SURFACE TEMPERATURE FROM MICROWAVE CONNECTION WITH THERMAL RADIO NOISE EMISSION MEASUREMENTS, NOTING THERMAL AN0 NONTHERMAL FROM VENUS SURFACE Nb6-38994 RAD1AT1 ON Abb-28129 MANNED GEOPHYSICAL OBSERVATIONS FROM SATELLITES AS BALLOON-CARRIED AUTOMATIC TELESCOPE-SPECTROMETER TRAINING GROUND FOR PLANETARY RESEARCH. ESPECIALLY OBSERVATION OF VENUS UPPER ATMOSPHERE AN0 VENUS ATMOSPHERE Ab7-11395 DETERMINATION OF WATER VAPOR CONTENT c Abb-30352 WATER VAPOR LINES IN SPECTRUM OF VENUS OBTAINED BY PHOTOELECTRIC SCANNING OF SPECTRUM LIMB DARKENING MEASUREMENTS OF VENUS AT 8-14 Ab7-11769 MICRONS WITH 200 INCH HALE TELESCOPE Abb-32517 DOPPLER-DISPLACE0 LINES OF WATER VAPOR ORIGINATING IN ATMOSPHERE OF VENUS OBSERVED ON THREE COUDE ~ VENUS ATMOSPHEREI SURFACE TEMPERATURE AND SPECTROGRAMS Ab7-11774 RADIATION CHARACTERISTICS Abb-35799 INOUCEO ABSORPTION COEFFICIENTS IN ATMOSPHERE SUPERCOOLED WATER DROPLETS HYPOTHESIZED IN VENUS MODEL MEASURED FOR CALCULATION OF VENUS LOWER CLOUD LAYER. BASE0 ON RAOIOMETRIC OBSERVATION IN ATMOSPHERE PROPERTIES FROM RADIO OBSERVATIONS SHF RANGE Abb-37016 Ab7-12949

RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN DEEP CIRCULATION IN VENUSIAN ATMOSPHERE MODEL VENUS ATMOSPHEREI NOTING GREENHOUSE EFFECT OPAQUE TO SOLAR AN0 PLANETARY RADIATION BUT WITH CAUSE0 BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE OIFFERENTIAL HEATING Ab7-14310 OF IR ABSORPTION Abb-40469 INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS RETROGRADE ROTATION OF CLOUD FORMATIONS OF VENUS THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS WITH ANGULAR VELOCITY CORRESPONDING TO ONE HAVE BEEN OBSERVED IN X-BAND FROM GLOW DISCHARGES ROTATION IN FOUR DAYS ANALYZE0 BY HIGH RESOLUTION Ab7-14952 PHOTOGRAPHY Abb-41181 SURFACE TEMPERATURE OF VENUS A67-16029 ABSORPTION LINES ON VENUS SPECTROGRAMS OF ROTATIONAL FINE STRUCTURE OF EXCITED VIBRATIONAL PHOTOMETRY OF INTEGRATED LIGHT OF VENUS. TRANSITION OF CARBON DIOXIDE Abb-41816 INFERRING PRESENCE OF ICE IN ATMOSPHERE FROM HALO EFFECT OF BRIGHTNESS DISPERSION VENUS ATMOSPHERE NOTING PRESSURE INOUCEO Ab7-16407 ABSORPTION IN CARBON DIOXIDE-NITROGEN ATMOSPHERE AS INOICATED IN DECLINE OF MICROWAVE BRIGHTNESS MARINER VENUS 1967 SPACE PROBE. OBTAINING TEMPERATURE Abb-42668 ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX FROM RADIO SIGNAL FREQUENCY, INTENSITY AN0 PHASE METEOROLOGY OF MARS AND VENUS CHANGES NASA-CR-75315 Nbb-27238 AIAA PAPER 67-118 Ab7-18310

MARINER/ VENUS SPACE PROBE EXPERIMENT PROPOSED TO THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS MEASURE ECLIPSE OF SOLAR X-RAYS BY VENUSIAN ATMOSPHERE COMPUTE0 FROM ATOMIC COMPOSITION ATMOSPHERE Nbb-27957 OEDUCED SPECTROSCOPICALLY 167-20022 ? CALCULATION OF THERMODYNAMIC EQUILIBRIUM ANISOTROPIC NONCONSERVATIVE SCATTERING IN MODIFIED COMPOSITION OF EARTH, VENUS, MARS AN0 SCHUSTER- SCHWARZSCHILO APPROXIMATION AND VENUS JUPITER ATMOSPHERES Nbb-28801 CLOUD LAYER 861-20931

DETERMINATION OF ICE CLOUDS AN0 WATER VAPOR IN OIELcCTRIC RELAXATION OF GASES AND SHARP RISE IN VENUS ATMOSPHERE FROM BALLOON OBSERVATIONS MICROWAVE ABSORPTION COEFFICIENT IN CYTHEREAN Nbb-31463 ATMOSPHERE Ab7-21372

PROBLEMS IN DETECTING ICE AN0 WATER CLOUDS ON VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON VENUS Nbb-31464 INTERFEROMETER, FINDING H CL LINES CONSISTENT

1-36 SUBJECT INDEX VENUS PROBE

WITH 2-MM AMAGAT OF GAS SPECTROSCOPIC AND PHOTOMETRIC ANALYSIS OF VENUS JP L-TR- 3 2- 1106 A67-24510 AN0 MARS ATMOSPHERES TO DETERMINE LUMINESCENCE AND OTHER PROPERTIES MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF NASA-TT-F-394 N67-16801 VENUS COMPARED WITH SEVERAL MODEL ATMOSPHERES L A67-24601 SPECTROSCOPIC INVESTIGATION OF VENUS ATMOSPHERE TO DETERMINE NITROGEN, OXYGEN, CARBON DIOXIDE, VOYAGER PROJECT GOALS, ORBITAL OPERATIONS, CAPSULE WATER VAPOR, AN0 OTHER COMPONENTS DESCENT. NAVIGATIONAL SYSTEMS, ETC N67-16802 A67-25232 LUMINESCENCE FROM LOWER ATMOSPHERIC LAYERS AN0 DISTRIBUTION OF RADIO BRIGHTNESS TEMPERATURE OVER IONOSPHERE OBSERVED IN VENUS NIGHT AIRGLOW DISK OF VENUS A67-27333 N67-16803

RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN IONOSPHERE MODEL TO EXPLAIN SPECTRUM OF BRIGHTNESS VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT TEMPERATURES FOUND IN RADIO EMISSION FROM VENUS CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE ATMOSPHERE Nb7-16804 OF IR ABSORPTION A67-27859 ATMOSPHERIC MODEL COMPARED WITH ASTRONOMICAL VOYAGER PROJECT GOALS, ORBITAL OPERATIONS, CAPSULE OBSERVATIONS TO DETERMINE EFFECT OF CLOUD COVER DESCENT, NAVIGATIONAL SYSTEMS, ETC AN0 RESULTING HIGH EFFECTIVE TEMPERATURE OF A67-31487 RADIO EMISSION FROM VENUS IN CENTIMETER RANGE N67-16805 TWO-LAYER MODEL OF VENUSIAN ATMOSPHERE SATISFYING RADIOASTRONOMIC AND RADAR SELF-RADIATION CURVES OF MONOCHRDMATIC ALBEDO FOR LIMB AN0 MEASUREMENTS A67-32322 TERMINATOR OF VENUS N67-16806

UPPER LIMITS ON LIQUID WATER CONTENT IN VENUS SHOCK LAYER RADIATION PREDICTIONS FROM MOLECULAR ATMOSPHERE A67-32652 BAND SYSTEMS IN MARTIAN AND VENUSIAN ATMOSPHERES ASHEN LIGHT AND MAGNETIC FIELD OF VENUS NASA-TN-D-3850 N67-17629 167-33096 ATMOSPHERIC DATA FOR EARTH. MARS, AND VENUS VOLCANIC AND TECTONIC ACTIVITY ON VENUS INFERRED 1967-19026 FROM HIGH SURFACE TEMPERATURE, CONSIDERING POSSIBLE EFFECT ON ATMOSPHERE OBSCURATION CHEMICAL REACTIONS BETWEEN SOLAR HYDROGEN AN0 A67-33232 CARBON MONOXIDE IN VENUS ATMOSPHERE NASA-CR-82960 N67-19904 ATOMIC AN0 MOLECULAR PROCESSES IN CYTHEREAN, 4 MARTIAN AN0 JOVIAN UPPER ATMOSPHERES IGNITION TEMPERATURES OF POWDERED METALS IN A67-34158 SIMULATED MARS AND VENUS ATMOSPHERES NASA-CR-82878 N67-20169 VENUS SURFACE TEMPERATURE AN0 MICROWAVE EMISSION, DISCUSSING IONOSPHERIC MODEL. GREENHOUSE EFFECT, LUNAR AND PLANETARY STUDIES DEALING WITH COUDE MICRODISCHARGE MODEL, RAOIO AURORA, ETC FACILITY WITH 24-INCH TELESCOPE, DICKE-TYPE d A67-34543 RADIOMETER TO MEASURE EMISSION FROM VENUS, AND EMISSION SPECTRA OF SILICATES N67-23660 VENUS AN0 MARS ATMOSPHERE AND SURFACE STUDIED BY RADIO ASTRONOMY A67-34796 MARINER VENUS PROJECT DESIGN CHANGES FOR FLYBY MISSION AND SENSING OF VENUS ATMOSPHERE HIGH RESOLUTION SPECTRA OF VENUS AND JUPITER N67-25094 USING IMAGE INTENSIFIER AN0 SOLAR SPECTROGRAPH, MEASURING ABUNDANCES IN PLANETARY ATMOSPHERES UPPER LIMITS ON LIQUID WATER IN VENUS ATMOSPHERE A67-36309 DUE TO PRESENCE OF HYDROGEN CHLORIDE NASA-CR-84601 N67-28001 NONTHERMAL RADIO EMISSION FROM ELECTRIC DISCHARGES WITHIN VENUS WATER CLOUDS Ab7-37480 DERIVATION OF ATMOSPHERIC PARAMETERS FOR GREENHOUSE MODEL OF VENUS ATMOSPHERE SIMULTANEOUS UV PHOTOGRAPHS AN0 RADAR CROSS NASA-TM-X-53497 N67-29983 SECTION MEASUREMENTS OF VENUS, DISCUSSING ATMOSPHERIC MOTION AND ROTATION ATMOSPHERE, TEMPERATURE, AND CLOUD COVER OF VENUS A67-38611 NASA-CR-86635 N67-32308

SOVIET BOOK ON PLANETARY PHYSICS COVERING SPHERICAL OUST PARTICLE TERMINAL VELOCITIES IN MARTIAN, VENUSIAN AN0 MERCURIAN ATMD,SPHERES, MODEL VENUS ATMOSPHERE VENUSIAN SURFACE TEMPERATURE AN0 JOVIAN RADIO LMSC-6-77-67-18 N67-34596 EMISSION A67-38933 TWILIGHT CUSP EXTENSIONS OF VENUS AN0 INDIGENOUS BIOLOGY IN VENUS CLOUDS, PROPOSING APPL.ICAfION TO DERIVING HEIGHTS OF SCATTERING ISOPYCNIC FLOAT BLADDER MACROORGANISM INGESTING ATMOSPHERE WATER AND MINERALS BLOWN UP FROM SURFACE BY P-3621 N67-35341 PINOCYTOSIS A67-39556 VENUS TWILIGHT SKY INVESTIGATED FOR DISCREPANCIES MARINER VENUS 1967 SPACE PROBE, OBTAINING BETWEEN PREDICTED AN0 OBSERVED SHAPE AND ATMOSPHERIC PRESSURE DENSITY AND REFRACTIVE INDEX PERIODIC APPEARANCE OF PLANET FROM RADIO SIGNAL FREQUENCY, INTENSITY AN0 PHASE RM-53B6-PR N67-37243 CHANGES AIAA PAPER 67-118 A67-40094 TWO-LAYER ATMOSPHERE MODEL OF VENUS P NASA-CR-88980 N67-38348 VENUS RADIATION SPECTRUM IN MM RANGE FROM VENUS ATMOSPHERE MODELS A67-40120 VENUS PROBE VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE EVOLUTION OF ATMOSPHERIC COMPONENTS OF VENUS INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AND OF A67-80916 WITHIN KAPLAN ATMOSPHERE Y STATIC EQUILIBRIUM A66-27887 INSTRUMENTS FOR MEASURING ALTITUDE DEPENDENT PHYSICAL PROPERTIES OF VENUS ATMOSPHERE FROM TERRESTRIAL OBSERVATIONS FROM MANNED GEOPHYSICAL ENTRY CAPSULE N67-15764 SATELLITE APPLIED TO PLANETARY ATMOSPHERIC PHENOMENA - VENUS PROBES

1-37 VENUS RADAR REFLECTION SUBJECT INDEX

P-3418 Nbb-39579 WATER AN0 MINERALS BMWN UP FROM SURFACE BY PINOCYTOSIS Ab7-39556 RADAR, RADIO ASTRONOMIC AN0 IR SPECTROSCOPIC OBSERVATIONS OF VENUS SURFACE AN0 ATMOSPHERE. WATER VAPOR EXAMINING GENERAL AN0 SURFACE DATA, CHEMICAL BALLOON-CARRIED AUTOMATIC TELESCOPE-SPECTROMETER COMPOSITION AN0 ATMOSPHERIC MODEL CONSTRUCTION OBSERVATION OF VENUS UPPER ATMOSPHERE AN0 Ab7-24843 DETERMINATION OF WATER VAPOR CONTENT Abb-30352 VENUS RADAR REFLECTION RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW DETERMINATION OF ICE CLOUDS AN0 WATER VAPOR IN VALUE OF CROSS SECTION, ECHO SPECTRUM, VENUS ATMOSPHERE FROM BALLOON OBSERVATIONS * POLARIZATION CHARACTERISTICS, ABSORPTION CROSS Nbb-31463 SECTION AN0 ATMOSPHERIC ATTENUATION 167-1 b2W PROBLEMS IN DETECTING ICE AN0 WATER CLOUDS ON VENUS Nbb-31464 SIMULTANEOUS UV PHOTOGRAPHS AN0 RADAR CROSS SECTION MEASUREMENTS OF VENUS, DISCUSSING SPECTROSCOPTIC MEASUREMENTS OF WATER VAPOR AND ATMOSPHERIC MOTION AN0 ROTATION CARBON DIOXIDE CONTENTS IN MARS ATMOSPHERE Ab7-38611 Nbb-31474

VERTICAL DISTRIBUTION DATA RECORDING AN0 REDUCTION OF WATER VAPOR VERTICAL TEMPERATURE DISTRIBUTION IN MARTIAN CONTENT IN UPPER ATMOSPHERE OF VENUS AS ATMOSPHERE, NOTING INSENSITIVITY TO SURFACE DETERMINED BY BALLOON CARRIED AUTOMATIC PRESSURE AN0 CARBON DIOXIDE VARIATIONS TELESCOPE-SPECTROMETER UNIT Nbb-31488 Abb-26132 WATER VAPOR LINES IN SPECTRUM OF VENUS OBTAINED VIBRATION TESTING BY PHOTOELECTRIC SCANNING OF SPECTRUM VIBRATION AN0 THERMAL RADIATION EFFECTS ON FILTER Ab7-11769 WEDGE INFRARED SPECTROMETER USE0 IN SPACECRAFT STUDIES OF PLANETARY ATMOSPHERES FROST PHENOMENA ON MARS EXAMINED ON BASIS OF NASA-CR-85797 Nb7-31336 MARTIAN WAVE OF OARKENINGv NOTING NECESSITY OF DELIQUESCENT SALTS TO ATTRACT AN0 RETAIN WATER ON VISIBLE RADIATION SURFACE Ab7-18645 MECHANISM REGULATING TOTAL AMOUNT OF EARTH AN0 MARS ATMOSPHERE TRANSPARENT TO VISIBLE AN0 IR HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR RADIATION Ab7-18052 WATER VAPOR PRESENCEI RESULTS INDICATE AMOUNT DEPENDS ON SIZE OF POLAR CAP VOLCANIC THEORY JPL-TR-32-1048 Ab7-22235 VOLCANIC AN0 TECTONIC ACTIVITY ON VENUS INFERRED FROM HIGH SURFACE TEMPERATURE, CONSIDERING NONTHERMAL RADIO EMISSION FROM ELECTRIC DISCHARGES ’ POSSIBLE EFFECT ON ATMOSPHERE OBSCURATION WITHIN VENUS WATER CLOUDS Ab7-37480 Ab7-33232 ABSORPTION SPECTROSCOPIC DETERMINATION OF WATER VOLTAGE BREAKDOWN VAPOR ABUNDANCE IN MARTIAN ATMOSPHERE DATA REPRESENTING MONOPOLE ANTENNA VOLTAGE Nb7-12668 Ir BREAKOWON IN SIMULATED MARS AN0 VENUS ATMOSPHERES Ab7-35829 FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTIAN ATMOSPHERE FOR DETERMINATION OF PROFILES OF VOYAGER PROJECT CARBON DIOXIDE, PARTICULATE MATTER AN0 WATER VOYAGER PROJECT GOALS, ORBITAL OPERATIONS. CAPSULE VAPOR DESCENT, NAVIGATIONAL SYSTEMS, ETC NASA-TN-0-4115 Nb7-34884 Ab7-25232 WEATHER FORECASTING VOYAGER PROJECT GOALS, ORBITAL OPERATIONSI CAPSULE WEITHER FORECASTING FOR MANNED MARS LANDING BY DESCENT, NAVIGATIONAL SYSTEMSt ETC USE OF METEOROLOGICAL SATELLITE Ab7-31487 Nbb-31491

MARTIAN SURFACE AN0 ATMOSPHERIC PARAMETER WEIGHT FACTOR MEASUREMENTS BY MEANS OF GAMMA RAY SPECTROMETRIC HEAT BALANCE, PRESSURIZATION, AN0 MINIMUM WEIGHT INSTRUMENTATION ABOARD VOYAGER MISSION DESIGN CRITERIA FOR INFLATABLE STRUCTURES IN Nb7-12667 NEAR-PLANETARY ATMOSPHERE NASA-CR-84829 Nb7-28769

