Descriptions of Planetary and He1 Iocent R Ic Spacecraft and Investigations

Home , Modra (Bithynia), Pioneer 1, Pioneer 5, WR 30a

NATIONAL SPACE SCIENCE DATA CENTER WORLD DATA CENTER A for ROCKETS6 AND SATELLITES 88-07

DATA CATALOG SERIES FOR SPACE SCIENCE AND APPLICATIOINS FLIGHT MISSIONS

Volume 1A

Descriptions of Planetary and He1iocent r ic Spacecraft and Investigations

Second Edition March 1988 ~

CATEGORIES PACECRAFT USED FN THIS

PLANETARY AND HELIOCENTRIC

This category includes probes to the various planets of the solar system and probes designed to make measurements of the characteristics of interplanetary space. Also included are the probes that will pass out of the solar system into interstellar space. NSSDC/WDC-A-R&S 88-07

DATA CATALOG SE:RIES FOR SPACE SCIENCE AND APPLICATIONS FLIGHT MISSIONS

Volume 1A

DESCRIPTIONS OF P:LANETARY AND HELIOCENTRIC SPACECRAFT AND INVESTIGATIONS

Edited By

Winifred Sawtell Cameron Robert W. Vostreys

Second Edition March 1988

National Space Science Data Center (NSSDC) / World Data Center A for Rc'ckets and Satellites (WDC-A-R&S National Aeronautics and Space Administration Goddard Space Flight Center Greenbelt, Maryland 20771 PREFACE TO THE SECOND EDITION

The decision to reprint Volume 1A of the Data Catalog Series for Space Science and Applications Flight Missions was made primarily because it was no longer available when its companion, Volume lB, was completed in April 1987. Although Volume 1A was printed in September 1982, in this second edition no changes were made to the original text, since it described spacecraft and experiments as they actually were durin~qthe acquisition of the data in Volume 1B‘. The only significantarevisionmade in the second edition was the addition of Appendix E, which is an index showing the pages in Volume 1A where one can find descriptions of the spacecraft and experiments corresponding to the data sets described in Volume 1B.

The organization of Appendix E is the same as that of Volume 1B. Thus, Appendix E to this second edition is ordered alphabetically by NSSDC spacecraft common name. The associated investigations, arranged alphabetically by Principal Investigator’s last name, follow each spacecraft name. Because of the organization of Volume 1A by planets and disciplines, many descriptions are repeated. For example, the description of the Voyager 2 spacecraft appears on page 68 under Jupiter, on page 83 under Saturn, and on page 94 under Interplanetary Investigations. Appendix E gives only the number of the first page on which a given description can be found. Thus, only page 68 is given for the Voyager 2 spacecraft. The index added to this edition should allow users to work smoothly from the organization of Volume 1B to that of Volume 1A. The second edition was prepared by employees of the on-site contractor, Science Applications Research (SAR).

March 1988 John E. Jackson

iii PREFACE TO THE FIRST EDITION

This volume, Brief Descriptions of Planetary and Heliocentric Spacecraft and Investigations, part of the Data Catalog Series for Space Science and Applications Flight Missions, represents the work of many people. The series will describe the data sets held by NSSDC, some of the data sets held by NASA-funded investigators, and some of the data sets held by foreign investigators; and the series will serve as pointer doc:uments for extensive data sets held and serviced by other government agencies. We would like to thank the many spacecraft and experiment personnel who over the years provided much of the information contained in this volume. The cooperation of the investigators in supplying current status information is gratefully acknowledged. Thanks also are extended to the other NSSDC personnel, employees of the on-site contractor, M/A-COM Sigma Data, Inc., who have been involved in the information handling necessary to produce this volume. Special acknowledgment is given to Mary Elsen for her extensive editorial assistance and to the File Management group, supervised by Dorothy Rosenblatt, for their special computer processing to accommodate the format of this volume.

The Data Center is continually striving to increase the usefulness of its data holdingsfsupporting indexes, and documentation. Scientists are invited to submit their space science data and comments to NSSDC. Catalog recipients are urged to inform potential data users of its availability.

September 1982 Winifred Sawtell Cameron Robert W. Vostreys TABLE OF CONTENTS

PREFACE TO THE SECOND EDITION ...... iii

PREFACE TO THE FIRST EDITION ...... v

INTRODUCTION ...... 1 1.1 Purpose ...... 3 1.2 Organization...... 5 1.3 NSSDC Purpose, Facilities, and Services ...... 7 1.4 Data Acquisit.ion...... 8

MERCURY ...... 13

VENUS ...... 21

MARS ...... 41

JUPITER ...... 61

SATURN ...... 77

INTERPLANETARY INVESTIGATIONS ...... 99

TABLES Table 1. Status of Data Available from Planetary and Interplanetary Missions ...... 9

Table 2. Planetary Missions, by Category of Data Available at NSSDC ...... 11 Table 3. U.S. Lunar Mission Data ...... 117

APPEND I XES A. Index to Planetary Investigations with Data Available at NSSDC ...... A-1

B. Index to Interplanetary Investigations (from Planetary Missions) with Data Available at NSSDC ...... B-1

C. Index to Interplanetary Missions with Data Available at NSSDC ...... C-1

D. Definitions ...... D-1

E. Index of Spacecraft and Investigations by Spacecraft Name and Principal Investigator ...... E-1

vii Introduction 1.1 PURPOSE

The National Space Science Data Center (NSSDC) was established by the National Aeronautics and Space Administration (NASA) to provide data and information from space science and applications flight investigations in support of additional studies beyond those performed as the principal part of any flight mission. This volume is one of a series of eleven that will describe (1) the holdings of all spacecraft flight investigations for which NSSDC possesses data or can direct people to the data source,.(2) all data sets held by NSSDC, (3) some of the data sets held and serviced by NASA-funded investigators, and (4) some of the data sets held and serviced by foreign investigators: and the series will serve as pointer documents for extensive data sets held and serviced by other government agencies, particularly the National Oceanographic and Atmospheric Administration (NOAA). There is one major omission from this series: the extensive set of data obtained from the lunar missions conducted by NASA, supplemented by a few small photographic data sets from Soviet missions. These are described in the Catalog of Lunar ?Lssion Data (NSSDC/WDC-A-R&S 77-02) and will not be repeated in this series, except for a few cases. The data from IMP-E, Apollo 15 subsatellite, and Apollo 16 subsatellite are included in the series, since these data are important to disciplines other than those connected with lunar studies. Some of the experiments of the Apollo ALSEP missions also yielded useful data for magnetospheric and interplanetary physics, but these are not included in the series, since the instruments were confined to the surface of the moon. Readers should consult the Catalog of Lunar Mission Data if they are interested in such data sets.

The series consists of (1) five volumes that describe the spacecraft and their associated investigations (experiments) separated, mainly, into various orbit categories, (2) five corresponding volumes that describe the various orbital information and investigation data sets, and (3) a master index volume. In some cases certain data sets appear in more than one data set volume, since they are important to a discipline not normally related to most of the investigations on a given spacecraft. The five categories of spacecraft are (i) Planetary and Heliocentric, which include planetary flybys and probes, (ii) Meteorology and Terrestrial Applications, (iii) Astronomy, Astrophysics, and Solar Physics, which are all geocentric except the selenocentric RAE-B, (iv) Geostationary and High-Altitude Scientific, and (VI Low- and Medium-Altitude Scientific. It is impossible to provide an organization of categories that separates the investigations cleanly into scientific disciplines, since many missions were multidisciplinary.

Each volume is organized in a way that is believed to be most useful to the user and is described for each such volume in the Organization Section. For standard types of orbital information, i.e., predicted, refined, and definitive, the information is given in a tabular form to avoid repeating the same brief description an inordinate number of times. The standard description of a data set from an investigation is a free text brief description, since the wide variety of instruments precludes using a tabular format in most cases.

3 This catalog series has been prepared following a two-year survey and follow-up activity by NSSDC personnel to obtain information about the completeness of the NSSDC holdings and to solicit the description of data sets that will be serviced by individual investigators; these latter data sets are referred to as directory data sets. This survey was conducted only for NASA missions launched after December 31, 1962, but it includes the majority of NSSDC holdings. Unfortunately, of the 100 investigators surveyed, representing 346 inactive (no longer associated with an active science working team or equivalent) experiments, a small percentage failed to respond in 17 months of concerted solicitation of information. Consequently, there are now 20 investigations for which NSSDC has no data that will be dropped from this catalog series, since it would be irresponsible for NSSDC to send requesters to a possible data source that no longer has data or is non-responsive. The investigations that are being dropped from the NSSDC catalogs are identified in the appropriate volumes in the series. A small, but non-trivial, number of investigations were identified for which data no longer exist or for which the instrument failed at launch. These investigations are included in the spacecraft/investigation volumes so that users will know that it is fruitless to try to obtain such data anywhere.

The main pur,pose of this series is to identify the data and the contact from whom the data can be obtained within the scope previously defined. In addition, we have tried to identify the personnel involved with the investigation, so that a user will know whom to contact for an obscure or detailed piece of information relative to a given data set that NSSDC may not possess. Consequently, we have tried to provide the current affiliation of the investigators. In some cases we know that people have retired or have gone into different areas of endeavor. The latter case is treated by showing the last affiliation of such an individual and denoting that he is no longer affiliated by printing NLA after the individual's name. Since this series is oriented toward helping interested persons to obtain data from flight investigations and helping NSSDC to serve as an effective switching center, the spacecraft/mission personnel are identified at the institution where they performed their relevant duties. The term NLA is printed with the names of these personnel if they are no longer associated with the given institution.

It is hoped that this series will serve for many years as the source documents for data in the disciplines that NSSDC handles. The annual NSSDC Data Listing will be used to update the time intervals for which data are available and to identify in brief form the new data sets that become available in the future. The annual Report of Active and Planned Spacecraft and Experiments will be used to describe the new spacecraft and experiments which are placed in orbit.

4 1 2 ORGANIZATION

This catalog contains descriptions of the planetary and heliocentric spacecraft launched for which NSSDC has information. Described for those spacecraft are the investigations for which NSSDC has archived data.

The catalog is organized by planet, out from the sun, and then by heliocentric missions that collected interplanetary data. Included are the Pioneers 10 and 11 spacecraft which are on trajectories to take them out of the solar system. A description of missions to the moon, with descriptions of the spacecraft, experiments, and data archived is contained in the Catalog of Lunar Missions Data (NSSDC/WDC-A-R&S 77-02) and is not repeated here. It was not possible to obtain information from the following investigations on the availability of data and they are not included in the catalog.

Spacecraft NSSDC ID Investigation Name Principal Investigator

Mariner 4 64-077A-03 Faraday Cup H. S. Bridge 64-077A-08 S-Band Occultation A. J. Kliore 64-077A-05 Cosmic Ray Protons and Electrons Van Allen Pioneer 7 66-075A-07 Celestial Mechanics Anderson Mariner 5 67-060A-01 S-Band Occultation Kliore 67-060A-04 Trapped Radiation Detector Van Allen Pioneer 8 67-12324-08 Celestial Mechanics Anderson Pioneer 9 68-l00A-08 Celestial Mechanics Anderson Pioneer 10 72-012A-08 Infrared Radiometer Inger so 11 Pioneer 11 73-019A-08 Infrared Radiometer Inge rso 11

The format for the experiments has been ordered by categories generally in order of the number of investigations. The categories discussed are (1) Imaging, (2) Particles and Fields, (3) Ultraviolet, (4) Infrared, (5) Radio Science and Celestial Mechanics, (6) Atmospheres, (7) Surface Chemistry, (8) Biology, and (9) Polarization.

Only investigations with some data either available from NSSDC or where the source of data is known are discussed. Table 1, however, lists all the experiments that were aboard the various spacecraft and indicates the status (all or partial, no data, or failed) of the data. Since NSSDC has only a few photographs from the U.S.S.R. -- Veneras 9, 10, 13, and 14 -- and no other data, only these investigations will be presented and included in Table 1; Table 2 contains planetary missions with planetary investigations listed by categories of data that are available at NSSDC. For complete coverage of the solar system, and for reference, Table 3 (from the Catalog of Lunar Missions), similar to Table 1, except that it covers lunar missions, is presented at the end of this catalog. Appendix A is an index to planetary missions, Appendix B is an index to missions that were primarily planetary but had investigations that only collected interplanetary data in the cruise mode, and Appendix C

5 contains an index to missions whose investigations were designed to collect only interplanetary data. Appendix D contains definitions for terms and acronyms that may not be readily recognized by the users of this document. In Table 1 there are many similar investigations with similar names, but they are listed separately in order to indicate status of availability of data. Under Radio Science and Celestial Mechanics, for example, there is only one investigation named Radio Occultation, yet occultation data were obtained at all the planets. These will be identified in Volume lB, which is a companion volume describing the data sets obtained by the experiments described in this volume. It should be pointed out that many of the investigations obtained data from the interplanetary region, particularly in the particles and fields category.

6 1.3 NSSDC PURPOSE, FACILITIES, AND SERVICES

Virtually all the data available at or through NSSDC result from individual experiments carried on hoard individual spacecraft. The Data Center has developed an information system utilizing a spacecraft/investigation/data identification hierarchy. This catalog is based on that information system.

NSSDC provides facilities for reproduction of data and for onsite data use. Resident and visiting researchers are invited to study the data while at the Data Center. The Data Center staff will assist users with additional data searches and with the use of equipment. In addition to spacecraft data, the Data Center maintains some supporting information and other supporting data that may be related to the needs of the researchers.

The Data Center's address for information (for U.S. researchers) follows:

National Space Science Data Center Code 601.4 Goddard Space Flight Center Greenbelt, Maryland 20771 Telephone: (301) 344-6695 Telex No.: 89675 TWX No.: 7108289716

Researchers who reside outside the U.S. should direct requests for information to the following address:

World Data Center A for Rockets and Satellites Code 601 Goddard Space Flight Center Greenbelt, Maryland 20771 U.S.A. Telephone: (301) 344-6695 Telex No.: 89675 TWX NO.: 7108289716

7 1.4 DATA ACQUISITION

NSSDC invites members of the scientific community involved in spaceflight investigations to submit data to the Data Center or to provide information about the data sets that they prefer to handle directly. The Data Center assigns a discipline specialist to work with each investigator or science working team to determine the forms of data that are likely to be most useful to the community of users that obtain data from NSSDC. The pamphlet Guidelines for Submitting Data to the National Space Science Data Center can be provided on request.

8 h 2 0 .r( c,a hfl .H c,m a,> c U % zE I un m mz W

4 U m a C 4

EU E L W I v) 9-I 5 3 a B 2 E h In H Table 2

planetary Missions, by Category of Data Available at NSSDC

INVESTIGATION CATEGORY PLANET MISSIONS CATEGORY PLANET MISSIONS I IMAGING MARINER 10 I INFRARED MERCURY MARINER 10 MARINER 10 VENUS MARINER 2 PIONEER VENUS I-ORBITER MARINER 10 VENERA 9 PIONEER VENUS ORBITER VENERA 10 PIONEER VENUS LARGE VENERA 13 PIONEER VENUS SMALL 1 VENERA 14 PIONEER VENUS SMALL 2 rMARINER 4 PIONEER VENUS SMALL 3 UARINER 6 MARINER 6 MARINER 7 MARINER 7 MARINER 9 MARINER 9 VIKING I-ORBITER VIKING I-ORBITER VIKING 2-ORBITER VIKING 2-ORBITER VIKING 1-m~~ VOYAGER 1 PVIKING 2-LANDER VOYAGER 2 PIONEER 10 PIONEER 11 RADIO SCIENCE 6 MERCURY MARINER 10 VOYAGER 1 MARINER 2 VOYAGER 2 MARINER 5 PIONEER 11 MARINER 10 VOYAGER 1 PIONEER VENUS 1-ORBITER VOYAGER 2 PIONEER VENUS 2-BUS PIONEER VENUS-LARGE lURIlRR 10 PIONEER VENUS-SMALL 1 UAJUNER 2 PIONEER VENUS-SMALL 2 MARINER 5 PIONEER VENUS-SMALL 3 MARINER 10 MAPS MARINER 4 PIONEER VENUS I-ORBITER MARINER 6 PIONnR "US 2-BUS MARINER 7 MARINER 4 MARINER 9 VIKING 1-ORBITER PIONEER 10 VIKING 2-ORBITER PIONELR 11 VIKING 1-LANDER VOYAGER 1 JUPITER PIONEER 11 VOYAGER 1 ULTRAVIOLIT UERCURY MRINER 10 VIMlS MARINER 10 SATURN :ONEEX "US 1-ORBITER ATMOSPHERE VENUS PIONEER VENUS 1-ORBITER rRINER 6 PIONEER VENUS 2-BUS rRINER 7 PIONEER VENUS LARGE UARINER 9 PIONEER VENUS-SMALL 1 JUPITER PIONEER 10 PIONEER VENUS-SMALL 2 PIONEER 11 PIONEER VENUS-SMALL 3 VOYAGER 1 VIKING 1-ORBITER VOYAGER 2 VIKING 2-ORBITER VIKING 1-LANDER 1 VIKING 2-LANDER

PIONEER 11 SATURN PIONEER 11 + SURFACE CHEMISTRY VIKING 1-LANDER VIKING 2-LANDER

VIKING I-LANDER 7VIKING 2-LANDEH Mercury

13 MERCURY

Plate 1. This is a collection of press release photographs of various aspects of the planet Mercury from the Mariner 10 mission, the only mission to go to Mercury. It was the first mission to use the gravitational assist from one planet (Venus) to go on to another planet (Mercury). (A) P14470 is a mosaic of medium-resolution images presenting the hemisphere of Mercury seen by the spacecraft on the incoming trajectory on the first encounter of the flyby. It shows the lunar highlands-like nature of Mercury. (B) P14580 is a mosaic of medium-resolution images of the hemisphere of Mercury seen by the spacecraft on its outgoing trajectory on the first encounter. It shows some smooth areas. The spacecraft later had two more encounters, each spaced 6 months apart. (C) P14469 is a high-resolution (about 100m) photo showing a two-level flow in a large crater. (D) P15046 is a high-resolution (about 100m) image showing some of the long ridges traversing all topography which are apparently unique to Mercury among the planets.

14 @!?!CINAC PAGE BLACK AhD '4v'i-iIl.E i'i-iO TOCRAPh INTRODUCTION

It was felt that the presentation of investigations in categories and by planets would be most useful to the scientific community. In this way, a possible user of data could determine quickly and easily the data that have been gathered at each planet. This information can be obtained most quickly by consulting Table 1 for all investigations and their status in regard to data archived at NSSDC from planetary and interplanetary missions, Table 2 for general categories at each planet, and Appendix A for details.

The first planet to be covered in this catalog is Mercury. There has been Only one mission to Mercury, namely Mariner 10. There were, however, three passes (encounters) past the planet. In the second part of this catalog, which contains discussions of the data sets pertaining to the investigations on Mariner 10 that covered Mercury, the data sets will be presented according to encounter. There were seven investigations for which NSSDC either has the data archived or knows the source of the archived data; these investigations fall under five categories: (1 ) Imaging, (2) Particles and Fields, (31 Ultraviolet, (4) Infrared, and (5) Radio Science and Celestial Mechanics, and they are presented in that order. All investigations that dealt with a category are discussed under that category.

Following the planetary investigations sections for the planets, those planetary missions that carried the interplanetary region investigations are presented. Appendix B indexes this section. This section, in turn, is followed by the interplanetary missions whose investigations collected only interplanetary data. These missions all had heliocentric orbits. Appendix C indexes this section in detail.

17 s*tellttts. lhr =Quiplent consisted of two spherical 1150 II~ diameter) Casaeirain t~liscoptswith right filters, attached to 6EC 1-inch vidicon tube Cameras (1500 length and 0.5 SPACECRAFI COMMON NlIE- MARINER 10 111 focal flcld of vier) for narrow-anqlc c,hotooraohv. An auxiliary ALTERNATE NAMES- MARINER 73, PL-732A deg Optical lyatem mounted on each ;amera provided wide-angle (62 MARINER-J VENUSIMERCURYr MARINER VENUSIMERCURI 7 6919 Im focal length and 11 x 14 dcg firld of view) photography by moving a mirror On a filter "heel to a position in the optical cath. Exposure time ranocd from 3 IS to 17 s. an.+ --rh ~ ~ *--era NSSDC ID- 73-0851 .. __ _. _-... ._I.. took a DictUrC ewrl 42s.- The Tv Picture consisted of 700 scan lines with 832 Picture eltnentrlline, uhlch ucre aioitally LlUNCH DATE- 11103173 WEfGHl- 504. KG coded into 6-bit words for transmission. lhere ~.were~ eight-- LAUNCH SITE- CAPL CANAVERAL, UNIlEO SlATES LAUNCH VEHICLE- ATLAS filter wheel cositions: (11 rrdr-angle image relay mirror. (2) blue bmdoassr 13) UV oolarizingr (+I ~I~YIUV high pass, (5) ClCalr (6) UW bandpa%%*(71 deforusinu lrn~(tar r-lih.srinqJ, SPONSORING COUNlRYIlGfNCV ~~ . -. .". and (8) yellor bandpars. About 7000 DhOtDgraphs were Obtained UNITED STATES NASA-OSSA of Venus and MCrCUryr with a aelinum resolution of 100 m for MCrcUrY. Three photog.aPhic SS~arated by 6-month INITIAL ORB11 PARAMflERS DaSSCfr intervals, YIIC milac for Mercury. Further details of the ORB11 TYPE- MERCURY FLYBY exp~ri~entCIP be obtained from NSSDC 75-lU. and IC~TYIIV. 15. n. 2, OCtOhCr 1971. Science results on Mcrculv ma1 h- nht-ioed PERSONNEL .. , ., - - - - .- . . 1. GCODh?l. Res., V. 80. p. 17, June 1975, and on Venus in PM Y.E. GIBERSON from - NASA-JPL Science, Y. lU31 P. 4131, March 1914. PS - J .A. DUNNE NASA-JPL BRIEF DESCRIPTION lhir spacecraft was the first to YIC the gravitational PARTICLES AND FIELDS Pull Of 0°C planet (Venus) to reach another (MCrCury). lhe 1PacCII.ft StruCtbre ua* ar, 18.15-kg (40 lb)r eight-sioed framework with eight electronics ~onp.~t*cnt~. IC .C.SUTC~ 1.39 diagonallr and 0.457 m in deeth. 110 solar panel^, each -----__MARINER 10, BRIDGE------2.7 . long and (-97 . ride. bere attached at the top, supporting 5.1 sa I of solar cell area. The rocket engine I~I liquid-fueled, with two sets of reaction jets used to stabilize INVESTIGATION NAME- MEASUREMEN1 OF PLASMA ENVIRONMENT the SPacCCraft on three axes. It carried a Lou-gain Osnidi~ectinnalantenna, COIPOIC~ of a honeycomb-dirk parab~lit NSSDC IO- 73-08%-03 INVESTlGATIVE PROGRAM reflector. 1.37 in diameterr rith focal length 55 cm. reeds CODE EL-4. SCIINCE enabled the spacecraft to transmit at S-band and a-band frequcnricl. The aparrrraft carried a C."ODUS star tracker, INVESTIGAllON OISCIPLINE(S) located On the UPLC~ring ftrultur~cf the Octag0ral satelliter PARTICLES AND FIELDS and acquisition sun on the tips of the solar panels. sensors PERSONNEL The interior of the SParrCraft was insulated with wlti1ay.r P1 H.S. BRIDGE thermal blankets It COD and bOttCr. A sunshade was declayed - MISS INS1 OF lECH after launch to Protect the SDactrraft on the rolar-orien1rd 01 - J.M. BINSACK MASS INST OF TECH side. Inltrumcnts aboard the spacecraft measured the 01 - A.J. LAZARUS MASS INS1 OF. 1FCH.. 01 5. OLBfRT atmosphcric~ surfacer and physical chbract.ristics of Mercury - MASS INS1 OF TECH md Venus. Eweriicnts intludea television photograpt.y. 01 - S.J. BARE LOS ALAMOS SC1 LAB 01 (1.0. MONTGOIIERY magnetic field, plasma, infrared radiometry. ultraviolet - LOS ALAMOS SC1 LAB SPectrOScODY~ and radio Icicncc detectors. An rrprrimcntal 01 - A.J. HUNDHAUSEN NATL ClR FOR AlllOS RES 01 J.R. ASBRIDGE X-band. high-frequercy transmitter bas flown for the first t7.e - LOS ALAMOS SCI LAB 01 K... DGILYIL on this SPOCCIC*ft. Mariner 10 111 pla~~din a parking ort,it - NASA-LSFC 01 L.F. BURLAGA after launch for aPproximatrLr 25 ninr then pla~edin Orbit - NASA-GSFC around the sun enroute to Venus. The Orbit direction was 01 R.E. HARlLE NASA-GhFC 01 C.W. SNVDER Cepolite to the motion of the earth around the sur. nid-course - NASA-JPL 01 G.L. SISCOf corrections were made. The spacccrift Pasled Venus on Fehruary - U OF CALlFr LA 5. 197qr at 1 distance Of 4200 k.. It CroilCd the Orbit at BRIEF OESCRIPllON krcurr on March 29. 1974, at 2046 UTI a1 a distance of about lht cxptrimcnt 1.5 designed to determine the mode of 7Cq k. from the surface. The 1V and UV *Xperi.rntS turreo WCIC interaction the planet Mercu,~ and the solar wind, to on the Comet Kohoutek while the ~p.~e~~.ftwas on the way to Letreen a conorehcnrivc study of the plasma regime at MCICUIY~ to Venus. A second encounter with MC~CUIYI rhcn nore photographs make verify ana previous Observations of the soiar wind Yere taken. occurred SeptCrbCr 21. 1974. at an altitude of extend on Interaction with Venus. to clarify the role at electvons in the about 4lr000 km. A third and last MC~CUI))encounter et an interaction.. and to study the solar rind from 1 to 0.. AU. altitude of 327 kmr rith additional photography of about 300 Instrueentation far the ~.p~riment consisted of two photOgraPhc and aagnctic field neasureltnts occurred on March sunuard-facing tlCctIOltatiC analyzcrr ISESA) and One backlard 161 1975. Enginerring tests were continued urtil march 2q. faring electron spCctrOmtter IBESA). lhese three detectors 1975. "hen the of attitude-control was depleted and SUDPLY 4.1 were mounted a scanning DLatfOlmr which could be swept at 1 the mission was terminated. On drgfi through an arc of 120 dcg centered on a direction in the rcliptic Plane 6 de9 east of the SPacCIraft-sUn line. Both SESlr failed to return data. They were to measure positive INVESTIGATIONS ions from 0.08 to 8 ktv cltrtronr from 4 to 400 CV. ihe IMAGING and BESA had a fan-shaped field of view of plus or minus 3.5 dcg by PLUS or minus 13.5 dcg. lhc larger angle was normal to, and symmetric about. the scan arc. An electron IDCT~IY~ war - - MARINE@ 10, MURRAY------obtained LYCIY 6 13 and ~Onsiit~dOf tlux meesur~rn~nfsin 15 - - - - - Logarith*irmlL), Isaced cnrrs.7 channels (rich channel width delta EIE=L.LI) within the cncryr range 13.4 to 690 cV. INVESllGATlON NAME- TELEV~SIONPHOTOGRAPHV Because solar wind flou past the s~dcecraftintroducer angular distortion of the electron distribution function ~omparedto NSSDC ID- 73-08%-01 INVESTIGATIVE PROGRAM what rould be ObiePved in the solar rind rest frame, it 1.3 CODE EL-4r SCIENCE POssiblC~ by taking info aCCOunt this distortion and the ID~CCC~=~~sheath characteristics, to derive some ot the solar lNVESTIGATION OlSCIPLINE(S) rind P1.S.a Par*ICtCrI such as ion bulk speed, tlrctron PLANETARY A~MOSPHERES tCmpelatUrC. and electron density. The reliability of these PLINElCLOGY ParamFtCrs is nccrrrarily dependent on the validity Of the spacecraft sheath model emDtOyed in the analysirr is thus PfRSONNEL and affected by time changer in the ambient solar wind. PI - B-C. MURRAY CALIF INST OF TECH 01 - M.J.S.BEL1ON KIll PEAK NATL ORs - - -_- -- MARl)ifR 10, NESS------01 - G.P. KUIPER(OfCEASf0) U OF ARIZONA 01 V.P. SUOPlI - ~~.. U OF YISCONSIN INVESlIGAlION NAML- FLUXGATE MAGNE1O)IElLRS 01 - N.J. TRASK, JR. US GEOLOGICAL SURwEi 01 D.E. GAULT - NASA-ARC NSSDC ID- 73-08511-04 01 B.Y. HAPKE INVESTIGAllWE PROGRAM - U OF PlTlSBURGH CODE EL-4. SCIENCE 01 - M.E. DAVlES RAND CORP 01 8.1. O'LEAIIl PRlNCtTON - U 1NVESllGAllON DISCIPLINE (S 1 BRIEF DESCRIPTION PARTICLES AND FIELDS The objectives Of this crperi.ent were to photograch the PLANtTOLOGY surfacer (upper atmosphere in the case of vrnus) of the planets Venus and Mercury. For Venus, the ob~rrtiver were to investigate the time-dependent pr~perti~~of the uv c10uas~and to obtain high-resolution imagery at the main clouds. FO~ Mercury. the objectives were to map its major phyliographic prorinccs- determine its spin axis orientation, ~itablisha cartograohic coorcinate systklr and Iearch for Mcrrurian