W WINO WATER OUST DEVILS IN RELATION TO MARTIAN YELLOW CLOUDS UPPER LIMITS ON LIQUID WATER IN VENUS ATMOSPHERE NASA-CR-89578 Nbl-40004 DUE TO PRESENCE OF HYDROGEN CHLORIDE NASA-CR-84601 Nb7-28001 WIND CIRCULATION MODEL COMPUTATIONS OF TEMPERATURE VARIATIONS AN0 WATER CONTENT WIND CIRCULATIONS IN MARTIAN ATMOSPHERE WATER CONTENT OF VENUS ATMOSPHERE, AEROSOLS, AN0 NASA-CR-85569 Nb7-30624 PRESSURE IN UPPER CLOUD LAYER, AN0 DEVIATIONS IN DIRECTION OF POLARIZED LIGHT Nbb-31471 WIND MEASUREMENT MARTIAN ATMOSPHERE CIRCULATION MODEL FROM MARINER WATER CONTENT AN0 DIFFUSION IN MARTIAN ATMOSPHERE IV OCCULTATION EXPERIMENT, STUDYING LATERAL EOOY AN0 PROPERTIES OF LIGHT AN0 DARK SIDES OF VISCOSITY. WINOS, SURFACE TEMPERATURE AN0 STRESS MARTIAN SOIL Nbb-3 1481 Ab7-34153 Bi MARTIAN TRANSIENT PHENOMENA CORRELATIONS AMONG MASS MOTION OF WATER IN ATMOSPHERE, POLAR CAP x GROWTH AN0 WHITE CLOUD APPEARANCE FREQUENCY X-BIND Abl-24501 INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS UPPER LIMITS ON LIQUID WATER CONTENT IN VENUS HAVE BEEN OBSERVED IN X-BAND FROM GLOW DISCHARGES v ATMOSPHERE Ab7-32652 Ab7-14952

WATER INTAKE X-RAY ABSORPTION INDIGENOUS BIOLOGY IN VENUS CLOUDS, PROPOSING MARTIAN AN0 CYTHEREAN ATMOSPHERIC COMPOSITION ISOPYCNIC FLOAT BLADDER MACROORGANISM INGESTING DETERMINATIONS USING ENTRY PROBE MEASUREMENTS OF

1-38 SUBJECT INDEX X-RAY TELESCOPE

ULTRAVIOLET AND X-RAY ATTENUATION DAC-60627 N67-33750

X-RAY TELESCOPE 9 RADIO AND X-RAY ASTRONOMY RESEARCH ON X-RAY POLARIZATION* X-RAY TELESCOPE AND PLANETARY ATMOSPHERE N67-26620

1-39

Personal uthor Index

PLANETARY ATMOSPHERES / a continuing bibliography with indexes JULY 1968

Typical Personal Author Index Listing

A.E.R.E/R.P.S. FILM APPLEBAUII. D. C. INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS REPORT/MEETINGPAPER NUMBER HAVE BEEN OBSERVED IN X-BAND FROM GLOW DISCHARGES ~~~, '8 Ab7-14952 ASAFs G. Listings in this index are arranged alphabetically by personal author. The Nota- MARTIAN SURFACE AND ATMOSPHERIC PARAMETER tion of Content (NOCI. rather than the title of the document. is used to provide MEASUREMENTS BY MEANS OF GAMMA RAY SPECTROMETRIC a more exact description of the subject matter When it appears, the report/ INSTRUMENTATION ABOARD VOYAGER MISSION Nb7-12667 meeting paper number may provide a clue to the type of document cited (e g . NASA report. NASA contractor report. conference paper. translation) The ac- AVRAMCHUK. V. V. cession number provides a key to the location of the citation in the abstract CURVES OF MONOCHROMATIC ALBEDO FOR LIMB AND section Under each personal author. the Notations of Content for published TERMINATOR OF VENUS Nb7-16806 literature references (A67) are listed first followed by report references (N67). each set of references is arranged in ascending number order 8 BARABASHOV. N. Pa OPTICAL THICKNESS OF MARS ATMOSPHERE DETERMINED BY PHOTOMETRIC OBSERVATIONS N67-16807

BARKER. E- SI A CARBON DIOXIDE ABUNDANCE AND SURFACE PRESSURE OF AKSENOVi A. N. MARTIAN ATMOSPHERE, NOTING SELF-BROADENING PHOTOMETRIC OBSERVATION DATA ON JUPITER CORRECTION Ab7-21250 ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- MONTH PERIODIC CHANGE Ab7-39299 BARRINGTON. A. E- FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTIAN ALLISON, D. 0. ATMOSPHERE FOR DETERMINATION OF PRDFILES OF DIRECT CALCULATION AND TABLES OF SPECIFIC HEATS CARBON DIOXIDE. PARTICULATE MATTER .AND WATER AND RELATED THERMODYNAMIC PROPERTIES OF VAPOR ARBITRARY GAS MIXTURES - MARS ATMOSPHERE MODEL NASA-TN-0-4115 Nb7-34084 NASA-TN-D-3540 Nbb-34373 BIRTH. C. A. AMBARTSURYAN. V- A. SOLAR RADIATION EFFECT ON PLANETARY ATMOSPHERE SCATTERING OF LIGHT IN PLANETARY ATMOSPHERES AND NOTING CHARGED PARTICLE BOMBARDMENT. DAYGLOW DIFFUSE REFLECTION OF LIGHT BY TURBID MEDIUM PHENOMENAp AURORAL EMISSION, ETC Nb7-23425 667-14699

ANDERSON, A. BASHARINOV. A- E. SELF-BROADENING COEFFICIENTS OF SPECTRAL LINES SUPERCOOLED WATER DROPLETS HYPOTHESIZED IN VENUS OF ABSORBING ATMOSPHERIC GASES MEASURE0 IN CLOUD LAYER. BASED ON RADIOMETRIC OBSERVATION IN COMPARISON WITH LINE BROADENING EFFECTS OF SHF RANGE Abb-31016 NITROGEN Ab7-22715 BASHARINOV. Ai YE. ANDERSON, A. D. POLARIZATION STUDIES OF RADIO EMISSION FROM UPPER MARTIAN DAYTIME ATMOSPHERE FROM ZERO TO 50 KM LAYER AND SURFACE COVERING OF PLANETS PRESENTING SPHERICAL PARTICLE TERMINAL VELOCITIES Nb7-16817 AND POSSIBLE SIZES FOR OBSCURATIONSt USING MARINER IV OCCULTATION Ab7-26314 BECKMAN. J. E. HIGH RESOLUTION SPECTRA OF VENUS AND JUPITER VOLCANIC AN0 TECTONIC ACTIVITY ON VENUS INFERRED USING IMAGE INTENSIFIER AND SOLAR SPECTROGRAPH, FROM HIGH SURFACE TEMPERATURE. CONSIDERING MEASURING ABUNOANCES IN PLANETARY ATMOSPHERES POSSIBLE EFFECT ON ATMOSPHERE OBSCURATION Ab7-36309 167-33232 ATMOSPHERIC PRESSURE AT CLOUD TOP AN0 HYDROGEN TERMINAL VELOCITY CALCULATIONS FOR SPHERICAL ABUNDANCE IN JUPITER ATMOSPHERE DETERMINED BY PARTICLES IN MARTIAN DAYTIME MODEL ATMOSPHERES ANALYZING METHANE SPECTRAL LINE WIDTHS LHSC-676-66-21 Nbb-37122 A67-37479

SPHERICAL DUST PARTICLE TERMINAL VELOCITIES IN BELLMAN. R. MODEL VENUS ATMOSPHERE INVARIANT IMBEDDING EQUATIONS FOR DETERMINING L MSC-6-77- 67- 18 Nb7-3459 6 VERTICAL STRATIFICATION OF TERRESTRIAL AND PLANETARY ATMOSPHERES ON BASIS OF SATELLITE ANDERSON. C. E- OBSERVATIONS SYSTEM DESIGN OF AUTOMATED LABORATORY AN0 RM-5229-PR Nb7-32463 ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN EXPLORATION Ab7-30628 BELLMAN. R. E. INITIAL VALUE APPROACH TO CHANDRASEKHAR PLANETARY ANDERSON, 0- M. PROBLEM TO ESTIMATE PLANETARY PROPERTIES AND FROST PHENOMENA ON MARS EXAMINED ON BASIS OF ATMOSPHERIC COVERS MARTIAN WAVE OF DARKENING, NOTING NECESSITY OF RM-4991-PR Nb6-29959 DELIQUESCENT SALTS TO ATTRACT AND RETAIN WATER ON SURFACE Ab7-18645

1-41 BELTONq Ma J. S. PERSONAL AUTHOR INDEX

BELTON, Me J. 5. PHOTOGRAPHY Ab6-41101 ABUNDANCE AN0 TEMPERATURE OF CARBON DIOXIDE IN MARTIAN ATMOSPHERE, NOTING IMPLICATIONS, SIMULTANEOUS UV PHOTOGRAPHS AN0 RADAR CROSS OBSERVATION METHODS AN0 RESULTS SECTION MEASUREMENTS OF VENUS, DISCUSSING Abb-39558 ATMOSPHERIC MOTION AN0 ROTATION e Ab7-38611 WATER VAPOR LINES IN SPECTRUM OF VENUS OBTAINED BY PHOTOELECTRIC SCANNING OF SPECTRUM BRANCAZIO, P. J. Ab7-11769 EARTH AN0 PLANETARY OCEAN AN0 ATMOSPHERIC ORIGIN, EVOLUTION, AN0 COMPOSITION Nbb-37965 I RADIATIVE RELAXATION TIMES FOR TEMPERATURE PERTURBATIONS IN CO 2 WITH SMALL WATER VAPOR BRERETON, R. 6. ADMIXTURE UNDER CONDITIONS SIMILAR TO MARTIAN INSTRUMENTS FOR MEASURING ALTITUDE DEPENDENT ATMOSPHERE, DISCUSSING OYNAMICAL PHENOMENA PHYSICAL PROPERTIES OF VENUS ATMOSPHERE FROM Ab7-33187 ENTRY CAPSULE Nb7-15764

BEN-ARYEH, YI BRONNER, Fa E. ABSORPTION SPECTROSCOPIC DETERMINATION OF WATER MARTIAN WAVE OF DARKENING ATTRIBUTED TO SOIL FROST VAPOR ABUNDANCE IN MARTIAN ATMOSPHERE PHENOMENA Abb-40478 Nb7-12668 BRONSHTEN, V. A- BENEDICTS W- Sa RADAR, RADIO ASTRONOMIC AN0 IR SPECTROSCOPIC VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON OBSERVATIONS OF VENUS SURFACE AN0 ATMOSPHERE, INTERFEROMETER. FINDING H CL LINES CONSISTENT EXAMINING GENERAL AN0 SURFACE DATA, CHEMICAL WITH 2-MU AMAGAT OF GAS COMPOSITION AN0 ATMOSPHERIC MODEL CONSTRUCTION JPL-TR-32-1106 Ab7-24510 Ab7-24843

BERGSTRALH, J- T. BROOKS, E. M. UPPER LIMIT OF CARBON DIOXIDE ABUNDANCE IN METEOROLOGY OF MARS AN0 VENUS MERCURY ATMOSPHERE Ab7-41836 NASA-CR-75315 N66-27230

BERKNERt L. V. BROWN. H. LIMITATION ON OXYGEN CONCENTRATION IN POSSIBLE OBSERVATIONS OF MOONt VENUS, MARS, AN0 PRIMITIVE ATMOSPHERES EXAMINED VIA PHYSICAL AN0 JUPITER - SURFACE FEATURES AN0 ATMOSPHERIC PHOTOCHEMICAL FACTORS A6b-2 6 122 CHARACTERISTICS - RADIO, RADAR, TELESCOPIC, AND SPECTROSCOPIC OBSERVATIONS OXYGENIC CONCENTRATIONS IN PRIMITIVE EARTH NASA-CR-76142 Nbb-31446 ATMOSPHERE, DISCUSSING MARTIAN ATMOSPHERE COMPOSITION Ab7-34095 BYRON, S. e MODEL OF NONEQUILIBRIUM PROPERTIES OF HIGH BEUF, F. 6. TEMPERATURE CARBON DIOXIDE AND OTHER GAS MIXTURES SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE, MARTIAN ATMOSPHERE 167-11436 TRACKING, COST AN0 SCHEDULE AIAA PAPER 65-219 Abb-27074 C 4y SYSTEM DESIGN OF AUTOMATED LABORATORY AND CAIN, 0- La ASSOCIATED ENTRY VEHICLE FOR UNMANNED MARTIAN RADIO OCCULTATION MEASUREMENT OF MARTIAN EXPLORATION Ab7-30628 ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE PROBE A6b-29958 BILWAKESH, K- R- CHEMICAL KINETICS OF CARBON DIOXIDE FOR MARTIAN MARINER VENUS 1967 SPACE PROBE. OBTAINING ATMOSPHERIC ENTRY APPLICATIONS ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX ARL-67-0113 Nb7-39458 FROM RADIO SIGNAL FREQUENCYq INTENSITY AN0 PHASE CHANGES BINDER, A. B. AIAA PAPER 67-110 Ab7-18310 CARBON DIOXIDE STUDY IN MERCURY ATMOSPHERE YIELDS NEGATIVE RESULTS FROM OBSERVATIONS MADE WITH IR RADIO OCCULTATION MEASUREMENT OF MARTIAN SPECTROMETER AN0 61 INCH REFLECTOR ATMOSPHERE OVER TWO REGIONS BY MARINER IV Ab7-22016 SPACE PROBE Ab7-34151

BIONOIq M- A- MARINER VENUS 1967 SPACE PROBE, OBTAINING CARBON DIOXIDE IONS WITH ELECTRONS DISSOCIATIVE ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX RECOMBINATION MEASUREMENTS WITH MICROWAVE- FROM RADIO SIGNAL FREQUENCY. INTENSITY AN0 PHASE AFTERGLOW DIFFERENTIALLY PUMPED QUADRUPOLE MASS- CHANGES SPECTROMETER APPARATUS. NOTING MARTIAN ATMOSPHERE AIAA PAPER 67-118 Ab7-40094 MODEL SRCC-55 Ab7-32826 MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS ATMOSPHERE N6b-31477 BOISSEVAINs A- 6. FREE FALLING PROBE TEST DURING TERMINAL DESCENT MARINER IV RADIO OCCULTATION MEASUREMENTS OF FOR DETERMINING UNKNOWN PLANETARY ATMOSPHERE MARS UPPER ATMOSPHERE Nbb-31478 PROFILE FROM ONBOARD MEASUREMENTS ALONE Ab7-22768 FREQUENCY, PHASE. AN0 AMPLITUDE CHANGES OF MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AN0 PLANETARY ATMOSPHERE STRUCTURE DETERMINED FROM IONOSPHERE OF MARS OBSERVE0 BEFORE AN0 AFTER ENTRY VEHICLE ONBOARD MEASUREMENTS OF PRESSURE, PLANETARY OCCULATATION N67-12754 TEMPERATURE. AN0 ACCELERATION Y NASA-TN-0-3933 Nb7-23302 CAMERON. A- 6. W- EARTH-MOON SYSTEM ORIGIN ASSUMING MOON WAS FORMED BOOBAR. M. 6. FROM TERRESTRIAL MATERIAL EJECTED FROM EARTH MANNED MARS ENTRY AN0 LANDING, DISCUSSING DURING ROTATIONAL INSTABILITY A67-42325 AEROBRAKING AS FEASIBLE ENTRY MODE I Abb-25272 ORIGIN OF ATMOSPHERES OF VENUS AN0 EARTH Nbb-32034 BOYER, C. RETROGRADE ROTATION OF CLOUD FORMATIONS OF VENUS EARTH AN0 PLANETARY OCEAN AN0 ATMOSPHERIC ORIGIN. WITH ANGULAR VELOCITY CORRESPONDING TO ONE EVOLUTION, AN0 COMPOSITION Nb6-37965 ROTATION IN FOUR DAYS ANALYZED BY HIGH RESOLUTION

1-42 PERSONAL AUTHOR INDEX DAYHOFFI M- 0.

CAPEN, C. F. CORTRIGHT, E. M. MULTICOLOR PHOTOGRAPHIC AN0 VISUAL PATROL OF VOYAGER PROJECT GOALS, ORBITAL OPERATIONS, CAPSULE ATMOSPHERE AND SURFACE OF MARTIAN NORTHERN DESCENT* NAVIGATIONAL SYSTEMS, ETC HEMISPHERE DURING SPRING AN0 SUMMER OF 1964-1965 Ab7-25232 APPARITION b NASA-CR-83123 Nb7-21180 VOYAGER PROJECT GOALS, ORBITAL OPERATIONS, CAPSULE DESCENT, NAVIGATIONAL SYSTEMS, ETC CARLSON9 R. W. Ab7-31487 PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS LANDING MISSION, OISCUSSING USE OF LIFTING COSTIGANs P. J. , VEHICLES Abb-25273 DYNAMIC MOOEL STUDY TO DETERMINE LOW SUBSONIC SPEED STABILITY AN0 DRAG CHARACTERISTICS DURING CARUSO, A. J. VERTICAL DESCENT OF ENTRY CONFIGURATIONS FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTIAN CONSIDERED FOR PROBES OF PLANETARY ATMOSPHERES ATMOSPHERE FOR OETERMINATION OF PROFILES OF NASA-TN-0-3499 Nbb-31351 CARBON DIOXIDE, PARTICULATE MATTER AND WATER VAPOR CRAVEN, C. W- NASA-TN-D-4115 Nb7-34684 PLANETARY QUARANTINE CONSTRAINTS, NOTING PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION CHAI, A.-T. Abb-299bb SELF-BROADENING COEFFICIENTS OF SPECTRAL LINES OF ABSORBING ATMOSPHERIC GASES MEASURE0 IN PLANETARY QUARANTINE CONSTRAINTS, NOTING COMPARISON WITH LINE BROADENING EFFECTS OF PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION NITROGEN A67-22715 Ab7-29098

CHAMBERLAIN, J- W- CRUIKSHANK, D- P. MARINER IV OCCULTATION EXPERIMENT CONCERNING CARBON OIOXIOE STUDY IN MERCURY ATMOSPHERE YIELDS CARBON DIOXIDE AND IONOSPHERIC PEAKS IN MARTIAN NEGATIVE RESULTS FROM OBSERVATIONS MADE WITH IR ATMOSPHERE 666-25834 SPECTROMETER AND 61 INCH REFLECTOR Ab7-22016 DIFFUSE REFLECTION BY PLANETARY INHOMOGENEOUS ATMOSPHERE WITH ALBEDO FOR SINGLE SCATTERING CURTIS, C- R- DECREASES EXPONENTIALLY WITH OPTICAL DEPTH RESPONSE OF FUNGI TO DIURNAL TEMPERATURE EXTREMES. Abb-34149 DESCRIBING SOIL. SIMULATED MARTIAN TEMPERATURE REGIME AN0 FUNGI GROWTH Ab7-21991 CHOWN. J. B. DATA REPRESENTING MONOPOLE ANTENNA VOLTAGE BREAKOWON IN SIMULATED MARS AND VENUS D ATMOSPHERES Ab7-35829 OANILOVs A. D. IONOSPHERE MOOEL TO EXPLAIN SPECTRUM OF BRIGHTNESS CLINE, M. 6. TEMPERATURES FOUND IN RADIO EMISSION FROM VENUS LEAF-KILL OF BLADES AN0 PINE NEEDLES BY SIMULATED ATMOSPHERE Nb7-16804 MARS, EARTH, AN0 VENUS SOLAR RADIATION A6b-81851 DAVIOSONs G- T. VOLCANIC AN0 TECTONIC ACTIVITY ON VENUS INFERRED a COHEN, N. 8. FROM HIGH SURFACE TEMPERATURE, CONSIDERING PROGRESS AND PROBLEMS IN ATMOSPHERIC ENTRY FOR POSSIBLE EFFECT ON ATMOSPHERE OBSCURATION MANNED AN0 UNMANNED PLANETARY PROBES - REENTRY Ab7-33232 PHYSICS NASA-TM-X-56855 Nb6-29405 DAVIES. M. E. PLANETARY CONTAMINATION BY VIABLE TERRESTRIAL CONNES, J. MICROORGANISMS TRANSPORTED ON SPACECRAFT NEW ABSORPTION BANDS IN NEAR IR SPECTRUM OF MARS AD-648864 Nb7-27042 FOUND BY FOURIER SPECTROSCOPY VIA CARBON DIOXIDE ABSORPTION MEASUREMENTS Abb-40486 OAVIES, R. W. INSTRUMENTS FOR MEASURING ALTITUDE DEPENDENT DETECTING PLANETARY LIFE FROM EARTH PHYSICAL PROPERTIES OF VENUS ATMOSPHERE FROM Ab7-24063 ENTRY CAPSULE Nb7-15764

VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON DAVIS, Re H. INTERFEROMETER. FINDING H CL LINES CONSISTENT AERODYNAMIC, THERMODYNAMIC AN0 STRUCTURAL DESIGN WITH 2-MM AMAGAT OF GAS ASPECTS OF FLIGHT CAPSULE ENTERING LOW DENSITY J PL-TR-32-1106 Ab7-24510 MARS ATMOSPHERE FROM ORBIT Ab7-11432

CONNES, Pa DAYHDFF. n. o. NEW ABSORPTION BANDS IN NEAR IR SPECTRUM OF MARS JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM FOUND BY FOURIER SPECTROSCOPY VIA CARBON DIOXIDE CORONA DISCHARGE. PRODUCING SIMPLE ORGANIC ABSORPTION MEASUREMENTS Abb-40486 MOLECULES A67-19057

DETECTING PLANETARY LIFE FROM EARTH THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS Ab7-24063 ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION DEDUCED SPECTROSCOPICALLY Ab7-20022 VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON INTERFEROMETER, FINDING H CL LINES CONSISTENT THERMOOYNAMIC EQUILIBRIUM COMPOSITION OF ALL WITH 2-MM AMAGAT OF GAS COMBINATIONS OF C, H, 0 AN0 N AT AVERAGE JPL-TR-32-1106 Ab7-24510 PRESSURE AN0 TEMPERATURE CALCULATED FOR ATMOSPHERES OF EARTH, VENUS, MARS AN0 JUPITER CONRATH, 6. J. Ab7-22236 p INVERSE PROBLEM OF RADIATIVE TRANSFER AS APPLIED TO REMOTE MEASUREMENTS OF INFRARED RADIATION EVOLUTION OF ATMOSPHERIC COMPONENTS OF VENUS FROM PLANETARY ATMOSPHERES Ab7-80916 NASA-TM-X-55857 N67-32849 THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES COOGAN, J. M. AN0 IN ORIGIN OF ORGANIC MATTER - OETERMINATION -. PLANETARY ATMOSPHERIC ABSORPTION SPECTROSCOPY OF AMINO ACID PAIRING AND SEQUENCES IN PROTEINS EMPLOYING SPLIT-TRAJECTORY DUAL FLYBY MODE NASA-CR-74559 N6b-28800 AIAA PAPER 67-121 Ab7-18311 CALCULATION OF THERMOOYNAMIC EQUILIBRIUM COMPOSITION OF EARTH, VENUS, MARS AN0

1-43 DE ROTTONI, 6. PERSONAL AUTHOR INDEX

JUPITER ATMOSPHERES Nbb-28801 OONAHOE, F. J. ABUNDANCE OF EARTH-LIKE PLANET-CONSIDERATIONS OF THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS EARTH AN0 VENUS ATMOSPHERES Abb-81966 ON CARBON, HYDROGEN, OXYGEN, AN0 NITROGEN IN EARTH, VENUS. MARS, AN0 JUPITER ATMOSPHERES DDNAHUE, T. n. a Nbb-31642 MARS UPPER ATMOSPHERE AN0 SINGLE-LAYER IONOSPHERE UV PHOTOIONIZATIONI TEMPERATURE PROFILE AN0 THERMODYNAMIC EQUILIBRIUM IN PREBIOLOGICAL CHEMICAL COMPOSITION Abb-29417 ATMOSPHERES, AN0 INORGANIC ORIGIN OF ORGANIC

COMPOUNDS MARTIAN ATMOSPHERE MOOEL OEOUCEO FROM MARINER IV ~ NASA-SP-3040 N67-27295 IONOSPHERE ELECTRON DENSITY MEASUREMENTS NASA-CR-84825 Nbl-28785 DE HOTTDNI, 6- VISIBLE BRIGHTNESS FEATURES IN MARINER IV DRAKE. F. D. PHOTOGRAPHS OF MARS INTERPRETEO AS CLOUDS NONTHERMAL RADIO EMISSION FROM ELECTRIC DISCHARGES Abl-34149 WITHIN VENUS WATER CLOUDS Abl-31480

DEIRWENDJIAN. D. MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS MANNED GEOPHYSICAL OBSERVATIONS FROM SATELLITES AS ATMOSPHERE Nbb-3 1411 TRAINING GROUND FOR PLANETARY RESEARCH, ESPECIALLY VENUS ATMOSPHERE Abl-11395 MARINER IV RADIO OCCULTATION MEASUREMENTS OF MARS UPPER ATMOSPHERE Nbb-31478 PROBLEMS IN DETECTING ICE AN0 WATER CLOUDS ON VENUS N 66-3 1464 FREQUENCY, PHASE, AN0 AMPLITUDE CHANGES OF MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AN0 TERRESTRIAL OBSERVATIONS FROM MANNED GEOPHYSICAL IONOSPHERE OF MARS OBSERVE0 BEFORE AN0 AFTER SATELLITE APPLIED TO PLANETARY ATMOSPHERIC PLANETARY OCCULATATION Nb7-12754 PHENOMENA - VENUS PROBES P-3418 Nbb-39579 DRESSLER. K- MOLECULAR HYDROGEN STRUCTURE, CONSIDERING ESTIMATES AN0 DEFINITIONS ON CHARACTERISTICS OF PLANETARY AN0 STELLAR ATMOSPHERES AN0 INTERSTELLAR VENUS LOWER ATMOSPHERE SPACE Abb-39487 P-3513 Nb7-22577 DRYER. M. DEIWERT, 6. S. MAGNETOSPHERIC BOUNDARY AN0 STANDING SHOCK WAVE HEATING RATES IN GAS MIXTURES OF PLANETARY FOR EARTH SCALE0 DOWN TO APPLY TO MARS ATMOSPHERES PREDICTED BY EQUATION USING TRANSPORT Ab7-35442 PROPERTIES OF GASES AT LOWER TEMPERATURES A 66-21 432 E DEMARCUS, W- C. ECK, R. V. JUPITER AN0 SATURN MODELS, GIVING PLANET JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM CONSTITUTION, HEAT BALANCE AN0 ATMOSPHERIC CORONA OISCHARGEI PRODUCING SIMPLE ORGANIC COMPOSITION Abl-39001 MOLECULES Ab7-19051

DIKII, L. A- THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS .* NUMERICAL CALCULATION OF PERIODS OF NATURAL ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION OSCILLATIONS AN0 CORRESPONDING EIGENFUNCTIONS OF DEDUCE0 SPECTROSCOPICALLY Ab7-20022 PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS ROTATIONAL SPEED Abb-27534 THERMODYNAMIC EQUILIBRIUM COMPOSITION OF ALL COMBINATIONS OF Cr HI 0 AN0 N AT AVERAGE NUMERICAL CALCULATION OF PERIODS OF NATURAL PRESSURE AN0 TEMPERATURE CALCULATED FOR OSCILLATIONS AN0 CORRESPONOING EIGENFUNCTIONS OF ATMOSPHERES OF EARTH, VENUS, MARS AN0 JUPITER PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS Abl-22236 ROTATIONAL SPEED Abb-42320 EVOLUTION OF ATMOSPHERIC COMPONENTS OF VENUS DOLE, S. H- Ab7-80916 PLANETARY ATMOSPHERES AND POSSIBILITY OF LIFE IN SOLAR SYSTEM THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES P-3669 Nb7-39518 AN0 IN ORIGIN OF ORGANIC MATTER - DETERMINATION OF AMINO ACID PAIRING AND SEQUENCES IN PROTEINS DOLEZALEK, H. NASA-CR-74559 Nb6-28800 GEROIEN TYPE CHAMBER FOR MEASUREMENTS OF ION MOBILITY SPECTRUM IN TERRESTRIAL MESOSPHERE AN0 CALCULATION OF THERMODYNAMIC EQUILIBRIUM MARS ATMOSPHERE Abb-34712 COMPOSITION OF EARTH, VENUS, MARS AN0 JUPITER ATMOSPHERES Nb6-26 8 0 1 DOLLFUS, A- LIGHT DIFFUSION OF MARTIAN ATMOSPHERE MEASURE0 BY THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS SPECTROSCOPIC EVALUATION OF POLARIZATION VARIATION ON CARBON, HYDROGEN, OXYGEN, AN0 NITROGEN IN FROM DISK CENTER TO EDGE Abb-25461 EARTH, VENUS, MARS, AND JUPITER ATMOSPHERES Nbb-31642 SPECTRAL VARIATION IN LIGHT POLARIZATION OF MARTIAN ATMOSPHERE FOR ALL OBSERVABLE PHASE THERMODYNAMIC EQUILIBRIUM IN PREBIOLOGICAL ANGLES Abb-29643 ATMOSPHERES, AN0 INORGANIC ORIGIN OF ORGANIC COMPOUNDS WATER CONTENT OF VENUS ATMOSPHERE, AEROSOLSv AN0 NASA-SP-3040 Nbl-27295 PRESSURE IN UPPER CLOUD LAYER, AN0 DEVIATIONS IN DIRECTION OF POLARIZED LIGHT Nbb-3147 1 ECKWAN, P. K. 9 PLANETARY CONTAMINATION BY VIABLE TERRESTRIAL WATER CONTENT AN0 DIFFUSION IN MARTIAN ATMOSPHERE MICROORGANISMS TRANSPORTED ON SPACECRAFT AN0 PROPERTIES OF LIGHT AN0 DARK SIDES OF AO-648864 Nbl-27042 MARTIAN SOIL Nbb-31481 EDSE, R- POLARIMETRIC STUDY OF PLANET MARS CHEMICAL KINETICS OF CARBON DIOXIDE FOR MARTIAN es AFCRL-bb-492 Nbb-36942 ATMOSPHERIC ENTRY APPLICATIONS ARL-67-0113 Nbl-39458 ATMOSPHERIC BRIGHTNESS OF MARS DETERMINED BY POLARIMETRIC AN0 PHOTOMETRIC MEASUREMENTS E6GERS. A- J., JR. TR-34 Nbl-24229 PROGRESS AN0 PROBLEMS IN ATMOSPHERIC ENTRY FOR

1-44 PERSONAL AUTHOR INDEX GAFFNEY, E. S.

MANNED AND UNMANNED PLANETARY PROBES - REENTRY FJELDBO. 6. PHYSICS MARS ATMOSPHERE MODELS BASED ON MARINER IV NASA-TM-X-56855 Nbb-29405 OCCULTATION DERIVING ELECTRON NUMBER DENSITY, TEMPERATURE, PRESSURE, MASS DENSITY, ETC, NOTING ELLIS, T. R. CARBON DIOXIDE PRESENCE Abb-30713 SYSTEM DESIGN FOR NONSURVIVABLE MARS PROBE DEPLOYED FROM ORBITING SPACECRAFT TO PERFORM MARINER IV MODELS OF THREE MARS ATMOSPHERIC ENGINEERING EXPERIMENTS FOR ATMOSPHERIC AN0 LAYERS ANALOGOUS TO TERRESTRIAL E, F-1 AND F-2 TERRAIN PROPERTY DETERMINATION LAYERS, CONSIDERING RELATIVE MASS DENSITIESs NASA-CR-66131 Nbb-31819 TEMPERATURES, CARBON DIOXIDE PHOTODISSOCIATION AND IONIZATION PROFILE Abb-41779 ESHLEMAN. V. R. MARS ATMOSPHERE MODELS BASED ON MARINER IV RADIO OCCULTATION TECHNIQUES FOR ANALYSIS OF OCCULTATION DERIVING ELECTRON NUMBER DENSITY, PLANETARY ATMOSPHERES AND SURFACE TOPOGRAPHY BY TEMPERATURE, PRESSUREI MASS DENSITY, ETC. NOTING MEASURING PERTURBATIONS TO AMPLITUDE AND FREQUENCY CARBON DIOXIDE PRESENCE Abb-30713 ON RADIO LINKS AIAA PAPER 67-119 Ab7-18454 MARINER IV MODELS OF THREE MARS ATMOSPHERIC LAYERS ANALOGOUS TO TERRESTRIAL El F-1 AND F-2 MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS LAYERS, CONSIDERING RELATIVE MASS DENSITIES, ATMOSPHERE Nbb-31477 TEMPERATURES, CARBON DIOXIDE PHOTODISSOCIATION AND IONIZATION PROFILE A6b-41779 MARINER IV RADIO OCCULTATION MEASUREMENTS OF MARS UPPER ATMOSPHERE N6b-31478 MARTIAN ATMOSPHERIC SURFACE PRESSURE BETWEEN OCCULTATION LEVELS AT ELECTRICS AN0 MARE COMPARING ATMOSPHERE MODELS OF MARS BASED ON AC IDALIUM MARINER IV OCCULATION DATA NASA-CR-75816 Nbb-29298 NASA-CR-78134 Nbb-37214

MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS FREQUENCY, PHASE. AND AMPLITUDE CHANGES OF ATMOSPHERE Nb6-3 1477 MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AND IONOSPHERE OF MARS OBSERVED BEFORE AND AFTER MARINER IV RADIO OCCULTATION MEASUREMENTS OF PLANETARY OCCULATATION Nb7-12754 MARS UPPER ATMOSPHERE Nbb-31478 FJELDBO, W. C. COMPARING ATMOSPHERE MODELS OF MARS BASED ON NARS ATMOSPHERE MODELS BASED ON MARINER IV MARINER IV OCCULATION DATA OCCULTATION DERIVING ELECTRON NUMBER DENSITY, NASA-CR-78134 Nbb-37214 TEMPERATURE, PRESSURE, MASS DENSITY, ETCI NOTING CARBON DIOXIDE PRESENCE 166-30713 FREQUENCY, PHASE, AND AMPLITUDE CHANGES OF MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AND MARINER IV MODELS OF THREE MARS ATMOSPHERIC IONOSPHERE OF MARS OBSERVED BEFORE AND AFTER LAYERS ANALOGOUS TO TERRESTRIAL El F-1 AN0 F-2 PLANETARY DCCULATATIDN Nb7-12754 LAYERS. CONSIDERING RELATIVE MASS DENSITIES, TEMPERATURES, CARBON DIOXIDE PHOTOOISSOCIATION AND EVANS. J. V. IONIZATION PROFILE Abb-41779 RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW VALUE OF CROSS SECTION, ECHO SPECTRUM. COMPARING ATMOSPHERE MODELS OF MARS BASED ON POLARIZATION CHARACTERISTICS, ABSORPTION CROSS MARINER IV OCCULATIDN DATA SECTION AND ATMOSPHERIC ATTENUATION NASA-CR-78134 Nbb-37214 Ab7-16298 FOCAS. J. SPECTRAL VARIATION IN LIGHT POLARIZATION OF F MARTIAN ATMOSPHERE FOR ALL OBSERVABLE PHASE FASTIES W. G. ANGLES Abb-29643 OPTICAL AN0 ELECTRONIC COMPONENTS FOR ULTRAVIOLET ROCKET SPECTROPHOTOMETRY IN PLANETARY ATMOSPHERE FOCAS. J. H. NASA-CR-78485 Nbb-38722 MARTIAN ATMOSPHERE TRANSPARENCY AN0 VISIBILITY OF SURFACE DETAILS IN BLUE AN0 UV LIGHT, SHOWING OPTICAL INSTRUMENTS FOR ULTRAVIOLET MEASUREMENTS DARK AND SEMITDNE AREAS INTENSITY, ETC IN PLANETARY ATMOSPHERES Nb7-17793 Ab7-34154

FELLGETTI P. POLARIMETRIC STUDY OF PLANET MARS DETECTING PLANETARY LIFE FROM EARTH AFCRL-66-492 Nbb-36942 Ab7-24063 FOSTER, R. M. FELLOWS, R. F. MODEL OF NONEQUILIBRIUM PROPERTIES OF HIGH ATMOSPHERIC DATA FOR EARTH. MARS, AN0 VENUS TEMPERATURE CARBON DIOXIDE AND OTHER GAS MIXTURES Nb7-19026 IN CONNECTION WITH STUDIES FOR VEHICLES ENTERING MARTIAN ATMOSPHERE Ab7-11436 FIELD, 6. B. MOLECULAR HYDROGEN STRUCTURE, CONSIDERING FRASER, R. S. PLANETARY AND STELLAR ATMOSPHERES AND INTERSTELLAR COMPUTED EFFECTS OF SPECULAR REFLECTION ON SPACE Abb-39487 SCATTERING OF LIGHT BY RAYLEIGH PLANETARY ATMOSPHERE FISH, F. F. NASA-CR-7b122 Nbb-30187 MARTIAN AN0 CYTHEREAN ATMOSPHERIC COMPOSITION DETERMINATIONS USING ENTRY PROBE MEASUREMENTS OF FRENKELt L. ULTRAVIOLET AN0 X-RAY ATTENUATION DIELECTRIC RELAXATION OF GASES AND SHARP RISE IN OAC-60627 N67-33758 MICROWAVE ABSORPTION COEFFICIENT IN CYTHEREAN F' F' ATMOSPHERE Ab7-21372 FISH, F. F., JR. DUST DEVILS IN RELATION TO MARTIAN YELLOW CLOUDS PLANETARY ATMOSPHERIC COMPOSITION STUDY UNDER NASA-CR-89578 Nb7-40004 AMBIENT CONDITIONS USING INSTRUMENT INVOLVING VERY HIGH P FABRY- PEROT MICROWAVE CAVITIES FISHBURNE, E- S. 167-25986 CHEMICAL KINETICS OF CARBON DIOXIDE FOR MARTIAN ATMOSPHERIC ENTRY APPLICATIONS ARL-67-0113 Nb7-39458 G GAFFNEY, E. S. FROST PHENOMENA ON MARS EXAMINE0 ON BASIS OF

1-45 GEORGIEV. Sa PERSONAL AUTHOR INDEX

MARTIAN WAVE OF DARKENING, NOTING NECESSITY OF VENUS COMPARED WITH SEVERAL MODEL ATMOSPHERES DELIQUESCENT SALTS TO ATTRACT AND RETAIN WATER ON Ab7-24601 SURFACE Ab7-18645 GRIGOREVA. 2- N- GEORGIEV, S. PHOTOMETRIC OBSERVATION DATA ON JUPITER DESIGN AND FEASIBILITY STUDIES OF MARS ATMOSPHERE ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- PROBE VEHICLE Abb-25292 MONTH PERIODIC CHANGE Ab7-39299 ' MARS PROBE DESIGN AND SUBSYSTEM PERFORMANCE GROSS. F- R. CHARACTERISTICS FOR INVESTIGATING MARTIAN VENUS PROBE DESIGN OF EXPANDABLE BALLOON-TYPE ATMOSPHERE INSTRUMENT PACKAGE CAPABLE OF ENTRY INTO AND OF NASA-CR-530 Nb7-32719 STATIC EQUILIBRIUM WITHIN KAPLAN ATMOSPHERE UI Ab6-27887 GIRAGOSIANs P- A. MARS ATMOSPHERE ENTRY PROBE CONFIGURATION, GROSS. S- H. AERODYNAMIC CHARACTERISTICS, FLOW FIELD. MERCURY ATMOSPHERIC TEMPERATURE, COMPOSITION AND STABILITY AUGMENTATION, INSTRUMENTATION, SURFACE PRESSURE AND EFFECT OF NONSYNCHRONOUS THERMAL SHIELDING* DATA HANDLING AN0 ROTATION Abb-40424 COMMUNI CATIONS Ab7-11424 ATMOSPHERE OF MERCURY AERODYNAMIC, THERMODYNAMIC. HEAT SHIELD AND NASA-TM-X-57322 Nb7-18273 STRUCTURAL DESIGN ASPECTS OF BALLISTIC VEHICLE ENTERING PLANETARY ATMOSPHERE Ab7-35315 THERMAL STRUCTURE OF UPPER MARS ATMOSPHERE NASA-TM-X-57327 Nb7-18652 SPHERICAL ENTRY VEHICLE USED TO DEFINE PLANETARY ATMOSPHERE STRUCTURE AND COMPOSITION FROM DYNAMIC FEASIBILITY OF USING RADIO SOUNDING TECHNIQUES TO RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC INVESTIGATE IONOSPHERIC PROPERTIES OF PLANETS CHARACTERISTICS Ab7-40177 NASA-CR-689 Nb7-28368

GIVER, L. P. GRUSZCZYNSKI. J- 5. CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K HIGH-TEMPERATURE GAS RADIANCE IN SIMULATED DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS PLANETARY ATMOSPHERE AT VARIOUS ENTRY VELOCITIES OF MARS Ab7-14309 AIAA PAPER 66-183 166-25169

HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR EQUILIBRIUM RADIATION IN AIR AN0 GAS MIXTURES WATER VAPOR PRESENCE, RESULTS INOICATE AMOUNT ASSUMED TO REPRESENT NEAR PLANET ATMOSPHERES DEPENDS ON SIZE OF POLAR CAP NASA-CR-81315 Nb7-16722 JPL-TR-32-1048 Ab7-22235 GUERIN. P. GLEDHILL. J. A- RETROGRADE ROTATION OF CLOUD FORMATIONS OF VENUS MAGNETOSPHERIC MODEL OF JUPITER FROM NUMERICAL WITH ANGULAR VELOCITY CORRESPONDING TO ONE CALCULATION OF MAXIMUM NUMBER DENSITY OF PLASMA ROTATION IN FOUR DAYS ANALYZED BY HIGH RESOLUTION Ab7-25206 PHOTOGRAPHY 166-41 181

GOLITSYN, G. S. NUMERICAL CALCULATION OF PERIODS OF NATURAL H OSCILLATIONS AND CORRESPONDING EIGENFUNCTIONS OF HAGEN. C. A. a PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS SIMULATED MARTIAN ATMOSPHERIC AND ECOLOGICAL ROTATIONAL SPEED Abb-27534 EFFECTS ON BACILLUS CEREUS SPORE GERMINATION NASA-CR-74969 Nbb-26263 NUMERICAL CALCULATION OF PERIODS OF NATURAL OSCILLATIONS AND CORRESPONDING EIGENFUNCTIONS OF HALL. L- Be PLANETARY ATMOSPHERES AS FUNCTION OF PLANETS PLANETARY QUARANTINE CONSTRAINTS* NOTING ROTATIONAL SPEED Abb-42320 PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION A6b-29966 GODDYI Re RADIATIVE RELAXATION TIMES FOR TEMPERATURE PLANETARY QUARANTINE CONSTRAINTS. NOTING PERTURBATIONS IN CO 2 WITH SMALL WATER VAPOR PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION ADMIXTURE UNDER CONDITIONS SIMILAR TO MARTIAN Ab7-29098 ATMOSPHERE, DISCUSSING DYNAMICAL PHENOMENA Ab7-33187 HANEL. Re A. GASEOUS COMPOSITION OF UNKNOWN PLANETARY GOOOY, R- M- ATMOSPHERE DETERMINED, USING ACOUSTIC EXPERIMENT DEEP CIRCULATION IN VENUSIAN ATMOSPHERE MODEL COMBINED WITH PRESSURE AND TEMPERATURE DATA OPAQUE TO SOLAR AND PLANETARY RADIATION BUT WITH Ab7-13215 DIFFERENTIAL HEATING Ab7-14310 HANSEN. F- V- GRAY. L- 0. SPATIAL AN0 TEMPORAL DISTRIBUTION OF GRADIENT RANDOM ELSASSER BAND MODEL TO COMPUTE ATMOSPHERIC RICHARDSON NUMBER IN SURFACE AND PLANETARY TRANSMISSION OF EARTH AND MARS FOR 2-MICRON BOUNDARY LAYERS CARBON DIOXIDE BANDS ECOM-5123 Nb7-35919 JPL-TR-32-969 Abb-38024 HARTECK. P- UPPER LIMIT OF CARBON DIOXIDE ABUNDANCE IN RADIATION EQUILIBRfA IN UV LIGHT ON AIR, OXYGEN, MERCURY ATMOSPHERE Ab7-41836 CARBON DIOXIDE, ETC. ANALYZED BY BROMINE LAMP IN CONNECTION WITH STUDIES OF PLANETARY ATMOSPHERES GREENSPAN, J. A- ~br-14aa~ STRUCTURE AND COMPOSITION OF JUPITER ATMOSPHERE, NOTING LABORATORY AND OBSERVATIONAL DATA INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS *( SUPPORTING HYPOTHESIS OF CONSISTENCY WITH SOLAR THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS ELEMENTS ABUNDANCE Ab?-30932 HAVE BEEN OBSERVED IN X-BAND FROM GLOW DISCHARGES Ab7-14952 GRIFFIN, C- E. INSTRUMENTS FOR MEASURING ALTITUDE DEPENDENT HASSELTINE. C. L- PHYSICAL PQOPERTIES OF VENUS ATMOSPHERE FROM JUPITER ENVIRONMENT, EFFECTS OF HUGE MASS, HIGH ENTRY CAPSULE Nb7-15764 ROTATION RATE. TEMPERATURE AND DOMINANT H AND HE ATMOSPHERE Ab7-40141 GRIFFITHI P- H. MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF DERIVATION OF ATMOSPHERIC PARAMETERS FOR

1-46 PERSONAL AUTHOR INDEX JOHNSON. Fa S.

GREENHOUSE MODEL OF VENUS ATMOSPHERE FREQUENCY BEAT OCCULTATION TECHNIQUE USED BY NASA-TM-X-53497 Nb7-29983 MARINER IV SPACE PROBE Nb7-12665

HECKMAN, G. R. HULL. J. A. MAGNETOSPHERIC BOUNDARY AND STANDING SHOCK WAVE OPTICAL RADIOMETER FEASIBILITY STUDY FOR FOR EARTH SCALED DOWN TO APPLY TO MARS DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM Ab7-35442 SHOCK LAYER RADIATION DURING ENTRY - INSTRUMENTATION HEDLAND. R. C. NASA-CR-73027 Nbb-35663 PLANETARY ATMOSPHERE STRUCTURE DETERMINED FROM rn ENTRY VEHICLE ONBOARO MEASUREMENTS OF PRESSURE, HUNTEN. D. n. TEMPERATURE* AND ACCELERATION ABUNOANCE AND TEMPERATURE OF CARBON DIOXIDE IN NASA-TN-D-3933 Nb7-23302 MARTIAN ATMOSPHERE. NOTING IMPLICATIONS. c OBSERVATION METHODS AND RESULTS HELLWELL, T. n. Abb-39558 MOLECULAR, CONTINUUM AN0 LINE RADIATION OF PLANETARY ATMOSPHERES, COMPARING MOLECULAR BAND WATER VAPOR LINES IN SPECTRUM OF VENUS OBTAINED STRUCTURE MODELS WITH SPECTRAL MEASUREMENTS OF CN BY PHOTOELECTRIC SCANNING OF SPECTRUM VIOLET BAND Ab7- 11769 AIAA PAPER 67-323 Ab7-26038 SPECTROSCOPIC MEASUREMENT OF CARBON DIOXIDE IN HEYDEN. F. J. MARS ATMOSPHERE FOR SURFACE PRESSURE AND SPECTROSCOPIC STUDY OF SOLAR AN0 PLANETARY ATMOSPHERIC COMPOSITION Nbb-31473 ATMOSPHERES - OBSERVATIONS OF VENUS AN0 JUPITER, AND ANALYSIS OF SIMULATED MARTIAN ATMOSPHERE HURWICZI H. IN VISIBLE AN0 INFRARED REGIONS AERODYNAMIC. THERMODYNAMIC AND STRUCTURAL DESIGN NASA-CR-75488 Nbb-27755 ASPECTS OF FLIGHT CAPSULE ENTERING LOW DENSITY MARS ATMOSPHERE FROM ORBIT Ab7-11432 HIDE. R- EXPERIMENTAL ANALYSIS OF TAYLOR COLUMNS LIKELY TO BEAR ON PROCESSES OCCURRING IN JUPITER ATMOSPHERE I Abb-33013 IBBETSONs A- EXPERIMENTAL ANALYSIS OF TAYLOR COLUMNS LIKELY TO PLANETARY SCALE ATMOSPHERIC CIRCULATIONS OF BEAR ON PROCESSES OCCURRING IN JUPITER ATMOSPHERE JUPITER AND SATURN USING FLUID DYNAMICS. NOTING Abb-33013 ROTATION EFFECTS Abb-41679 TAYLOR COLUMNS OCCURRENCE CRITERION IN JUPITER TAYLOR COLUMNS OCCURRENCE CRITERION IN JUPITER ATMOSPHERE INVESTIGATED EXPERIMENTALLYI GIVING ATMOSPHERE INVESTIGATED EXPERIMENTALLY. GIVING FLOW PATTERNS 867-38999 PI FLOW PATTERNS Ab7-38999 INGALLS, R. P- HIPSHER. H- RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW ATMOSPHERIC DATA FOR EARTH, MARS, AND VENUS VALUE OF CROSS SECTION* ECHO SPECTRUM, Nb7-19026 POLARIZATION CHARACTERISTICS, ABSORPTION CROSS SECTION AND ATMOSPHERIC ATTENUATION *I HITCHCOCK. D. R- Ab7-16298 DETECTING PLANETARY LIFE FROM EARTH Ab7-24063 ISRAEL. G. VENUS BRIGHTNESS TEMPERATURE AND ATMOSPHERE AND EXTRATERRESTRIAL LIFE DETECTION STUDIED FROM MARS ATMOSPHERE SOUNDED BY MARINER I1 SPACE KNOWLEDGE OF MAJOR AND TRACE COMPONENTS OF PROBE. NOTING DATA ON MARS MAGNETIC FIELD ATMOSPHERES Ab7-40999 Ab7-28964

STATISTICAL DECISION THEORY APPLIED TO MARTIAN ATMOSPHERE ANALYSIS. LIFE DETECTION EXPERIMENTS, J AN0 GAS CHROMATOGRAM MEASUREMENTS OF N-ALKANE JAMES. J- DISTRIBUTIONS IN MATERIALS MARINER SPACE VEHICLES DESIGN EVOLUTION NOTING NASA-CR-77234 Nbb-34667 CONTRIBUTION TO FUTURE SPACE FLIGHTS THROUGH MEASUREMENT OF ATMOSPHERIC OENSITY OF MARS Hot W. Ab7-42399 INDUCE0 ABSORPTION COEFFICIENTS IN ATMOSPHERE MODEL MEASURED FOR CALCULATION OF VENUS LOWER JASTROWs R. ATMOSPHERE PROPERTIES FROM RADIO OBSERVATIONS VENUS ATMOSPHERE, SURFACE TEMPERATURE AND Ab7-12949 RADIATION CHARACTERISTICS Abb-35799

HOLMAN. F. S. COMPARISON OF SURFACE AN0 ATMOSPHERIC SPHERICAL SEMIPASSIVE PROBE FOR DENSITY/ATTITUOE CHARACTERISTICS OF EARTH AN0 VENUS AN0 PRESSURE/ALTITUOE PROFILE OF PLANETARY NASA-TM-X-57351 Nb7-1843 5 ATMOSPHERES, NOTABLY MARS AN0 VENUS Abb-30889 JEFFRIES. A- J. ASHEN LIGHT AN0 MAGNETIC FIELD OF VENUS HOOP, H, H. 667-33096 BIBLIOGRAPHY AND AUTHOR ON MERCURY SURFACE, ATMOSPHERE, ROTATION. TEMPERATURE, AND TERRAIN JIJI. L. n. NASA-CR-84113 Nb7-26454 TRANSIENT TEMPERATURE RESPONSE OF T'RANSPIRATION- COOLED POROUS MATRIX ENTERING PLANETARY ATMOSPHERE HOROWITZS R. WITH CONSTANT VELOCITY AN0 NEGATIVE ENTRY ANGLE ATMOSPHERIC OATA FOR EARTH, MARS, AN0 VENUS Abb-39455 PL Nb7-19026 JOHNSON. Fa S. HOSHIZAKI. H. MARS ATMOSPHERE SURFACE PRESSURE. RADIATIVE CONVECTIVE AND RADIATIVE HEAT TRANSFER TO EQUILIBRIUM TEMPERATURESI SUNLIGHT RESONANCE SPACE VEHICLES ENTERING PLANETARY ATMOSPHERES SCATTERING DISTRIBUTION^ ETC Ab7-34152 AT SUPERORBITAL VELOCITIES * NASA-CR-584 Nbb-37027 EFFECTS OF MARINER IV IONOSPHERIC DATA ON MARS ATMOSPHERE COMPOSITION PREDICTIONS HOUMINERt Z- NASA-CR-7bbbb Nbb-32302 MARTIAN ATMOSPHERE AND IONOSPHERE ELECTRON DENSITY AND REFRACTIVITY PROFILES DETERMINED BY TWO

1-41 KAGIWADA. Ha H- PERSONAL AUTHOR INDEX

PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE, TRACKING, COST AND SCHEDULE K AIAA PAPER 65-219 A66-27874 KAGIWADA. Ha H, INITIAL VALUE APPROACH TO CHANORASEKHAR PLANETARY KLIORE. AI r* PROBLEM TO ESTIMATE PLANETARY PROPERTIES AN0 MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY ATMOSPHERIC COVERS MEASURING EFFECT ON RADIO OCCULTATION OF PLANET. RM-4991-PR N66-29959 DETERMINING SHAPE. ATMOSPHERE DENSITY PROFILE, DIURNAL VARIATIONS. ETC A66-25235 THEORY AN0 NUMERICAL PROCEDURE FOR DIGITAL COMPUTER APPLICATION OF GREENHOUSE EFFECT FOR RADIO OCCULTATION MEASUREMENT OF MARTIAN x PLANETARY ATMOSPHERE OF FINITE DEPTH ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE RM-5076-PR N67-22562 PROBE 666-29958

INVARIANT IMBEDDING EQUATIONS FOR DETERMINING MARINER VENUS 1967 SPACE PROBE. OBTAINING VERTICAL STRATIFICATION OF TERRESTRIAL AN0 ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX PLANETARY ATMOSPHERES ON BASIS OF SATELLITE FROM RADIO SIGNAL FREQUENCY, INTENSITY AN0 PHASE OBSERVATIONS CHANGES RM-5229-PR ~67-32463 AIAA PAPER 67-118 A67-18310

KAHLE. A- B- MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY CALCULATION OF TOTAL RADIATION EMERGING FROM MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, PLANETARY ATMOSPHERES OPTICALLY THICKER THAN DETERMINING SHAPE, ATMOSPHERE DENSITY PROFILE. THOSE OF EARTH DIURNAL VARIATIONS, ETC RM-5343-PR N67-32966 JPL-TR-32-1157 A67-26819