19 PERSONNEL uv flu. to the sp.ct.O..t.r. tu0 zero-order rnannels were PI -N.f. NESS NASA-6Sf C florn. The effective field of vier of the instrum*nt mas 0.13 01 - K.Y. BEHANNON NASA-LSFC dcg by 3.6 deg. 1101- e.perlmrnt details and some m.asur.ments 01 - R.P. LEPPING NASA-CSfC arr containem in tuo papars: (1) 'Ultraviolet 0bs.wations of 01 - Y.C. YHANG CATHOLIC U Of AMERICA Ytnus from Mariner IO -- Pveliminary Reswlts.' A. L. B.o.dfoot. et 11.. science. I. 183. March 29. 1914. and (2) -Mercury's BRIEF DESCRIPllON AtmOsph*re from Mariner 10 -Preliminary Results.' A. L. This experiment consisted of ti0 tria.i.1 flux9.te BrO.dfOOt. et .I.. srimcr. (I. 1b51 July 12. i91+. A magnetomrt~rsmounted on a common boo. 2.3 a and 5.8 from the description of the inrtrument'tion Is prrcn in two later spare~raftand designed to measwe the vector *agnetiL field in papers: (1) 'M.rincr 10 Ultraiiolet So.ctrO-et*r: Airglow the vicinity of Mercury and Venbs and in the interplanetary Experiment,' A. L. Broadfoot. 5. 5. Clapp and F. E. Stuart. medium. outputs fro. the two magnetoacterr wcrc simultaneously Svace Sri. lnstr. I. 3. 199 (1911); (2) -Marine, 10 Ultr.violet analyzed to sepalate ambient fields fro. spac.craft fields. Spectromster: Occultation Experiment#- A. L. Broadfoot. 5. S. Each Sensor had Cu.1 operating ranges Of minus 10 PLUS 16 nl Clapp and F. E. Stuart. Space Sci. Instr. v. 31 P. 209 (1911). and 128 nTr with digitization acc~raci~fof 0.03 nT and 0.26 Data also include the interplanetary region. nT. respe~ti~ely.Bias offset Capability extended thr Operating range to minus or PIUS3188 nT. During the priaary phase of the mission (Novr*ter 3. 1913, tC Parch 29. 1974) and during the Second and third MeICurY enrountersr 25 vtCtOrS PtI ICCand INFRARED "ere sampled by the primary outboard magnetometer and transmitted to Earth. At Other 1i.e.r a lorcr data rate mode was used during which fire YectOis &e, second utle transmitted. The eweri.ent functioned noraally throughout the life of the spacecraft. For further details. see N. F. NESS et al.. Science, Y. 183. P. 1301. - - -_-- - MARINER 10, SIMPSO*----'------

IhVESlIGATION NAME- ENERGETIC PARIICLES

NSSDC ID- 13-085A-01 INVESTIGATIVE PROGRAM CODE EL-4. SCIENCE

INVESTIGATION DISCIPLINEIS) PERSONNEL PARTICLES AND FIELDS PI - S.C. CHASE. JR. SAW1 BARBARA RES CTR 01 - E.D. MINER NASA-JPL PERSONNEL 01 - 0. MORRISON U Of HAUL11 PI - 1.1. SIMPSCN U OF CHICAGO 01~ - 6.~. MUNCH MPI-HEIDELBERG. ~.~-~~ . 01 - J.E. LAMPORT U OF CHICAGO 01 - 6. NEUGEBAUER CALIF INST OF TECH 01 - J.M. SAARI(DECEASE0) BOElN6 SCI RES LAB BRIEF OESCRIPTION This erpcrinent "as disiprtd to .easLre energetic BRIEF DESCRIPTION CIC~~VD~S~piotons~ and alpha piititleI In the interplanetary An infrared radiometrr having two channels, 22 to 39 medium and in the wl=inificr 01 Yenus and Mercury. The .iLIO.Cters 180 X to 500 I1 .nd IO to 17 mScrO.e1e11 (200 K to initiumtntetion co~sistedof a main telescope and lor-energy 650 I).was used to Observe the therm.1 emission fro. venur and t.lescOpi. The main teleliope ronsisted of si. colinear Mercury in two broad spectral bands. The 111 thermal emission IC~SOIS (five silicon detectors and One Cs1 scintillator) fvom the surface Of Mercury between late afternoon and early surrounded by a plastic scintillator anticoincidence CUP. One morning (local ti..) and deviations fro. the average thermal culse height an.lisil "as performed every 0.33 SI and counts behavior of the surface were measured. Measurements w.re also arrunulatcd in each coin~idcnrrl.nti~oin~id~n~~mode were made of the brightness temperaturCs of Venusian cloud tops and measured every 0.6 I. Particles stcpping in the first sensor Limb darkening PhCnO.Cn.. Attempts were made to correlate were protons and alpha particles in the range 0.62-10.3 unusual tLmDeratUIe Yariationl "4th photographs and II.v/nuclion and electrons above ~c~lOli.~t~ly170 Lev. The measureaents by Other instruments to identify mountains. acerture half angle for this .Ode "as 41 degr and the ge0mctriC W~ILCYS.v~lcmoei, and unusual surface materials. factors were 14 sq cm Iter for electrons and 7.4 sq cm st~rfor protcns and alpha PII~~CLCI. The telescope .p~rt~r*hmlf angle decreased to 32 dtg for coincident counts in the first and third sens~rs. The lor-energy teICsCOpt~a two-rlenent (plus RADIO SCIENCE AND CELESTIAL MECHANlCS anticoinridrnrs) detector with a 38-6.. half angle aperture and a 0.49 sq CI stel gromrtrical tarter. 1.1 desigled to measure 0.55-1.9 and 1.9-8.9 MeV plDtOnl iithout responding tO electrons over 1 "id- range of electron energies and intensities. See 1. GCOPhYS. ICs.* 1- 80- 0. 4018 and rrfrrcnrri therein for further details. INUESTlbAlION NAME- S- AND I-BAND RADIO PROPACATION

NSSDC ID- 15-0851-02 INVESTlGATIVE PROGRAM CODE EL-4. SCIENCE ULTRAVIOLET INVESTI6ATlON DISCIPLINE(S) IONOSPHERES AND RADIO PHVSICS PARTICLES AND FIELDS - - -_- - - *ARlNER 10, BROADFOOT------PLANETARY ATPOSPHERES

lNVESllGATION NAME- EUV SPECTROSCOPT PERSONNEL PI - H.T. HOYARD STANFORD U NSSDC 10- 73-0851-05 INVESTIGATIVE PROGRAM 01 - 6.5. LEV* NASA-JPL CODE EL-), SCIENCE 01 - 1.1. SHAPIRO MASS INST OF TECH 01 - 6. FJELDBOINLA) NASA-JPL I NVE ST IGAll ON DlS C I PLINE (5 ) 01 - A.J. KLIORE NASA-JPL PLANETART ATMOSPHERES 01 - J.D. ANDERSON NASA-JPL

PERSONNEL BRIEF DESCRlPllON PI - A.L. BROADFOOT U OF SOUTHERN CALIF lhis experiment used I- (8400 Mu*) and S- (2113 MHz) 01 - M.B. ELRO ROT HARVARD U band. on-board radio ~ysternsfor uhltwer stientifie PU~~OSCS 01 - M.J.S.BEL1Oh KllT PEM NllL OBS could be dewised. Two primary appro~ches were made. one utilizing tracking information, the Other taking advantagt of BRIEF OESCRIPTION radio traicrtory variations associated with occultation of the TWO instruments icrc florn: an orrult*tron soeitrom-ter eaith-sp.cecraft signal. Tracking information was analyzed to that was body-fixed tO the sC.CCCraft and an sirglcr determine .*IS and gravitational rh.r.rtrristirs (including s~~~troiettithat ras mounted on the scan rlatform. Yhtn the planetary internal composition and density estimatts) of both sun 11s obscured by the limbs of the planet, the OCc~ItatiOn Venus and Mercury. fro. .nomalous rh~ractcrirticsObserved in sc~ctromet~r.ees~itd thr ertirrtion propertie$ of the the I- and I-tand signill during Ip.CeCllft paISaOC through the atmosphere. The Orcultation spectrOletCr had a plane grating planetary atmOSphcrcS just prior to, and subsequent to. which operated at grazing incidence. The fluxes were m~asured orrultation. tempetature and PICIIU~~ pr~filc~YCI~ c.lcuIated. at 470. 140. @IC. and 890 A using channel vlcctran multipliers. These profiles "ere useful to adjust atmospheric romporition Pinholes defined the effectilc field of view of the instrument models. Signal rutoff provided useful information for rhi~hwas 6.15 de9 full width It half ..ri.u. IFYHM). Isolated determination of plinetary radius. spectral bands at apprO.i.atClY 15 A (FYHM) were also measured. The objective gratirg airglow IPCC~~C,C~CI was flcrn to measure aiigloi radiation fro. Venus and Mercury in the spect?al rmgc from 200 to 1100 A. Yith a spectral resolution of 20 Ar the instrument mcasurrd radiation at the folloring *.vcIengthl: 3C41 430, 584, 140, 869. 1048. 1216~1304, 1480. and 1651 A. In addition, 10 cro~idca check on the total incident eatrem~

OREQE?%i. PAGE IS OF POOR QUALITY Venus VENUS

Plate 2. This is a composite of press release illustrations of features on the surface of Venus. (A) P80-25 is an artist's rendition of the continent- sized structures and most of the planet's surface derived from the results from the Radar Altimeter investigation on the Pioneer Venus 1 - Orbiter spacecraft. (B) P80-13A is an artist's rendition of the continent-sized mass, Aphrodite, with the outline of the United States on it for comparison. This was also derived from the Pioneer Venus 1 - Orbiter Radar Altimeter. (C) P80-17 is an air brush map of the surface of Venus as revealed by the Pioneer Venus 1 - Orbiter Radar Altimeter measurements. (D) YI-000811 is a reproduction of the photos of the surface of Venus surrounding each Descent Craft landing area of Veneras 9 and 10 launched by the U.S.S.R. Note the different appearance of the rocks at the two sites which are separated by several thousand kilometers. (E) YG-06848 is a photograph of the surface surrounding the USSR's Venera 14 Descent Craft at its landing site. Note the still different structure of the platy, rocky outcrops compared with those of Veneras 9 and 10. Venera 14 landed in still another part of Venus, near the Phoebe Regio part of Venus.

22 OR!GIMAL PAGE BLACK AI"\ID WHITE PiiOTOGRAPh

BEHEPA-9 22. 28.2.1976

RFHFPA-In ?cI in I975 OBPASOTKA MnnW AH CCCP 28.2.137~

650 1- _x) .- - - .- - "1011'1e PRELIWINARY TOPOGRAPHIC VAP OF VCNUP CONTOUR INTERVAL 1 km ALL ELEV REFER TO A RMlMOf 10(6 It- C INTRODUCTION

The next planet out from the sun is Venus. There were four U.S. missions and four U.S.S.R. missions (for which data are available) that either flew by, orbited, or entered the atmosphere and landed on the surface of Venus. The last U.S. mission, Pioneer Venus was composed of six separate spacecraft: (1) Pioneer Venus 1 - Orbiter, (2) Pioneer Venus 2 - Bus, (3) Pioneer Venus - Large Probe, (4) Pioneer Venus - Small Probe 1, (5) Pioneer Venus - Small Probe 2, and (6) Pioneer Venus - SmaN Probe 3. All of the probes and the bus traveled together as one unit, Pioneer Venus 2, from the earth to Venus. The Large Probe and Small Probe 3 entered on the day side of Venus, and the Small Probes 1 and 2 entered on the night side. Two of the Small Probes actually survived and transmitted data for a short time, while the other two may have survived but were oriented wrong to transmit their data to the Orbiter. There were 65 separate investigations when each spacecraft on the Pioneer Venus mission is treated separately. These cover seven categories which are (1) Imaging, (2) Particles and Fields, (3) Ultraviolet, (4) Infrared, (5) Radio Science and Celestial Mechanics, (6) Atmosphere, and (7) Polarization. See Tables 1 and 2 and Appendix A for more details. The U.S.S.R. has sent many missions to Venus, many of which were successful. NSSDC, however, has data archived from only four missions -- namely Veneras 9, 10, 13 and 14 -- from which imaging was obtained. Only these are presented in this catalog.

25 PXCEDENG PAGE BLANK NOT FILMED SPACECW ...... BRlEF DESCRIPTION This ~pacicrift was the first to use the gravitational pull ot one planet lvenusl to reach another (M~ILUIYI. The SPACECRAFT COMMON NAME- MARINER 2 spacecraft stiucture 111% an 1U.lS-kg 00 lb), right-sided ALTERNATE NAMES- 1962 ALPHA RHO Ir P 38 francwort with right electronics compartments. It measured MARINER R-2. 00374 1.39 diagonally and 0.457 I in depth. Two solar panels, each 2.7 long and @.VI I) wide. uece attached at the top, HSSDC ID- 62-04lA supp~rting 5.1 so of solar cell .IC.. The rocket engine 1.1 LiqUid-fUeled~ with two sets 01 reaction jets used to stabilize LAUNCH DATE- 08/27/62 YEIGHT- 201. KG the spacecraft on three axes. It carried a lor-gain LAUNCH SITE- CAPE CANAVERAL. UNITED STATES 0.nidirrction.l .ntcnna, composed of a honeycomb-dish parabolic LAUNCH VEHICLE- AlLLS retleCtorr 1-37 in diameter. with focal length 55 cm. Feeds enabled the sp.cecratt to transmit at I-band and X-band SPONSORING COUNTRIlA6ENCI frcquenciti. The sp.ceiratt carried a Canopus st., tiatker. UNITED STATES NASA-OSSA Located on the upper ring structure of the octagonal ~atellite, and acquisition sun sensors on the tips of the 101.1 panels. INITIAL ORBIT PARAMETERS The interior of the spacec~attI.% insulated rith lultilaye~ ORBIT TIPE- VENUS NIB? thermal blankets at top and bottom. A sunshade was dcploycd SttCr launch to p~otectthe spacecraft on the solar-oriented PERSONNEL side. Instrumenti aboard the IPaCetratt mCasUred the PM - J.S. MARTIN(NLA1 NASA-JPL 8tm0lpheri~1 ~urtace. and physical rharartcrirtirr at Mercury PI - R.C. WICKOFF(NLA1 NASA-JPL and Venus. EIoeri.entl included tClCYision photography. magnetic field, plasma. infrared radiometry, u1traiiol.t BRIEF DESCRIPTION sPCCtrOscOpyr and radio science detectors. An experimental The Mariner 2 spacecraft was the second of a series Et I-band, high-trrquenry transnittrr 1.5 flown for the tirit time spacecraft used tor planetary eaploration in the tlybyr or On this spacecraft. Mariner 10 was placed in a parking Orbit nonlanding. mode. Mariner 2 was a backup tor the Mariner 1 after launch tor appr~~imat~ly25 nin. then Placed in orbit aission which tailro shortly after launch tC Venus. The around the sun enroute to Venus. The orbit direction was spacecraft was attitude-stabilized using the sun and earth as OoDODite to the notion of the earth around the run. Mid-course retrrences. It was solar portrtd and Capable Ot continubus corrections rere made. The spacecratt passed Venus on februari telewtry operatior. The spaCeCI.tt obtained data on the 5, 1974. at a distance ot 4200 kn. It crasscd the orbit 01 intcrrlanctary mrdium during the flight to Venus and beyend. Mercury on March 29. 1974, at 2046 UTI at r distance of about and it Obtained pL.n.1.r~ data during the encounter of YCIUI. 704 kn from the surflce. The TV and UV cXDerimcntS were turned The IpacecIatt passed vtnur at a distance 01 41.000 hm on on the comet Kohoutrk rhilc the IP.CCLI.ft was On thr way to Decerber 14. 1962. Wenus. A Second CncounteI with Mercury. when IOrC phOtOgraphS were taken, OCCYIIC~ on September 21. 1974, at an altitude Of ...... #bout +7rO00 km. A third and last IICICYIY tncounter st an altitude of 327 hmr with additional PhOtOqlaphy ot about It0 photographs and ragnrtir field mCasUIClents occurred on March SPACECRAFT COMMON NAttE- MARINER 5 16, 1975. Engineering tests wept continued until March 24, ALTERNATE NAMES- MARINER VENUS 67. 02845 1975. when the s~pplyOt .ttitude-control gas "1% depleted and VENUS-67 the mission "as terminated. NSSDC ID- 67-0601 ...... LAUNCH DATE- 06114167 WEIGHT- 245. KG LAUNCH SITE- CAPE CANAVERALI UNITED STATES SPACECRAFT COMMON NAME- PIONEER VENUS 1 LAUNCH VEHICLE- ATLAS ALTERNATE NARES- PIONEER VENUS 1978 ORBIT. 10911 PIONEER VENUS ORBITER SPONSORING COUNTRIIAGENCI UNITED STATES HASA-OSSA NSSDC ID- 78-051A

LAUNCH DATE- 05120170 YEIGHT- 517. KG PERSONNEL LAUNCH SITE- CAPE CANAVERAL, UNITED STATES PM - D. SCHNEIDERMAN NASA-JPL LAUNCH VEHICLE - A 1LA S -C EN1 PM - 1.H. PARIER(NLA1 NASA-JPL PM - 6.1. RElFFlNLAI NASA HEADPUARTERS SPONSORING CCLNTRVIAGENCI PS - C.Y. SNIDER NASA-JPL UNITED STATES NASA-OSSA

BRIEF DESCRIPTION INITIAL ORBIT PARAMETERS lhc Mariner 5 .pac*cr.tt bas the tifth in series ot ORBIT TIPE- VENUS ORBllER EPOCH DATE- 12/04/78 spacecraft usrd for planetary exploration in the flyby mode. ORBIT PERIOD- 1440. MIN INCLINATION- 10s. DEG Mariner 5 was a refurbished backup spacecr8ft tor the Mariner 4 PERIAPSIS- 200. KM ALT APOAPSIS- 66611. KM ALT mission and was converted trom a Mars mission ti Yenus mission. The spacerratt 1.1 fully attitude stabilized. urirg PERSONNEL the sun and CinOpus as reterrnces. A Central Computer and PM - C.F. HALL(NLA) NASA-ARC sequencer subsystem supplied timing sc~~ucncesand LOmCuting PS - L. COLIN NASA-ARC strvircs tor other spacecratt subsystems. The ~pacecratt passed 4.000 km fro. Vrnus on October 19. 1967. The sP.cecIa1t BRIEF DESCRIFTION inrtiuntnts mees~redboth interplanetary and Venusian magnetic Pioneer Venus 1 was the tirst of two nirrionr designed to ficldsr charged particles. and plaslisr as rrll as the radio conduct a rcnprchenrirc investigation ot the atmOIphere ot retiactivity arm UU emissions 01 the Venusian atmosphere. The UenuS. The IpacCCCaft was a S0l.I-po~CIed Cylinder about 250 mission was termed a SUCC~IS. cm in diameter with its spin axis spin-stabilized perpendicular to the crliptir plane. A high-gain antenna was mechanically ...... drspun to remain tocused on the earth. The instrunenti icrc mounted on a shelf within the rpacetrrtt esctpt for a IagnrtOleter mounted at the end of boom to ensure against SPACECRAFT COMMON NAME- MARINER 10 magnetic intartcrrnce from the IDILCLI~~~. Pioneer Venus 1 ALTERNATE NAMES- MARINER 73. PL-7321 measured the dctajled structure of the upper atn~sph~reand MARINER-J VENUSIMERCURI. MARINER VENUSIMERCURV 1 iono*ohcre of Venusr inve.tigafcd the interaction of the SOL~I bVlV rind with the ionOsDhCre and the magnetic ticld in the ricrnity ot Venus, deteiiined the chararterirtirr of the atmosphere and NSSDC ID- 73-DeSA surface Of wenus on a planetary sc.Lc. determined the planet's gravitatianal field harmonics from pcrtuibations oi the LAUNCH DATE- 11/03/73 YEIGHT- 504. KG IpaCCtiatt orbit, and detected gammi-ray bursts. LAUNCH SITE- CAPE CANAVERAL. UNITED STATES LAUNCH VEHICLE- ATLAS ...... SPONSORING COUN~RI~AGENCI UNITED STATES NASA-OSSA SPACECRAFT COMMON NAME- PIONEER VENUS 2 ALTERNATE NAMES- PIONEER VENUS 1978 lNlTIAL ORBIT PARAMETERS ORB11 TIPE- MERCURY FLIBI NSSDC ID- 78-C78A

PERSONNEL LAUNCH DATE- 08108118 YEIGHT- 380. KG PM - Y.E. GIBERSON NASA-JPL LAUNCH SITE- CAPE CANAVERAL, UNITED STATES PS - J.A. DUNNE NASA-JPL LAUNCH VEHICLE- ATLAS

21 SPONSORING COUNTRVIAGENCV 1N111AL ORBIT PARAUETERS UNITED STATES NASA-OSSA or1011 TYPE- VENUS PsoBE

IhlTlAL ORBIT PARAMPIERS fERSONNEL ORBIT TYPE- VENUS PROBE PII - C.F. HALLINLA) NASA-ARC PI - L. COLIN NASA-ARC PERSONNEL PI - C.F. HALL(hLA1 NASA-ARC BRIEF DESCRIPTION PS - L. COLIN MA SA-ARC Thia space~~aftwas the first Shll Probe of the Pioneer Venus Uultipiobe mission. On tbis mission four instrument.d BRIEF DESCRIPTION at.Ofpheric entry PiObCs were tarried by a aoacecraft Bus to The spacecr.ft 1.11 the Bus portion Of the PiomIr VenYa the vicinity of Venua for dearent throuph the atm0sph.r. to the Multiprobr mission. On this mission four inat,u.tPtea clanetarr surface. Tu0 Small Probe. entered on the nightaide. atmosphrrir entry Probes lele carried by this Bus to the and one Small Probe and one Large Probe entered On the dayside vicinity of Venus and released for descent through the of the pl.net. The spacetraft BUS entered the atmosphere and atmosphere to the ~1lnct.r~Iuiface. Tu0 Small Probes sitered obtained .tmOsoheric composition data until burnup. on the nightside, and one Small Probe and the Large Probe Inrestigations emph.sized tht study of the structur. entered on the dayside of the la net. The spacerraft ".a 'omposition and nature of the atrn0sphe.e down to the awfare. spin-stabilized. The trio to Venus toot 123 days. The four and of the cloud8r the radiation field and energy .ashang. in Probes separated 110. the Bus about 10 to 20 days before entry. the lower *t*osphere# and local Information on the atmospheric The Large Probe took 1-112 h to descend through the mtmosphiter circulation pattern. A lister mission. Pioneer Venus Orbiter. while the three small~r Probes reached the surface of the ~Li~edan orbiting soacecraft around Venus two Meek. befor. the planet 15 .in after entry. lhe BLI portion of the spacecraft c~obei "ere released. Siaultanrous .easurrments by the PlObea "as targeted to enter the Venusian atmosphere at ~hallo~ and Orbiter Permitted relating specific local .e.sur.mnts to entry angle an0 transmit data to earth until the Bus MIS the gcncr.1 Itate of the plmet and its ~nvironment.a observed aestroy-d by the heat Of atmospheric friction during its from orbit. descent. In~eitigatcrs emphisizea the study of the structure and comp~iition of the atmosphere down to the surfacer the ...... nature and composition of the clouds. the radiation field and ertrgy exchange ir the lower at.Os~herer and Lor.1 information on the atmospheiis circulation pattern. A sister mission, SPACECRAiT COURON NAME- PIONEER VENUS PROBE 5112 Pioneer Venus Orbiterr placed an Orbiting spac~craftaround ALTERNATE NARES- PIONEER VENUS 1978 Venus two ueCka before the Probes I~ICreleased. Si.ultaneouS measur~rnents by the probes and crbiter peiaitted relatirg NSSDC 10- 78-078i specific Local measure.enta to the general state of the planet and its environment as Observed from orbit. The Probes ItOoPed LAUNCH DATE- 08108178 UEIGlil- 75. K6 transmitting te.ptriture data about 15 km above the surface of LAUNCH SITE- CAPE CANAVERAL, UNITED STATES Venus. but tic Prctts survived on tke surface ard trrnsnittec LAUNCH VEHICLE- ATLAS other data for a matter of IcrondS to minuter. The BUS ceased transmitting data at an altitude of about 165 ti. SPONSORING COUNlRV1A6ENCV ...... UNITED STATES NASA-OSSA INITIAL ORBIT PARAMETERS ORBIT TYPE- VENUS PROBE SPACECRAil CONNON NAmE- PIONEER VENUS PROBE LR6 ILTERNAlE NAIES- PIONEER VENUS 1978 PERSONNEL PI - C.i. HALL(NLA) NASA-ARC NSSOC ID- 78-0780 PS - I.. COLIN NASA-ARC

LLUNCH DATE- 08/08/78 UEIGHT- 300. K6 BRlEi OESCRIPTION LAUNCH SITE- CAPE CANAVERAL. UNllED STATES This SFItCCratt YaI the aerond Small Plobe Of the Pioneer LAUNCH VEHICLE- ATLAS Venus NultiprOb* mission. On this missien four initrumroted atmospheric entry w robes were carried by a spacecraft Bus to SPONSORING COUNTRVIAGENCV the vicinity of Venua for descent through the atmosphere to the UNITED STAlES NASA-OSSA planetary aurfase. Two Small Probes antered On the nightside. and one Small Probe and One Large Probe entered on the dayside INITIAL ORBIT PARAUETERS of the planet. The SpaCeCIaft Bus entered the atmOsph*re and ORBIT TYPE- VENUS PROBE cltainrd atmospheric coaposition data until burnup. Inrcrtigations esPh.sized the study of the structure PERSONNEL ro.position and nature of the atmosphere down to the surfacer PM - C.i. HALLCNLA) NASA-ARC and of the clouds. the radiation field and energy exchange in PS - L. COLIN NASA-ARC the lower at.osDherC. and local inbarmation on the atmospheric circulation pattern. A sister mission. Pioneer Venus Orbiter. BRIEF DESCRIPTION placid an orbiting spacecraft around Venus two weeks brforc the This sparerraft was the Large Probe pcrticn cf the Probes mere relI.Sed. Si.ult.ncOuS .CaSurt.cntS by the Probes Pioneer Venus Multiorobe mission. On this aission four and Orbiter permitted relating s~ecifiiLocal measurements to instrumented atiosphcric entry probes were cavried by the general state of the plsnet and its mvironment as Observed spacecraft bus tc the vicinity cf Venus and released for fro. orbit. descent through the atmosphere to the planetary rurfarr. Tbo S.al1 Probes entered on the nightside and a Small Probe ana ...... this Large Probe entered on the dayside of the planet. The sca~~craftBus ertirrd the .tiosphere and obtainaa .tmOscheri< composition data until bulnup. ln~~stigationsemphasized the SPACECIAFT COUUON NAME- PIONEER VENUS PROBE.SR3 study of the structure and romporition of the atmospheie down ALTERNATE NARES- PIONEER VENUS 1978 tc the surfacer tti nature and ro.pclition of the t10~ds. the cadiation field and rncrgi exchange in the loit, atmosphtrer NSSDC 10' 111-0786 and local information on the atmospheric circ~lationpattern. A sister mission, Pioneer Venus Orbiter- placed an Orbiting LAUNCH DATE- 08108178 YEIGHT- 75. KG ~pa~~craftaround Venus two weeks befare the Probes ere LAUNCH SITE- CAPE CANAIERAlr UNITED STATES released. Simultanrous meas~iementiby the Probes and Orbiter LAUNCH VEHICLE- ATLAS permitted relating specific local measurementi to the general state of the planet and its environment as observed from Orbit. SPONSORIN6 COUNTRV1A6FNCV ...... UNITED STATES NASA-OSSA INITIAL ORB11 PARAMETERS ORBIT TYPE- VENUS PROBE SPACECRAil COIMON NLIE- PIONEER VEhUS PROBE SM1 ALTERNATE NARES- PIONEER VENUS I978 PERSONNEL PI - C.F. HALL(NLA) NASA-ARC hSSDC IO- 78-0781 PS - L. COLIN NAS A-ARC

LAUNCH DATE- Ob108ITU UEIGHT- 75. KG BRIEF DESCIIPTION LLUNCH SITE- CAPE CANAVERAIL, UNITED STAlES This aP.cecratt was the third Small Probe Of the Pioneer LAUNCH VEHICLE- ATLAS Venus IultiClobc mission. On this mission four instrumented atmospheric entry Probes were carried by a spacecratt Bus to SPONSORING COUNTRVIAGENCV the vicinity cf Venus for descent through the atmosphere to the UNITED STLTES NASA-OSSA planetary surface. TWO small Probes entered on the nightside, and one Small Probe and one Large Probe entered on the dayside of the planet. The SPDrerraft BUS entered the atmospheve and cbtaincd atmospheric composition data until burnup. Inrcstipationr emphasize the study Of the structur.1 c~m~~~itionand nature of the atmOspheIe down to the surface, and of the clouds, the radiation field and energy exchange in thc lover atlasphere; and local information On the atrnos~h*ric SPONSORINS COLNTRYIAGENCY u .I .s .R. SAS

INITIAL ORBIT PARAUETERS ORBIT TIPE- VENUS LANDER

PERSONNEL pn - UNKNOYN PS - UNKNOWN

SPACECRAFT COMMON NAME- VENERA 9 DESCENT CRAFT BRIEF DESCRIPTION ALTERNATE NAUES- Venera 13 Landed at I dcg 30 mi” S by 303 degr just ealt Et the e4ste.n rxtcnsion Of an elevated region known as Phoebe NSSDC ID- 75-OIOD Regio. It survived for 2 h 7 “in in an enii,on.ent with a temperature Of 457 de9 C and a PICI~YIC of a9 earth LAUNCH DATE- 06/08115 YEIGHT- KG atrno~~h~r~s.wenera 13 Carvied instruments to take ChemicaL LAUNCH SITE- TYURATAU (BAIKONUR COSMODROUE )r U .S .S .R. and isotopic aeas~r~mentsrmonitored the sptctiu. of scattered LAUNCH VEHICLE- D-1-E svntightr and recorded electric discharges during its descent phase through the Venusian .tmlphCIC. The spacecraft utilized SPONSORIN6 COUNTRYIAGENCY a camera systemr an x-ray fluorescence spectiorneterr and a u .s .s .I . SAS Seismometrr tc conduct investigations on the surface. INITIAL ORBIT PARAMETERS ...... ORBIT TYPE- VENUS LANDER

PERSONNEL SPAC€CRAFT CDPMON NAME- VENERA 14 DESCENT CRAFl pn - UNKNOWN ALTERNATE NAUES- PS - UNKNOYN NSSDC ID- 81-1100 BRIEF DESCRIPTION On October 20. 1915. this ¶parecraft “as 1epar.trd from LAUNCH DATE- 11/04/81 WEIGHT- KG the Orbiter. and landing was made rith the sun neap zenith at LAUNCH SITE- TYURATAM (BAIKONUR COSMODR0ME)r U.S.S.R. U513 UT On OctOber 22. A System Of circulating fluid was used LAUNCH VEHICLE- D-1-E to distribute the heat load. This 1yStt.r PLUS preccoli~g prior to .ntryr permitted operation of the ipacec,aft tor 53 SPONSORING COUNTRYIAGENCY lin after Landing. During descent. heat diSliDation and U .I .S .I. SAS dec.ter.tion accomplish~d SIru.nt)a\Ly by DlOteCtiYI hemispheric shells. three parachutes. disk-shaped drag brake, INITIAL ORBIT PARAUETERS and a ~Omp~Cl~ibLe.netal. doughnut-shaped, landing cushion. ORBIT TYPE- VENUS LANDER The Landing “a1 about 2.200 ha from the wcnrra 10 Landing site. Prelininary results indicated: (A) clouds 30-40 km thick uith PERSONNLL baser at 30-35 tm altitude. (8) atLOsDheliC constituent3 PU - UNKNOWN including HCLI HF, err and I, IC) 1urt.rr ~ressureabout 90 PS - UNKNOWN (earth) .tmOsDheresr (D) surface 1C.Ptl.tUIC 485 deg C. (E) light lrvels CO.D..~DL~ to those at earth midlatitudes or a BRIEF DESCR1PlION cloudy summer dayr and IF) surcesstu1 TV DhOtOg.aphy shoring Wenera 14 Landed at 13 dtg 15 .in 5 by 310 dtg, about 950 shadowl. no apparent dult in the air. and variety of 30-40 CII k. southwest of Yenera 13. Surface temperature I~I465 dcg C rocks which wrre rot eroded. and LIe11U.e was 94 eerth .t.OSDhCIeS. Ventra 14 carried instru~entl to take chemical and isotopic measurements, ...... monitoied the spCIt.~m Of SCattLrCd sunlight, and recorded electric discharges during its descent phase through the VCnuSi.n atmC1DhLIC. The SP.cCc~alt utilized a camera Systemr SPACECRAFT COMUON NAME- VENERL 10 DESCENT CRLfT an X-p.7 ftuoierc-nce s~ectrm~terrand a seirnonctcr to ALTERNATE NAUES- conduct investigations on the surface.

NSSDC ID- 75-054D IUAGlNG IMSTIGATIMIS LAUNCH DATE- 06/14/15 WEIGHT- KG LAUNCH SITE- TYURATAM (BAIKONUR COSUODROME). U.S.S.R. LAUNCH VEHICLE- D-I-€

SPONSORING COUNTRYIAGENCY --__-__)I)iR*htR 10, MuRRAy------U.S .S.R. SAS INVESTIGAT~ON NAUE- TELEVISION PHOTOGRAPHY INITIAL ORBIT PARAMETERS ORBIT TYPE- VENUS LANDER NSSDC IO- 73-0851-01 INVESTIGATIVE PROGRAM CODE EL-4. SCIENCE PERSONNEL pn - UNKNOWN INVESTIGATION DISCIPLlNEtS) PS - UNKNObN PLANETARY ATMOSPHERES PLANETOLOGY BRIEF DESCRIPTION On October 23, 1975. thil SD.Cerr.ft Was SeDalatcd troll PERSONNEL the Orbiter. ard Larcing was wade bith the sun near zenith, at PI - B.C. nunR#v CALIf INS1 OF TECH 0517 UT. On 0ctOb.r 25. A system Of ciiculatlng iluid was used 01 - l4.J .I .BELTON KIlI PEAK NAIL OBI to distribute the heat load. This SyStCmr plus PreCODling 01 - G.P. KUlPER(0ECEASED) U Of ARIZONA prior to entry. p~~.itt~doperation of the ~pa~e~i.ftio1 65 01 - V.E. suonr U OF YISCONSIN .in after Landing. During descent. heat dillip~tiOE .no 01 - N.J. TRASK, JR. US GEOLOGICAL SURVEV deceleration Mere arc0aplish.d sequentially by pfotectiie 01 - D.E. GAULT NASA-IRC hemispheric Ihells~three ~.r.chUt~S. a disk-shaped drag brake, 01 - B.Y. HAPKE U 0) PITTSBURGH and a Campr~aaiblr. mCtaL, doughnut-ihaprdr larding rurhicr. 01 - n.~. DAVIES RAND CORP The Landing ”as about 2.200 km distant from Vrner. 9. 01 - 8.1. O*LEARY PRINCETON U Preliminary relultr provided: (1) profile of altitude (km)IDltssurC (earth .t.OlDhtle*)/tC.PLI.tYrC (dcg C) of BRIEF DESCRIPTION 4213.31158, 15/37/363. and 0192/465r (8) IUCIISS~Y~ TU The objectives Of this e.perinent were to photograph the phDtOgraDhy shouing Large panrake mcts with Lira or other Surfacer (upper atmolphcrc in the case 01 Venus) Of the DlanrtS ucithcrcd rocks in between. and IC) surface wind Speed of 3.5 Venus and Mercury. For Venus, the objectives were to *IS. invcltigatc the time-dependent propcrtics Of the UV rloudr. end to obtain high-resolution imagery of the main tlouds. Foe ...... Meptury, the objectives were to ..D its major Dhysiographic prorincer, detrr-inr its spin axis orientation. establish a cartographic coordinate system. and search for Mrrcurim SPACECRAFT COMMON NAUE- VENERA 13 DESCENT CRAFT satellites. The equipment consisted of two spherical (150 II ALTERNATE NAMES- diameter) Cassrgrain ~CLCICOPCI with eight filters, attached to 6EC 1-inch ridiron tube Cameras (1500 mn focal Length and 0.5 NSSDC ID- 81-106D dcg field at vier) for narror-angle phatography. An auxiliary Cptical system mounted On each ramera provided wide-angle (62 LAUNCH DATE- 10130181 YEIGHT- KG .m focal Length and 11 X 14 deg Iicld Of vier) phDtOglaDhy by LAUNCH SITE- TYURATAM IBAIKONUR COSUODROME). U.S.S.R. noving 0 mirror on a filter wheel to a position in the optical LAUNCH VEHICLE- D-I-E Cath. ElpDlurc tine ranged from 3 mS to 12 SI and rath camera took a D~C~UI~every 42s. The 1V picture consisted ot 700 stan tines rich 832 FiDturC clancntrllinc. uhith *ere digitally coded into e-bit words tor transmission. There lele eight filter uhrrl positions: (1) wide-angle image relay mirror. (2)

29 blue bandpass. (3) UV pol.rizlngr I+>minus UY high pasir 0) USSIC ID- 81-11OD-01 INVESTIGATIVE PROGRAM clear. (6) uv bandmass. (7) deforusing lens (for calibration). LUNAR AND PLANETARV and (8) yellor bandpars. About TOO0 photographs were obtained of wenus and Mercury, rlth a manisu. resol~tionof 100 for INVESTIGATION DISCIPLINE(S) MercuIy. Three photographic P.SICI. Sep.r.t=d by 6-month PLAUETOLOCl intervals, "ere made for Mercury. Further details of the cxprri.ent Can be obtained from NSSDC 11-18. and Icarusr v. 15. PERSONNEL n. 2, October 1911. Science results cn Meciucy may be Obtalrea PI - UNKUOYN from J. Geophyr. Ref., 1. 801 D. 11. June 1975. and on Venul in Srirntcr v. I831 D. 4131, March 1974. BRIEF DESCRIPTION The camera ayste. carried on vrn*m 14 ".a an i.prorem.nt ------PlONEER VENUS 1, HANS€*------On the ones carried on Vanrras 9 and 10. Four (magas I.I. obtained of the surface of Venus- lNVESTlGATlON NAIE- CLOUD PHOTOPOLARIMETER

NSSDC ID- 78-05lA-06 INVESTIGATIVE PROGRAM CODE EL-+# SCIENCE PARTICLES AND FIELDS

INVESTIGATION DISCIPLINE(SI PLANETAPI ATMOSPHERES ------qARlNER 2, NEU6EBAUER------PERSONNEL PI - J.E. HANSEN NASA-6151 INVESTLGATION NAME- SOLAR PLASlA ANALlZEI 01 - P.H. STONE MASS INST OF TECH 01 - A.A. LACIS NASA-6155 NSSDC ID- 62-0111-06 INVESTIGATIVE PROGRAM 01 - D.L. COiFEEN NASA-GISS CODE EL-4r SCIENCE 01 - L.D. TRAVIS NASA-GISS INVESTIGATION DISCIPLIME(S) 0RlEF DESCRIPTION SOLAR PHYSICS This enpeiimirt used simplifi~dversion cf the ImagiPg PhotOpoLarim.zter (IPP) flown on Pioneers 10 and I1 to DrOlide PERSONNEL lor-resolution. four-color mapi of the Venusian cloud cover PI - M.1. NEUDEBAUER NASA-JPL rith 1 high-resElUtiOn imaging CaDatilitY near aporentrr. The 01 - C.Y. SNYDER NASA-JPL principal objectire of this inveitig.tion was to determine the ~rop~rtiesof the clouds and hazer including the Ueitic.1 and BRIEF DESCRIPTION horizontal distribution of the p.iti~leS. cloud Particle size This r#per+mcnt "8% drsign.d to study the flu. and energ), ard refractive irrai, the clf~a-tcp height. and the rusbef ~pe~tr~.of the positive ion co.ponent of the solar rind density of particles. mlasm.. The experiment ronaistrd of a cylindrical electrostatic analyzer with a faraday CUD detector. This -_----- VENERA 9 DESCENT CRAFlr UNKNCYN------'------System SIparated positiv.iy-chargrd ions according to their energy per urit charge. The entrance aperture 1.5 5 sq cm and INVESTIGATION NAME- PANORAUIC IELEPHOTOMETER TOR SURFACE rectangular. The aperture pointed to within 0.1 deg of thr sun IMAGEUY throughout the flight. The voltage On the analyzer plate. "as changed at intervals of about I8 s in an ascending srquenee ot NSSDC ID- 75-0500-(1 INVESTIGATIVE PROGRAM 10 r.1u.S from 231 V tO 8824 V. A zero current reading and a LUNAR AND PLANETARl calibration reading were thin taken. The complrt. sequence of 12 .easurem*cts was reprated every 3.696 .in (every 2.016 min INVESTIGATION DISCIPLINL(S) near Venus). The instrument functioned normaily over the entire PLANETOLOGY flight and provided data .LmOSt COntinUOUSly until Drcember 30, 1962. PERSONNEL PI - UNKNOYN ----_--MARINEI 10, BRIDGE------

BRIEF~ ~~ DESCRIPTION~.~~ ~ INVESTIGATION NAME- MEASUREMENT OF PLASMA ENVIRONRENT This experi.ent used trlerision camera to photogvaDh the surface of Venus. One rurccssful image "as obtained. NSSDC ID- 13-OSSA-03 INVEST16ATLVE PROSRAM CODE EL-4. SCIENCE ------VENERA 10 DESCENT CRAFT. UNKNOYN------"' INVESTI6ATION DISCIPLINE(S) INVESTlGATION NAME- PANORMIC TELEPHOTOMETER FOR SURFACE PARTICLES AND FIELDS IMAGERY PERSONNEL NSSDC ID- 75-054D-01 INVESTIGATIVE PROGRAM PI - ns. BRIDGE MASS INST OF TECH LUNAR AND PLANETARV 61 - J.H. BINSACK MASS INST OF TECH 01 - l.J. LAZARUS MASS INS1 OF TECH INVESTIGATION DISCIPLINE(S) 01 - s. oLnERi MASS INST Oi TECH PLANETOLOGY 01 - S.J. BAME LOS ALAMOS SCI LAB 01 - M.D. IONTGOMERT LOS ALAMOS SC1 LAB PERSONNEL 01 - A.J. HUNDHAUSEN NATL CTR FOR ATMOS RfS PI - UNKNOYN 01 - J.R. ASBRIDGE LOS ALAMOS SCI LAB 01 - K.Y. 061LVIE NAS.A -60 F C 8RIEi DESCRIPTION 01 - L.F. BURLAGA NArA-GSFC This crpcrimcrt used a television samer. to photcgraph 01 - R.E. HARTLE NASA-GSFC the surfac~of Venus. one suoressful image 1.5 obtained. 01 - C.Y. SNYDER NASA-JPL 01 - G.L. SISCOE U OF CALIF, LA ------VENERA 13 DESCENT CRAiT. UNKICYN------BRIEF DESCRIPTION INVESTIGATION NAME- PANORAMIC TELEPHOTOMETER FOR SURFACE The esoeri.cnt vas dcslgn*d to determine the mod. 01 IMAGERY interaction betieen the planet n.rcury and the solar rind, to .ate a ~0.prehen~i~estudy of the plasm. regime at MercYryr to NSSDC ID- 81-1060-01 INVESTlGATIVE PROGRAM rarify and extend previous observations Of the Solar rind LUNAR AND PLANETARl interaction rith Ve11us.1 to clarify the role of electrons in the interactions, and to study the solar rind from 1 to 0.4 AU. INVESTIGATION Instrumrntaticn for the e.periaent consisted of two PLANETOLOGT sunward-facing clcctrortmtlr an.lrzers (SESA) and one backward facing electron ~p~~tiom~t.,(BESAI. These three detectors were mounted on 1 scanning platform. rhirh could be swept at 1 degls through an arc of 120 drg centered on a direction in the ecliptic plane 6 deg east of the spacecr.ft-sun lint. 00th SESAs failed to return data. They were to measure positiue ions from 0.08 to 8 Lev and tltctronr from 4 to 400 cV. The BESA had fan-shared field of vier Of PLUS or minus 3.5 deg br plus or minus 13.5 deg. The larger angle was normal to, and sy..etric about, the stan arc. An electron SDCC~IU. "as Cbtainid every 6 SI and r0nsist.d Of flux .L.SUIe.CntS in 15 LOgarithmic~lLy spaced enerpy channels (with channel width delta €11-6.62) within the energy range 13.4 to 690 eV. BeCIUSt IOLll rind flow pasf the Spacecraft introduces angular distortion of the elCCtron distribution function ~~.p.r~dto "hat would be Observed In th. solar rind rest frame, It 10s possible, by taking into account this distortion and the s~.recraft sheath characteristics. to dcrirr some of the solar rind p1.l.a PaV.mCtCII Such as ion bulk Speed* eLtrtrOn tCmpeWatUrer and cIcctron density. The reliability of these

30 NSSDC ID- 61-0601-03 INVESTI6ATIUE PROGRAM NSSDC ID- 18-051A-I3 lNVESTl6AllVf PROGRAM CODE EL-). SCIENCE CODE EL-). SCIENCE INYLSllGATlON DISClPLINElS) INVLST161110N DISCIPLINE IS) PARTICLES AND fIfLDS PARTICLES AND FIELDS INTERPLANETAR1 PHVSlCS SPACE PLASMAS PERSONNEL PERSONNEL PI - H.S. BRIDGE MASS lkST OF TECH PI - f.L. SCARF TRY SVSTEMS 6ROUP 01 - C.Y. SVNDER NASA-JPL 01 - 1-11. GREEN TRY SVSTEIIS 6ROUP BRIEF DESCRlPTION BRIEF DESCRIPTION This thi~c-~~~tion.l-~~llCItDImodulatrd-grid faraday cup This erp.ri.rnt conaistrd of 8 modified version of the me8sured positive ions from 40 to 9400 eVlP in eight Pioneer 8 and Pioneer 9 experiments to measure the .pproximltely LOgarithlirally equispacld energy windows. Aa electric-tisld rc.~~nsnt$ ir tour 30%. nairOi-b.no channel, the inltrumert alriys pointed toward the run. vector data were centered at lo01 1301 7350. and 30.000 Hi. The aims of the obtained by comparing the relative signals from the three investigation were to pcrtorm the fiest analysis ot VlF 120-de9 Pie-shaped collector sections. During each telemetry elrrtric fields at Venus to elucidate the p1.s.a interactions sequence# the instrument was stepped forward and backward brtrrtn the solar rind and the ionosDherir or esosrheric thiough the eight windows to I~~SYICthe sum of the currents pl.sma. The role of plasma instabilities in modifying the heat from the three pl=tei. Then it "as stepped torrard and tlux from the aolar rind and in thermalizing newly-born ions barkrard to measureI tor each voltage setting. the currents to from Venus MIS alrc studied. A self-contained b.lanced Y-tyce the three plates in succcrrion. The entire 32 steps in voltage antenna with a dittercntial pirmp1ifi.r was cmploytd to makc rindow PCI teleICtry SeqUCnCc produced 64 CuIrtnt .IasUVCmCntl. the meaa~rCmC11ts. At the 512-bpi sat.llit. modes one frequency These mCasUrImenti were repeated every 5 mi". The instrument acan per second was ottained. Operated nominally throughout its mission. -- -_-- - PIONEER VENUS 1, KN"DSLN------______-MARINER 2, COLEMAN, ,R.------

INVESTIGATION NAME- RETARDING POIENTIAL ANALVZER INVESTIGATION NAME- FLUXGATE MAGNElOMtTER

NSSDC ID- 18-051A-07 INVE S116ATIVE PROGRAM NSSDC ID- 62-041A-03 INVESTIGATIVE PROGRAM CODE EL-4ICO-OP. SCIENCE CODE El-4. SCIENCE

INVESTI6ATION OISCIPLINE(S) INVESTIGATION DlSClPLINE(S) PLANEIARV AIMOSPHERES INTERPLANETARV PHISICS PLANElLRV IONOSPHERES PLANEIARV MIGNETlC FIELD

Pf RSONNE L PERSONNEL PI - Y.C. KNUDSEN LOCUHEED PAL0 ALTO PI - P.J. COLEMAN, JR. U OF CALIF. LA 01 - K. SPENNER INS1 FUR PHVS YELTRAUM 01 - R.C. WHITTEN NASA-ARC BRIEF DESCRIPTION lhis experiment "as designed to measure the magnitude and BRIEF DESCRIPTlON direction 01 the interplanetary and Venusian magnetic fields. This irrtstigation usee langiuii-probe It consisted 01 three orthogonal fluxgate magnetometers uountrd retarding-pOt+otial anmlyzer d.sign.d to .C.SYI~ elertrcn cn top 01 I 152.4-1 towel. One magnet~l.ter asis "1s parallel concentration and tempetatur., majcr ion ronc*ntrationi and to the ipacecratt roll axis. In the high-sensitivity made, temperaturear ion dritt urloriti.sr and the mcrgy distribution each m.gnetomCter had a dynamic range 01 -6* to 164 nl rith an tvnction of ambiert photoelrctrora. It uas an adlDtatioP el accuraLy 01 t 01 -0.5 "1. In the lO~-SenSitivitymode. this the instrument tlorn on the German Aeros satellite in 1912. range was -320 to +320 nT with an accuracy at or -2.5 "1. Lither one Of tu0 sensor hc8da could be used.,=.ch consisting A11 three magnetometers were sampled rithin 8.64 I. ana this ct a multigrid c~pand electro,rter. rhieh could OpClatt in sequence ot Sampling was repeated every 36.96 I (or every 20.16 electron. ion. or phOtOLlertlOn modes. initiated by spacecratt s during the Venus ~nrounter on Dec.mber 14. 1962). An roll p~ls~a.The meas~~ernentstaken when the senior asis *as inflight calibration system was deaigncd to check the rloaest to the PI.... flow w10~Ityvector were trmamittcd. sensitivity ct the three magnito.eters once during each 15.11-h The aims Of the irrestigatior were tc i.pr0Wc kncwlcdge ct the peiiod. Due to failure in the tonti01 ciicuit. intlight important ionic reactions in the Venusian i0noSpht.e. io study ralibrations icrc performed move often rnd in a random tashion. the ~L~SLItransport ~IOCCSIIS to determine it Venus has a Other than the failure in the intlight calibration system, the polar wind, to study the proc~~sesat the anta1 rind-ionosphere rxperinrnt performed normally until January I, 1963. rhrn boundary. and to study Similar ai.. roncrrning the ambient contact uith Mariner 2 was lost. electron population. --____-MARINER 10, NESI-'------___---_PIONEER VENUS 1, YOLFE------INVESTIGATION NAME- FLUXGATE MAGNETOMETERS INVESTIGATION NAME- PLASMA ANALVIER IOPA) NSSDC ID- 13-0851-04 lNVESTlGAIlVf PROGRAM NSSDC 10- 78-0511-18 IWYEBlIGAlIVE PROGRAP CODE fL-.. SCIENCE CODE EL-4. SCIENCE INVESTlGAlION DISCIPLINf(S) lNVESTlGATlON DISCIPLINL(S) PARTICLES AND FIELDS SPACE TLASMAS PLANETOLOGI PARTICLES AND FIELDS PERSONNEL PERSONNEL PI - N.f. NESS NASA-GSFC PI - J.H. YOLFE NASA-ARC 01 - K.Y. BEHANNON NASA-GSFC 01 - A. BARNES NASA-ARC 01 - R.P. LEPPING NASA-GSFC 01 - H.R. COLLARD NA SA-ARC 01 - 1.C. YHANG CATHOLIC U OF AMERICA 01 - D.D. RCKIBBIN NASA-ARC 01 - 1.D. UlHALOV HA SA -ARC eRlEF DESCRIPTION 01 - R.C. YHITTEN NASA-ARC This e.peri.ent consisted at two triaxi.1 fluxgate 01 - D.S. INlRIL16ATOR CARREL RES CENTER magnetometers mounted on a com.on boom 2.3 rn and 5.8 I tlol the spacicratt and designed to measure the vector magnetic field in BRIEF DESCRIPTION the vicinity 01 Mercury and Venus and in the intrrpl*nctary The instrumrrt top this rxp.ri.ent "as guadrispheric.1 .=diu.. Outnuts from the ti0 magnetometers ICI~ simultanrourly electrostatic analyzer 1det.ctOr 0 at plaama instrument an ana1yl.d to sepav.te ambient fields tron spacIcratt fields. Pioneera 10 and 11). uith tire current ccllectors and Each sensor had dual operating ranges ot minus to plus 16 nT .lect.omrtcrr. The mergylcharge range "as 50-8000 (ions) in and 128 "1. uith digitization accuracies of 0.03 nT and 0.26 32 steps and 1-500 lelectrons) in 16 steps. The angular range 011 respecti~ely. Bias otfrct capability extended the Operating ccvcrrd was plus cr minus 85 dru elevation by 360 deg azimuth. range to minus or plus 3188 "1. Owing the primapy phase Ot and the detector field Of vier was 15 d.9 times 25 dcg or 15 the miaaion (November 3, 1913. to March 29, 1914) and during deg times 45 deg. depending an po~ition. The logic design "as the second and third MCILUIY enco~nters, 25 vectors PCI second essentially that used on Pioneer. 8 and 9. The Objectives ierc ICI. Sampled by the primary OutbOald llagnCt01rtCI and tC meaaure solar wind conditions outsldi the Venusian bcr transmitted to Earth. At other times. a loicr data rate lode aback. inside the magnetosheath tlor field. and to study the was used during rhich tiw Vectors per second YCIC transmitted. ionopausal structure. Solar-rind measurements were made during The experiment functicned normally throughout the lite at the the transit tn Venus. particularly to study m.rrorr.lt problem= SPaCCcIItt. for further details, Ice N. F. NESS et at., and to determine awerage gradierts. The near-planet wake Science. V. 183, P. 1101.