KALABAs R. E. RADIO OCCULTATION MEASUREMENT OF MARTIAN INITIAL VALUE APPROACH TO CHANORASEKHAR PLANETARY ATMOSPHERE OVER TWO REGIONS BY MARINER IV PROBLEM TO ESTIMATE PLANETARY PROPERTIES AN0 SPACE PROBE 167-34151 ATMOSPHERIC COVERS RM-4991-PR N66-29959 MARINER VENUS 1967 SPACE PROBE, OBTAINING ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX THEORY AN0 NUMERICAL PROCEDURE FOR DIGITAL FROM RADIO SIGNAL FREQUENCY. INTENSITY AN0 PHASE COMPUTER APPLICATION OF GREENHOUSE EFFECT FOR CHANGES PLANETARY ATMOSPHERE OF FINITE DEPTH AIAA PAPER 67-118 A67-40094 RM-5076-PR N67-22562 MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS INVARIANT IMBEDDING EQUATIONS FOR DETERMINING ATMOSPHERE ~66-31477 VERTICAL STRATIFICATION OF TERRESTRIAL AN0 PLANETARY ATMOSPHERES ON BASIS OF SATELLITE MARINER IV RADIO OCCULTATION MEASUREMENTS OF OBSERVATIONS MARS UPPER ATMOSPHERE N66-31478 * RM-5229-PR N67-32463 FREQUENCY, PHASE. AN0 AMPLITUDE CHANGES OF KANEVSKII, Ma 8. MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AND VENUS RADIATION SPECTRUM IN MM RANGE FROM VENUS IONOSPHERE OF MARS OBSERVED BEFORE AN0 AFTER ATMOSPHERE MODELS A67-40120 PLANETARY OCCULATATION N67-12754. * KAPLAN. L. 0. NEW ABSORPTION BANDS IN NEAR IR SPECTRUM OF MARS KOKOTTw W. FOUND BY FOURIER SPECTROSCOPY VIA CARBON DIOXIDE PLANET JUPITER RESEARCH, NOTING UNRESOLVED ABSORPTION MEASUREMENTS A66-40486 QUESTIONS DF COSMOLOGYt INTERIOR STRUCTURE AN0 GREAT REO SPOT ~6r-39092 DETECTING PLANETARY LIFE FROM EARTH ~67-24063 KOLOSOV. M. A- POLARIZATION STUDIES OF RADIO EMISSION FROM UPPER VENUS ATMOSPHERE SPECTRA OBTAINED BY MICHELSON LAYER AN0 SURFACE COVERING OF PLANETS INTERFEROMETER. FINDING H CL LINES CONSISTENT N67-16817 WITH 2-MM AMAGAT OF GAS JPL-TR-32-1106 A67-24510 KOMABAYASI. M. MECHANISM REGULATING TOTAL AMOUNT OF EARTH AN0 KAT29 G- D- MARS ATMOSPHERE TRANSPARENT TO VISIBLE AN0 IR SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST RAD1AT1 ON 667-18052 PROGRAM SHOWING REQUIREMENTS FOR LAUNCH VEHICLE. TRACKING, COST AN0 SCHEDULE DISCRETE EQUILIBRIUM TEMPERATURES OF HYPOTHETICAL AIAA PAPER 65-219 AM-27874 PLANET WITH ATMOSPHERE AN0 HYDROSPHERE OF ONE- COMPONENT TWO-PHASE SYSTEM UNDER CONSTANT SOLAR KATZ, 1- RAD1AT1 ON A67-27462 STRUCTURES OF TERRESTRIAL AN0 EXTRATERRESTRIAL ATMOSPHERES A67-18997 KOVALs 11 K. SPECTROPHOTOMETRY AN0 POLARIMETRY OF LUNAR KAUFMAN. I. A- REGIONS. OPTICAL PROPERTIES OF ATMOSPHERE AND INDUCED ABSORPTION COEFFICIENTS IN ATMOSPHERE SURFACE OF MARS. AN0 COMETARY TAILS MODEL MEASURE0 FOR CALCULATION OF VENUS LOWER NASA-TT-F-382 N66-33526 ATMOSPHERE PROPERTIES FROM RADIO OBSERVATIONS ~67-12949 OPTICAL PROPERTIES OF ATMOSPHERE AN0 SURFACE OF MARS N66-33530 KENNET. ti. EARTH REENTRY SIMULATION OF PLANETARY ENTRY SPECTROSCOPIC AND PHOTOMETRIC ANALYSIS OF VENUS ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF MARS AN0 MARS ATMOSPHERES TO DETERMINE LUMINESCENCE f AN0 VENUS TYPE AND OTHER PROPERTIES AIAA PAPER 65-218 A66-27875 NASA-TT-F-394 N67-16801

SPHERICAL SEMIPASSIVE PROBE FOR DENSITYlATTITUDE CURVES OF MONOCHROMATIC ALBEDO FOR LIMB AND

AN0 PRESSURE/ALTITUOE PROFILE OF PLANETARY TERMINATOR OF VENUS N67-16806 ~~ ATMOSPHERE$. NOTABLY MARS AN0 VENUS A66-30889 KOZYREV. N. A- LUMINESCENCE FROM LOWER ATMOSPHERIC LAYERS AN0 KERN. RI J. IONOSPHERE OBSERVED IN VENUS NIGHT AIRGLOW SIMULATED MARTIAN ENTRY CONDITIONS IN EARTH TEST N67-16803

1-40 .- PERSONAL AUTHOR INDEX LIPPINCOTTt E- R.

KRAFTq 6. LEOVY. C. FEASIBILITY OF USING RADIO SOUNOING TECHNIQUES TO ESTIMATES OF VERTICAL TEMPERATURE STRUCTURE. HEAT INVESTIGATE IONOSPHERIC PROPERTIES OF PLANETS BALANCE. SOLSTICE CIRCULATION. AN0 THERMALLY NASA-CR-bE9 Nb7-28368 DRIVEN TIDES ON MARS IN COMPARISON WITH LIKE CONDITIONS ON EARTH ?D KRUGERq Sa T. NASA-CR-8b912 Nb7-32494 MARTIAN SURFACE AND ATMOSPHERIC PARAMETER MEASUREMENTS BY MEANS OF GAMMA RAY SPECTROMETRIC LEOVY. c. 8. INSTRUMENTATION ABOARD VOYAGER MISSION RADIATIVE-CONVECTIVE EQUILIBRIUM CALCULATIONS FOR Nbl-12667 TWO-LAYER MARTIAN ATMOSPHERE NASA-CR-15633 Nbb-29732 KUNDEl V, 6. I EM 7094 COMPUTER PROGRAM FOR THEORETICAL NUMERICAL MODEL FOR SIMULATING GENERAL CIRCULATION CALCULATION OF OUTGOING INFRARED RADIANCES FROM OF ATMOSPHERE OF MARS ATMOSPHERES OF EARTH AN0 MARS AS AI0 IN NASA-CR-81146 N67-15280 SATELLITE MEASUREMENT INTERPRETATIONS NASA-TN-0-4045 N67-32936 LEVANON. N. SURFACE AN0 ATMOSPHERIC PARAMETER MEASUREMENTS BY KURSKAYA. A. A- USE OF POLARIZATION INSTRUMENTATION ABOARD POLARIZATION STUDIES OF RADIO EMISSION FROM UPPER MARINER ORBITER SPACE PROBE N67-12666 LAYER AN0 SURFACE COVERING OF PLANETS Nb7-16617 LEVINTHALI E. C. DECISION THEORY BIOLOGICAL SEARCH STRATEGIES AN0 KUTUZA. B. 6- PLANETARY QUARANTINE ASPECTS OF MARS SUPERCOOLED WATER DROPLETS HYPOTHESIZED IN VENUS EXPLORATORY MISSIONS CLOUD LAYER, BASED ON RADIOMETRIC OBSERVATION IN NASA-CR-89772 Nbl-40462 SHF RANGE A6b-37016 LEVY. 6- S- KUZMINi A. 0- RADIO OCCULTATION MEASUREMENT OF MARTIAN TWO-LAYER MOOEL OF VENUSIAN ATMOSPHERE SATISFYING ATMOSPHERE OVER TWO REGIONS BY MARINER IV SPACE RADIOASTRONOMIC AN0 RADAR SELF-RADIATION PROBE 866-29958 MEASUREMENTS 167-32322 MARINER VENUS 1967 SPACE PROBEt OBTAINING RADIO ASTRONOMICAL OBSERVATIONS OF VENUS - ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX AEROSOL ATMOSPHERIC MODEL FOR EXPLAINING RADIO FROM RADIO SIGNAL FREQUENCY. INTENSITY AND PHASE SPECTRUM Nbb-31470 CHANGES AIAA PAPER 67-118 Ab?’-18310 TWO-LAYER ATMOSPHERE MODEL OF VENUS NASA-CR-BE980 Nb7-38348 RADIO OCCULTATION MEASUREMENT OF MARTIAN ATMOSPHERE OVER TWO REGIONS BY MARINER IV KYRISS. C. L. SPACE PROBE Ab7-34151 INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS FOR POINTED AND SPHERICALLY BLUNT BODIES IN GROUND INSTRUMENTATION SYSTEM FOR MARINER IV UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE OCCULTATION EXPERIMENT. USING DOPPLER FREQUENCY Abb-25275 PERTURBATION METHOD FOR MARS ATMOSPHERIC Q PARAMETERS DETERMINATION Ab7-34498 INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS FOR POINTED AND SPHERICALLY BLUNT BODIES IN MARINER VENUS 1961 SPACE PROBE. OBTAINING UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX Ab7-19380 FROM RADIO SIGNAL FREQUENCY, INTENSITY AND PHASE CHANGES THERMODYNAMIC PROPERTIES OF THREE MARTIAN MODEL AIAA PAPER 67-118 Ab7-40094 ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOW FIELDS FOR REAL GASES - TABLES MARINER IV RADIO OCCULTATION MEASUREMENT OF MARS ATDM-66-1 Nb7-34135 ATMOSPHERE Nb6-31477

MARINER IV RAOIO OCCULTATION MEASUREMENTS OF L MARS UPPER ATMOSPHERE Nbb-31478 LEBEDINSKI 9 A. SURFACE TEMPERATURE OF VENUS Ab7-16029 FREQUENCY. PHASES AND AMPLITUDE CHANGES OF MARINER IV RADIO SIGNAL THROUGH ATMOSPHERE AND LEBEDINSKIYi A- I. IONOSPHERE OF MARS OBSERVED BEFORE AN0 AFTER UPPER ATMOSPHERE GLOW DISCHARGES STUDIED IN PLANETARY OCCULATATION ~67-12754 CONNECTION WITH THERMAL RADIO NOISE EMISSION FROM VENUS SURFACE Nbb-38994 LIBBY. W. F. STIMULATION OF JUPITER RADIO EMISSION BY IO LEDERBERG. J. Abl-25204 DECISION THEORY BIOLOGICAL SEARCH STRATEGIES AND PLANETARY QUARANTINE ASPECTS OF MARS LIGHT. J. 0. EXPLORATORY MISSIONS PLANETARY QUARANTINE CONSTRAINTS1 NOTING NASA-CR-89772 Nbl-40462 PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION A6b-29966 LEMAIREi JI ATMOSPHERIC MODELS. COMPARING CHAMBERLAIN PLANETARY QUARANTINE CONSTRAINTSI NOTING EVAPORATIVE AND SOLAR BREEZE MODELS. OPIK AN0 PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION SINGER EVAPORATIVE MODEL AN0 PARKER SOLAR Ab7-29098 WIND MODEL Abb-36605 LINK. F.

~ LEORY. C. RELATIONSHIP BETWEEN TERRESTRIAL AN0 JOVIAN MARS ATMOSPHERIC CIRCULATION, DIURNAL HEATING, ATMOSPHERIC CIRCULATIONS DUE TO SOLAR ACTIVITY THERMAL TIDES AND EFFECTS ON EARTH ATMOSPHERE Ab7-2 1215 Ab6-30353 LIPPINCOTTt E- R- MARTIAN ATMOSPHERIC CIRCULATION - VERTICAL JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM .I TEMPERATURE OISTRIBUTION, DIURNAL HEATING AND CORONA DISCHARGE, PRODUCING SIMPLE ORGANIC TIDES1 AN0 DIFFERENTIAL HEATING AN0 GENERAL MOLECULES Ab7-19057 CIRCULATION AT SOLSTICES Nbb-31489 THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION

1-49 LOVELOCKS J- E- PERSONAL AUTHOR INDEX

DEDUCED SPECTROSCOPICALLY A67-20022 MARSHALL, L- C. LIMITATION ON OXYGEN CONCENTRATION IN POSSIBLE THERMODYNAMIC EQUILIBRIUM COMPOSITION OF ALL PRIMITIVE ATMOSPHERES EXAMINED VIA PHYSICAL AND COMBINATIONS OF CI H, 0 AN0 N AT AVERAGE PHOTOCHEMICAL FACTORS A66-26122 PRESSURE AND TEMPERATURE CALCULATED FOR u ATMbSPHERES OF EARTH, VENUS, MARS AN0 JUPITER OXYGENIC CONCENTRATIONS IN PRIMITIVE EARTH A67-22236 ATMOSPHERE, DISCUSSING MARTIAN ATMOSPHERE COMPOSITION A67-34095 EVOLUTION OF ATMOSPHERIC COMPONENTS OF VENUS A67-80916 MARTIN. J. A. DATA REPRESENTING MONOPOLE ANTENNA VOLTAGE * THERMODYNAMIC EQUILIBRIA IN PLANETARY ATMOSPHERES BREAKOWON IN SIMULATED MARS AND VENUS AND IN ORIGIN OF ORGANIC MATTER - DETERMINATION $TWOSPHERES A67-35829 OF AMINO ACID PAIRING AND SEQUENCES IN PROTEINS NASA-CR-74559 N66-28800 IARTYNOV. 0- ATMOSPHERE, TEMPERATURE. AND CLOUD COVER OF VENUS CALCULATION OF THERMODYNAMIC EQUILIBRIUM NASA-CR-86635 N67-32308 COMPOSITION OF EARTH, VENUS. MARS AND JUPITER ATMOSPHERES N66-28801 MARVIN, J- G. MARS ATMOSPHERIC COMPOSITION AND LAMINAR THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS CONVECTIVE HEATING AND ABLATION STUDIED TO PREDICT ON CARBON. HYDROGEN. OXYGEN, AND NITROGEN IN PERFORMANCE OF HEAT PROTECTION SYSTEMS DURrNG EARTH, VENUS, MARS. AND JUPITER ATMOSPHERES ENTRY A66-2 5 2 74 N66-31642 HEATING RATES IN GAS MIXTURES OF PLANETARY THERMODYNAMIC EQUILIBRIUM IN PRE8IDLOGICAL ATMOSPHERES PREDICTED BY EQUATION USING TRANSPORT ATMOSPHERES, AND INORGANIC ORIGIN OF ORGANIC PROPERTIES OF GASES AT LOWER TEMPERATURES COMPOUNDS A66-27432 NASA-SP-3040 N67-27 295 MARS ATMOSPHERIC COMPOSITION AN0 LAMINAR LOVELOCK, J- E- CONVECTIVE HEATING AND ABLATION STUDIED TO PREDICT DETECTING PLANETARY LIFE FROM EARTH PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING A67-24063 ENTRY A67-18849

EXTRATERRESTRIAL LIFE DETECTION STUDIED FROM MAYER. C- H. KNOWLEDGE OF MAJOR AND TRACE COMPONENTS OF RADIO ASTRONOMY STUDIES OF VENUS AND MARS ATMOSPHERES 867-40999 NOTING SURFACE PROPERTIES, ATMOSPHERIC STRUCTURE. ETC A66-26031 LOW, P- F. FROST PHENOMENA ON MARS EXAMINED ON BASIS OF VENUS AN0 MARS ATMOSPHERE AND SURFACE STUDIED BY MARTIAN WAVE OF DARKENING, NOTING NECESSITY OF RADIO ASTRONOMY A67-34796 DELIQUESCENT SALTS TO ATTRACT AND RETAIN WATER ON SURFACE A67-18645 MC CRACKEN, C. W. CONDITIONS OF ENCOUNTER BETWEEN INTERPLANETARY LUGANSKI, De DUST PARTICLES AN0 PLANETS FEASIBILITY OF USING RADIO SOUNDING TECHNIQUES TO NASA-TM-X-57009 N66-35309 -* INVESTIGATE IONOSPHERIC PROPERTIES OF PLANETS NASA-CR-689 N67-28368 MC GOVERN, W, E.- M MERCURY ATMOSPHERIC TEMPERATURE, COMPOSITION AN0 SURFACE PRESSURE AN0 EFFECT OF NONSYNCHRONOUS MANNELLA, GI G- ROTATION A6640424 FLYBY INFRARED ABSORPTION MEASUREMENTS IN MARTIAN ATMOSPHERE FOR DETERMINATION OF PROFILES OF RESEARCH ON PLANETARY ATMOSPHERES, VENUS OARK CARBON DIDXIDEI PARTICULATE MATTER AND WATER SIDE EMISSIONt OZONE CONCENTRATION, CLOUD AN0 VAPOR AEROSOL SCATTERING, ATMOSPHERIC RADIATION NASA-TN-0-4115 N67-34884 SCATTERING, AND EARTH HEAT BUDGET AN0 ALBEDO NASA-CR-77048 N66-33437 MARIANO, J. VERTICAL TEMPERATURE DISTRIBUTION IN MARTIAN ATMOSPHERE OF MERCURY ATMOSPHERE* NOTING INSENSITIVITY TO SURFACE NASA-TM-X-57322 N67-18273 PRESSURE AND CARBON DIOXIDE VARIATIONS A66-26132 THERMAL STRUCTURE OF UPPER MARS ATMOSPHERE NASA-TM-X-57327 N67-1865 2 METEOROLOGY OF MARS AND VENUS NASA-CR-75315 N66-27238 MCELROYs M. B. MARINER IV OCCULTATION EXPERIMENT CONCERNING MODEL COMPUTATIONS OF TEMPERATURE VARIATIONS AND CARBON DIOXIDE AND IONOSPHERIC PEAKS IN MARTIAN WIND CIRCULATIONS IN MARTIAN ATMOSPHERE ATMOSPHERE A66-25834 NASA-CR-85569 N67-30624 DIFFUSE REFLECTION BY PLANETARY INHOMOGENEOUS MARIN. M. ATHOSPHERE WITH ALBEDO FOR SINGLE SCATTERING JUPITER PLANETARY SURFACE OBSERVATIONS SHOW SLOW DECREASES EXPONENTIALLY WITH OPTICAL DEPTH EVOLUTION OF ATMOSPHERIC PHENOMENA 866-34 149 A66-31310 MCKENZIE, R. L- MARHOs Fa F- CHEMICAL SYSTEM AND REACTION RATES BEHIND STRONG PHOTOCHEMISTRY OF PLANETARY GASES AN0 PLANETARY SHOCK WAVES IN MIXTURES OF CARBON DIOXIDE AND

AERONOMY NITROGEN USE0 TO STUDY ENTRY CONDITIONS INTO MARS + NASA-CR-81262 N67-16515 ATMOSPHERE A66-25276

EXPERIMENTAL AND THEORETICAL STUDIES IN PLANETARY MELROSE. D. B. A ER 0N 0 M Y JOVIAN ROTATIONAL EFFECTS ON MAGNETOSPHERIC MODEL NASA-CR-82937 N67-19929 AND CONDITIONS OF FLUTING AND TWO-STREAM INSTABILITY A66-29952 * MARSHALL. L. STIMULATION OF JUPITER RADIO EMISSION BY IO MODEL FOR DISTRIBUTION OF THERMAL PLASMA IN A67-25 204 MAGNETOSPHERE OF JUPITER UNDER ASSUMPTION OF COROTATION WITH PLANET A67-33196

1-50 PERSONAL AUTHOR INDEX NIEDERER, P- 6.

MENARD, We A. DETERMINE OPTICAL PARAMETERS OF ITS ATMOSPHERE MOLECULAR, CONTINUUM AND LINE RADIATION OF AN0 SURFACE FROM ABSOLUTE PHOTOMETRIC DATA PLANETARY ATMOSPHERES, COMPARING MOLECULAR BAND N66-33533 STRUCTURE MODELS WITH SPECTRAL MEASUREMENTS OF CN VIOLET BAND SCATTERING ANISOTROPY EFFECT ON OPTICAL PARAMETERS AIAA PAPER 67-323 A67-26038 OF MARTIAN ATMOSPHERE AND SURFACE - PHOTOHETRY N67- 160 2 0 MILAS. A- THERMODYNAMIC PROPERTIES OF THREE MARTIAN MODEL MUENCH. G- ATMOSPHERES FOR CALCULATING EQUILIBRIUM FLOW OBSERVATIONS OF MOON, VENUS, MARS, AND FIELDS FOR REAL GASES - TABLES JUPITER - SURFACE FEATURES AND ATMOSPHERIC ATOM-66-1 N67-34135 CHARACTERISTICS - RADIO, RADAR, TELESCOPIC, AND SPECTROSCOPIC OBSERVATIONS HINTZ. Y. NASA-CR-76142 N66-31446 NUMERICAL MOOEL FOR SIMULATING GENERAL CIRCULATION OF ATMOSPHERE OF MARS MUHLEMAN, D. 0. NASA-CR-81146 N67-15280 OBSERVATIONS OF MOON, VENUS. MARS, AND JUPITER - SURFACE FEATURES AND ATMOSPHERIC MINZNER, R. A. CHARACTERISTICS - RADIO, RADAR, TELESCOPICt AN0 SINGLE AN0 DOUBLE GAS NUMBER-DENSITY EQUATIONS FOR SPECTROSCOPIC OBSERVATIONS DETERMINING TEMPERATURE-ALTITUDE PROFILE, HIGH NASA-CR-76142 N66-31446 AN0 LOW SOLAR ACTIVITY ATMOSPHERIC MODELS, AN0 ERROR ANALYSIS MURRAY. 8. GI NASA-CR-79525 N67- 130 18 PLANETARY CONTAMINATION BY VIABLE TERRESTRIAL MICROORGANISMS TRANSPORTED ON SPACECRAFT MIYAMOTO, S. AD-648864 N67-27042 MARTIAN ATMOSPHERE AND CRUST ANALYZED, BASE0 ON MARINER IV CLOUD PHOTOGRAPHS 166-38022 MUSILI J. L- EXPANDABLE, TERMINAL DECELERATORS FOR MARS ANALYSIS OF MARTIAN ATMOSPHERE AND CRUST FROM ATMOSPHERE ENTRY VISUAL OBSERVATION A67-80329 NASA-CR-79496 N67-12052

MDHRt B- MYERS. E. T. FEASIBILITY OF USING RADIO SOUNDING TECHNIQUES TO AERODYNAMIC, THERMODYNAMIC, HEAT SHIELD AND INVESTIGATE IONOSPHERIC PROPERTIES OF PLANETS STRUCTURAL DESIGN ASPECTS OF BALLISTIC VEHICLE NASA-CR-689 N67-28368 ENTERING PLANETARY ATMOSPHERE A67-35315

MDDNANI P. J. SPHERICAL ENTRY VEHICLE USE0 TO DEFINE PLANETARY GUIDE0 PROPULSIVE SOLUTION TO MARS ATMOSPHERE- ATMOSPHERE STRUCTURE AN0 COMPOSITION FROM DYNAMIC DECELERATED SOFT LANDING VEHICLE TRAJECTORY RESPONSE DURING ENTRY, DISCUSSING AERODYNAMIC AIAA PAPER 67-170 A67-18508 CHARACTERISTICS A67-40177

MOORE, R. CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K M DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS NAGARAJAN. 6- OF MARS A67-14309 THERMODYNAMIC EQUILIBRIUM IN PREBIOLOGICAL ATMOSPHERES, AND INORGANIC ORIGIN OF ORGANIC MOORE, R. C- COMPOUNDS HIGH DISPERSION SPECTROGRAMS OF HARS EXAMINE0 FOR NASA-SP-3040 N67-27295 WATER VAPOR PRESENCE, RESULTS INDICATE AMOUNT DEPENDS ON SIZE OF POLAR CAP NAGLER, R. G. J PL-TR-32-1048 Ab7-22235 INTERPLANETARY TRANSIT AN0 ATMOSPHERIC ENTRY OF UNMANNED VEHICLE LANDING ON MARS SURFACE, WITH TWILIGHT CUSP EXTENSIONS OF VENUS AN0 REFERENCE TO HEAT SHIELD TECHNOLOGY APPLICATION TO DERIVING HEIGHTS OF SCATTERING JPL-TR-32-1145 A67-25715 ATMOSPHERE P-3621 N67-35341 NAUMOV. A. PI VENUS RADIATION SPECTRUM IN MM RANGE FROM VENUS VENUS TWILIGHT SKY INVESTIGATED FOR DISCREPANCIES ATMOSPHERE MODELS 167-40120 BETWEEN PREDICTED AND OBSERVED SHAPE AND PERIODIC APPEARANCE OF PLANET NEUBAUER, F. H. RM-5386-PR N67-37243 OUST CLOUD FORMATION BY THERMAL CONVECTION IN MARTIAN ATMOSPHERE A66-30925 MDROWITZ. H. INDIGENOUS BIOLOGY IN VENUS CLOUDS, PROPOSING NEWELL. H. E. ISOPYCNIC FLOAT BLADDER MACROORGANISM INGESTING HIGHLIGHTS OF SPACE SCIENCE ACHIEVEMENTS IN 1965 WATER AND MINERALS BLOWN UP FROM SURFACE BY NASA-SP-136 N67-19022 PINOCYTOSIS A67-39556 NEWELL, R. E. MOROZt V- I. VENUS SURFACE TEMPERATURE AND MICROWAVE EMISSION, SPECTRAL STUDY OF JUPITER, SATURN AND RINGS OF DISCUSSING IONOSPHERIC MODEL. GREENHOUSE EFFECT. SATURN, DETERMINING METHANE CONCENTRATION IN MICROOISCHARGE MODEL, RADIO AURORA, ETC CLOUD LAYERS A66-37035 A67-34543

SPECTRAL STUDY OF JUPITER, SATURN AND RINGS OF SIMULTANEOUS UV PHOTOGRAPHS AND RADAR CROSS SATURN, DETERMINING METHANE CONCENTRATION IN SECTION MEASUREMENTS OF VENUS, DISCUSSING CLOUD LAYERS A67-15557 ATMOSPHERIC MOTION AND ROTATION A67-38611 SOVIET BOOK ON PLANETARY PHYSICS COVERING MARTIAN, VENUSIAN AND MERCURIAN ATMOSPHERES, NEWMAN, P. A- VENUSIAN SURFACE TEMPE‘RATURE AND JOVIAN RADIO DIRECT CALCULATION AND TABLES OF SPECIFIC HEATS EMISSION A67-38933 AND RELATED THERMOOYNAMIC PROPERTIES OF ARBITRARY GAS MIXTURES - MARS ATMOSPHERE MOOEL INFRARED SPECTROSCOPY TO DETERMINE TEMPERATURE, NASA-TN-0-3540 N66-34373 PRESSURE. AN0 CHEMICAL COMPOSITION OF MARTIAN ATMOSPHERE N67-16813 NIEDERER. P. 6. HEAT BALANCE, PRESSURIZATION, AND MINIMUM WEIGHT MDRDZHENKO, A. V. DESIGN CRITERIA FOR INFLATABLE STRUCTURES IN BRIGHTNESS OISTRIBUTION OF MARTIAN DISK USED TO NEAR-PLANETARY ATMOSPHERE

1-51 PERSONAL AUTHOR INDEX

NASA-CR-84829 Nb7-28789 I R OBSERVATIONS FOR PRESENCE OF ETHANE IN ATMOSPHERES OF JUPITER AN0 SATURN REANALYZED AN0 NIER, A. 0. C- FOUND CONSISTENT WITH PREVIOUS RESULTS MAGNETIC-SECTOR MASS SPECTROMETER FOR MARS Ab7-21218 ATMOSPHERE ANALYSIS NASA-CR-76498 Nbb-3192 b STRUCTURE AN0 COMPOSITION OF JUPITER ATMOSPHERE. * NOTING LABORATORY AN0 OBSERVATIONAL DATA NORTON, R. H. SUPPORTING HYPOTHESIS OF CONSISTENCY WITH SOLAR LUNAR AN0 PLANETARY STUDIES DEALING WITH COUDE ELEMENTS ABUNDANCE Ab7-30932 FACILITY WITH 24-INCH TELESCOPE, DICK€-TYPE RADIOMETER TO MEASURE EMISSION FROM VENUS, AN0 CARBON OIDXIOE ABUNDANCE AND SURFACE PRESSURE OF 1 EMISSION SPECTRA OF SILICATES Nb7-23660 MARTIAN ATMOSPHERE Nbb-31475 NYLANO, F. S. AERODYNAMIC LIFT IN FUTURE SPACE VEHICLE DESIGN P DURING VARIOUS FLIGHT REGIMES IN ATMOSPHERES OF PALH. A- EARTH AN0 PLANETS BLUE CLEARINGS OF MARS ATMOSPHERE AS FUNCTION OF P-3559 Nb7-28513 NUMBER OF METEOR SHOWERS INTERSECTING MARS ORBIT AT INTERVALS OF HELIOCENTRIC LONGITUDE 0 NASA-CR-59938 Nbb-33414 OHMSTEOE, W. 0. PANAGAKOS. N. HI NUMERICAL SOLUTION OF TRANSPORT AN0 ENERGY EARTH AN0 PLANETARY OCEAN AND ATMOSPHERIC ORIGIN, EQUATIONS IN PLANETARY BOUNDARY LAYER EVOLUTION, AND COMPOSITION Nbb-37965 ECOM-bo20 Nbb-33271 PARKER, n. s. OHRING, 6. MARS ATMOSPHERE ENTRY PROBE CONFIGURATION, VERTICAL TEMPERATURE DISTRIBUTION IN MARTIAN AERODYNAMIC CHARACTERISTICS. FLOW FIELD. ATMOSPHERE, NOTING INSENSITIVITY TO SURFACE STABILITY AUGMENTATION, INSTRUMENTATION. PRESSURE AN0 CARBON DIOXIDE VARIATIONS THERMAL SHIELOINGt DATA HANDLING AN0 Abb-26132 COMMUNICATIONS Ab7-11424

METEOROLOGY OF MARS AND VENUS PATAKI. L. NASA-CR-75315 Nbb-27238 SPACE RECEIVER OBSERVATIONS OF JOVIAN DECAMETER FLUX MODEL COMPUTATIONS OF TEMPERATURE VARIATIONS AN0 NASA-CR-82654 Nb7- 19 113 WIND CIRCULATIONS IN MARTIAN ATMOSPHERE NASA-CR-85569 Nb7-30624 PAVELEV. A. 6. DISTRIBUTION OF RADIO BRIGHTNESS TEMPERATURE OVER OLEARY, 8- T- DISK OF VENUS Ab?-27333 $, PHOTOMETRY OF INTEGRATED LIGHT OF VENUS, INFERRING PRESENCE OF ICE IN ATMOSPHERE FROM HALO PIHENTEL, 6. C- EFFECT OF BRIGHTNESS DISPERSION VIBRATION AND THERMAL RADIATION EFFECTS ON FILTER Ab7-16407 HEDGE INFRARED SPECTROMETER USED IN SPACECRAFT STUDIES OF PLANETARY ATMDSPHERES POLARIZATION PROPERTIES OF MERCURY EXPLAINED BY NASA-CR-85797 Nb7-31336 I* SURFACE ONLY, SO THERE IS NO POLARIMETRIC EVIDENCE FOR ATMOSPHERE ON MERCURY Ab7-26244 PLUMHER. W. VENUS SURFACE TEMPERATURE FROM MICROWAVE OSTER, A. La MEASUREMENTS, NOTING THERMAL AN0 NONTHERMAL GEROIEN TYPE CHAMBER FOR MEASUREMENTS OF ION RAD1AT1 ON Abb-28129 MOBILITY SPECTRUM IN TERRESTRIAL MESOSPHERE AN0 MARS ATMOSPHERE Abb-34712 POLLACK. J. 6- ANISOTROPIC NONCONSERVATIVE SCATTERING IN MODIFIED OTOSHI, T. Y. SCHUSTER- SCHHARZSCHILO APPROXIMATION AN0 VENUS GROUND INSTRUMENTATION SYSTEM FOR MARINER IV CLOUD LAYER 167-20931 OCCULTATION EXPERIMENT, USING DOPPLER FREQUENCY PERTURBATION METHOD FOR MARS ATMOSPHERIC RELATION BETWEEN SURFACE PRESSURE AND ATMOSPHERIC PARAMETERS DETERMINATION Ab7-34498 BRIGHTNESS IN OPTICALLY THIN RAYLEIGH SCATTERING ATMOSPHERE, CONSIDERING APPLICATION TO MARS OTTERMAN, J. Ab7-34536 MARTIAN HAVE DF DARKENING ATTRIBUTED TO SOIL FROST PHENOMENA Abb-40478 METHOD FOR CALCULATING PROPERTIES OF MONOCHROMATIC RADIATION THROUGH LAYER OF DISPERSED PARTICLES ELEVATION DIFFERENCES BETHEEN MARTIAN DARK AREAS AND ITS APPLICATION TO VENUS CLOUDS /MARIA/ AN0 BRIGHT AREAS /DESERTS/, DISCUSSING 166-31465 SURFACE PRESSURE AND TEMPERATURE 167-22957 LIMB-DARKENING OBSERVATIONS OF VENUS BY MARINER I1 SPACECRAFT MICROWAVE RAOIOHETERS OWEN, R- 8. Nbb-31640 DERIVATION OF ATMOSPHERIC PARAMETERS FOR GREENHOUSE MODEL OF VENUS ATMOSPHERE APPROXIMATION FORMULA DESCRIBING MONOCHROMATIC NASA-TM-X-53497 Nb7-29983 TRANSMISSION, REFLECTION, AN0 ABSORPTION OF VENUS CLOUD LAYER Nbb-31641 OWEN, T. COMPOSITION AN0 SURFACE PRESSURE OF MARTIAN POPES R- 8. ATMOSPHERE DETERMINED FROH PHOTOGRAPHIC SPECTRUM MARS ATMOSPHERIC COMPOSITION AN0 LAMINAR OF MARS OBTAINED AT MARCH 1965 OPPOSITION CONVECTIVE HEATING AND ABLATION STUDIED TO PREDICT Ab7-11695 PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING , ENTRY Abb-25274 MEAN VALUES OF HETHANE WAVELENGTHS IN URANUS SPECTRUM MEASURED FOR DETERMINATION OF ATMOSPHERIC MARS ATMOSPHERIC COMPDSITION AN0 LAMINAR TEMPERATURE Ab7-14327 CONVECTIVE HEATING AN0 ABLATION STUDIED TO PREDICT PERFORMANCE OF HEAT PROTECTION SYSTEMS DURING URANUS AND' NEPTUNE SPECTRAL ABSORPTIONS COMPARED ENTRY Ab7-18849 WITH LABORATORY SPECTRA OBTAINED WITH VERY LONG OPTICAL PATHS INDICATE METHANE ROLE IN PLANETARY POZNANSKI. 2- ABSORPTION Ab7-21213 FEASIBILITY OF USING RADIO SOUNDING TECHNIQUES TO INVESTIGATE IONOSPHERIC PROPERTIES OF PLANETS

1-52 PERSONAL AUTHOR INDEX SAGAN. C.

NASA-CR-689 Nb7-28368 SHOW CORRELATION BETWEEN OVAL ROTATIONAL VELOCITY AND LONGITUDINAL DISTANCE FROM RED SPOT PRIBOEVA, N- VI ~6r-37400 PHOTOMETRIC OBSERVATION DATA ON JUPITER ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- REEVES. R. Rat JR- * MONTH PERIODIC CHANGE Ab7-39299 RADIATION EQUILIBRIA IN UV LIGHT ON AIR, OXYGEN, CARBON OIOXIOE, ETC. ANALYZED BY BROMINE LAMP IN PROKOFYEV, V. K. CONNECTION WITH STUDIES OF PLANETARY ATMOSPHERES SPECTROSCOPIC INVESTIGATION OF VENUS ATMOSPHERE A67-14088 TO DETERMINE NITROGEN, OXYGEN, CARBON OIOXIDEI WATER VAPOR, AND OTHER COMPONENTS INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS Nb7-16802 THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS HAVE BEEN OBSERVED IN X-BAND FROM GLOW DISCHARGES R Abl-1495 2 RAINVILLE. L. P. REPIN. L. RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW SIMULATION FACILITY FOR ATMOSPHERIC COMPOSITIONI VALUE OF CROSS SECTION, ECHO SPECTRUM, PRESSURE, AND DAILY VARIATIONS OF MARS AN0 POLARIZATION CHARACTERISTICS, ABSORPTION CROSS OTHER PLANETS SECTION AN0 ATMOSPHERIC ATTENUATION NASA-TI-F-11062 Nb7-27533 A67-16298 RHEIN, Re A. RAKOSt K- 0. IGNITION TEMPERATURES OF POWDERED METALS IN MARS ATMOSPHERIC DENSITY DETERMINED FROM SIMULATE0 MARS AND VENUS ATMOSPHERES PHOTOELECTRIC MEASUREMENTS OF ECLIPSES OF PHOBOS NASA-CR-02878 Nb7-20169 Abb-30049 RIEs Ha RASOOL, S- 1. INVISCID EQUILI8RIUH GAS STABILITY CHARACTERISTICS VENUS ATMOSPHERE, SURFACE TEMPERATURE AND FOR POINTED AND SPHERICALLY BLUNT BODIES IN RADIATION CHARACTERISTICS Abb-35799 UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE Abb-25275 MERCURY ATMOSPHERIC TEMPERATURE. COMPOSITION AND SURFACE PRESSURE AND EFFECT OF NONSYNCHRONOUS INVISCID EQUILIBRIUM GAS STABILITY CHARACTERISTICS ROTATION Abb-40424 FOR POINTED AND SPHERICALLY BLUNT BODIES IN UNSTEADY SUPERSONIC FLIGHT IN MARS ATMOSPHERE PROPERTIES OF ATMOSPHERES OF MARS, JUPITER AND Ab7-19380 VENUS Nbb-32039 RING. J- ATMOSPHERE OF MERCURY DETECTING PLANETARY LIFE FROM EARTH NASA-TM-X-57322 N67-18273 Ab7-24063 48 COMPARISON OF SURFACE AND ATMOSPHERIC ROBBINS, R- C- CHARACTERISTICS OF EARTH AND VENUS CHEMICAL REACTIONS BETWEEN SOLAR HYDROGEN AND NASA-TM-X-57351 N67-18435 CARBON MONOXIDE IN VENUS ATMOSPHERE NASA-CR-82960 Nb7-1 9904 vs THERMAL STRUCTURE OF UPPER MARS ATMOSPHERE NASA-TM-X-57327 Nb7-18652 ROBERTS. W. T. MARTIAN ATMOSPHERE MODELS WITH DIFFERENT REA, 0. G. COMPOSITION, PRESSURE AND TEMPERATURE POLARIZATION PROPERTIES OF MERCURY EXPLAINED 8Y A67-25685 SURFACE ONLY, SO THERE IS NO POLARIMETRIC EVIDENCE FOR ATMOSPHERE ON MERCURY A67-26244 ATMOSPHERE OF MARS STUDIED USING THREE MODELS GENERATED TO SHOW HIGH, MEAN AN0 LOW DENSITY UPPER LIMITS ON LIQUIO WATER CONTENT IN VENUS COMPOSITIONS TO ACCOUNT FOR GRAVITATIONAL AND ATMOSPHERE A67-32652 MAGNETIC FIELDS A67-40140