31 - - -- _--PIONEEI) VENUS 1, RUSSELL------

INYESTlGATlON NAME- MAGNETOMETER (01116)

NSSDC ID- 18-0511-12 INVESTIGATIVE PROGRAR CODE EL-4. SCIENCE

INVESTIGATION DISCIPLINE(S1 MAGNETOSPHERIC PHYSICS PARTICLES AND FIELDS ATMOSFMERIC PHVSICS

PERSONWE1 PI - C.T. RUSSELL U OF CALIF. LA 01 - P.J. COLEMAN. JR. U OF CALIFr LA 01 - F.V. ~~ CORONITI ~ U~ OF CALIF,.~~ LA~ 01 - C.F. KENNEL U OF CALIF. LA 01 - R.L. MCPHERRON U OF CALIF. LA 01 - G.L. SISCOE U OF CALIF. LA

BRIEF DESCRIPTION This cxptrimrnt used a triaxi.1 fluxgate magnetometer rith two ring-core aenaora at the tnd of a magnetometer boom ard cne ring-rare ienso,. at 45 des tC the spin rxiar ha1fb.y down the boom. The drive and elartronirs design had been used on the ApolLo 15 and 16 subs.te1Lit.s. The ObjSltivtS were to dttcrminc any planetary and Itmanen1 magnetic field.. to deduct thr Location and strength of the iorcspheric current syste., tc determine the energy and mass balance in the upper atmOsphere of Venus. to determine the nature of the solar rind intrrartion with Vtrus, and tC study the near-bile rrpion of Venus and the structure of the Vtnurian bor shock. lntrrplrnrtary objrrtires "ere to determine the pcrt~rb.tion of the near-plsnct region by Venus and to ~0.p.r~ the propcities of the arerage field at 0.1 a~d1.9 AU. The irrtru.cnt .as intrrdtd to, in the IOrst C.S. of Lou-bit and lou-l~.plc rates, ~C~SUICone vector per 32 s. Yhile in Venus orbit, when the sparerraft was coasting through the intcrplanrtary rrpion in the accacsis .me. the sample rate 11s one vector per 8 s. uhilt the SC~CCCT.~~was passing through the Venusian ionorpherr in the periapfis mode. the sample rate was four vectors per I. ------MARINER 5, SLIT"-----'-----'------'------

INVESlIGAllON NAME- TRIAXIAL LOU FIELD HELIUM MAGhETOIETER

NSSDC ID- 61-0601-05 lNVE STIGATIVE PROGRAM CODE EL-4. SCIENCE

INYESTIGLTlON DISClPLINE(S) PARTICLES AND FIELDS PLANETARV MAGNETIC FIELD

PERSONNEL NSSDC ID- 78-0511-17 INVESTIGATIVE PRO~RAM PI - E.J. sniin NASA-JPL CODE EL-4. SCIENCE

BRIEF DESCRIPTION lNVEST16AlION DISCIPLINE(S) For this t.peri.ent a Lou-field hcliu. magnetomiter I.. PLANETAPI IONOSPHERES used to obtain triaxi.1 .eas~re.entl of interplanetary and PLANETARY AlMOSPHERES Venusian magnetic fields. Its c~eration dtpendca on the variation in absoIDtivity of excited helium to ~ircu1arIy PERSONNEL polaril~dinfrartd Light rith .PpLicd firld. Slept H~Lmh01tz PI - H.A. TAVLOR. JR. NlSA-bSFC coils nulled the ambient fitld by use of ferdtict circuits. 01 - S.J. BAUER 6111 U Mounted on 1.5-m b0O.r the inlt,u.cnt's dynamic range I.. 01 - R.E. HARTLE NLSA -61 FC plus or minus 204 nT PCI axis. rith measur*ment precision 01 - H.C. BRINTON NASA-CSFC dctcrmintd by telemetry constraints of plus or minus 0.2 "1. 01 - J.R. HERMAN NASA-6SFC Offset fields uere CCrrrCtlblr tO rlttln 0-25 nT Stl Co.pOn*nt. 01 - T.M. DONAHUE U OF MICHIGAN Tht experiment operated in high (Lor) bit-rate mode of 3 01 - PA. CLOUTIER RICE U vector samples spaced 111. 211. and 411 Of the sequence eve,, 01 - F.C. M1CHEL RICE u 12.6 (50.4) s; thus the Nyguist frequencies were about 0.12 and 0.03 Hz rerpcrtirely. High-rate data uerc obtained from Jbne BRIEF DESCRIFTION 14 to JULY 29, 19bl. and for 4 hours on OctObeI 25, 1967. Lou The composition and roneentr.ti0n of thermal p~fiti~e blt-rate data were obtained for the remainder of thr ions in the ionosphete of Vrnu. were drterdined and intrrpretrd e.p~liment's useful Lifetime. Puality of data "if high except in terms of vertical and horizontal components. Thr inltrumrnt during Stotember 23 to October Ir 1967. when t=le.et*red date used was Bennett radio-frequ.nry ..SS SplCtlO.et*l baaed On wire of uncertain quality. NSSDC has all the data from this tht design of those flown on 060 and Atmorphrrir Exp101.r experiment. satellites. A mass range of 1 to 60 u was cowred rith variety of autoe8tic Sean-ararth modra available. -__----MARINER 2, VAN ALLEN------PIONEER VENUS 2, T&YLORr JR.------INVESll6ATION NLnE- PARlICLE DETfCTOR INVESTIGATION NAME- ION-MASS SPECTROIIETER NSSDC ID- 62-0111-07 INVESTIGATIVE PROGRAM CODE EL-4. SCIENCE NSSDC ID- 18-0181-02 INVESTIGATIVE PROGRAM CODE El-4. SCIENCE INVESTIGATION DISCIPLlNE(S) PARllCLES AND FIELDS INVESTIGATION DISCIPLINE(S1 PLANETARV PHVSICS PLANETARV AlMOSPHERES PLANETARV IONOSPHERES PERSOUNEL AERONOMI PI - J.A. VAN ALLEN U OF lOYA PERSONNEL BRIEF DESCRIPTION PI - H.A. TAVLOR. JR. NASA-SSFC A collimated. directional, Anton type 213 Geiger-nwller 01 - 5.1. BAUER GRA1 U tube (rith energy thresholds of 40 Lev for electrons and 500 01 - 1.n. DONAHUE U OF IIlCHISAN Lev for prot~na) was Used 10 search for charged oartiL1.s 01 - P.A. CLOUTIER RICE U magnrtiraLLy tiacpea in the vicinity of the plaret Venus and, 01 - 1.1. HARTLE NASA-6SFC if such particlti were found. to obtain preliminary 01 - H.C. BRINTON NASA-GSFC .easu~ements 01 their 1p.ti.1 distribution and intensity. 01 - F-C. 111CHEL RICE U Throughout the flight, including the planttary flyby. the .xis of the detector's CCrir.1 field Of Vier (90 alg full Ingle) was directed at 78 deg plus or minus 1 deg to the SPICCCllft-IUn Line. This axis Lay in the plans containing the sun. e.rthr

I2 BRIEF DESCRIPTION NSSDC ID- 71-0851-05 INVESIIGATIVE PROGRAU This Ion mass spectrOm*ter exp~iimint Obtained CODE EL-4r SCIENCE measUrem.nts ~hichprovided intoraation on the solar rind interaction with Venus. upcer st.csphere photochemistryr rnc INVESTIGATION DISCIPLINE(S) the mass 8nd heat transport characteristics of the atmosphere. PLANETARY ATMOSPHERES A Bennett ion spectrometev. similar to units tlom on many earth satelliter arc rockets. .easrrma Venus' upcer at.osphere PERSONNEL ion roncmtrations in the mass range tip. 1 to 60 atomic ..IS PI - A.L. BROADFOOT U OF SOUTHERN CALlf units (u) tiom the time Of crossing Venus' borshotk to bur 01 - 11.0. MCELROY HARVARD U burnup. 01 - M.J.S.BEL1ON LIT1 PEAK NATL OBS __---_-PIONEER VENUS 1. EVANS------BRIff DESCRIPllON Two instrunmtf ICI~tlorn: an occultation sp~ctr~m~tii INVESTIGATION NAME- GAMMA-RAI BURST DEIECIOR that was body-fixed to the spacecratt and an airglow IpeCtrOmCtCI that was mounted on the scan plattorm. when the NSSDC ID- 78-051A-C5 INVEST16ATIVE PROGRAM sun was cbirured by the Limbs of the planet, the occultation CODE EL-4. SCIENCE spectlometer measured the extinction proper ti^^ ot the atmosphere. The occultation sp~~tr~meterhad a plane grating INVESTIGLTION DISCIPLINEIS) which Operated at grazing incidence. The fluxes UCII measured GAMMA-RAY ASTRONOMY at 4701 740. 810. and 890 A using channel electron multipliers. Pinholes defined the effective ticld 01 view 01 the instrument PER S 0 N N E L which was 0.11 dcg full width at halt mxinum (FYHM). Isolated PI - Y.D. EVANS LOS ALAMOS NAT LAB spectral bands at apPiOiiiately 75 A (fYHM) YCII also measured. 01 - J.P. CONNER LOS ALAMOS HAT LAB The Objectire grating airglow sp~~tro~eterwas flown to ~C~IUII 01 - P.R. HIGBIE LOS ALAMOS WAT LAB airplow radiation (10. Yenus and Mrrrury in the spectral range 01 - R.Y. KLEBESADEL LOS ALAMCS NAT LAB trm 200 IO 1700 A. Yith a spectral r~solutionot 20 A. the 01 - R.A. OLSON LOS ALAMOS NAT LAB instrument wrasured radiation at the tollwing wavelengths: 01 - 1.0. STRONG LOS ALAMOS NAT LAB 3011 430. 584. 740, 869. 10481 1216, 1304, 1480. and 1657 A- 01 - R.E. SPALDING SANDIA LABORATORIES In addition. to provide a check on the total incident extieme UY flux to the Spectr~m~terrtwo zero-order channrlr were BRlEf DESCRIPTION flown. The ettectiw field of vier of the instrument was 0.13 An omnidirectional gamm.-r.y detector e.pl~ying tuo dtg by 3.6 deg. More ~xperimentdetails and SOW measu~ements Phosiich scintillation spectrometers sensitive to protons tro. arc contained in two papcis: (1) '*ultraviol~tObservations ot 0.2 to 2.0 MeV bas used uith lcoir circuitry to aetect the Venus tro. Iarinel 10 -- Pre1i.inary Wesultsr A. L. BroadtOOtr beginning of a gam.. ewent and to initiate period 01 rapid et a1.r Science, Y. 183, March 29, 1974. and (2) "MCICY~Y'S data ~011.cti0n. Data IS,. stored in 8 memory unit tor At.olphere trom Mariner 10 -Preliminaty Rts~ltir" A. L. subsequent transrission to earth. Contirmaticn thet I true 010adf00tr et .I., Scienter Y. 185. July 12. 1974. A gamma event had occurred was obtained DY romr.riron uith description ct the instrumentation is given in ti0 later results 1-0. other ezp~~i~entsin eaith satellites. This papers: (1) "Mariner 10 UltrariOlet Sp~cti~mete.: Airglor e~periment provided the long-baseline time correlations Experiment.- A. L. Broadfootr 5. S. (Lapp and F. E. Stuart, necessary tor calculating accurate sc~rcelocatiors. Space Sci. Inrtr. Y. 3. 199 (1977); (2) 'Mariner 10 Ultiaviolrt SpCCt~Ol~tCC: Occultation E.periment." A. L. B~oadtootr5. I. __-----MARINER 2. ANDERSON------'------CtapD and f. E. Stuart. Spare SLi. Inltr. Y. 3, 0. 209 (1917). Dall also include the interplanetary region. INVESTIGATION NAME- COSMIC-RAY IONIZATION ------PIONEER VENUS 1, slEYAlT-----'------NSSDC ID- 62-OllA-04 INVESTI6ATIVE PROGRAM CODE EL-4r SCIENCE INVESTIGATION NAME- PROGRAMMABLE ULTRAVIOLET SPECIROMETER

INVESTIGATION DISCIPLINE(S) NSSDC ID- 78-0511-15 INVESTIGATIVE PROGRAM COSMIC RATS CODE EL-+, SCIENCE

PERSONNEL INVESTIGATION DISCIPLINEIS) PI - H.R. ANDERSON SCIENCE APPL. INC PLANEIARY ATMOSPHERES 01 - J.A. VAN ALLEN U OF IOYA AERONOMY 01 - V.H. NEHER CALIF INST OF TECH IONOSPHERES

BRIEF DESCRIPTION PERSONNEL Tht particle experiment I.% designed to investigate 11) PI - A.I. SlEllART U OF COLORADO the dependence 01 the intensity ot icnizinp particles in space 01 - C.A. BIRTH U OF COLORADO upon distance 110. the sun; (2) tl.pOr81 variation. 01 the 01 - C.Y. HORD U Of COLORADO particles and their corr~lationwith variations 01 the magnetic 01 - G.E. IHOMAS U Of COLORADO field 8nd p1aS.a flux at the location at the spac.cratt and 01 - D. ANDERSON NOAA-SEL rith solar-terrestrial disturbances; and 13) the intensity and extent ot magnetically trapped particles. it any. around VCOYS. BRIEF DESCRIPTION The instrumentation ronristrd Of three detectors: (1) a This investigation used 8 125-in Casrcgrain telescope an gas-tillcdr integrating. ionization chamber with a wall ot 8 125-nm Ebrrt-Fartie IpCCtrOmCtCI rith I prOg1.1mable grating ?t4inLe11 steeL; (2) an OmnidirtCt4cr.L thin-uallsd rylinoriral drive. Airglorr fcatte~ed Sunlight. and hydrogen Lyman-alpha glass GM tube shielded with stainless steel; and (3) an emissions wtrt detected in the thermosphere. mesosphere. and identical glass G11 tube shielded rith beryllium. The ti0 611 erosohrre at Venus. These neasur.ments dcrc used to establish tubes dittcrtd in the etticiency with which they detected and -10 the rompositionr temperature. and photochemistry 01 the noncenetrating electrons by the tremsstrahlunp pmce~s. All thrr.osphere ana ionosphere. to astermine the pressure at and three detectors "ere sensitive to electrons of energies greater abwe the visible cloud tops. and to establish the distribution than SO0 Lev mnd protons of energic~greater than 10 MeV. The and escape rate of atomic hydrogen. The instrument Optva1.d in ionization Eha.bCl I.. Samp1.E fcr 221.76 I once every 443.52 the 1100-3.00 A region. I. The Count .CCu.ulation 01 the GM tube shielded rlth rt*inl.s* steel "as sampled once tar 0.828 I and Once tor 9.6 s every 4+3.52 I. and the count 8rrumulation ot the berylliu.-shi.ld.d 611 tub. ual sa.pIed once tcr 0.828 s and INFRARED Once fOI 9.6 5 CYCIY 887.04 S. The deteCtDrs were mounted close together with the axes 01 the GM tubts pcrpmdirular to the roll wxis of the spaceiiatt and hrncr to the radius vector from the sun. The GM tubes shirldea rith stainless steel anc beryllium had omnidirectional geometric tartors 01 6.91 and 6.91 sq cm- resPIctiVely. The cxcrriment Operated nor..llv INVESTIGATION WARE- LYfRARED RADLORETER throughout the mission. NSSDC ID- 62-0+1A-02 INVESTIGATIVE PROGRAM CODE EL-). SCIENCE

ULTRAVlOLEl INVESTIGATION DILCIPLINE(S) PLANETOLOGY PLANETARY ATMOSPHERES

PERSONNEL PI - G. NEUGEBAUER CALIf INST OF TECH

BRIEF DESCRIPTION The infrared radiometer on Mariner 2 was designed to measure the radiation temperatures 01 small areas 01 Venus in the 8.4- and 10.4-nirroactrr bands. optic ally^ the radiomrtcr consisted of two similar lens systems whose sics were separated by 45 deg. One system. establishing the chopping reterencer viered dark IC~CC. and the other viewed the planet. The energy through the two systems was combined into a single chopped bra. ------PIONEER VENUS PROBE SWI. suont------

INVESTI6AIION NAME- NET fLUK RADIOMElER (SNfR)

NSSDC ID- 18-Sl8E-04 INVESlI6ATIVE PROGRAM CODE EL-4ICO-OP. SCIENCE

INVESTIGATION DlSClPLINE(S1 PLANETAEJ ATWOSPHERES AERONOWV

PERSONNEL PI - V.E. SUOWI U Of YISCONSIN 01 - J. LENOBLE U OF LlLLE 01 - L.A. SROMOVSKY U OF YISCONSIN 01 - A. fYMAT NASA-JPL 01 - 6.1. DANIELSON CALIF INS1 OF TECH 01 - 1. HERMAN U OF LlLLE BRIEF DESCRIPTION Ihr objectives weir to locate ropions of radiative coniergince and dirergencr as 8 function of 8ltitud* and to indicate the height at rhirh solar energy ia absorbed by the .tmOaph.ir. This experiment usrd a lm81L net flu. radiom.ter cn the Probe t8rgeted to the dayside ot Venus to .SUI. the net solar flu. in the 0.2- to 4-mirrometer ..pion. The 1.0 Probes targeted to the nightside of the planet carried net infrared flux amsort cowiring the 1- to 25-micr0nrt.r region. The instrument reighrd about 0.4 kg and Used 2.2 Y of p01.1. _------PIONEER VENUS PROBE ~112. SUOWI------INVESTl6AlION NAME- NET FLUY RADIOMEIER (SNFII

NSSDC ID- 18-018f-E4 INVESTICATIVE PRO6111 CODE EL-4ICO-OP. SCIENCE

INVESl16AlION DlSClPLINE(S1 PLANEIARY ATMOSPHERES AERONOW

PERSONNEL PI - V.E. SUOIII U OF YISCONSIN 01 - J. LENOBLE U OF LlLLE 01 - I.-A. SROWOVSKY U OF YISCONSIN INVESTIGLIION NAME- INfRARED RADIOWElER COIR) 01 - A.L. FVMAT NASA-JPL 01 - G.E. DANIELSON CALIF INST Of TECH NSSDC ID- 78-0511-16 INVESTlGAlIVE PR06RAM 01 - M. HERMAN U OF LlLLE CODE EL-~/CO-OPI SCIENCE BRIEF DESCRlPllON INVESlI6ATION DISCIPLINE(S1 lhi obj.ctivrs were to locatr regions of radiatiw PLANETARY ATMOSPHERES rorrrgmcr and diverpens. as 8 function ot 8ltitudr and to AERONOMV indicate the height at ihirh aO1.r energy is absoibed by the atmosphere. This experiment used small net flus radiometer PERSOHNEC on the Probe tDlgetrd 10 the dayaide Of Venus to measur. th. PI - F. TAVLOR(NLA1 NASA-JPL net solar flux in the 0.2 to 4 micromete, region. lh. two 01 - H.Y. AUWANN NASU-JPL Probrs targetrd to the nightside ol the p18net carried net 01 - W.T. CHAHlNE NASA-JPL infrared tlvr s.nsors cov.rlng the 1 to 25 .icro..t.r region. 01 - C.B. FARWER NASA-JPL Tbr instiu.rnt rriphed about 0.4 kg 8nd usrd 2.2 Y Of mow,. 01 - J.V. MARTONCHIK NASA-JPL 01 - A.P. INGERSOLL CALIF INS1 Of TECH _-_____PIONEER VENUS PROBE SW3, SUOWI------01 - J.T. HOUOHTON OXFORD. .. U 01 - G.D. PESKETT CLARENDON LAB INVESTICATION NAME- NET FLUK RADloMElER (SNFR) 01 - C.D. ROOGERS OKFOkO U 01 - E.J. YlLLlAMSON CLARENDOL LAB NSSDC ID- 71-0786-04 INVEST16ATIVE PR06RALll 01 - R.E. DICK1NSON NATL CTR FOR ATWOS RES CODE EL-4ICO-OP, SCIENCE 01 - J.C. GILLE NATL CTR FOR AlMOS RES INVESll6AT'lON DISCIPLINE(S) BRIEF DESCRIPTION PLANETARV LTNOSPHEeES This investigation usrd an 8-rh8nnrl r.di0mtel for AERONOWV vertical temperatur. sounding of the atmosphcrr from the tlaud tODS (60 k.) tO 150 k. and for inYeStig.tiona Of Cloud PERSONNEL morphology. rnrludirg the identificaticn of possible .ultlple PI - Y.E. SUOMI U 0.F YISCONSIN liyers and water vapoi marp3ng. Thr instrument 1.1 based on 01 - J. LENOBLE U DF LILLE the srlrttiuc chopper r.diomrtcr and the pressur. modulator 01 - A. FVMAT NASA-IPL. .- radiometer designs flown On Nimbus Sateltitea. 01 - L.1. SROWOVSKY U OF YISCONSlN 01 - 6.1. DANIELSON CALIF INST OF TECH ------PIONEER VENUS PROBE Let. BOESE------01 - II. HERWAN U Of LlLLE