PRESSURE. COMPOSITIONI AND PARTICLE CONTENT OF MARS ATMOSPHERE MODELS AT THREE DENSITY LEVELS MARTIAN ATMOSPHERE - POLARIZATIONI SPECTRAL NASA-TM-X-53484 Nbb-31944 BRIGHTNESS, AN0 TEMPERATURE OF MARTIAN SURFACE N6b-31472 DERIVATION OF ATMOSPHERIC PARAMETERS FOR GREENHOUSE MODEL OF VENUS ATMOSPHERE UPPER LIMITS ON LIQUID HATER IN VENUS ATMOSPHERE NASA-TM-X-53497 Nb7-29983 DUE TO PRESENCE OF HYDROGEN CHLORIDE NASA-CR-84601 Nb7-28001 ROBINSON. A. R. DEEP CIRCULATION IN VENUSIAN ATMOSPHERE MODEL REDMONO, J. C. OPAQUE TO SOLAR AN0 PLANETARY RADIATION BUT WITH SCIENCE SUBSYSTEMS FOR JUPITER FLYBY MISSIONS, DIFFERENTIAL HEATING Ab7-14310 OISCUSSING EQUIPMENT SELECTION. MISSION PLANNING, SPACECRAFT DESIGN AN0 TRAJECTORY AN0 CONSTRAINTS ROMANENKO, Z. G. ON VEHICLE CONFIGURATION PHOTOMETRIC OBSERVATION DATA ON JUPITER AIAA PAPER 67-120 Ab7-18287 ATMOSPHERIC ACTIVITY /1964-1965/ NOTING THREE- MONTH PERIODIC CHANGE A67-39299 REESE, 0- E-r JR- DESIGN AN0 FEASIBILITY STUDIES OF MARS ATMOSPHERE ROZENBERG, G. V. PROBE VEHICLE A6b-25292 TWILIGHT INVESTIGATIONS OF PLANETARY ATMOSPHERES FROM SPACE PROBES HYPERSONIC ENTRY VEHICLE MEASUREMENT OF MARS FTD-MT-65-400 Nb7-19543 ATMOSPHERIC DENSITY, PRESSURE. COMPOSITION, TEMPERATURE AND DETECTION SPECTROMETRY OF CHEMICAL RYAN. J- A- SPECIES IN SHOCK LAYER 166-42680 OUST DEVILS IN RELATION TO MARTIAN YELLOW CLOUDS NASA-CR-89578 Nb7-40004 REESEt E. J- RAPID DRIFT IN LONGITUDE OF SMALL DARK SPOT ON SOUTH EDGE OF JUPITER NORTH TEMPERATE BELT, S 8. NOTING SINUSOIDAL DISPLACEMENT CHARACTERISTICS SAGAN, C. AND MEASUREMENT WITH BLUE AND UV PHOTOGRAPHY MARINER IV MARS OBSERVATION DATA ANALYSIS AN0 Abb-33009 INTERPRETATION A6b-34896

JUPITER GREAT RED SPOT AND THREE WHITE OVALS THERMODYNAMIC EQUILIBRIUM COMPOSITION OF VENUS

1-53 SAGAN, C. E- PERSONAL AUTHOR INDEX

ATMOSPHERE COMPUTED FROM ATOMIC COMPOSITION DETERMINING TEMPERATURE-ALTITUDE PROFILE. HIGH DEDUCED SPECTROSCOPICALLY Ab7-20022 AN0 LOW SOLAR ACTIVITY ATMOSPHERIC MODELS. AN0 ERROR ANALYSIS ANISOTROPIC NONCONSERVATIVE SCATTERING IN MODIFIED NASA-CR-79525 Nb7-13018 SCHUSTER- SCHWARZSCHILD APPROXIMATION AN0 VENUS CLOUD LAYER A67-20931 SCHILLING, G. F. TWILIGHT CUSP EXTENSIONS OF VENUS AND t THERMODYNAMIC EQUILIBRIUM COMPOSITION OF ALL APPLICATION TO DERIVING HEIGHTS OF SCATTERING COMBINATIONS OF CI He 0 AND N AT AVERAGE ATMOSPHERE PRESSURE AN0 TEMPERATURE CALCULATED FOR P-3b21 Nb7-35341 ATMOSPHERES OF EARTH, VENUS, MARS AN0 JUPITER Ab7-22236 VENUS TWILIGHT SKY INVESTIGATED FOR DISCREPANCIES BETWEEN PREDICTED AN0 OBSERVE0 SHAPE AND INDIGENOUS BIOLOGY IN VENUS CLOUDS, PROPOSING PERIODIC APPEARANCE OF PLANET ISOPYCNIC FLOAT BLADDER MACROORGANISM INGESTING RM-5386-PR Nb7-37243 WATER AND MINERALS BLOWN UP FROM SURFACE BY PINOCYTOS IS Ab7-39556 SCHORN, R. A. CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K MARTIAN ATMOSPHERE COMPONENT DUE TO PROTON DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS PENETRATION INTO ATMOSPHERE FROM SOLAR WIND, OF MARS Ab7-14309 SUGGESTING RADIO OCCULTATION BY MARS ORBITER Ab7-40799 HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR WATER VAPOR PRESENCE, RESULTS INDICATE AMOUNT EVOLUTION OF ATMOSPHERIC COMPONENTS OF VENUS DEPENDS ON SIZE OF POLAR CAP Ab7-80916 JPL-TR-32-1048 Ab7-22235

CALCULATION OF THERMODYNAMIC EQUILIBRIUM SCHWEIGER, R- N. COMPOSITION OF EARTH, VENUS, MARS AND OPTICAL RADIOMETER FEASIBILITY STUDY FOR JUPITER ATMOSPHERES Nbb-28801 DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM SHOCK LAYER RADIATION DURING ENTRY - METHOD FOR CALCULATING PROPERTIES OF MONOCHROMATIC INSTRUMENTATION RADIATION THROUGH LAYER OF DISPERSED PARTICLES NASA-CR-73027 Nbb-35663 AN0 ITS APPLICATION TO VENUS CLOUDS N6b-31465 SCISSUM. J. A. DERIVATION OF ATMOSPHERIC PARAMETERS FOR ASTROPHYSICAL EVALUATION OF VENUS OBSERVATIONS GREENHOUSE MODEL OF VENUS ATMOSPHERE FROM MARINER I1 RADIOMETER DATA, AN0 NASA-TM-X-53497 Nb7-29983 THERMODYNAMIC ANALYSES OF PLANETARY ATMOSPHERES NASA-CR-76106 Nbb-31639 SCRANAGE, C. ON-BOAR0 TRACKING SYSTEM OF TWO-WAY COHERENT LIMB-DARKENING OBSERVATIONS OF VENUS BY MARINER DOPPLER BETWEEN ENTRY CAPSULE AND ORBITING BUS e I1 SPACECRAFT MICROWAVE RAOIOMETERS FOR DETERMINING ORBIT OF ENTRY CAPSULE AND Nbb-31640 ESTIMATING ATMOSPHERIC PARAMETERS Nb7-15904 APPROXIMATION FORMULA DESCRIBING MONOCHROMATIC TRANSMISSION, REFLECTIONI AND ABSORPTION OF SEIOEL. B. L- VENUS CLOUD LAYER Nbb-31641 GROUND INSTRUMENTATION SYSTEM FOR MARINER IV t4 OCCULTATION EXPERIMENT, USING DOPPLER FREQUENCY THERMODYNAMIC EQUILIBRIUM COMPOSITION CALCULATIONS PERTURBATION METHOD FOR MARS ATMOSPHERIC ON CARBON, HYDROGEN. OXYGEN. AN0 NITROGEN IN PARAMETERS DETERMINATION Ab7-34498 EARTH, VENUS, MARS, AND JUPITER ATMOSPHERES Nbb-31642 SEIFFI A. HYPERSONIC ENTRY VEHICLE MEASUREMENT OF MARS COMPONENT OF MARS IONOSPHERE DUE TO SOLAR PROTONS ATMOSPHERIC DENSITY, PRESSURE, COMPOSITIONI NASA-CR-84411 Nb7-27370 TEMPERATURE AN0 DETECTION SPECTROMETRY OF CHEMICAL SPECIES IN SHOCK LAYER Ab6-42 68 D DECISION THEORY BIOLOGICAL SEARCH STRATEGIES AN0 PLANETARY QUARANTINE ASPECTS OF MARS ENERGY DISSIPATION AND OTHER PROBLEMS FOR ALIEN EXPLORATORY MISSIONS PLANETARY ATMOSPHERIC ENTRY AT HIGH SPEEDS OF NASA-CR-89772 Nb7-40462 INTERPLANETARY FLIGHT 167-21155

SAGAN, C. E. EARTH AN0 PLANETARY ATMOSPHERE ENTRY PROBLEMS FOR JOVIAN ATMOSPHERE SIMULATION WITH ENERGY FROM BLUNT NOSED SLENDER VEHICLES NOTING AERODYNAMICS. CORONA DISCHARGE, PRODUCING SIMPLE ORGANIC STABILITY, HEATING. ABLATION AND INTERACTION OF MOLECULES Ab7-19057 EFFECTS AIAA PAPER 67-803 Ab7-42963 SALISBURY, F. 8. LEAF-KILL OF BLADES AND PINE NEEDLES BY SIMULATED SEKERA, 2. MARS, EARTH, AND VENUS SOLAR RADIATION MATRIX ALGEBRAIC REDUCTION OF EQUATIONS OF Abb-81851 RADIATIVE HEAT TRANSFER FOR PLANETARY ATMOSPHERE RM-4951-PR. PT. I Nb6-34876 SAMUELSONs R. E. SOLUTION OF ANGULAR DISTRIBUTION OF DUTGOING REDUCTION OF INTEGRAL EQUATIONS OF RADIATIVE THERMAL RADIATION FROM PLANETARY ATMOSPHERE, USING TRANSFER FOR PLANETARY ATMOSPHERE WITH RAYLEIGH CHANDRASEKHAR DIFFUSE SCATTERING AND TRANSMISSION SCATTERING FUNCTIONS Ab7-22240 RM-5056-PR Nbb-35579

LIMB DARKENING OF PLANETARY ATMOSPHERES IN THERMAL SHAFRIR, U. INFRARED EFFECTIVE BRAKING HEIGHT / EBH/ FOR SMALL NASA-TM-X-57359 Nb7-18280 INTERPLANETARY PARTICLES OF COSMIC VELOCITY 9 ENTERING MARTIAN UPPER ATMOSPHERE SASLAW, W. C. Ab7-34541 ION-MOLECULE CHEMISTRY OF JUPITER UPPER ATMOSPHERE, STUOYING EQUILIBRIUM AND PLANETARY PHYSICS SEMINAR - POLARIZATIONI NONEQUILIBRIUM ABUNDANCES OF HYDROCARBON PRODUCTS SPECTROMETRIC, AND RADIO SIGNAL TECHNIQUES FOR c DUE TO UV'RADIATION REACTION Ab7-34540 MEASURING MARTIAN SURFACE AND ATMOSPHERIC PARAMETERS Nb7-12664 SAUERMANN, G. 0. SINGLE AND DOUBLE GAS NUMBER-DENSITY EQUATIONS FOR

1-54 PERSONAL AUTHOR INDEX STRONG, J. 0-

SHARONOV, V- V. SOMMER, Sa C- MODELS THAT ASSUME MARS ATMOSPHERE HAS ABSORPTIVE FREE FALLING PROBE TEST DURING TERMINAL DESCENT RATHER THAN SCATTERING PROPERTIES, AN0 THAT FOR DETERMINING UNKNOWN PLANETARY ATMOSPHERE REDNESS OF PLANET IS DUE TO SELECTIVE ABSORPTION PROFILE FROM ONBOARO MEASUREMENTS ALONE * Nb7-16808 Ab7-22768 MODEL FOR MARTIAN ATMOSPHERE AN0 PLANETARY PLANETARY ATMOSPHERE STRUCTURE DETERMINED FROM SURFACE ASSUMING ATMOSPHERIC SPECTRUM WITH ENTRY VEHICLE ONBOARO MEASUREMENTS OF PRESSURE, PURELY SCATTERING PROPERTIES AN0 SURFACE TEMPERATURE, AN0 ACCELERATION COVERED WITH LIMONITE OUST Nb7-16809 NASA-TN-0-3933 N67-23302 v SHAWL, S. J- SPENCER. De F. DOPPLER-DISPLACED LINES OF WATER VAPOR ORIGINATING MARTIAN SURFACE PRESSURE AN0 SURFACE DENSITY FROM IN ATMOSPHERE OF VENUS OBSERVED ON THREE COUDE INTERPRETATION OF OBSERVATIONAL DATA SPECTROGRAMS Ab7-11774 Abb-25291

SHIMIZU, M. SPENCER, Ne W. DISSOCIATION LAYER HEIGHTS ON VENUS, MARS AN0 MARTIAN ATMOSPHERE SAMPLING BY SENSORS OF JUPITER. NOTING CO FLAME AIRGLOW INTENSITIES PARACHUTE DROPPED CAPSULE N6b-32064 Abb-30050 SPINRAO. H- ATOMIC AN0 MOLECULAR PROCESSES IN UPPER ABSORPTION LINES ON VENUS SPECTROGRAMS OF ATMOSPHERES OF VENUS, MARS AN0 JUPITER ROTATIONAL FINE STRUCTURE OF EXCITED VIBRATIONAL INVESTIGATED BY ATMOSPHERIC MODELS, PRESENTING TRANSITION OF CARBON DIOXIDE Abb-41016 SOLAR-PLANETARY RELATIONSHIP Ab7-18429 PLANETARY ATMOSPHERE RESOLUTION SPECTRUM NOTING ATOMIC AN0 MOLECULAR PROCESSES IN CYTHEREAN, CARBON DIOXIDE LINES, RADIATION TRANSFER, MARTIAN AN0 JOVIAN UPPER ATMOSPHERES COMPOSITION, TEMPERATURES, PRESSURES, ETC Ab7-34158 Abb-42667

SHUMSKY, J. DOPPLER-DISPLACED LINES OF WATER VAPOR ORIGINATING OPTICAL RADIOMETER FEASIBILITY STUDY FOR IN ATMOSPHERE OF VENUS OBSERVED ON THREE COUDE DETERMINING COMPOSITION OF MARS ATMOSPHERE FROM SPECTROGRAMS Ab7-11774 SHOCK LAYER RADIATION DURING ENTRY - INSTRUMENTATION CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K NASA-CR-73027 Nbb-35663 DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS OF MARS Ab7-14309 SILVA, R. Re RADAR OBSERVATIONS OF VENUS AT 3.8 CM NOTING LOW HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR VALUE OF CROSS SECTION, ECHO SPECTRUM, WATER VAPOR PRESENCE, RESULTS INDICATE AMOUNT POLARIZATION CHARACTERISTICS, ABSORPTION CROSS DEPENDS ON SIZE OF POLAR CAP SECTION AN0 ATMOSPHERIC ATTENUATION JPL-TR-32-1048 Ab7-22235 167-16290 SPECTROSCOPTIC MEASUREMENTS OF WATER VAPOR AN0 SIROUNIAN. V. A. CARBON DIOXIDE CONTENTS IN MARS ATMOSPHERE 89 MARTIAN AN0 CYTHEREAN ATMOSPHERIC COMPOSITION Nbb-31474 DETERMINATIONS USING ENTRY PROBE MEASUREMENTS OF ULTRAVIOLET AN0 X-RAY ATTENUATION STANLEY. G. J. OAC- bob27 Nb7-33758 OBSERVATIONS OF MOON, VENUS, MARS, AN0 JUPITER - SURFACE FEATURES AN0 ATMOSPHERIC SMITH, 6. A. CHARACTERISTICS - RAOIOI RADAR, TELESCOPIC, AN0 RAPID DRIFT IN LONGITUDE OF SMALL DARK SPOT ON SPECTROSCOPIC OBSERVATIONS SOUTH EDGE OF JUPITER NORTH TEMPERATE BELT. NASA-CR-76142 Nb6-31446 NOTING SINUSOIDAL DISPLACEMENT CHARACTERISTICS AN0 MEASUREMENT WITH BLUE AN0 UV PHOTOGRAPHY STRANGE, M. G. Abb-33009 GASEOUS COMPOSITION OF UNKNOWN PLANETARY ATMOSPHERE DETERMINED. USING ACOUSTIC EXPERIMENT SMITH, H- J- COMBINED WITH PRESSURE AN0 TEMPERATURE DATA CARBON DIOXIDE ABUNDANCE AT 200 DEGREES K Ab7-13215 DETERMINED FROM HIGH DISPERSION IR SPECTROGRAMS OF MARS 167-14309 STRELKOV. G. Me RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN HIGH DISPERSION SPECTROGRAMS OF MARS EXAMINED FOR VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT WATER VAPOR PRESENCE, RESULTS INDICATE AMOUNT CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE DEPENDS ON SIZE OF POLAR CAP OF IR ABSORPTION Abb-40469 JPL-TR-32- 1046 Ab7-2 2 235 DISTRIBUTION OF RADIO BRIGHTNESS TEMPERATURE OVER UPPER LIMIT OF CARBON DIOXIDE ABUNDANCE IN DISK OF VENUS Ab7-27333 MERCURY ATMOSPHERE Ab7-41836 RADIANT ENERGY TRANSFER BELOW CLOUD COVER IN SOOEK, 6- A. VENUS ATMOSPHERE, NOTING GREENHOUSE EFFECT SCIENCE SUBSYSTEMS FOR JUPITER FLYBY MISSIONS, CAUSED BY ATMOSPHERE CONTAINING COMPONENTS CAPABLE DISCUSSING EQUIPMENT SELECTION. MISSION PLANNING, OF IR ABSORPTION Ab7-27659 SPACECRAFT DESIGN AN0 TRAJECTORY AN0 CONSTRAINTS ON VEHICLE CONFIGURATION ATMOSPHERIC MOOFL COMPARED WITH ASTRONOMICAL AIAA PAPER 67-120 Ab7-10287 OBSERVATIONS TO DETERMINE EFFECT OF CLOUD COVER AN0 RESULTING HIGH EFFECTIVE TEMPERATURE OF SOLBERG, H. G., JR. RADIO EMISSION FROM VENUS IN CENTIMETER RANGE p LATITUDE AN0 LONGITUDE OF JUPITER REO SPOT Nb7-16805 MEASURE0 FROM PHOTOGRAPHS OBTAINED DURING 1965 AN0 1966 STRONG, J- NASA-CR-05560 Nb7-31106 VENUS SURFACE TEMPERATURE FROM MICROWAVE MEASUREMENTS, NOTING THERMAL AN0 NONTHERMAL SOMERVILLE, W. 6. RADIATION Abb-28129 a MOLECULAR HYDROGEN STRUCTURE, CONSIDERING PLANETARY AN0 STELLAR ATMOSPHERES AN0 INTERSTELLAR STRONG. J- 0. SPACE A6b-39407 BALLOON-CARRIED AUTOMATIC TELESCOPE-SPECTROMETER OBSERVATION OF VENUS UPPER ATMOSPHERE AN0 DETERMINATION OF WATER VAPOR CONTENT