INVESTI6ATlON NAME- INFRARED RADIOWETER (LIRI BRIEF DESCRIPTION The objcrtivcs "err to 10C8tC repiona Of radiative NSSDC ID- 18-018D-05 INVESTIGATIVE PROGRAM ronvelgtnce 8nd divergence as 8 funrtion Of altitude and IO CODE EL-4. SCIENCE indicate the height at Ihich aolar rnrrgy is 8blorbed by the 8t.O.pkert. This experiment used a Small net flu. r8diom.t.r INVESTISATION DISCIPLINE(S) on the Probe targeted to the dayside of Venus to m.asUrr the PLANETARY ATWOSPHERES net ao1.r flux in the 0.2- tD 4-~irromrter region. Thr tu0 AERONOWY Piobes targeted to thr nightside of the pl8n.t carry net infrared flu. sensors covering thr 1- to 25 micrometer region. PERSONNEL The Instrument rri9h.d about 0.4 kg and Used 2.2 Y Of power. PI - R.Y. BOESE NASA-ARC 01 - J.B. POLLACK NASA-ARC 01 - J.Y. MILLER NASA-ARC NASA -ARC RADIO SCIENCE AND CELESTIAL WECHANICS NSSDC ID- 62-0411-08 INVESTICATIVE PROGRAU BRIEF DESCRIPTION CODE EL-4, SCIENCE Deep Space Network tracking data on Uarinrr 5 "err used to obtain imDr6red detcrainations of the masses of vrnus and INVESTIGATION DISCIPLINE(S) the moon. of the astr0nomic.l unit. and improved ephemerides of CELESTIAL UECHANICS rarth and Venus. The rxperimcnt Used the onboard receiver and trlnslitter equipnent in conjunction uith Deep Space Station PERSONNEL equipumt to obtain D0ppl.r mL.SUr1Ient*. The syst~. performed PI - J.D. ANDERSON NASA-JPL rrll to distarcrs of 48.E6 km 1NOvr.b.r 5, 1967). BRIEF DESCRIPTION ---____MARINER 10, HOYARD------Drep Space Network tracking data from Uariner 2 were used to obtain iwrovrd raaaurements of tbe messrs of Venus ard the INVESlIGATlCL NAME- S- AND X-BAND RADIO PROPAGATION moon. the a*tronomicol unit. and improvrd ephemrridcs of thr earth and Venus. The C.pcriment used the Onboard receivrr and NSSDC ID- 73-0811-02 INVESTIGATIVE PROGRAU trensmitter *quipm.nt in conjunction with the Deep space CODE EL-4. SCIENCE Station *guipmrnt tc obtain Doppler .eas~,e..nts. Data uer. obtainrd at 12-h intervals fro. September 5 to DeDrmber 14. INVLSTIGATION DISCIPLINE(S) 1962. at 1-h intervals until D*re-b.t 16. and then again at IONOSPHERES AND RADIO PHYSICS 12-h intorvats until January 4. 1963. PARTICLES AND FIELDS PLANETARY ATUOSPHLRES ------PlONLER VENUS 1, SHAPlRO------PERSONNEL INVESTlSATlON NAUE- CELESTIAL ULCHANICS (OCU) PI - H.T. HOUARD STANFORD U 01 - 6.5. LEVY NAS A-J PL NSSDC ID- 78-0511-21 INVESTIGATIVE PROGRAM 01 - 1.1. SHAPIRO ulss INST OF TEcn CODE EL-4. SCIENCE 01 - 6. FJELDBOINLA) NASA-JPL 01 - A.J. KLIORE HAS A -J PL INVEIIIGAIION DISClPLINElS) 01 - J.D. ANDERSON NASA-JPL PLANETARV AlUOSPHERES CELESlIAL MECHANICS BRIEF DESCRIPTION This ClPCrilent used X- (8400 UHz) and 5- 12113 UHz) PERSONNEL band. on-board radio systems for IhateV.r scientific purposes PI - 1.1. SHAPIRO UASS INST OF TECH could be drvised. Tu0 pP<..ry aoproachc. U~IC mader one utilizing tracking infor*ation, the other taking adrantape of BRIEF DESCRlPllON radio trajectory variations alaOLiated with occuitation of the This eaperiment used the S-bard end X-band radio signals .arth-spacecraft signal. Tracking Information I.. analyzed to for data mealUrCmrnts. The objectives were: 11) to model the determine mass and gravitational ch.ract+ristirs (including gravity field of VrnUsr 12) to estimate the direction and planetary internal composition and density estimates) of both magnitude Of thr VenLS spin vector. (3) to bound the magnitude Venua and Mercury. From anomalous characterirtirs observed in Of land pOSSiblY aSti.at*) the POlw motion Of VenYlr (4) to the I- and S-band signals during SLoCecraft Passage through the determine the density PIOfll. Of the Uppel atmospherer and (5) planetary atmOsphCrCI just prior to. and subseguent to. to aeternine a rcnnection betreen the coordinate system of OccuLtationr temPeratUre and pressure p~fi1~1were calrulatcd. Dlanrtary rphenerides and an inertial coordinate systev Thes* profiles Were useful to adjust ~tlOlPheliLcomposition reference to extragalactic radio IOUICCS. mdels. Signal cutoff provided Usefui information for d.termlnation of planetary ,.diu%. ------)IARINER 5, EIHLEUAN----'------.--.------PIONEER VENUS 1. KLIORC------INVESTIGATION NAUE- TYO-FREPUENCI BEACON RECEIVER INVESlISATION NAUE- RADIO OCCULTATION (OOCC) NSSDC ID- 67-0601-02 lNVESTlGAlIVE PROGRAM CODE EL-4. SCIENCE NSSDC ID- 18-0111-20 INVESllGAllVE PROGRAII CODE EL-4, SCIENCE 1NVfSlISAlION DISCIPLINE (I) PARTICLES AND FIELDS INVESTIGATION DISCIPLINEIS) SOLAR PHYSICS PLANETARV ATUOSPHERES IONOSPHERES AND RADIO PHlSICS PERSONNEL PERSONNEL PI - A.J. KLIORE NASA-JPL PI - V.R. ESHLEUAN STAMFORD U 01 - 1.1. CROFT SRI INTERNATIOMAL BRIEF DESCllPllON This exprrinrnt made use of the S-band and X-band radio BRIEF DESCRIPTION signals for data meas~rem~nti. Thr objectives icrc (1) to Both 423.3-11Hz and the 2/11 rubhermmir 49.8-MHI 3ign.L. m.asur* refractivity ProtiLrs. (2) to measurr 5- and X-band Urrr transmittrd from a 4.6-• steerable'parabolic antenna at disrersion and absorption. 13) to measure electron density Stanford Uniwrrrity to the two-frecurncy rami0 receiver cn the hright protitrsr and 10 to determine the dynamics Of the lower spacecraft. The high-frequency sign01 served as a reference atmOsphCrC. signs1 ainre ita propagation time was not aPPrCciablY delayed. The lor-freguency signal was deleyed in piopoltior to thr total __c____PICNEER VENUS 1, CROFT------electron content in the propagetion path. On the spatrc~att, phase-lOck*d receiver counted the beat-frequency le10 crossings INVESTISATION NAUE- GAS AND PLASMA ENVIRONUENT 106PE) of the rrrrined signals to obtain ne.sur*ments of phase-path differences. Differ.rti~l delay of tlr group wclctity was also NSSDC ID- 76-051A-03 INVESTIGATIVE PROGRAM obserrtd. and these walues wve teie..t*red to the gvound CODE EL-,. SCIENCE station. Fro. Cal

NSSDC ID- 18-078D-06 INVESTILATIYE PROGRAU ATIOSPHERE CODE €L-1. SCIENCE

INVESlIGATION DISCIPLINE(S) PLANETARY ATIOSPHERES AERONOIY

PERSONNEL PI - J.H. HOFFMAY U OF TEXAS. DALLAS NSSDC ID- 78-051A-01 INVESTIGLT IVE PROSRAI 01 - 1.1. MOD6ES. JR. U OF 1EXAS. DALLAS CODE EL-+/CO-OP. SCIfNCE 01 - I. KOLPIN TRY SYSTEIS SROUP 01 - n.n. MCELROI MARVARD U INVESTIGATION DISCI?LIME(S) 01 - T.I. DONAHUE U OF IICHIOAN PLANEIARY ATIOSPHERES PLANETARY IONOSPHERES BRIEF DESCRIPTXON The objcrtirr Of this inrestiqation "ai to measure the PERSONNEL rompd

16 BRIEF DESCRIPTION lhis cxptrlmrnt used the Dtep Space N.tiOik (DSN) telcmttry data. The obitrtirr Mas to measwe and atudy the i~~ll-sc~l~turbulence characteristics of the atmospher. of Venus. Information obtained intlvdrd the v.vi.tIon of NSSDC ID- 78-0781-06 INVESTIGATIVE PROGRAM intensity of turbulence with altitude. rind welocIty tranartrae CODE EL-). SCIENCE to the line-of-aight path. and diatributIon of acale size In the atmoapheie. The.. measuremt ts contributed to an IHYESllGAllOIl DISCIPLlNElS) understanding Of the atmospheve'i circ$latlon and dynamics. PLANETARY ATMOSPHERES METEORCLOGY ------PIONEER VENUS 1, yOO------PLANETOLOGY INVESl16AlION NAME- AlMOSPHERIC AND SOLAR CORONA 1URBULENCE PERSONNEL (OTUR) PI - C.C. COUNSELllAN MASS INS1 OF TECH 01~~ - 1.1..~. SHAPIRO. . MLSS INSl OF TECH NSSDC ID- 18-051A-22 lNVESTlGAllVE PROGRAM 01 - R.G. PRlNN MASS INSl OF TECH CODE EL-). SCIENCE 01 - J. CHARNEY MASS INS1 OF TECH 01 - 6. PETTENGILL MASS INSl OF 1ECH INYESTIGATION DISCIPLINf(S) PLANETAR1 AlMOSPHERES BRIEF DESCRIPTION This elperillent Used the DCCD 5p.c~ Network (DSN) PERSONNEL tsli=ttry signals. lhe objcctivcs bert to measure vector rind PI - R. YO0 NASA-JPL ~~10~itie1by earth-based interferometric tracking for all four probes as they descended through the atmOsphCrC of Venus uslng BRIEF DESCRlPllON the bus telemetry ligna1 as a reference. lhe results YII.C lhia cxprrimtnt made use of the S-band and X-band radlo combined with riaultencous temperaturer presaure~therm.1 flux, signals for data measurements. The objectivas of the and composition measurementi from Other CIPeriments to test experiment "ere to measure: (1) the intensity variation of models of the atmospheric circulation. turbulence with altitude. (2) planetary Latitude and longitude. and (3) the dirtributlon of seal. sizes in the at.OSphele. ---_--- PIONEER VENUS PROBE fM1, yoo------PIONEER VENUS PROBE LP6. RAGENl------INVESTIGATION NAME- AIMOIPHERIC TURBULENCE (MlUR) IIIVESl16A110N NAME- NEPHELOMETER (LN) NSSOC ID- 78-0781-06 INVESlIGAl1VE PROGRAM CODE EL-+. SCIENCE NSSDC ID- 78-078D-02 INVESTIGATIVE PROGRAM CODE EL-+ICO-OP. SCIENCE INVESTIGAllON DISCIPLINE (I) PLANETARY IONOSPHERES lNVESlIGAlI0N DISCIPLINE(S) RADIO PHYSICS PLANETARY IlMOSPHERES CELESlIAL MECHANICS AERONOMY PLANETARY AlMOSPHERES METEOROLOGY

PERSONNEL PERSONNEL PI - R. YO0 NASA-JPL PI - B. RAGENT NASA-ARC PI - J.E. ELAMOIIT CNRS -I A BRIEF DESCRIPTION This czprrirrnt Used the Deeo Spare Network (DIN) BRIEF DESCRIPTION telemetry data. The Objective was to .easUre and atudy the This experiment ronsisted Of nePhe1om.t.r to ...SUII r.al1-scale turbulence rharact*rirticr at the .tmcspheie cf the entrgy tickscattered from cloud partic1.s. It Used a Venus. Intormation obtained included the rariatlon of uulsed 9alIIUm arsenide laser diode to Illuminatt the clouds. intensity Of turbulence with altitude. wind velocity transversi The altitude history of the backacattrred signal indicated the tc the line-of-light pathr and distribution of scale size in Presence and vertical cztcnt of clouds along the trajectory. the atmoiphcre. lhest mtawrements contributed to an COwarilOns "4th the .*asure*ents from the small probea understanding of the .t.OSphllC'S circulation and dyn.*irs. Indicated the spatial v.riability of the cloud structur.. The laser Ouermttd at about 9000 A. The r.ptriment weighed about --___-_PIONEER VENLS PROBE SM2. 1oc------.- 0.5 kg and used about 1.1 u of po~er. INVESTIGATION NAME- AlMOSPHERlC 1URBULENtE (MTUR) ------PIONEER VENUS PROBE $)llrRlGENl------

NSSDC ID- 78-0781-06 INVESTIGATIVE PROGRAM INVESlIGAlION NAME- NEPHELOI)E?ER (IN) CODE EL-). SCIENCE NSSDC ID- 78-018E-02 1NVESTIGAlIVE PR06RAM lNVESllGATlON DlSCIPLIk'E(S) CODE EL-+/CO-OP. SCIENCE PLANElARY IONOSPHERES RADIO PHYSICS INVESl1GATION DISCIPLINE(S) CELESTIAL MECHANICS PLANEIARY AlMOSPHERES PLANElARY ATMOSPHERES AERONOMl METEOROLOGY PERSONNEL PI - R. YO0 NASA-JPL PERSONNEL PI - 8. RAGEN1 NASA-ARC BRIEF DESCRIPTION PI - J.E. ELAMON1 CNRS-SA This C.D.riment used she Deep Space htf-ork (DSNI fele.etly data. The objective ..I to #L.SUIe and study the BRIEF DESCRIPTION rr.11-scale turbulence ch.r.~teristics of the atmosphere of This experiment confisted of a nrphe1omet.r to measure Venus. Information obtained included the variation of tht entrgy backacattrrtd from cloud partlclta. It uaed a irtcnsity of turbulence with altitude, rind Yelocity transverse pulsed gallium arsenide laser diode to illurninat. the clouds. to the lint-of-light path. and distribution of scale size in The altitude history Of the bmCksc.ttCled signal lndfcated the the atmosphere. These measurements contributed to an Prestnce and vertical extent of clouds along the trajectory. understanding of the atmosphere's circulation and dynamics. Comp.risona with the me.~wem~ntl from the other Probea indicattd the apati.1 varIabillty of tht cloud structur.. The ------PIONEER VENUS PROBE SMS, moo------laser 0per.t.d at about 9000 A. The e.otrim*nt ml0h.d about 0.6 kg and ustd about 1.3 Y Of pOYtr. INVESTIGATION NAME- AlMOSPHERlC IUREULENCE (MlUR) -______PIONEER VENUS PROBE SMz, RAGENl------NSSDC ID- 78-018G-06 INVESTIGATIVE PROGRAM CODE EL-). SCIENCE INVESl16AlION NAME- NEPHELOMETER (111)

INVESlI6Al1ON DISCIPLINE(S) NSSDC ID- 78-D78F-02 INVESTIGATIVE PR06RAM PLANElARl IONOSPHERES CODE EL-~ICO-OPI SCIENCE RADIO PHYSICS CELESlIAL MECHANICS INYESlICAl1ON DISCIPLINE(S) PLANElARY AlMOSPHERES PLANETARY AlMOSPHERES AERONOMY PERSONNEL IIETEOROLOOY PI - R. YO0 NASA-JPL PERSONNEL BRIEF DESCRIPTION PI - 0. RAGENl NASA-ARC The InStru#rntS 101 this experiment included a PI - J.E. BLAlOll CNRS-SA single-axis acrsleromrttrr PI~IIUI~ sensors. and temper8ture rensorr. They were based on the technology de.onstiatd by the BRIEF DESCRIPTION PIE1 rocket vehicle (Planetary At.olpherc E.p.ri.ent Test R This experi.ent rmlirtd Of 1 nsphelomttc. to .e.lU,. 7106-2001). The mt.su~..entl IC.~ used to construct protil* the energy b8ckscattei~d trom cloud Tarticlei. It urrd 8 Of at.OSphCric Itate ptoprrtlal for the trajtrtoly fro. the pu1s.d gallium arsenide laiar diode to illuminate the clouas. rurtare to ~pprOIim~tely140 t. altitude. lhcy were all0 used The altitude histo,). 01 the baCtsC.ttered signal indic8tcd the to deterrin. rcrtic.1 rind ~elo~ityrhorizontal rind welocity, pICS~nct 8nd vertlC.1 extent Of ClOUdS along the t*.j*CtOrY. 8nd tuvbulrnte. By ~o.p.rina atmospheric conditions along this C~.paii~oni with the measLrements trom the 0th.. Protei trajectory with those ...lurid by the other Probes. rirrulation indicated the spati8l wariability ot the cloud structure. The models 01 the atmolpheie icrc determined. ?he instruments laser 0p~1.t-d at about 9000 A. The experiment #sighed abaut weighed about 1.2 kp and ronlumed about q.8 Y of power. 0.6 kg and "led abcut 1.2 Y 01 Power. ------PICNEER VENUS PROBE SN2r SElFF------

INVESTIGATION NAME- ATMOSPHERE STRUCTURE INVESTIGATION NAME- NEPHELOMETER (SN) NSSDC ID- 78-078F-01 INVESTI6ATIVE PROGRAM NSSDC ID- 78-0786-02 INVESl16A11VE PROGRAR CODE EL-4. SCIENCE CODE EL-4lCO-OP. SCIENCE INVEST1GllION DISCIPLINEG) INVESl16ATION DISCIPLINE(S) PLANETAR1 ATUOSPHERES PLANETARY AlMOSPHERES METEOROL06Y AEIONCIY AERONOMY METEOROLOGY PERSONNEL PERSONNEL PI - A. SEIFF NASA-ARC PI - 0. RAGEN1 NASA-ARC 01 - S.C. sonntn NASA-GSFC PI - J.E. BLAUONT CNRS-SA 01 - D.B. KIRK NASA-ARC 01 - IS. BLANCHARD NASA-LAIC BRIEF DESCRIPTION 01 - R.E. YOUN6 NASA-ARC This rrperiment consilted ct nephrlometer to measure 01 - 1. DERR US 6EOL061CAL SURVEY the energy bactsc.tteltd fro. cloud DarticlCS. It u1.d pulled gallium arrenide laser diode to illuminate the clouds. The altitude history 01 the backfc8ttered ligna1 indicated the p.tscn~c and vertical extent of clouds along the tr.jectcry. Co.p.~i~oni with the m~alUre.mts trom the Other probe1 indicated the spatial variability of the cloud structure. lhc laser Operated 8t about 9000 A. The experiment weighed .bCUt 0.6 kg and used about 1.3 Y ot Pob~er. ------PIONEER VENUS PROBE LR6r SEIFF------INVESTlGAllON NAUE- ATMOSPHERE SlRUClURE

NSSDC ID- 78-078D-01 IYVESlIGATIVE PROGRAM CODE EL-*# SCIENCE

INVESTl6AlION DISCIPLINECS) PLANEILRY ATMOSPHERES MElEOROLOGl INVEST16AT1ON NAME- AlMOSPHERE SIRUCTURE AERONOMY NSSDC ID- 78-0786-01 INVESTIGATIVE PROGRAM PERSONNEL CODE EL-4. SCIENCE PI - A. SEIFF NASA-ARC 01 - S.C. SOUMER NASA-ARC INVESTIGATION DISCIPLINE(S) 01 - R.C. BLANCHARD NASA-LARC PLANETARY AlMOSPHERES 01 - D.0. KIRK NASA-ARC 01 - R.E. YOUNG NASA-ARC PERSONNEL 01 - J.S. DERR US 6EOLOGlCAL SURVEY PI - A. SElFF NASA-ARC 01 - S.C. SOMUER NASA-GSfC BRIEF DESCRIPTION 01 - R.C. BLANCHARO NASA-LARC The instrum.nt1 for this rxpevimcnt included three-axis 01 - D.B. KIRK NASA-ARC 8rcri*romrtrrr PCISIUTt SenSO*lI and ICmPCratUIC SlnlorS. They 01 - R.E. YOUN6 NASA-ARC usre based on the technology de.clltrated by the PAEl rocket 01 - J. DERR US GEOLOGICAL SURVEl vehicle (Planrt8ry Atmosphere E~peri.cnt Test R7106-2001). The .e.lur..cntS we,* Used tO LOnstruLt a protile Of atmolphsre BRIEF DESCRIPTION state PIODCItieS tor the large probe trajectory tro. the The instruments tor this experiment included a thi.e-.xis surtarr to approxi.ately 140 km altitude. ~hcybere atso "sea arreleromtterr pressure rtnsorsr and tCmperatYre sensorr. They to determine vertical rind velocity. horizontal rind welacity, were based on the technolagy demonstrated by the PAET roct*t and turbulence. By comparing atmoreherir conditions along the vehicle (PLanetaIY At.OSPhIrC EXprrimcnt test R 1106-2001). Lars* probe trajectcry with those measured by the small probes, The .rrlure.entS lCIC Used tO ~DllltlUCt a protile Of rirrulation modcis of the atmosphere were dettrmined. The atmospheric state pi~peiti~~tor the trajectoey tram the instruments weighed about 2.5 tg and ronrumed about +.7 U ot SurfaCC to approxi..tely I40 k. altitude. lhcy were also used pouer. to determine vertical wind relocityr horizontal rind Velocity, and turbulence. By comparing atmospheric conditions along thir trajectory with those mrasurod by the other Probes. circulation eodels ot the atmosphere #ire dctcminca. The instruments INVESTIGATION NAUE- ATMOSPHERE SlRUClbRE (SAS) ueighcd about 1.2 kg and confumed about 3.4 u ot pouer. NSSDC ID- 78-078E-01 INVESTIGITIVE PlOGRAl - - __ - -- PIONEER VENUS PROBE LRGr CROFT------CODE EL-4. SCIENCE INVEST1GATlON NAME- AlMOSPHERlC PROPA6ATION (MPRO) INVESlI6ITION DISCIPLINE(S) PLANETARY ATMOSPHERES NSSDC ID- 78-O78D-11 lNVESllGATlVE PRO6RAU 3ElEOROLOGY CODE EL-4. SCIENCE AERONOPY INVESTIGATION DISCIPLINE(S) PERSONNEL PI - A. SEIFF NASA-ARC PERSONNEL 01 - S.C. SOMMER HAS A-65 F C PI - T.A. CROFl Sill 1NTERNATIONAI 01 - 0.0. KIRK NASA-ARC 01 - R.C. BLANCHARD NASA-LARC BRIEF DESCRlPTION 01 - R.E. IOUNG NASA-ARC The objertjvr Of this C~pCriICntwas to determine the 01 - J. DERR US GEOL061CAl SURVEY atmosphcrir structure ot Venus as it affected the intensity and refraction ot probe tClImCtry signals. An investigation of the interfcrencr between the direct ray and a ~~rt~~e-~~tlrttrd component "as undertaken as means of assessing c~iiunications reliability tor the design of future probe missions. _--_-_-PIONEER VENUS PROBE sni. CROFT------scientific rvaluatlon. INVESTIGATION NAME- ATMOSPHERlC PROPAIAT1ON IMPRO) ------PIONEER VENUS PROBE 511. COUNSELMAN------

NSSDC ID- 18-018E-07 INVESTlGATlVE PROGRAM INVEST1GATlON NAME- DIFFERENTIAL LONG BASELINE CODE EL-+. SCIENCE INTERFEROMETER (DLBI)

INVESTIGATION DISCIPLINE(S) NSSDC ID- 78-0781-03 INVESTIGATIVE PROGRAM PLANETARY IONOSPHERES COOP EL-+, SCIENCE RADIO PHISICS CELESTIAL MECHANICS INYESTlGAllON DISCIPLINE(S) PLANETARY ATMOSPHERES PLANETARY ATMOSPHERES METEOROLOGY PERSONNEL IERONOMY PI - 1.1. CROFT SR1 INTERNATIONAL PERSONNEL BRIEF DESCRIPTION PI - C.C. COUNSELMAN MASS INS1 OF TECH This r.pcti.ent used the Drep Space NetioIk (DSL) 01 - 1.1. SHAPIRO MASS INST OF TECH telemetry data. The objectives "ere (1) to determine the 01 - R.G. PRINN MASS INS1 OF TECH atmospheric structure of Venus as it affects the intensity and 01 - 1. CHARNEY MASS INST OF TECH refraction of Probe telemetry signals. and (21 to inv.stigatc 01 - G. PETTENGILL MASS INST OF TECH the interference between the direct ray and a f~rfo~r-reflected coaponrnt as "ran8 of assessing communications reliability BRIEF DESCRIPTION for the design of future probe missions. This e~perimcnt involved applying differential very-long-basrlin. interfrromctry teehniques to the radio ------PIONEER VENUS PROBE 1112, CROFT------signols from the entry Probe and Bus in Ordrr to infrr or place upper limits on rind speeds in the 1or.r .tmOsphere. These INVESTIGATION NAME- AlMOSPHERIC PROPASATION (MPRO) IesUlts were used in modeling thr circulation patterns of Venus' atnosphir.. Dit. taken prior to Probe entry weit used, NSSDC ID- 78-0781-01 INVESTIGATIVE PROGRAM where feasible, to infer characteristics of Venus' gravity CODE EL-4, SCIENCE field far usc rith Probe entry operations as well as in later srirntifir evaluation. lNVESTIGATION OlSClPLINE(S) PLANETARY IONOSPHERES ------PIONEER VENUS PROBE 112, COUNSELMAN------RAD10 FHYSICS CELESTIAL MECHANICS INVESTIGATION NAME- DIFFERENTIAL LONG BASELINE PLANETARY ATMOSPHERES INTERFEROMETER (DLBI)

PERSONNEL NSSDC ID- 78-018F-03 INVESTIGATIVE PROGRAM PI - 1.1. CROFT 5111 INTERNIllONAL CODE EL-+. SCIENCE

BRIEF DESCRIPTION INVESTIGATION DISCIPLINE(S) This Cxperiwrnt Used the Deep Space Network (DSN) PLANETARY ATMOSPHERES trlIs*tly data. The objcrtivrs urre (1) to det.rllne the METEOROLOGY ot.oiph*iic StiuitLIe of Venus ms it affects the intensity ard AERONOMY refraction of Probe tel..etry signals. and (2) to ~nrrrtigatr the interferwce between the direct ray ond a sUrfaC~-r~fliCted PERSONNEL ccmponent as reans of ~SSCISIII~communicatio~s rrliatility PI - C.C. COUNSELMAN MASS INS1 Of TECH for the design of future probe nirsions. 01 - 1.1. SHAPIRO MASS INST OF TECH 01 - R.G. PRINN MASS lNST OF TECH ------PIONEER VENLS PROBE 5113. CROFT------01 - J.G. CHARNEI MASS INST OF TECH 01 - 6. PETTEN6lLL MASS INST OF TECH INVESTIGATlON NAME- ATMOSPHERIC PRDPA6ATION (MPROI BRIEF DESCRIPTION NSSDC ID- 18-0786-01 INVESTIGATlVE PROGRAV lhii c.pcri.cnt involved applying difttrrntial CODE EL-+. SCIENCE wry-long-baseline interftrometiy techniques to the radio signals from the entiy Probe and Bus in order to infer or p1.r. INVESlIGATION DlSCIPLlNE(S1 upper limits an Mind speeds in the lorrr atm~spherr. These PLANETARY IONOSPHERES results wrre used in modeling the circulation patterns of RADIO PHYSICS Venus' .tmorphere. Data taken prior to Probe entry "ere used. CELESTIAL MECHANICS where feasible. to infer char.rtrristirs of Venus' gravity PLANETLRY ATMOSPHERES field for use rith Probe entry operations as re11 as in later scientific evaluation. PERSONNEL PI - 1.1. CROFT SR1 INTERNAIIONAL ------PIONEER VENUS PROBE 5113. COUNSELMAN------

BRIEF DESCRIPTION INVESTIGATION NAME- DIFFERENTIAL LONG BASELINE This experiment used the Derp Space Network (DSN) INTERFEROMETER (DLBI) telemetry data. The objectives were (1) to determine the .t.CschCrlC struct~reOf Venus IS It affect1 the intensity and NSSDC ID- 78-0186-03 INVESTIGATIVE PROGRAM refraction~ ~~~ of Probe~~ trlrmetrr ~~~ rian.13. and 12) to inwrstiaatr CODE EL-*. SCIENCE I~_~~~~ ~ ~ ~~~ -~ the interference brtrcrn the direct ray and a Surfarr-reflected componint as a mrms of aiscrsing rommunirations r.Iiability INVESTIGATION DISCIPLINE(S) for the design of fLturc probe missicrs. PLANElARI ATMOSPHERES METEOROLOGI ------PIONEER VENUS PROBE LRGI COUNSELMAN------AERONOMY INVESTlGATlON NAME- DlFFEYENTIAL LONG BASELINE FERSONNEL INTERFEROMETER (DLBI) PI - C.C. COUNSELMAN MASS INS1 Of TECH 01 - 1.1. SHAPIRO MASS INS1 OF TECH NSSDC ID- 78-07BD-09 INVESlI6AlIVE PROGeAI1 01 - R.G. PRINN 1ASS INS1 OF TECH CODE EL-). SCIENCE 01 - J. CHARNEI MASS INS1 OF TECH 01 - G. PETTENGILL MASS INST OF TECH INVESTIGATION DISCIPLINE (5) PLANETARI ATMOSPHERES BR IEF DES CRlPTlON METEOROLOGI This expcriicnt involved applying differential AERONOMY uer~-long-barelinr interfrromctry techniques to the radio rignalr fro. the entry Probe and Bus in order to inter or place PERSONNEL upper limits on wind speeds in the loicr atmosphere. lhei~ PI - C.C. COUNSELMAN fuss INST OF TECH r~iulti"ere used in madeling the rirrulation patterns of 01 - G. PETTENGILL MASS INST Of TECH Venus' atmospherr. Dit8 takrn prior to probe entry were used, 01 - 1.1. SHAPIRO MASS INST OF TECH where feaiitle, to infer characteristics of V~IIYI' gravity 01 - R.G. PRlNN MASS INST OF TECH field for use rith Probe entry opecationr as re11 .I in later 01 - J. CHARNEY MASS INST OF TECH scientific evaluation. BRIEF DESCRIPTION - -_- - __ PICNEER VENUS PROBE LRGI KNOLLENBERG------This c.peri.en t involud applying d if f c~ent i a 1 utry-long-b*sclinr interferometry techniques to the radio INVESTI6ATION NAME- CLOUD PARTICLE SIZE SPECTROMETER (LCPS) signals from the entry probe and bur in order to infer or place upper limits cn bind speeds in tte lower atiospheit. These ~e~ultsIC~C used in modcling the circulation patterns of Venus' atmOsphCIC. Data taken prior to probe entry "ere used. where feasible. tC infer cha,acteristics of Yenus' gravity field for use rith probe entry oprrationr as re11 IS in later

ORIGINAL PAGE IS OF POOR QUALlrV NSSDC ID- 18-078D-C3 INVESlIGAlIVE PROGRAM CODE EL-*. SCIENCE

1YVESl16Al10N DISCIPLINE (I) PLANElLRT ATMOSPHERES AERONOMT

PERSONNEL PI - R. KNOLLENBERG U OF CHICAGO 01 - D.M. HUNlEN U OF ARIZONA

BRIEF DESCRIPTION The objective of this expcrimrnt was to measure venui' cloud particle sizes and concentrations. A laser was used to illu.in,te clfud particles. Optlral lenses imaged the particle rhadorr on ~11.~1 of detectcrs. lhe particle sladcwa rcre used to detersine particle rile and conrentration. The flight sensor was similar to thoar flown in aircraft and ballacns. ____--_PIONEER VENUS PROBE LRG, O"AnA------.