1-55 STUMPFe He Ja PERSONAL AUTHOR INDEX

Abb-30352 TEMPERATURE Abb-42668

DETERMINATION OF ICE CLOUDS AN0 WATER VAPOR IN INDUCED ABSORPTION COEFFICIENTS IN ATMOSPHERE VENUS ATMOSPHERE FROM BALLOON OBSERVATIONS MODEL MEASURED FOR CALCULATION OF VENUS LOWER Nbb-31463 ATMOSPHERE PROPERTIES FROM RADIO OBSERVATIONS Ab7-12949 *c DATA RECORDING AN0 REDUCTION OF WATER VAPOR CONTENT IN UPPER ATMOSPHERE OF VENUS AS THOMAS. 6. 8. DETERMINED BY BALLOON CARRIED AUTOMATIC STATISTICAL DECISION THEORY APPLIED TO MARTIAN TELESCOPE-SPECTROMETER UNIT Nbb-31488 ATMOSPHERE ANALYSIS, LIFE DETECTION EXPERIMENTSv AN0 GAS CHROMATOGRAM MEASUREMENTS OF N-ALKANE STUMPFv Hm J. DISTRIBUTIONS IN MATERIALS TOTAL EQUILIBRIUM SHOCK LAYER RADIATIVE HEAT NASA-03-77234 Nbb-34667 TRANSFER FOR ENTRY BODY CONFIGURATIONS IN SIMULATED MARS ATMOSPHERE Nb7-12 109 THOMAS, 6. M. MOLECULAR, CONTINUUM AN0 LINE RADIATION OF SWENSONI Be La PLANETARY ATMOSPHERES9 COMPARING MOLECULAR BAND PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS STRUCTURE MODELS WITH SPECTRAL MEASUREMENTS OF CN LANDING MISSIONI DISCUSSING USE OF LIFTING VIOLET BAN0 VEHICLES 166-25273 AIAA PAPER 67-323 667-26038 SYTINSKAYA, N- NI THOMAS. K- n. PHOTOMETRIC ANALYSIS OF AEROSOL COMPONENT OF MARS HIGH-TEMPERATURE GAS RADIANCE IN SIMULATED ATMOSPHERE Nb7-16810 PLANETARY ATMOSPHERE AT VARIOUS ENTRY VELOCITIES AIAA PAPER 66-183 Abb-25169

T THOMPSONs 6- A. TANG9 We RADIATION EQUILIBRIA IN UV LIGHT ON AIR, OXYGEN, MARTIAN ATMOSPHERE CIRCULATION MODEL FROM MARINER CARBON DIOXIDE, ETC, ANALYZEO BY BROMINE LAMP IN IV OCCULTATION EXPERIMENT, STUDYING LATERAL EDDY CONNECTION WITH STUDIES OF PLANETARY ATMOSPHERES VISCOSITY, WINOS. SURFACE TEMPERATURE AN0 STRESS Ab7-14088 Ab7-34153 INTERPRETATIONS OF MICROWAVE EMISSION FROM VENUS MODEL COMPUTATIONS OF TEMPERATURE VARIATIONS AND THROUGH EXPERIMENTS IN WHICH ANOMALOUS SIGNALS WINO CIRCULATIONS IN MARTIAN ATMOSPHERE HAVE BEEN OBSERVED IN X-BAND FROM GLOW DISCHARGES NASA-CR-85569 Nb7-30624 Ab7-14952

TANNHAEUSER. 1. THORNTON. De D. EARTH ATMOSPHERIC RADIATION SPECTRAL INFLUENCES ON MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF INFRARED MEASUREMENTS OF PLANETARY ATMOSPHERES VENUS COMPARED WITH SEVERAL MODEL ATMOSPHERES NASA-CR-84157 Nb7-26507 Ab7-24601 METHOD FOR CALCULATING INFRARED RADIATION FROM TINOLE. E, L. PLANETARY ATMOSPHERES PROBLEM OF OPERATIONAL FLEXIBILITY IN MARS BMWF-FB-W-67-02 Nb7-30793 LANDING MISSIONI DISCUSSING USE OF LIFTING VEHICLES Abb-25273 3 TARDIr Me SOLAR SYSTEM PLANETS CHARACTERISTICS, TITNANs Ce Ma TEMPERATURES, ATMOSPHERES AN0 INTERNAL EXPERIMENTAL METHOD FOR STUDYING TAYLOR COLUMNS STRUCTURE 167-28959 OVER HILLS AN0 HOLES IN JUPITER ATMOSPHERE Ab7-39000 TAYLOR% R. A. EARTH REENTRY SIMULATION OF PLANETARY ENTRY TITO. 01 A. ENVIRONMENT WITH EXPONENTIAL ATMOSPHERES OF MARS MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY AND VENUS TYPE MEASURING EFFECT ON RADIO OCCULTATION OF PLANET9 AIAA PAPER 65-218 Abb-27875 DETERMINING SHAPE. ATMOSPHERE DENSITY PROFILE, DIURNAL VARIATIONS. ETC Abb-25235 TEIFEL, '4- 6, IMAGE CONVERTER TUBE SPECTROPHOTOMETRY OF ZONAL MARINER VENUS 1967 SPACE PROBE, OBTAINING VARIATION OF METHANE ABSORPTION BANDS ON JOVIAN ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX DISK IN NEAR IR REGION Abb-37017 FROM RADIO SIGNAL FREQUENCYI INTENSITY AND PHASE CHANGES PHOTOMETRIC OBSERVATION DATA ON JUPITER AIAA PAPER 67-118 Ab7-18310 ATMOSPHERIC ACTIVITY /1964-19b5/ NOTING THREE- MONTH PERIODIC CHANGE Ab7-39299 MARS ATMOSPHERE AN0 IONOSPHERE ANALYZED BY MEASURING EFFECT ON RADIO OCCULTATION OF PLANET, TEPPER. N, DETERMINING SHAPES ATNOSPHERE DENSITY PROFILE, WEATHER CONDITIONS ON MARS AN0 RELATION TO DIURNAL VARIATIONS, ETC PROJECTED MANNED EXPLORATION Abb-30355 JPL-TR-32-1157 Ab7-26819

WEATHER FORECASTING FOR MANNED MARS LANDING BY MARINER VENUS 1967 SPACE PROBE? OBTAINING USE OF METEOROLOGICAL SATELLITE ATMOSPHERIC PRESSURE DENSITY AN0 REFRACTIVE INDEX Nbb-31491 FROM RADIO SIGNAL FREQUENCY, INTENSITY AND PHASE CHANGES N ASA METEOROLOGICAL FLIGHT PROGRAM PLANS. AIAA PAPER 67-118 Ab7-40094 PROCEDURES FOR PARTICIPATION IN SPACE FLIGHT PROGRAMS, AN0 REQUIREMENTS FOR METEOROLOGICAL TRAFTON~ L- n. RESEARCH ON MARS Nb7-24309 NONGRAY MDDEL ATMOSPHERES OF JOVIAN PLANETS CONSTRUCTED FOR DIFFERENT RELATIVE CONCENTRATIONS I( TEYFELI V- 6- OF HELIUM AND DIATOMIC HYDROGEN AN0 VARIOUS LIKELY ' SPECTROSCOPIC OBSERVATION AN0 SPECTRAL ANALYSIS OF EFFECTIVE TEMPERATURES AS CHIEF SOURCES OF THERMAL ASTRONOMICAL DATA ON PLANETARY ATMOSPHERE, LUNAR OPACITY Ab7-22237 SURFACE AND RADIO EMISSION NASA-TT-F-8881 Nbb-29398 TURNER. L. PROPERTIES OF MARS ATMOSPHERE ANALYZEO BY THADDEUSv P, EJECTED CAPSULE FROM SPACECRAFT, NOTING VENUS ATMOSPHERE NOTING PRESSURE INDUCED COMMUNICATIONS SYSTEM Abb-30556 ABSORPTION IN CARBON DIOXIDE-NITROGEN ATMOSPHERE AS INDICATED IN DECLINE OF MICROWAVE BRIGHTNESS

1-56 PERSONAL AUTHOR INDEX

DUE TO PRESENCE OF HYDROGEN CHLORIDE NASA-CR-84601 Nb7-28001

UENOv S. WELLER. Ce 5. * INITIAL VALUE APPROACH TO CHANORASEKHAR PLANETARY CARBON OIOXIOE IONS WITH ELECTRONS OISSOCIATIVE PROBLEM TO ESTIMATE PLANETARY PROPERTIES AN0 RECOMBINATION MEASUREMENTS WITH MICROWAVE- ATMOSPHERIC COVERS AFTERGLOW DIFFERENTIALLY PUMPED QUADRUPOLE MASS- RM-4991-PR Nbb-29959 SPECTROMETER APPARATUS. NOTING MARTIAN ATMOSPHERE MODEL INVARIANT IMBEOOING EQUATIONS FOR DETERMINING SRCC-55 Ab7-32826 ’ VERTICAL STRATIFICATION OF TERRESTRIAL Ah0 PLANETARY ATMOSPHERES ON BASIS OF SATELLITE WELLSv Rs A. OBSERVATIONS MARTIAN CLOUDS ANALYSIS AN0 TOPOGRAPHICAL RM-5229-PR Nb7-32463 RELATIONSHIPS9 DISCUSSING WHITE AN0 YELLOW CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES v Ab6-29951 VAKHNIN, V. M. MARTIAN TRANSIENT PHENOMENA CORRELATIONS AMONG UPPER ATMOSPHERE GLOW DISCHARGES STUDIED IN MASS MOTION OF WATER IN ATMOSPHERE. POLAR CAP CONNECTION WITH THERMAL RADIO NOISE EMISSION GROWTH AN0 WHITE CLOUD APPEARANCE FREQUENCY FROM VENUS SURFACE Nb6-38994 Ab7-24501

VAN ALLEN, J. A. MARTIAN CLOUDS ANALYSIS AN0 TOPOGRAPHICAL MARINER/ VENUS SPACE PROBE EXPERIMENT PROPOSED TO RELATIONSHIPS* DISCUSSING WHITE AN0 YELLOW MEASURE ECLIPSE OF SOLAR X-RAYS BY VENUSIAN CLASSIFICATION AN0 FREQUENCY OF OCCURRENCES ATMOSPHERE Nbb-27957 Ab7-34156

VETUKHNOVSKAIA, IU. N. MARTIAN CLOUD ANALYSIS AND TOPOGRAPHICAL TWO-LAYER MODEL OF VENUSIAN ATMOSPHERE SATISFYING RELATIONSHIPS RAOIOASTRONOMIC AN0 RADAR SELF-RAOIATION ESRO-SN-54 N6b-31187 MEASUREMENTS Ab7-32322 WEST. G. S- VETUKHNOVSKAYA. Y. N. MARS ATMOSPHERE MODELS AT THREE DENSITY LEVELS TWO-LAYER ATMOSPHERE MOOEL OF VENUS NASA-TM-X-53484 Nbb-31944 NASA-CR-88980 Nb7-38348 DERIVATION OF ATMOSPHERIC PARAMETERS FOR VEVERKA9 J. GREENHOUSE MODEL OF VENUS ATMOSPHERE MARTIAN ATMOSPHERE COMPONENT DUE TO PROTON NASA-TM-X-53497 Nb7-29983 PENETRATION INTO ATMOSPHERE FROM SOLAR WINO, 4 SUGGESTtNG RADIO OCCULTATION BY MARS ORBITER WEST. 6- SI. JR. Ab7-40799 MARTIAN ATMOSPHERE MODELS WITH DIFFERENT COMPOSITION^ PRESSURE AN0 TEMPERATURE COMPONENT OF MARS IONOSPHERE DUE TO SOLAR PROTONS Ab7-25685 NASA-CR-84411 Nb7-27370 ATMOSPHERE OF MARS STUDIED USING THREE MODELS VISHNIACg W. GENERATED TO SHOW HIGH, MEAN AN0 LOW DENSITY PLANETARY QUARANTINE CONSTRAINTS. NOTING COMPOSITIONS TO ACCOUNT FOR GRAVITATIONAL AN0 PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION MAGNETIC FIELDS Ab7-40140 Abb-29966 WESTPHAL. J. A. PLANETARY QUARANTINE CONSTRAINTS, NOTING LIMB DARKENING MEASUREMENTS OF VENUS AT 6-14 PREVENTION OF MARTIAN ATMOSPHERE CONTAMINATION MICRONS WITH 200 INCH HALE TELESCOPE 667-29098 Ab6-32517

WHITING, Ea E. MARS ATMOSPHERIC COMPOSITION OETERMINATION BY WACHNIN. We SHOCK LAYER RADIOMETRY TECHNIQUE DURING PROBE SURFACE TEMPERATURE OF VENUS Ab?-16029 EXPERIMENT AIAA PAPER 67-293 Ab7-26009 WALBAUMr Me JUPITER PLANETARY SURFACE OBSERVATIONS SHOW SLOW WILOEY. Re Le EVOLUTION OF ATMOSPHERIC PHENOMENA ION-MOLECULE CHEMISTRY OF JUPITER UPPER Abb-31310 ATMOSPHERE, STUDYING EQUILIBRIUM AN0 NONEQUILIBRIUM ABUNOANCES OF HYDROCARBON PRODUCTS WALDRON. R. W. DUE TO UV RADIATION REACTION Ab7-34540 RADIATION EQUILIBRIA IN UV LIGHT ON AIR. OXYGEN, CARBON DIOXIOEs ETC, ANALYZED BY BROMINE LAMP IN MILDTI R- CONNECTION WITH STUDIES OF PLANETARY ATMOSPHERES GREENHOUSE EFFECT IN GRAY PLANETARY ATMOSPHERE Ab7-14088 Ab 6-8 1145

WARREN9 We R.. JR. THEORY AN0 NUMERICAL PROCEDURE FOR DIGITAL EQUILIBRIUM RADIATION IN AIR AN0 GAS MIXTURES COMPUTER APPLICATION OF GREENHOUSE EFFECT FOR ASSUMED TO REPRESENT NEAR PLANET ATMOSPHERES PLANETARY ATMOSPHERE OF FINITE DEPTH NASA-CR-81315 N67-16722 RM-5076-PR Nb7-22562

WARWICK. J- W- WILHITEv Me F. NONTHERMAL RADIO EMISSION FROM JUPITER MICRO GAS CHROMATOGRAPHIC SYSTEM FOR MARS ATMOSPHERE, STUDYING IO MOOULATION EFFECT ATMOSPHERE ANALYSIS DURING CAPSULE DESCENT + A67-34933 666-27278

WELCH9 We J. GAS CHROMATOGRAPHY COLUMN PACKED WITH POROUS MICROWAVE SPECTRAL BRIGHTNESS MEASUREMENTS OF POLYMER BEADS FOR USE WITH MASS SPECTROMETER FOR VENUS COMPARED WITH SEVERAL MODEL ATMOSPHERES RESOLVING MARTIAN ATMOSPHERE COMPONENTS * A67-24601 Nb7-12128 UPPER LIMITS ON LIQUID WATER CONTENT IN VENUS MILLXAMSs 0. ATMOSPHERE Ab?-32652 SELF-BROAOENING COEFFICIENTS OF SPECTRAL LINES OF ABSORBING ATMOSPHERIC GASES MEASURE0 IN UPPER LIMITS ON LIQUID WATER IN VENUS ATMOSPHERE COMPARISON WITH LINE BROADENING EFFECTS OF

1-57 WILSON, K- H- PERSONAL AUTHOR INDEX

NITROGEN Abl-22715

WILSON. KI H. CONVECTIVE AN0 RADIATIVE HEAT TRANSFER TO SPACE VEHICLES ENTERING PLANETARY ATMOSPHERES AT SUPERORBITAL VELOCITIES NASA-CR-584 Nbb-37027

WINGROVE. R- C. FLIGHT DYNAMICS OF BALLISTIC AN0 LIFTING VEHICLE 7 ENTRIES INTO PLANETARY ATMOSPHERES OF MARS, EARTH, VENUS AN0 JUPITER Abl-20623

WOOOCOCK, 6. R. MANNED MARS EXCURSION VEHICLE FOR THIN MARS ATMOSPHERE NASA-TM-X-53475 Nbb-30788

WOOOWARDI He T- SHOCK LAYER RADIATION PREDICTIONS FROM MOLECULAR BAN0 SYSTEMS IN MARTIAN AN0 VENUSIAN ATMOSPHERES NASA-TN-0-3850 Nbl-11629 Y YABUSHITA, S- CYLINDRICAL FUNCTIONS FOR CALCULATING FREE OSCILLATIONS OF SATURN RINGS AN0 ESTIMATION OF UPPER LIMIT TO MASS OF RING IF MOTION IS STABLE AGAINST AXISYMMETRIC PERTURBATIONS 166-41063

YANIV, A. SURFACE AN0 ATMOSPHERIC PARAMETER MEASUREMENTS BY USE OF POLARIZATION INSTRUMENTATION ABOARD MARINER ORBITER SPACE PROBE Nb7-12666

YANOVITSKIII E- 6- BRIGHTNESS DISTRIBUTION OF MARTIAN DISK USE0 TO DETERMINE OPTICAL PARAMETERS OF ITS ATMOSPHERE AN0 SURFACE FROM ABSOLUTE PHOTOMETRIC DATA Nbb-33533

APPROXIMATION METHODS FOR SOLUTION OF EQUATION OF RADIATIVE TRANSFER IN PLANETARY ATMOSPHERES Nbb-33534

YANOVITSKIY. E. 6- DISCREPANCY BETWEEN MARS ATMOSPHERIC PRESSURE DATA FROM SPECTROSCOPIC MEASUREMENTS AN0 FROM PHOTOMETRIC AN0 POLARIMETRIC OBSERVATIONS Nbl-16811

SCATTERING ANISOTROPY EFFECT ON OPTICAL PARAMETERS OF MARTIAN ATMOSPHERE AN0 SURFACE - PHOTOMETRY Nb7-16820 YATSENKO. S- P. IONOSPHERE MODEL TO EXPLAIN SPECTRUM OF BRIGHTNESS TEMPERATURES FOUND IN RADIO EMISSION FROM VENUS ATMOSPHERE Nb7-lbB04

YEEI L. PLANETARY ATMOSPHERE STRUCTURE DETERMINE0 FROM ENTRY VEHICLE ONBOARO MEASUREMENTS OF PRESSURE, TEMPERATURE, AN0 ACLELERATION NASA-TN-0-3933 Nbl-23302 Z ZAPPA. 0. Le AERODYNAMIC. THERMODYNAMIC AN0 STRUCTURAL DESIGN ASPECTS OF FLIGHT CAPSULE ENTERING LOW DENSITY MARS ATMOSPHERE FROM ORBIT Abl-11432

ZIRKINO, R. BOUNOARIES AN0 ATTENUATING MEDIA EFFECT ON RADIOMETRIC SOUNDING OF PLANETARY ATMOSPHERES BY t REMOTE SENSING TECHNIQUES Abl-12406

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