INVESlIGAlION NAIIE- GAS CHROMATOGRAPH (LGCI

NSSDC ID- 18-018D-CI INVESllGlllVE PROGRAM CODE EL-4, SCIENCE

INVESlIGAlION OISCIPLINE(S1 PLANETART AlROSPHERES AEROIICWT

PERSONNEL PI - V.I. OTAIIA NASA-ARC 01 - J.B. POLLACK NASA -ARC 01 - 6. CARLE NASA-ARC 01 - F. YOELLER NASA-ARC

BRIEF DESCRIPTION The objective of this experiment IIS to determine the cc.~csition cf Venus' lower atmorphrrt. From these measurements. deductions were made Of the gaseous sources of infrared Opacity. the dcgrea Of differentiation of Venus. interior, the degree of similarity between the solid bodies of earth and VCIIYI, and evolution of Venus' atmoschere. Tu0 gas ch.omatograph COLY.~~ icrc used to analy2e fam~l.l of the at.olphere during probe dcrrcnt. -___---PIONEER VENUS PROBE LRG, 10nASKO------

INVESlIGAlION NAME- SOLAR FLUX RADIO(IE1ER (LSFRI

NSSDC ID- 78-0180-01 INVESlIGAlIVE PROGRAM CODE El-). SCIENCE

INVESllGAllON DISCIPLINE

PERSONNEL PI - n.~. TOMASKO U OF ARIZONA 01 - Y. YOLFE U OF ARIZONA 01 - A. CLEIIENTS U OF ARIZONA

BRIEF DESCRIPTION lnc objtctiv. cf this investisation "as to determire the regions in Venus' atmosphere "her. solar energy is deposited. Six narrow-field-of-vicy detectors were used to measure the irtensity of scattered solar light. As the Probe descended thrOUsh the atmosphere. the difference bttuccn upuard-LcOking and dornrard-Looking detectors indicated the net dornrard flux.

POLARIZAlION Mars MARS

Plate 3. This is a composite of press release photographs from the Mariner 9, Vikings 1 and 2 Orbiter, and Vikings 1 and 2 Lander missions. (A) 211-5050 is a mosaic of Viking Orbiters' medium-resolution photos depicting most of one hemisphere of Mars and showing the Valles Marineris (4000-km-long canyon), the Tharsis bulge's giant volcanoes, and the very large Argyre basin. (B) P12732 is a Mariner 9 high-resolution photo of part of the Valles Marineris, discovered on this mission, showing some of the arroyos, the largest of which resembles our Grand Canyon in size and appearance. (C) 211-5248 is a mosaic from Viking Orbiter photography of Arsia Mons, one of the giant shield volcanoes on Mars. (D) P17002 is a Viking 1 Orbiter mosaic photo of the terrain near the Viking 1 Lander's site showing features that are best explained as the products from flowing water. Conditions in the past must have been different, permitting free water to form in large quantities, which is not possible at present on Mars. (E) 211-5685 is a Viking 1 Lander photo of the immediate surroundings of the spacecraft at its landing site in Chryse Planitia. Note the presence of many loose rocks, rock outcroppings, and dune-like areas. (F) P16848 is a Viking 1 Orbiter photo of Yuti, showing a type of crater unique to Mars which has an enormous, high central peak with a summit crater. The large central peak and large, multi-layered ejecta envelopes do not follow the Schroter rule for impact craters. (G) P12694 is a Mariner 9 photo of Phobos, the larger and closer of the two tiny satellites of Mars. The photo shows the moon to be irregular in shape (only 20 krn long) and highly cratered. Mariner 9 was the first to obtain detailed photos of these moons. Viking Orbiter photos later revealed long grooves and crater chains on Phobos and deep dust on Deimos. (HI Viking 2 Lander photo shows the immediate surroundings of the spacecraft in the Utopia region of Mars. Note that most of the rocks have a pocked or vesicular surface and that they are quite different from those at the Lander 1 site in (E). One of the footpads landed on a rock.

42 A

I 1-1 INTRODUCTION

Mars is the next planet out from the sun that is treated in this catalog. Six missions have been sent to Mars by the U.S. and several by the U.S.S.R., but since NSSDC has no data from the U.S.S.R. missions, they are omitted in this catalog. The last missions, Vikings 1 and 2, consisted of two spacecraft each: (1) Viking Orbiter and (2) Viking Lander. Each spacecraft is treated separately. On these missions there were 49 investigations for which NSSDC has data or sources from which data may be obtained. These investigations cover eight categories: (1) Imaging, (2) Particles and Fields, (3) Ultra- violet, (4) Infrared, (5) Radio Science and Celestial Mechanics, (6) Atmo- sphere, (7) Surface Chemistry, and (8) Biology. The last two categories of investigations are unique to Mars. Tables 1 and 2 and Appendix A give more details of these investigations. SPACECRAFT ...... PERSONNEL PM - H.M. SCHURMEIER NASA-JPL PS - J.A. STALLKAlP NASA-JPL SPACECRAFT COMMON NAME- MARINER 4 ALTERNATE NAMES- 00942 BRIEF DESCRIPTION Mariner 7 was the Seventh In a series Of IpbCCIIaft used NSSDC ID- 64-0114 for ptanetary cxplor.tion in the flyby mode. It was identical to the Marlner 6 sp.cecraft. Mariner 1 I.. attltude stabilized LAUNCH DATE- 11128164 YEIGHT- 262. KG in three axes (referenced to the sun bnd the star. Canopusl. LAUNCH SITE- CAPE CANAVERALI UNITED STATES The spacecraft "as solar powered and rapbblr of continuous LAUNCH VEHICLE- ATLAS telemetry transmission. It was fully automatic in operation although it could be rrpr0gramm.d fro. earth during the SPONSORING COUNTRYlAGENCY mission. The ~p.errr.ft "as oriented entirely to ~1anrt.r~ UNITED STATES NASA-OSSA data acquisition, and no data were obtained during the trip to Mars or beycnd I.,.. mariner 1 pairid 3.430 k. from mars on INITIAL ORBIT PARAMETERS August 5, 1969. Thr spacecraft instru.rnts took TV images of ORBIT TYPE- MARS FLYBY Mars and measured the cadi0 1.1r.ctivity and UV and IR emissions of the Martian atmosphere. The mission was a PERSONNEL ."CLC*I. PM - J.N. JAMES NASA -J PL PS - R.K. SLOANiNLAl NASA-JPL ...... BRIEF DESCRIPTION Mariner 4 was the fourth in 8 series of SP~Cecrbftused SPACECRAFT COMMON NAME- MARINER 9 for planetary exploration in a flyby .Ode. It was designed to ALTERNATE NAMES- MARINER-1, MARINER MARS 71 conduct closeup scie~tificobservaticns of the planet Mars an0 MARIN-1. PL-1120 to transmit these observations to ebrth. Other mission 05261 objectives "ere to perform field and particle IeasUICmCntI in interplanetary space in the vicinity of Mars and to provide NSSDC 10- 11-0511 experience in and hro.LCdge of the ersinerring cacabilities for interplanetary flights of long duration. After 1.5 months of LAUNCH DATE- 05130111 YEIGHT- 907. KG flight. the ~p.~~~ibftflew by Mars on July 14s 1965, and LAUNCH SITE- CAPE CANAVERAL, UNITED STATES returned 21 pictures PIUS21 liner cf picture 22. The closest LAUNCH VEHICLE- ATLAS-CENT 1DDIO.Ch 11s 9.846 hm from the Martian Surf.re. The SP.cecrift Performed all p*OgTa*.Cd activities ruccrsrtully at the proper SPONSORING COUNTRYIAGENCY times and returned useful data from Launch until October 1965, UNITED STATES NASA -OSSA rhcn the dirtanre from earth anc its antrnra orientaticr temporarily halted the signal arguisition. Oat. acquisition INITIAL ORBIT PARAMETERS resumed in Late 1967 and continued until Dit*mbCr 20, 1967. ORBIT TVPE- AREOCENTRIC EPOCH DATE- 11114171 ORBIT PERICD- 754. MIN INCLINATION- 64.1 DEG ...... PERIAPSIS- 1381. KM ALT APOAPSIS- 16000. KM ALT PERSONNEL SPACECRAFT COMMON NAME- MARIkER 6 PP - D. SCHNEIDERMAN NASA-JPL ALTERNATE NAMES- PL-691E. MARINER MARS 691 PS - R.H. STEINBACHER NASA-JPL 03759 BRIEF DESCRIPTION NSSDC ID- 69-014A The narinrr lirr 11 mission was ptanned to consist of two SD.CCCIaft On COmplemrtlt.rY lissionsr but due tO the failure Of LAUNCH DATE- 02124169 YEIOHT- 180. KG Mariner 8 to Launch PIOPCI~YI only one spacecr.ft vas LAUNCH SITE- CAPE CANAVERAL. UNITED STATES available. Mariner 9 combined mission objectives of both LAUNCH VEHICLE- ATLAS Mariner 8 (.a~pino 70 1 of the Martian surface1 end Mariner Y (a study of tempOr.1 changes in the Martian atmosphere and on SPONSORING COUNTRYIAGENCY the Martian surfare). For the i~rveypoition of the mission, UNITED STATES NASA-CSSA the planetbry surface ubs to be mapped iith the same resolution as planned fcI the original missionr although the resolution of INITIAL ORBIT PARAMETERS pictures Of the polar regions would be dcCrc.Std due to the ORBIT TYPE- MARS FLYBY increarrd slant range. The variable fcbturcr experiments were changed frcm studies of six given areas every 5 days to studies PERSONNEL of sma1111 regions every 11 days. Mariner 9 arrived at Mars on PM - H.M. SCHURMEIER NASL-JPL Novenbei 14, 1911. The spaoecrsft gathered data on the PS - J.A. STALLKAlP NASA-JPL atmospheric composition. density, I)~CSIUIC. and temperature and also the surface composition. teapirature, and topography of BRIEF DESCRIPTION M8-S. After depleting its Supply Of attitude rDntrDL gas# the Mariner 6 was the sixth in a series of spa~tciaftused ~pac~craftwas turned off October 21. 1912. for Flanetary sn~lcration in the flyby mod.. Mariner 6 ras attitude stabilized in three axes (referenced to the sun and ...... the stair C~~ODYI). The ~pi~ecraftwas solar polered and capable of continuous telemetry transmission. It was futly autonatic in oFerationr although it could be reprogrammed frcr SPACECRAFT CClMON NAME- VIKING 1 ORBITER earth during the mission. The spacecraft was oriented entirely ILTERNATE NAMES- PL-1330. VIKING-0 ORBITER to Dlonetary data mcquisitionr and no datb yere obtained during VIKNG-8 the trip to Mars or bcyona Mac*. Mariner 6 passed 3.431 b. fro- Mars on July 31, 1969. The SP~CCII.~~ instruments took TV NSSOC 10- 15-0751 il.gcS Of 1.11 and .C.sYrCd the radio r.fr.LtiviIy and UV and IR emissions of the Martian atmoiph.re. The aission was a LAUNCH DATE- 08120115 YEIGHT- 1110. KG sbcc.ss. and data lrcn it yere "sea to progrba Mariner 7. LAUNCH SITE- CAPE CANAYERALI UNITED STATES ...... LAUNCH VEHICLE- TIlAN SPONSORING COLNTRIIAGENCY UNITED STATES NASA-OSSA SPACECRAFT COMMON NAME- MARINER 7 ALTERNATE NAMES- PL-691F. MARINER MARS 698 ORBIT PARAMETERS (3831 ORBIT TIPE- AREOCENTRIC EPOCH DATE- 06121116 ORBIT PERIOD- 1479. MlN INCLINATION- 31.9 OEG NSSDC ID- 69-0304 PERIAPSIS- 1513. KM ALl APOAPSIS- 32600. KM ALT

LAUNCH PATE- OS121169 uEiGni- 380. KG PERSONNEL LAUNCH SITE- CAPE CANAVERAL, UNITED STATES PM - J.S. MARTIN(NLA) NASA-JPL LAUNCH VEHICLE- ATLAS PS - G.A. SOFFEN(NLA) NASA-LARC SPONSORING COUNTRYIAGENCY BRIEF DESCRIPTION UNITED STATES NASA-OSSA The Viking spacecraft consisted of an orbiter and a lander. The lander Separated from the orbiterr entered the INITIAL ORBIT PARAMETERS Martian .tmOsphere. and Soft-landed July 20. 1916. Scientific ORBIT TYPE- MARS FLYBY data lCIL CCllCct~d and transmitted to Earth from the lander during entry and rhile it was on the surface, and from the orbiter before and after lander ~*p.r.tion. The orbiter was a solar-cell-porcrrd satellite stabilized in three axes using inertial and celestial references. There was a 500-Y power cawtity for the orbiter. lt carried instruments for conductino imaminor itiorohcric rater YIOOI, thermal macoinar and radio Fhotographic 72 kg (158 lb). Thr crbitrr 11s an crtagon appio~imately2.5 m NSSDC ID- 75-f83C access. The right sides of the ring-like stiuctur. uw. -457 high and “ere alternately 1.4 .M 0.6 ride. Thr Viking Orbit.. LAUNCM DATE- 09109175 YEI6YT- 590. 16 1 oprrations wrre ttrminatrd on Sipt.sber 30. 1980. Enpertmrnt LAUlCM SITE- CAPE CANAVERAL. UNITE@ SlATfS oprrations wre terminated on August 7, 1980. for detailed LAUNCH VEHICLE- 7lTAN description of thr Viking mission and rxperi.entir ser -Scientific R*suIts of the Viking Pmj.ct.’ J. 6eophys. Res.. SPONSORlNC COUNlRTlASENCT v. 82, n. 28. 1917. UlITED SlAlES NASA-OSSA ...... INITIAL 09011 PARAMETERS OR017 TVPE- MARS LANDER

SPACECRAfT COMMON NAME- V1KLN6 2 OR0ITER FERSONNEL ALIERNATE NAMES- PL-733Ar VIKN6-A PM - J.S. MARTIN(NLA) NASA-JPL VIKIN6-A ORBITER PS - 5.1. SOFFEl(NLA) NASA-CAllC NSSDC 10- 75-0831 0RIEf DESCRlPTlON Ihi8 sPacecr.ft was tho Imding v.hicle for the two-part LAUNCH DATE- 09109115 YEIGHT- 1092. 16 spar.rraft mission. 11 soft-landed on s.ptemb., 3. 1916. in LAUNCH SITE- CAPE CLNAVERALI UNITED SIATES the UtOpIa regton Of Mars at 47.67 dRg N latitude and 225.71 LAUNCH VEHlCLE- 11TAN d-9 Y longitude. The land., carrird instmmrnta to study the biologyr chemical romporltion (organic and iaorgmirJr SPONSORING COUNlRTlAbENCT metroralogyr seismology. magnetic proprttirs. surface UNllED SlAlES NASA-OSSA appearance. and physical pr0p.rties of tho Martian surfac. and atsosphrrr. The lander had 70-Y pow- capactty and a ORBIT PARAIIETERS Sri.ntifiC D.YL0.d Of .PpIOIi..tely 91 kg (20) lb). SO.. Of ORSIT TTPE- AREOCENIRIC EPOCH DAIE- 08/09/76 the data collrctad sere returned by direct ea410 link 10 earth. 011011 PERIOD- 1639. n1N INCLINATION- 55.2 DE6 but most of the data were returned by r.lay th,ough one of the PERIAPSIS- 1499. KM AL1 APOAPSIS- 15800. KM ALT Oibtt*is. The Iandrr was approximat~ly3 rn across and about 2 high. Thr Viking Lander 2 reasrd oprrating on April 11. 1980. PfRSONNEL for drtailed description of thr Viking mission and PI - J.S. MARTIN(NLA1 NASA-JPL rnp.rimonts see ‘Scientific R.suIts Of the Vlking Project.- J. PI - G.A. SOffEN(NLA) NASA-LARC 6cophya. Res.. v. 82, n. 28. 1971.

BR1ff DESCRIPTION DNESTIGAM)Is The Viking stac.cr.ft consirled of an orbiter and a lander. Thr lander ~tp.,.tcd from the 0rbitr.e entered the IMA61N6 nartian .t.osph.rrr and soft-l*ndrd September 3r 1976. Scientific data lire collected ana transmitted to Earth from the lander during entry and while it Uas On the surface. and from the orbiter before and *iter lander s.p.r.tion. lhe ------MARINER 4, LE16HTON------orbitrr was a s0l.r-cill-porered satellite stabilixrd in threr axes using inertial and celestial refrrmces. 1h.r- 1.1 a INVEST161110l NAME- MARS TV CAMERA 500-Y power capacity for the orbiter. It carried instruments 101 ronductinp I.aging. atmospheriC water VaDOIs th*l.*l NSSDC ID- 64-@111-01 INVESlISAlIVE PROSRAM mapping. and radio science investigations. The scientific and CODE EL-4. SCIENCE photog rip hi^ .n.lysir instru.rntr tad a -1s. of .pprO~i~~tOlY 72 kg (158 Ib). Because of thr loss of altitude furl. the INVESTI6ATION DISCIPLINE(S) transmitters and e~p+ri..nt~ rere turned off July 25, 1978. The PLANElOLOST orbiter 10s an citagon .ppr~ii.at.Iy 2.S ac10.s. The light sides of thr ring-like atiucturr wrrr .a57 high and Mrrr PERSONNEL alternately 1.4 ard 0.6 ride. For a detailed description of ri - 1.0. LEISHTON CALlf INST OF TECH the Viking mission and .xp.ri.entsr see ‘Scientiftr R.suIts of the Viking Project,’ 1. 6eophyl. Res.* V. 82. n. 28, 1977. BRIEF DESCRIPIION The mars t.lerision eiperimrnt 1.1 designed to obtain ...... photographs of tho Martian surface and lelr..ter them to ..ith. The 1v subsyft.. ronsts1.d of (1) a Caaseprain n.rror-mglo refl*rting telrscop. with 30.5-rm effective focal length and SPACECRAFT COMMON NAME- VIKING 1 LANDER a 1.05- by 1.05-dep field of view. (2) a shutter and fittrr ALTERNATE NAMES- VIKIN6-0 LANDER assmmbly that had 0-08- and 0.20-~ t.pOaur. times and uaed rrd and Omen littrrs. (3) a slow scan ridicon tube. with a 0.22- NSSDC ID- 75-075C by 0.22-in. sq target. vhich tranalatrd thr optical image into an .lectrical video sipn.1, and (4) related .l.clronics LAUNCH DATE- 08/21/75 YEIGHT- 605. K6 ineluding a TV data encoder. On July 14. 1965. at 0018 Ul. thr LAUNCH SITE- CAPE CANAVERAL. UNIIED STATES plctu,. rrCOrCing srgurnce COmmenCmd. Vidicon Output underrent LAUNCH VEHICLE- TITAN anatog-todigital conrrrsion and data stored at 2401000 bits per pirtuvc on a tio-trackr 114-in.. 330-ft long. magn.tir SPONSORlNG COUNTRVIAGENCT tape loop on the spacecraft. 110 of every thire pictures taken UNITED SIATES NASA-OSSA were recorded on thr tape. resulting in a chain of Pairs of overlapping. alternatrly filtered pictures r#trnding acroas the IYIIIAL ORBIT PARAMETERS dirk of Mar.. Data were transmitted after occult.tion of thr ORBIT TYPE- MARS LANDER sp.~ecraft by Mats by the radio subsystr. from July I5 to 241 1965. and were processed in vr.1 time by a .704417094 system to PERSONNEL format magnetic tapes of the image data fnv processing by thr pn - J.S. MARTIN(NLA) NASA-JPL Ranger trlevision proresslng programs and for convcraion to PS - G.A. SOffEN(NLA) NASA-LARC film record. Conversion from .lwtriral signals to an optical image ma prrformed by the vidro-to-111. recoidar uatng 64 BRIEF DESCRlPTlON shadrs. The .xp.ri.cnt yielded 21 Picturrs plus 21 linrs of This spacectaft was the landing vehicle for the tiOvar1 pi~t~ri22. This prrformancr indicated a normal rrcording sp.tecratt mission. It soft-landea on July 20. 1976. in the sequmcr. Com~u1.1 proc*ssing .rograms yieldid photographs Chryse region of Cars at 22.27 deg L latitude and 41.94 dcg Y with pilater contra11 than the raw image data. A drt4il.d longitude. The lander carried inatrumcnts to study the description cf the telerision .xpeii.ent. data piocrssing. and biology, chrmic.1 coiposition (organic and inorganic). the wmriour versions Of the photography ran br found in the JPL mete~rology~ srir.ology. magnetic propeities. surface -Mariner Mars 1964 Project R.pOrtr lelrrision Eiprrimentr Part atpearancer and th,sical propelties cf thr Martian surface ard 1. Investigators. Reports- of the Rarinrr IY Pictures of Mar.. atmosphere. The lander had a 71-Y pouer capacity 8nd a TR 32-884. 1961. scientific payload of appioximattly 91 kg (200 Ib). Same Of the data collcct~d here rcturrrd by cirect radio Link to earth. ------M’lR1)ltR (, LEI6HTON------+------but most of the data were returned by relay through one of the orbiters. lht lander *as .ppr~iimatcly 3 rn across and about 2 INVESTISATION NAME- MARS 7V CAMERA high. for a detailed descriptioF of thr Viking mission-and experiments see ‘*Scientific Results Of the Viking Prolectr J- NSSDC ID- 69-0141-01 INVfSTIGATIVE PRObRA1 GeOphyS. ICs., Y. 82. n. 28. 1977. CODE EL-4, SClENCE ...... INVEST16ATION DISClPLINE(S) PLANETOLOCI

SPACECRAFT COMMON HAME- VIKlNG 2 LANDER ALlERNATE NAMES- VIKING-A LANDER

OR161NAf PAGE IS OF POOR QUALITY PERSONNEL PI - R.B. LEIGHTON CALIF INST OF TECH BRIEF DESCRIPTION Tu0 trlwisicn c...rasr one of medium resolution (uidr NSSDC ID- 11-051A-04 INVLSTICATIVE PRO61AM angle) and the other of high IeSClUtiOn (narror angle). were CODE EL-4. SCIENCE part of the Marine, 6 scientific inat.umrntation. The wide-angle camera. which had field of vier of 11 de9 by 14 de9 and a fOc.1 length of 50 rmr ~nc0Dpass.d 100 tiwa .CII surface area than the narrow-angle came.. and was used only for near-encounter pictures. The n8rror-angl. ca-era. which waa PERSONNEL used for both near- and f.r-cnrountrr Pictureir had focal PI - m. MASURSKV US 6EOLOCICAL SURVEV length of 508 ma anc provid*d 10 tiwea the linear resolution of 01 - 6. DE YAUCOULEURS U OF TEXIS. AUSTIN the ride-angle L~VLI.. Ca..ra shutt.,~ were alternated and 01 - J. LEDERBERG STANFORD U 1ia.d to provide overlapping of the ride-angle and 01 - Y. THORPSON BELLCORRr IYC narrow-angle pictures. providing 1I pictures from the tic syatens (25 ne.r-cncounttv and SO far-encounter). The BRIEF DESCRIPTION nrar-encounter pic1ur.a usre taken between I3 "in 59 s before This rxpcrinmt conslated of a 2-in. ridiron teleriaion ercounter and 2 .in 55 s after encounter along track that camera which transmittrd photography from Mar.. It was a crossed the equatoii.1 ionta of the planet and included nany phOto~~tiic8llycalibrated inatrumrnt providing overlapping, known light and dark features of the Martian surface. The selectiw.1~ filt.ied. low-resolution pictures and broadband far-encounter pictures were obtained in tu0 series of (unfii1cr.d) high-resolution pictures. each nes1.d in a operations. In the first series. 33 pictures were obtained lor-reaolutior overlap. 00th types of pictures had between 48 h and 28 h before encounter. In the second series, .purOximat.ly 1 100- by 38O-rlrment format. and an 17 picturea I.IC obtained between 22 h and 7 h from rloscst Order-Of-magnitude differem. in resolution betreen them. 8EprOa~h. The pict~redata "ere erc0d.d and recorded within Resolution of 500 mlTV line and SP ./TU line resulted fron IOU the onboard television and dat8 storag. aubayttems. for tach (11 d.9 by 14 d.9) and high (1.1 de9 by 1.4 deg) resolution PiCtUIe produced by the Cameras. three SepalmtC encoded pictures taken at a pcriapais altitud* of 2000 k.. The rcrsions ICI. trans.itted to earth -- a cornposit. analog video official Ordering system of id.ntifiration of pictures uaa by a (CAY) picture. digital video (DV) picture. and an every 9-digit number called Data Automation Sit (DAS) which ia turnty-eighth (ETE) digital DiltYIC. Video r.construrtion chconological and a kind of ti... More than 1.300 pictut.8 of rcnsisted of ro-bining the three data stmama (CAW. DV. and the martian surfare. the Martian aatellitea. Saturn. and star FTE). This generatee video data as they *listed coming Out of fields acquired during the mission. A variety of picture the camera heads. The teIem.tered video .agn.tic tapes were enhancement techniques h8d been applied to th. original data displayed on a CRT and photographed on 70-mm film to produce resulting in more than 30.000 photographa being available the rad images. They usre also digitally processed by an IBM through NSSDC. Theae different versions of the original 360144 CO.pUter for enhancement and by an IBM 360111 for noiar imagery I.,. proc.aa*d using the Ris8ion Test Video System removal to obtain the rrrsiona contained in data aets -011. (MTVS) and the Image Processing Laboratory (IPL) at.JPL. through -01H. Detailed information on the digital proceasing procedures can be found in "Digital Proc.ssing Of the Mariner 6 and 7 pictures.' 1. C. Rindfleish et al. J. 6eophya. Res. . v. 16. p. 394-417, Jaruary 1971. Accurate tiajectOry and related INVESTl6ATION NAME- ORBITER IMAGlN6 geometrical data ran be found in Mariner Mars 1969 SimYl.ted TV Pictures (Final). J. N. Campbell. 19101 which 1.5 issued by NSSDC ID- 75-0151-01 INVESTIGATIVE PRO6RAM JPL. CODE EL-4ICO-OP. SCIENCE

- - -_- - - MARINER 7, LEIGHTON------.------*-- INVESTIGATION DISCIPLINE(S) PLANLTARV ATROSPHERES INVESTIGATION NAME- MARS TV CAMERA PLANETOLOGV

NSSDC ID- 69-0301-01 INVESTIGATIVE PROGRAP PERSONNEL CODE EL-4. SCIENCE TL - n.H. CARR US 6EOL061CAL SURVEY in - Y.A. BAUR LOYELL OBSERVATORV INVESTIGATION DISCIPLINE(S) in - H. RASURSKY US GEOLOGICAL SURVEY PLANE 1CLOGV TP - 6.1. 011665 NASA HEADOUIRTERS TM - J.A. CUTlS SCIENCE APPL. INC PERSONNEL in - T.C. DUXBURY NASA-JPL PI - R.B. LE16HTON CALIF INST Of TECH in - K.R. BLASIUS SCIENCE APPL. INC Tll - R. SREELEY IRIIONA STATE U BRIEF DESCRIPTION in - J.E. GUEST U OF LONDON Two tclcrision vidicon cameras. one of .-diu. rtaolution in - K.A. HOYARD US 6EOL061CIL SURVEY (ride angle) and the other rf higI reaOlUtiOn (narrow angle). in - 0.1. sniiH U OF ARILONA *e,. part of the Mariner 1 scientific instrumentstion. The in - L.A. SODERBLOM US 6EOLO6lCAL SURVEV wide-angle cam.r.. rhich had a FOV of 11 deg by 14 deg and a in - J. VEVERNA CORNELL U focal length of 50 .sr encompaaaed IC0 times mare surface area TI - J.O. YELLMAN NASA-JPL than the narrow-angle camera and 10s Used only for near-encountcr pict~res. The nar*cw-angle cameras which "sa BRIEF DESCRIPTION used for both near- and f.r-tnCOuntcr Pirturcsr had fora1 The Viking uiaual imaging aubsyatem (VIS) ronsis1.d of length of 508 II.and provided lo tiwes the linear r.aolution of tiin high-resOlUtiOnr alor-arm tel.riaion framing cam.ies the rids-angle C~CIS. C~C.. shutters were a1trrnst.d and mounted On the acan Platform ot each orbiter with the optic81 timed to PIOY~~C ovcil.pping of the wide-angle and narrow-angle axes offset by 1-38 deg. Each Of the tu0 identical cameras On pictures. providirg 126 picturea fro. the two syst.ma (33 each orbiter had 475-mm fw.1 length 1.l.acop.; a 37-mm neav-encountei and 93 far-encounter). The n.ar-mcOunler diameter ridiron. the central s.ction of rh'ich vaa .canned in pictures YC~Ctaken betreen 20 min 26 8 before closeat approach raster format of 1056 lines by 1182 samples; and six color ard 2 rin 6 I alter cL0SC.t. approach along roughly filters to relfrlct the sp.Cti.1 bandpass Of an #.age 10 nolth-sO~th COUIS. that 3nt.VSLlt.d the Mariner 6 track and 1i.it.d portion. of the n.ar-visu.l response Ch.ract.rtstics. included the Martian south polar cap. The far-encounter Each field of vier was 1.54 d.g z 1.69 dep with each pictu,. picturea were obtained in three aeriea of oprrstiona between 68 clement (pixel) subtending 25 microradian8. The alight offaet h and 5 h before iloa~atapproacb. Two frartional picturea cf the Optical axes and the alternate ahutteting mode of "ere obtained at the end of the first two series. The picture operation (the *ntrrw.l betwern frames being 4.48 s) urorid.d data isre encoded and recorded within the onboard television overlapping. wide-aiath coverage of the aurface. Individual and data storage s~bsyiteis. For rich pictuce produced ty the imigea art identified by picture number (PICNO). which ia a (.metas three separate encoded versions were trmamitted to unique identifier of the scene. Elementa of the PICNO are .a earth: a composite analog video (CAY) picture. I digital video follors: the fivit thrrr digits denote the revolution (REV) (DY) PicturC. and an every twenty-eighth (ET€> digital picture. during uhirh the image was ahuttercdi the 1.tter A is Viking video reconstruetion consisted of combining the three data Orbiter Ir B is Yiking Orbiter 2; and the 1.81 two digits are streams (CAV, DV. ana ETE). This ger.ra1.d iidao data as they the frame number. Operation of this experiment I.. terminated Cxiattd coming out of the cmmera heada. The tel.met.red video on Auguat 1. 1980. magnetic tapes bere displayed OE a CUT and photographed on 70-mm film 10 Produce the raw imagea. They "ere also digitally ------VIKING 2 ORBITER, (ARR--'------prorrrsrd by an IBM 360144 c~~p~teifor .nhancem+nt and by an IeM 360115 for noise rcnoval to obtbin the versions contained INVESTIGATION NAME- ORBITER IMAGING in data sets -0lC through -01H. Detailed informatio: on the digital piocessing proced~r~scan be found in Digital NSSDC ID- 15-083A-01 INVESTIGATIVE PROGRAR Prorclsing of the Mariner 6 and 7 Pictu1.8r' 1. C. Rindfleiah CODE EL-4ICO-OP, SCIENCE et at.. J. Gcophys. Res.. Y. 76. pp. 394-417, January 1971. AccUIate trajectcry and r.lated 9eCr.tliCal data can be found INVESTIGATION DISCIPLINF(S) in Mariner Mars 1969 Simulated TV Picture. (Final)r J. K. PLANLTARV ATMOSPHERES Campbelle 19701 which was iaaued by JPL. PLANETOLO61

49 PERSONNEL PERSONNfL TL - a.m. CARS 1L - 1.1. RUTCH(DECEASED) NASA HEADQUARTERS in - Y.A. Bun TU - C. SAGAN CORNELL U in - H. MASURSKV TU - A.0. BINDER U OF KIEL TU - 6.1. BRlGGS TI - E.C. MORRIS US GEOLOGICAL SURVEY in - 1.1. Culls SCIENCE AWL. 1NC in - FA. MUCK NASA-LARC in - T.C. DUIBURV N,A SA -J PL TI - E.C. LEVINTHIL IUCLLAR REGULAlOPV COR in - K.R. BLASIUS SCIENCE APPL. INC TI - 5. LIEBES, JR SlANFORD U TI - 1. GREELEV ARIZONA STATE U TU - J.B. POLLACK NASA-ARC 1M - J.E. GUEST U OF LONDON in - R.E. ARVIDSON YASHINGlON U TI - K.A. HOUARD US GEOLOGICAL SURVEY in - 8.1. SMIIH U OF ARIlONA eRlEF DESCRIPTION Tn - L.A. SODERBLOM US GEOLOGICAL SURVEV The lander imaging txperiacnt viered the scene in - J. VEVERKA CORNELL U surroundino the lander. the suif.ct sampler and other parts Of 1M - J.B. YELLIAN NASA-JPL the lander. the sun, Dcimor. and Phobos to provide data for cpcrationll EUrposCs and for geologic.1 and .atcorologirz.L BRIEF DESCRIPTION investigations. Two scanning cameras. capable of resolving lhe Viking visual ibaging IUbsyste. (VIS) consisted of 0.04 dcg (high--.ts01utionI 01 0.12 dcg (Lor-icrol~tion~cola,, trin high-i*sOIutiCnr slow-scan television framing cameras and IR) IeIC used On Cath lander. Each image acquired r0YeICd mounted on the scan pl.tfOl. of tach orbiter rith the Optical a rcrtiral field of 20 de9 (high-rc~olution) or 60 deg axes offset by 1.38 aeg. Each of the two identical cameras on (lor-resoluticn, rolorr and IR) and a horizontal field that #as each orbiter had 1 475-mm focal length ttlescope; 1 37-mm ro.mandablc from 2.5 dcg to 342.5 dcg in 2.5-deg increments. diameter ridiron, the central secticn of which was scanned in I.agCS Were acquired fro. 40 dCg above the nominal horfzon to raster format of 1056 lines by 1182 samples; and si. color bo deg below, and were romm.nd.bla in 10-drg increments. The filttrs to IC=tliCt the Spectral b.ndp.SS Of an image tO C..CI.S "ere mounted 1.3 above the nominal landing plane and Limited poitlons ct the cameras' near-visual IespOnSr itre rapable of vicring tu0 tootpads and most of the area characteristics. Each field of rieu was 1.54 deg a 1.69 deg accessibLI to the surfare ranpler. lhc two cameras rith each Dictum element (pile0 subtending 25 microradims. Separated by 0.8 me and StCreOSCOpiC pirturcs were obtained The sllght Offset of the Optical ..e. and the alternate over most of the scene. BLack-Nvd-rhitr i.apci in either lor shuttering mode of operation (the interval bctIcen tr.mes being 0. high rcroluti~nincluded vadiation wavelengths from 0.4 to 4.48 s) provided overlapping. ride-.lath

------"IKING 1 L"#DER, I"T(H------PARTICLES AND FIELDS

INvESllGATION NME- LANDER 1MA61NG

NSSDC ID- 15-015C-t6 INVESTlGAllVE PROGRAn CODE EL-). SCIENCE INVEST1bAllON NAME- HELIUI (IAGNETOIIPTER INVESIICAlIDN DISCIPLINE(S1 PLAWETARV ATMOSPHERES NSSDC ID- 64-07TA-02 INVESTIGATIVE PROGRAM MElEOROLOGV CODE EL-4r SCIENCE PLANETOLOOY lNVESllGATlON DISCIPLINE(S1 PERSONNEL PARllCLES AND FIELDS TL - 1.1. IUlCH(DECEASED1 NASA HEADPUARTERS INlEIIPLANETARY PHYSICS TM - C. SAGAN CORNELL U 111 - A.B. BINDER U OF KILL PERSONNIL in - E.C. noanis US GEOLOGICAL SURVEV PI - E.J. SIIITh NASA-JPL in - F.O. MUCK NASA-LARC TI - E.C. LEVlNlHAL NUCLEAR REGULAlORV Con BRIEF DESCRIPTION in - s. LIEBES. JR. SlANFORD U A wector lor-field helium m.gnCtO.ete1. not to be in - J .E. POLLACK NLSA-ARC confused with the rubidium vapor or helium vapor m.gnCtOmeterr TM - R.E. ARVIDSON YASHlNGlON U 11s used to measure the interplanetary magnetic field. The three components Of the field were measured CssenIialLy BRIEF DESCRlPllON si.ult.n.ously but later tranr~ittcd sequentially. Each The Iandtr imsging e.perimrnt rirurd the scene observation reprtrmtcd an average over ~p~ro~imat~ly1 I. The surrounding the lander. the surfart samnler and other parts Of r~sp011sC dropped 3 dB for frequrnrics Of 1 Hz. and higher the lander. the sun. Phobos. and Dei.0. to provide data tor frequency information MIS essentially lost. In each data op.r.tion.L pu.poses and for geclcgic~l and met~omlcgical frame. four ~~ctormrarurcmcntr were made separat~d by investigations. lro scanning ca.er.sr capable of reiolring intervals Of 1.5, 0.9. and 2.4 I. The whole frame was repeated 0.04 deg (hiph-r.rolution) or 0.12 dcg (low-rcrolution. rolorr every 12.5 I. There was an uncertainty of plus or minus 0.35 and In) yere Used cn each larder. Each image arcuirrd coverem nT per rooponent. NSSDC has all the data from this experiment. a vertical field Of 20 d.9 (high-resolution) 01 61 deg Most Of the data from this investigation was of the (Low-resolution, colorr and In) wnd a horizontal field that was interplanetary region. but some data were obtained at Mars. r0m.mdablc fro. 2.5 deg to 342.5 deg in 2.5-de9 intrc.rnts. Images wce arquireo from 40 dcg .tCVI the nomir.1 horizon to 60 deg belour and I~IC commandable in IO-drg increments. The c..eras were mounted 1.3 above the nominal Landing plane and ULTRAVIOLET 111. Capable Of viewing 110 f0Ctg.d. and mast Of the area rrr.ssible to the surface sampler. The tu0 cameras #*IC Separated by 0.8 Re and stcreoscoFic pictures were obtained over most of the scene. Black-and-white images in either low 01 high rrroluticr inrludQd radiaticn uavelengths from 0.4 to 1.1 mirrometrrs. lhc use Of a single detector to image an lNVESTlGAllON NAME- UV SPECTROIIETER entire frame allored a relatiwe radiometric accuracy of plus or minus 10 percent. For more information concerning the caaeras, NSSDC ID- 69-014A-04 INVESTIGATIVE PROGRAM see muck et al.. Space Science Instrumentation. Y. 1, 0. CODE EL-4. SCIENCE 189-214. 1915. INVESTIGATION DISClPLINE(S) ______VlKlNG 2 LANDER, MulCH------PLANETARV AlIOSPHERES

IhvESllGAl10N NAnE- LANDER 1nAGING PERSONNEL PI - C.A. BARTH U OF COLORADO NSSDC ID- 15-083C-06 INVESl16Al1VE PROGRAM 01 - C.U. HORD U OF COLORADO CODE EL-4. SCIENCE 01 - J.B. PEARCE RADIOPHVSICS. INC INVEST16&lION DISCIPLINE (S) BRIEF DESCRIPTION PLAMETARY AlIIOSPHERES Spectral measurements were made of the UV radiation MElEORCLOGV emitted from the U4rti.n atmosphere dmc to resonmce scattering PLAN ElOL 06 1 Et solav radiation 110. the upper atmosphere, risonmce reradiation. fluoresrcnrrr and PhDtoCLeCtlOn excitation of neutral and ionic constit~entsfound in the lower part of the atmosphere. The follouing parameters were determined: the ~iesince of certain atoms. ions and molrrules in the upper and lore. atmOsphire. their rtrpectire scale heights. the degree of atmospheric Raylciph scattering due to carbon dionide- and surface reflectivity in the UY. The instrument was an

50 Eteit-Fastis scanning fl0nochr0mator with dual photomultiplier NSSDC ID- 11-0511-02 INVEST16ATIVE PR06RAM det.ctOisr used in the focal Dlwr. of roflrrting plwn.tary CODE EL-). SCIENCE coronogrwph. Incoming light passed through a baffled light shade wnd struck the primary telescope mirror, which focused INVESTIGATION DISCIPLINE (I) the light through a preslit Ontc 8 s.cOndary uirror. From PLANETOLOGY there. the light us. tocu%ed onto the mtrmre slit Of the PLANETARY ATMOSPHERES spCctrO.etCr. Entering the spectrometer, the rwdiation was collimated by the first half of the ,Eb.rt mirror Onto 8 PERSONNEL diffraction grating. Diffracted light us ther focused onto PI - C.A. BARTC U Of COLORADO exit slits by the second half of the Ebert mirror. A separate 01 - d.5. PEARCE RADlOPHYSICS~ INC rift slit was provided for each Of the two det.CtOrs. The 01 - C.Y. HORD U OF COLORADO position Of the spectral images with respect to the exit slits was rontrnlled by ryclically scanning the grating. with a scan BRIEF DESCRIPTION iron lor- to high-rwvclcngth tak1Pg 2.82 sr and the grating The Mariner 9 ultraviolet spectrometer (UVS) experiment return taking 0.18 I. The rivelength region from 1900 A to "8% deSigncd tO rrrrlve UV radiation (1100 to 1520 A) fro. the 4300 A was c0vti.d in first order as seen by Cne of the two Surfare and .t.OsphCrC Of Mars, Scan selected bands Of this slits. and the rwnge from 1100 A to 2100 A measured in second radiation. and provide an intensity ralur as function of order by the other. The photO.ultiplier detector used for the ~avelength on the basis of scan-cycle tine. The scientific long-ravwlcngth rwrge Operated in tbc gain modes. so that Valid objectives of this c.perim*nt fell into tu0 broad ratepories. mewsureimts could be made over the entire dynaflic rmge from UV cait0gr.phy and UV aeronomy. The UV cartography inuo1v.d 100 to 101000 Rayleighs. The SFeLtrat reroiution Of the neasurements in the UV of the (11 local atmspheric PIIS%U,~ instrument was 20 A at 2950 A in first ordei. A spe~trum1.5 over the major portion of the planet. (21 local ozone produced every 3 sr and contained 6CO vwlurs frcn tach of the Conrcntrltion. (3) nave of darkening, (4) uaiiwbility of tu0 detectors. Thirty-si. values Here used as fiducial period surf*ce fsaturrs. (51 yellor clouds. blue hazer and blue mcwsur...nts and 564 for spectral measUrem.nts. Measu~~ments clearing, and (61 10c.l v.ri.tions in the oxygen-ozone of Lymwn-alpha raciation at 1216 A were also taken after ibundanccs fcr detecting signs of biological activity. The Uv encounter. LLIS than 30 .in Of data "ere Obtained from both aeronomy inwolved measwementi in the UV of the (1) composition channels during the Mariner 6 near-encounter .quatari.l scan on and structure of the upper atmosphere as a function of July 31. 1969. The uuality of the Oat. 1.8 com~wrablrto the Latitude, 1onl)itude. and ti.?. (2) uaii.bility et the rat. of best obtained by rockets in the 13O-km-.nd-.bore region of the escape of wtomic hydrogen from the exosphere. and (3) earth's atmosphere. More experiment dctwils can be found in, distribution and variability of the UV ~UIOI~and determination 'Carinrr 6 and 1 ultraviolet Spectrometers.- J. 0. PC~ICC. et Of the induced planetary magnetic field. In addition. when a1.r Applied Optics. Y. 10. n. 4, April 1911. Marl "as occulted fro# the instrument FOY. Observations of strong stellar sou~cesof UV were made. The optics and sensing ------MARINER 1, BIRTH------.-.------portion of the UVS consisted of an Ebert grating sp~~t~om~ttr with ti0 snit slitsr a light baffle. an ocrulting slit INVESTIGATION NAME- UV SPECTROMETER telescoPe~ and two photoeultiplier tube (PMl) light fens~ri. The incident UY radiation passed through the baffling systei, NSSDC ID- 69-0301-04 INVESTIGLTIVE PROSRAM which cliainatcd any stray light, and entered into the CODE EL-4. SCIENCE te~escOP~. The tClescOp~ prilary mirror reflected the radiation to secondary mirror through a pitslit where it "as ZNVESTIGATION DISClPLINE(S) focused onto the entrance slit Of the Ebert sp~~trometerrwhich PLANEIARY ATMOSPHERES isolated monochromatic radiation from the incoming radiation. The radiation from the entrance slit filled hwlf the Ebert PERSONNEL mirror rhcrr it was coll~matedand reflected onto the grating PI - C.A. BARTH U Of COLORADO (2160 1intrl.m) so that the radiation filled the grating. The 01 - C.Y. HORD U OF COLCRADO grating roteted over a small angle by .@ins of a ran-follorrr 01 - J.B. PEARCE RADIOPHYSICSI INC drive and diffrwcted the radiation. Diffracted radiation of different vavelengthrr depending on the grating angle, fell on BRIEF DESCRIPTION the other half Of the Ebert mirror, which focusid it onto the Spectral newsurements were *ad+ Of the UV radiation two exit slits, thus providing the wavelength scan. The two emitted from the Martian at.0sph.i. due to resonance scattering photomultiplier tubes sensed radiation from their respecti~e Of solar radiwticn from the urcer atmospherer resomanee exit slit and were sensitive only to selected bands in the uv rciadi.tion. fluor.srence. and photoelectron eacitation of SPectlUW -- 1100 to 2000 A (channel 1) and 1450 to 3520 A neutrwl and ionic constituents found in the lower part of the (channel 2). Channel 1 I.. detected by the PMT rith a rcrivi ataosphere. The tOlLOYing Parameters were determined: the iodide photocathode and lithiu. fluoride Yindou and included prts.ncc of certain atoms. ions and .al~cul~sin the upp.v *PO the date used in the UV arronory study. Channel 2 IIS lorer atmosphere. their respective scalt heights. the degree of detected by the PMT eith a cerium telluride photocathode and atmoiph.ric Rayleigh scwtterinp due to carbon dio.id.r and sapphire uirdor and included the data used in the UV surface rcflectiwity in the UV. lhi instrument LIS an cartography study. The UVS scanned the uavclcngth range with a Ebert-Fastie scanning monorhro~wto. with dual phOtOmult$plier 3-s period and a spectral resolution to, first-Order spectra of detectors used in the focal DIw~.of a reflecting planetary 15 A. The ravelength of any given photometric sampl~in the UV ccionograph. Inccmi~g light pisseo through 1 baffled light spectrum mas known to plus or minus C A or better. The Mariner shade and struck a primary telescope mirror that f0CUs.d the 9 Data AUtCIatiOn Subsystem (DASI caused each channel to be light through a prs-slit Onto a %econdary mirror. Ffo. there. SamDICd every 5 ms. Channel 2 11.1 sampled 2.5 .I afte, channel the Light was focused onto the entrance slit of the 1. There uerc 200 ssmplcslslrhanncl. total of 400 uvs spectrometer. Entering the spictrcm.tevr the radiaticn ~lss SwmPIesIs. tach sarplr was digitized to eight bits ana one Collimattd by the first half of the Ebert mirror Onto s sign bit in the DAS. The instrument had dynamic range Of 200 diffraction grating. Diffracted light was then focused onto Rayleighs pet 20-A interval to 50 LilORayleighs PCI 20-1 -,it slits by the r.cond hwlf of tte Ebert mirroi. A sepafate interval for channel I wnd 200 Rayleighs per 20-1 interval to exit atit was provided for each of the two detectors. The SO mrgaRayleighr per 20-1 interval for channel 2. Channel I position of the spectral images rith respect to the exit slits had a field of view sufficient to permit imaging a portion of was controlled by cyclically scanning the grating, with scan the Martian surface subtending 0.19 by 1.9 deg of arcI while fro* Lou- to high-warelcngth takirg 2.82 sr ard the grating channel 2 was limited to 0.19- by 0.55-dcp field of YicI. return taking 0.18 s. The ~avelengthregion from l9DD A to Channel 1, at slant range of 5,700 Umr ricued a column of 4300 A ID8 Covered in first Older as Seen by 0°C of the tu0 space 100 km above the Martian surface that "as 24 by 240 La. slits. and the rarOI fro. 11DO A tc 2100 a measured in ICCC~I channel 2. on the other hand. at a vertical distance of 1.250 Order by the other. The photomultiplier detector used for the kmr rievcd 2.21- by 6.5-kn area at the subsparerrwft point on long-~.v.l.ngth range Operated in two gain modes so that valid the planet's Iurfacer while at a vertical distance Of 850 kn measYrCI.nts could be made over the entire dynamic range from the are. viewed was 1.5 by 4.5 km. The UVS had four 100 ta 101000 Rwlcighs. The spectral resolution of the fundamental reasuring geometries during an orbit: (1) bright instrument uas 20 A at 2950 A in fivst order. A spectr~mwas limb, (2) illumin.tcd dirk. (3) terminatorr and (41 dark limb. Produced evcry 3 wnd COntBined 6CO values from each of the In addition to taking complete UV sp*ctrar the instrument two detectors. Thirty-sir valuer bere Usad as fiducial ~cricd design a110 allorrd for rampling at 1216 A (L~m.n-.lph.l to .essur*msnts and 564 for spectral measuremmts. neasucements utilize a Iorrr data rate iode. This altored Lyman-alpha data Of Lyman-alpha radiation at 1216 A were also taken .way fro. to be taken for a large percentage Of each Orbit. The encounter. Less than 30 rinutes cf data were obtained from experiment began Collctting tlccllcnt data SOD" after Orbital both channels during the Mariner 1 newt-encounter scan of high insertion on November 13, 1911. and continued until April 2. Latitude and polwr regions in the Martiwn southern hemisphere 1912. rhcn the CxpCri.Cnt Was shut Off tO LDns~lvCspacecraft On August 5. 1969. The UualitY of the data I.. ro.p.rwblr to poicr during s01.r occultation. The rnperimcnt MIS reactivated thr belt obtained by sounding rockets in the 130-k. and abcve on June 8, 1912. after the spwcec~aft emerged fro. solar region of the earth's atmosphere. Additional experiment occultation. It continued to op~rat~normally until 2200 UT On details can be found in 'narinsr 6 and 1 ultra~ioiet October 21. 1912. when the crperinent "as shut off along with SPCctrOmeters~" 1. 8. Pearce. et at.. Appliwd Optics, V. IO. n. the rest of the Mariner 9 sp.cecraft. 4, April 1911. - - -_-_- RARlNER p, B~s,"------INFRARED INVESTIGATIDN NAME- ULTRAVIOLET SPECTlOlETER (UVSI

51 F ERSONNEL PI - 1.1. HANEL YASASSFC 01 - D.J. CONR&TU NAIA-CSFC 01 - 1. VRABWAKARA(NLA1 NASAdSTC NSSDC ID- 69-014A-DZ INWEST16ATlVE PRO61111 01 - 6.Y. BIOSPIIER1CS. IlC CODE EL-4. SCIENCE 01 - 8. NASASSfC 01 - W.A. NOLA -NE SI 01 - 11.6. NASA-61 FC 01 - ?.D. NASA-CSFC 01 - J-A. NASA-CSfC 01 - 1.E. NASA-JVL PERSOUNEL 01 - J.C. NASA-CSFL PI - G.C. PIMEMIEL U Of CALIF, BERKELEI 01 - K.C. HERR U Of CALIF. BERKELEI Bllftf DESCRlPlION lh. Mariner 9 infrared inteiferom.tei apoctmm.1.r (1nIS) esperimmt I.. designed to provide Informtion on the v.iticot a1ructur.r rompoaition. and dynamlrs of the atmosphere and on the emirsire pr0pertl.s of the surface of Mars. Meas~r.momta were mode in the region of thermai emission apoctra from 6 to SI micrometers. using modified Nichelaon in1.rf.rom.t.r with a ape'tr.1 r*aolution Of 2.4 inverse cm (apodiied) and 1.2 inuerse cm (unapodized). to determino tho vertical tempwature profiler general atmospheric circulation, minor atmospheric constituent.. and surface 1.rnperatw.e. composition. and th.rm.1 pVODertieS aa function Of latitude and loc.1 tlme lor dark and bripht ore.. and the polor cmv region. lho inatrumentatlcn. m0Ynt.d on the bottom of the apacocroft on a multiple-pointingr motor-driwen acan platform. senaiatad prlmaiily of (1) 0 acon mirror. (2) a cootad c.siUm Iodide entrance rindcrr (3) a ceaiu. iodido beam sp1itt.r. (4) a find mirror. (5) a mor.ble mirrov with e(.rt.omagnetlc dvivs. (6) condensing mirror. (1) 0 thermistor bolo.eter d.t.ctOr. (8) a referenre intorfirometer. (91 an intornal wim blackbody catibrator. and (la) 0 progrom~r. The .can mirror ae1sct.d In radiation from one of throe directions; Mwsr deep S~~CII01 the intern01 "arm blockbody. Fro- thia mirror, tho radiation "ma reflected to the interferom.ter through th. mtranro window. which acted as an 111 flltor ond hsd an effectlvo aperturr are0 of 10 sq em. The baa- sp1ltt.r then divided tho incoming radiation into two ~pp101imot~Iy.qual romponenta. After reflections fvom the fixed and moving mirrors. respectively. the tu0 beams interfered with each other ond 10r8 focused by the rondenaing mirror onto the bolomotrir detector. which provided an *l*CtrlCal Output prOp0Ctlon.L to the infensit), .I a fvnrtlon of the path Linsth diff...na. 0. ph.se different. between the 111 r.diation Id1ect.d or tr0nrmitt.d by the be.. splitter. The .lLLtrSCml Output. converted fro. NSSDC IO- 69-0301-02 INVESTIGATIVE PROGRAM analog to digital foil. was called an interferogram and CODE EL-4. SClENCE rrprrrmtrd a circular fringe potter" that appearad at tho fOi.1 plane of th. rond.nrln9 mirror. Emch interf.rogr.m had 1NVESl16AT10N DISCIPLINE(S) duration of 18.2 s and rantmined 4,096 smplts. After sewan PLANETARY ATNOSPHERES interferograms were taken in tho opmrating mode, on. ".a token PLANElCLOGY of the internal 10,. (298 plua or mlnus 3 dtg I) blackbodyr f01101.d by another Set Of seven mars 4ntorf.rogra.s. .nd PERSOUNEL finally by an interf.rogrom from the de00 apmto background (4 PI - G.C. PIMENTEL U Of CALlfr BERUELEI des). The ln1S1 rhlrh had field of vier of 4.5 deg. viered 01 - K.C. HERR U Of CALIF. BERKELEI an area 116 k. in diameter from an orbital altltude of 1.600 km. The instrument "as identirml in all critical a1.0a to the inte.femmet..s designod for the Nimbus-8 and -D rnot~~r~l~gicol s.tellites. ezceDt that the Mariner 9 IRIS had better ap.strol resolution. The experiment bsgon coll.cting 0.r.llont data soon after Orbital insertion. NSSDC has all th. useful data that exist from thia investigation. ---_---MARINER 6. NEUGEBAUER------

I*YEST16ATION NAME- TWO-CHANNEL IR RADIONETER MARS SURFACE TENPLRAlURE

NSSDC ID- 69-014~-oa 1NVESTIGAlIWE PROGRAM CODE EL-+. SClENCE

INVESlI6AlION D-ISCIPLINE(S) PLANElOLOSY . PERSONNEL PI - 6. NEUOEBAUER CALIF INS1 OF 1ECM 01 - 6. NUNCII NPI-IEIDELBERO 01 - S.C. CHASE. JR. SAY11 BARBARA RES ClR BRIEF DESCRIPTION The equivalent blackbody temperature of the M0rti.n surface "e. determ1n.d by means of 0 two-channel infrared radioaeter. rhirh measured the infrared energy emitted in the 8- to 12-micrO.cter and 18- lo 25-.icro.ct*r bands and had 0 dynanic range of 120 to 330 drg I. lhe two chann.lar located in atmospheric rindori. emphasized the upper and lower lNVESTlGATlON UAME- INFRARED INTERFEROMETEII SPECTROMETER te.per.turef of this range. reipectiv~ly. lh. experiment package located on the bottom of the octagonal .con platform of the spac.craft. The radi0met.r conslated of two NSSDC ID- 71-0511-03 IUVESTlGAllVE PRO61111 refracting te1rscop.s each equippod rith an uncaoled CODE EL-4r SCIENCE anti.ony-birmuth thirmopilt detector. The e.p.riment used an optical trait that included a rotatable plane mitror. rhirh INVESTIGATlON DISCIPLINECI) reflected the incident energy into the detector telearopes. PLANETARY AlMOSPHEllES The mirror had three orthogonal position.. The firat posltion PLANEICLOGV ricvrd empty space and obtoinrd 0 zero energy r.ference. the second viewed the planet. and the third measured the therm01 energy radiated by 1 temperature calibration plate. After space 1.1 rirrtd for one frame Count (4.2 5). 13 obstrvationa of the planet were mode at 2.1-s interrals in each rarelength channel. lhrn. folloiing short look at the temperotur. rrfrrmcr plater 14 more planetory Observations were mad.. The cyclc~ rhlch Ialted 63 a (15 frame rounta). 10s then repeated. Leginning with vier of SD.I*. lbout 21 .in of dato wore

52 digit81 stepping motor. The 42-1 scan cycle was contrOll*d by the Mariner 9 Data Automation Subsystem (DAS) and consisted Of the folloring vleuing .Odes each s*p8l.t.d by 0.25-a 8c.n interr.1: planet (19.2 a), space (2.4 s), planet (18.0 1). and thermal rrfermrr (2.e a). The radiation from the source being viewed at 8 given ti.. entered the IRRr "8. I.fl*ltd Off the Scan mirror. P.8S.d through the objective lens. SpeCtr8L filter. and field Lens. and I.. focused Onto the detector. The detector then converted the incident radiant flux to 8 VOlt890. INVESTISATION WARE' ~~~-CHANNELIR RAD1OMETER RARS SURFACE The Inn data samples were taken in pairs. each pair consisting TEMPERATURE Of . rh8nnel-1 l..ple and channel-2 sample. Data Pails appeared at 1.2-5 intrrr8l.r rhilc the intrrv8l betieen s.mp1.s NSSDC ID- 69-0301-13 lNVESTICCTIYE PROSRAM in a pair I., 200 ms. The dynric range of the instrument was CODE EL-4. SCIENCE optimal from 150 to 325 deg K. The sensitivity of the 111 "as PLUS Or minus 0.12 deg K at 300 deg K and plus Or minus 0.6 de9 INVESTICCTION DISCIPLINE(S) K 81 140 dig 1. Mounted on the M8rinrr 9 pL8net8ry sc8n PLANETOLOGV platform. the IRR h8d a 20-sq-cm aperture with 8n unobstructed vier of 11a.s subtending a minimum of 15 deg half-angle. At 90 PERSONNEL deg to this aperture and directly opposite the thermal PI - 6. NEUCEBAUER CALIF INST OF TECH r.f.rence plate (f18t-bl8ck curved aluminum pl8te)r the 01 - 6. MUNCH MPI-HEIDELBERC aperture h8d 8n unobstructed vier of deep space subtending 20 01 - S.C. CHASE. JR. SANTA BARBARA RES CTR by 20 deg. The IRRI which was boresighted with the n8rror-anplr TV camera to within plus or minul 0.3 deg. h8d 8 BRIEF DESCRlPTlON r~rolution at the subsatellite point on the SUrf8Ct Of Mars of The rquiralrrt blackbody t..F.r.tYII Of the Martian 20 by 20 km and 25 by 25 km for channels I and 2. vespe~tivelye Surface "8s deterwired by arans Cf 8 tho-rh8nn.l infrared fro. the ptriapfis altitude of 2000 fa. The instrument vas r8diOmtter, uhich measured the infr8r.d energy emitted in the basically the same as th8t flown on the M8riner Mars 1969 8- to 12-microm.ter and 18- 10 25-.icra.+ter b8ndl and had a missionrr escept th8t 1 focal-p18n* diaphragm (field stop) had dyn8mic range of 120 to 330 deg I. The two rhmnrls. Located been pl8ced in front of the deteetols to reduce the response to in 8tmospheric rindous, emphasized the upper and lover off-.lis radiation. The e.piiiment began coll.rtinp temp.r81UICs of this ranger ~~specti~~ly.The .iprriment high-quality dat8 soon aftel Orbital insertion on Novembe, 13. packag. was located on the bottom of the OCt8gOn.l scan 1911. 8nd continued until April 2. 1972. "hen the txP*ti..nt p1atfoPm of the sc.ceCraft. The radiometer corsisted of tu0 was shut off to ronsirve sparerraft power during solar refracting tclesccpes. e8ch equipped with an uncooled 01c~lt8tion. The experiment 1.5 turned back on June 81 1972, antimony-bismuth thermopile detertor. The experiment used 8n aft., the spa~~iraftemerged from solar occultation. It optic8l train that included 8 rct8tmble plane mirror. rhfrh continued 10 operate norm.lly until 2200 UT on 0ctOb.r 27. rrf1.rt.d the incident energy into the detector telescopes. 1912, "hen the ~werinentwas turned off along with the ,.st of The mirror had three orthogonal positions. The first position the Rariner 9 spacCcr8ft. viewed empty 1p1ce and obtained I z.,o energy referenre. the second viewed the planet. and the third m.8sured the therm81 _------VIKING 1 ORBIlER, KIEFFER------energy I8di8ted by t.9p.rltUI. Calibr8tion plate. After scar. "as viewed for one fr.*s co~rt(4.2 s)r 13 observatiors INVESTIGA1101 NAME- INFRARED THERRAL MAPPING (IRTM) oi the p1an.t were ..de at 2.1-1 int.vra1s in c.ch wavelength channel. Then. fcllowing short look 81 the t.mper.ture NSSDC IO- 75-0151-02 INVESTIGATIVE PR06RAR reference pL8te. 14 mor. planetary ObSeIY81iOnS were made. The CODE EL-4. SCIENCE cycler uhich Lasted 63 1 (15 fN.e ~C~nts).Mas then rlpeat*dr beginning with vir" Of SP8Ce. D8t8 for about 21 .in "ere 1NVEST16ATION DISCIPLINE(S) obtained on AUoUst 5, 1969. over hiah latitude8 and Polar PLANETARY ATMOSPHERES PLANETOLOGY

US GEOLOGICAL SURVEl RPI-HEIDELBERG NASA-JPL CALIF INST OF TEcn SANlA BARBARA RES CTR NASA-JPL INVESTIGATION NAME- INFRARED RADIOMETER 1111)

NSSDC ID- 11-0111-01 INVEST16ATIVE PRO61111 CODE EL-4, SCIENCE

INVESTIGATION DlSClPLINE(S) PLANETOLO61

PERSONNEL PI - 6. NEUDEBAUER CALIf INS1 OF TECH 01 - H.H. KIEFFER US 6EOL061CAL SURVEI 01 - 6. MUNCH MPI-HEIDELBER6 01 - S.C. CHASES JR- SANTA BAR0ARA RES CTR 01 - €3. MINER NASA-JPL

BRlEf DESCRIPTION The I4.rin.r 9 infrmred V.di0m.t.r (IRR) .xprri..nt .Is% INVESTIGAIION NAME- INFRARED THERRAL MAPPING (lRIR1 designed to p,oiide. over rid. cove~ag. of the sUr1.C. 01 1181s. brightness temp1r8turis of the soil as a function of NSSDC ID- 15-083A-02 lNVESTlGATlVE PROGRAM loc8L t4.e by me81uring the energy r8diat.d in the 8-10 CODE EL-4. SCIENCE 12-microm.1.r 8nd 18- to 25-micro.eter r8uelength bands. From these temo.ra1Ur.s. the folloring information I.. derived: (1) lNVESTlGATlON DISCIPLINE(S) the 18r9.-SC81e distribution of ttm thermal ic.rti.1 cf the PLANITARY ATMOSPHERES surf8ce materials. (2) the occurrence of irregularities in the PLANETOLO61 cooling curve. (3) the eiistenr. of 'hot spots" that may irdic8le 80~1c.s cf internal heat. and (4) the tempel8tUr. of PERSONNEL the polar Cap 8nd .djac*nt ate.. The instwment r0nriSt.d Of TL - H.H. KlEFFER US GEOLOGICAL SURVEI tu0 teltscoprlth.r-opi Le-deteCtOr assemblies. Each 8ss*mbly TM - 6. MUNCH CALIF INST OF TECH contained tlO 1.nse.r spectral filter. 8 field Stop. 8nd TR - E.D. MINER NASA-JPL thermopile-d*tectOi. The detectovi in each assesbly ww TM - 6. NEUOE0AUER CALIF INST OF TECH identIr.1. Ho~ewer. the Lenses 8nd fi1tS.s through which the in - S.C. CHASE. JI. SANTA BARBARA RES CTR radiation must pass were of different materials so that one in - F.D. PALLUCONI NASA-JPL detector responded 10 the radiaticr in the 8-to 12-.irrc..trr b8nd (ch8nn.L 1) whlr~as the other detector responded to BRIEF DESCRlPTlON radiation in the ln-to 2S-~icro.e1er b8nd (rh8nnel 2). The The purpose of the IRTR erperimrnt was to measure the channel 1 assembly. uhirh h8d a field of uier of 0.55 by 0.53 t..p.r.tures of the atm~lphere and areas on the surface of degr hmd a germmiurn sp*Ctial filter and field lens and an Mars. The ..aunt of sunlipht reflected by the planet was also infrared tr8n8mission (1RTRAN) -2 Objectire lens. The chsnnel measured. The ISTM was a multichannel radiometer mounted On 2 ass.mblyr rhirh had a 0.1 by 0.1 deg field of vier. had a the orbiter's scan pl8tform. Four small telescopes, each with silicon sp.ct,aL filter. an IRTRAN-6 field lens. and an seven infrared dstectolsr yere aimed p.r8ll*l to the visual 1RTRAN-6 objective lens. The det.ctaif yere 13-junction im8ging Optical .xis. and made observations every 1.12 s. The bismuth-antimony diffrr.nti8l 1hermopil.s. which genera1.d a instrument "8, capable of measuring differences of 1 dcg C voltage in r.sponse to incident r8ai.m heat flu.. Chanrels 1 throughout te.pe18ture range of -130 C to 157 C. The field and 2 had sensitive artas of 0.25 by 0.25 mm and 0.4 by 0.4 mm. of rlrr 1.5 circular. 5 milliradians in diam.ter. respectively. Radiation "8% mr8surcd from three aources (spat.. Mar's. 8nd 8 thermal r.ference Source) by .tan1 Of thrwe-position scan mirror rotated clockwise by a bidircrtional RADIO SCIENCE AND CELESTIAL MECHANICS

NSSDC ID- 69-03#A-~6 INVESTI6ATlVE P106RA1 CODE EL-4. SCIENCE INVESTIGATION NAME- CELESTIAL MECHANICS INVESTICA110N DISCIPLINE(S) NSSDC ID- 64-0771-09 lNVESTlGATlVE PROGRAM PLANETAR1 ATMOSPHERES CODE EL-4. SCIENCE IOMOSPHEREI AND RADIO Pwsics

INVESTI6AT10N DISCIPLINE(S) PERSONMEL CELESTIAL nEcmmics PI - A.J. KLIORE NASA-JPL PERSONNEL BRIEF DESCRIPTION PI - J.D. ANDERSON NASA-JPL In this expe+i*.nt. the changes in the frequency. phase. 01 - G.Y. NULL NASA-JPL and amplitude of the S-band (2300 #HI) trarkinp and telem.try signal (immediately prior to and follDrlng the occultation of the spaiecraft by the planet) were used to derlv. the temperatur.. prcsiurc~ and density of the lower gaseous atmosphem of nara. and the denslty of charged particles in the Cartian ionosphere. ------m&R1*E, 9, ILIO~E-----'------

INVEST16ATION NAME- SdAND OCCULTATION

NSSDC ID- 71-05lA-08 INVESTIIATIVE PROGRA.11 CODE EL-+* SCIENCE

INVEST16AT1ON DISCIPLINE(S) ionosPmEREs AND RADIO pmvsics PLANETAR1 ATMOSPHERES NSSDC ID- 69-014A-05 INVESTIGATIVE PROGRAM CODE EL-4. SCIENCE PERSONNEL PI - A.J. KLIORE NASA-JPL INVESTIGATION DISCIPLINE(S) 01 - D.L. CAIN NASA-JPL CELESTIAL MECHANICS 01 - 6. FJELDBOtNLA) NASA-JPL 01 - B.L. SEIDEL NASA-JPL PERSONNEL PI - J.O. ANOERSON NASA-JPI BRIEF DESCRIPTION The Doppler shift of the S-band telemetry signal during occultation of the sp.cecraft by Mars prOvid.4 the v.rtir.1 distributton of th. Index of rrfrartlon of the Martian atmosphwe. These data yield the vertic.1 distribution 01 neutral and Ionized species.

------VIKlN6 1 ORBITERr MICHAEL, JR.------INYEP1lGAllOL NAME- ORUITER RADIO SCIENCE

NSSDC ID- 71-0151-04 INVESTIOATIVE PRO6RAM CODE EL-4ICO-OP. SCIENCE

INVESTICATION DISClPLINE(S) PLANETARY IONOSPHERES METEOROLOGY

PERSONNEL INVESTIGATION DISCIPLINE(S1 TL - Y.H. ~ICHAEL. JR. NASA-LAIC CELESTIAL MECHANICS in - 1.1. SHAPIRO MASS INS1 OF TECH TI - 6.F. LINDAL NASA-JPL PERSONNEL TR - J.G. DAVIES U OF MANCHESTER PI - J.D. ANDERSON NASA-JPL in - D.L. CAIN NASA-JPL in - I.D. ~ROSSI RAYTHEOM CORP TM - G.L. TlLER STANFORD U in - J.P. BRENKLE NASA-JPL in - a.m. TOLION NASA-LAIC TM - C.T. STELZRlED NASA -JPL TI - 6. BORN NASA-JPL TM - R. REASENBERO MASS INS7 OF TECH

BRIEF DESCRIPTION There are four distinct sets of Viking radlo science data, three using orbiter data and one plim.rily using lander data with ralibratlona from orbiter data. The orbiter tracking data. obtaineo from the two-iay orbiter-earth S-band and I-band radio links. consist of Doppler frequencies and timr-of-fli*ht range .easuriments. These determined the position and motion Of the orbiters. and ran be used to study the Mars gr.vitationa1 field. the plasma in interplanetary space. and the structure of the solar corona. Th. occultation data we.* INVESTIGATION DISCIPLINE(S) obtained from these SDSe radio link. by analog recording Of the IONOSFHERES AND RADIO PHYSICS signal when a spacecraft was passing into or Out of orrultation PLANETlRl ATMOSPHERES with Mars. The data ran be used to produce altitude piofiles of the timpiratur.. density. and pressure of the atmosphere PERSONNEL (including the ionosphere) and IO measure the radius of the PI - A.J. KLIORE NASA-JPL planet usinp a large number Of surface points. The sUrfaCe-prOpe.ties .sP.ct of thli investigation Utilized the BRIEF DESCRIPTION UHF (181 Mnz) signal on which the landers transmitted data to In this enperimcnt the ch.ngis in the irtquency, phase. the Orbiters. At the beginning Or end of a data transnission and amplitude of the I-band (2100 MHZ) tracking and teLemCtry session. when the Orbiter wes near the lander's horlzonr the signal. immediately prior IO and foilouing the occultation of strength of the received signal 1.5 rec0rd.d as a function of the spacecraft by the planet, ltlC used to derive the time. These signal "fading Catterns.~ resulting from temperature, E~CSILII. and density of the IOI~Igasec~s interaction of the radio wmves with the Martian sUrf.ce. .tm~spher~ of Mars and the density Of charged particles in the contain information about the physical propirtie. of the Martian ionosphere. surface near the landers. The lander tracking data from the two-way direct lander-earth I-band links permit drtermlnation cf the location Of the landers and SIudies Of the motion Of the planet. Op@.*tion of this cxperlmcnt #as terminated on August Tr 1980. ------VIKING 2 ORBITER. MICHAEL. J0.------

INVESTlGAllON NAME- ORBITER RADIO SCIENCE INVESTIGATION NAME- LANDER RADIO SCIENCE

NSSDC ID- 15-083A-Ck INVESTIGATIVE PROGRAM NSSDC ID- 71-083C-11 INVESllGAllVE PROGRAM CODE EL-4lCO-OP, SCIENCE CODE EL-4ICO-OP. SCIENCE

1 NVESTIGATION DISCIPLINE(S) lNVESTlGATlON DISCIPLINE IS) PLANETARY IONOSPHERES ...cronrn*r ... - .. -. . PLANETARY ATMOSPHERES IONOSPHERES AND RAD10 PHYSICS PLANETOLOGY PLANETARY ATMOSPHERES PLANETOLOGY PERSONNEL TL - Y.H. MICHAEL, JR. NASA-LARC PERSONNEL TM - 1.1. SHAPIRO MASS INST OF TECH TL - Y.H. MICHAEL, JR. NAS A-LAIC TM - G.F. LINDAL NASA-JPL 1M - 1.1. SHAPIRO MASS INST OF TECH TM - J .G. DAVIES U OF MANCHESIER 1N - 6. FJfLDBO(NLA) NASA-JPL TM - D.L. CAIN NASA-JPL TI - J.G. DAVlES U OF MANCHESTER TM - M.D. GROSS1 RAYTHEON CORP TM - D.L. CAIN NASA -JPL 111 - G.L. TYLER STANFORD U 1P - M.D. GROSS1 RAYTHEON CORP TM - J .P. BRENKLE NASA-JPL TM - G.L. TILER STANFORD U TM - R.H. TOLSON NASA-LAIC TM - J.P. BRENKLE NASA-JPL TM - C.T. STELZRIED NASA-JPL TM - R.H. TOLSON NASA-LARC TM - G. BORN NASA-JPL TI - C.T. STELlRlED NASA-JPL TM - R. REASENBERG MASS INS1 OF TECH TM - G. BORN NASA-JPL TM - R. REASENBERG MASS INS1 OF TECH BRIEF DESCRlPTlON There are fcur distinct sets of Viking radio srirrcr BRIEF DESCRIFllON data. three using orbitcr dit4 and one primarily using lander This experiment used the S-band radio transmitter to data with calibrations from orbiter data. The orbiter tracking acquire D~ppll, and range data for the Landerr utilizing the data. obtained from the two-way. orbiter-earth S-band and same DCCP Space Network facilitirr that Yere used by the X-band radio Links, consist of D~pclli frequencies ara Crbiters. The resulting data were used to determine the time-of-flight range measure.enti. These determined the location of the lander On the planet surface. They also position and motion of the orbiters, and can be used to study provided more prrrirc information about the Orbital. the Mars gravit.tion.l field, the plas.. in inteipl.FCtiiy rctational. and DT~L~SS~OWLmotion of Mars than had pr-viou~ly SP.C.. and the stru~ture of the solar corona "hen the been available. The tio principal diffcrcnrcl between orbiter splle~raft was On the 0pp0~ite side of the sun. The and lander tracking data are (1) lander tracking periods are otrultation data usre obtained 110. these same radio links by never longer than i h and are sonctimcr much shorter because of analog recording of the signal when a spacecraft was passir9 therr.1 constraints on the duration of lander transmitter into or out of occultation with Mars. The data can be used lo 0per.ti0". and (2) landers hawe no a-band riqnals to PCOY~~L product altitude pl0fiL.S Of the t*.PelatUIC, density, and the t~rrections to range data for the interplanetary plas.i E~~SSYICof tbe atlOsphCrt (inclLaing the ionosphere) and to effects. Corsequently~ Lander ranging sessions iert scheduled ~L~SYIC the radius of the planet using a large number of to be nearly rinultanrour rith Orbiter ranging whenever surface points. The surface prcperties aspect of this possible, $0 that the orbiter S- and X-band data r0uld Supply investigation utilized the UHF (381 MHr) signal on uhich the these corrections. 1ande.s transmitted data to the Olbit.ls. At the beginning cr end Of a data tranSmiSSiOn S.Ssionr when the OlbitLr ".I near the Lander's horizon. the strength of the rcr.irrd signal I~S rrrcrdrd as a fLnction Of tile. These signal "faairg ATMOSPHERE patt~ini~"ies~lting from interaction of the radio waves ~ith the Martian surface, contain information about the phlrical pr~p~iti~sof the surface near the Landers. The lander trarkinq Oat. fro. the two-1ay direct lander-cartt S-tand Lirkr ------"1KlhG 1 ORB1TE8, FARMER------perlit dttcrmination of the Location of the landers and studies of the motion of the planet. INVESTIGATION NAME- MARS ATMOSPHERIC YATER DETECTION (MAYD) ______-VIKING 1 LAhDEn. MICHAEL, JR.------NSSDC ID- 75-0151-03 lNVESllGATlVE PROGRAM CODE El-4, SCIENCE INVESTIGATION NAME- LANDER RADIO SCIENCE INVESTIGATION DISCIPLINE(S) NSSDC ID- 15-075C-11 INVESTIGATIVE PROGRAM PLANETARY ATMOSPHERES CODE EL-+ICO-OPI SCIENCE PLANETOLOGY

INVESTlGAlION DISCIPLINE(S) PERSONNEL ASTRONOMY TL - C.B. FARMER NASA-JPL IONOSFIERES TP - D.D. LAPORTE SANTA BARBARA RES CTR PLANETARY ATMOSPHERES TI - D.Y. DAVIES NASA- J PL PLANETOLOGY BRIEF DESCRIPTION PERSONNEL The 11AUD used an infrared grating SDectrO~~tCrmounted on 1L - Y.H. MICHAELI JR NASA-LARC thc orbiter scan plitf~~~that was boresighted with the TM - 1.1. SHAPlRO MASS INS1 OF TECH television cameras snd the 11111. The instrument ~CISYIC~ solar TM - G.F. LINDAL NASA-JPL infrared radiation reflected itom the surfarc through the TM - J.G. DAVlES U OF MANCHESTER at.OsChCrI tc the spacecraft. Spectral intervals were selected 1M - O.L. CAIN NASA-JPL colnrident with the wavelength of raf~r-vapo~ab.OPEtiOn LlneI TM - M-0. GROSS1 RAITHEON CORP in the 1.q-miCIOmCteI band. The quantity of I~~CIvapor along TM - G.L. TYLER STANFORD U the line of sight was mCaSUred fro- 1 to 100 miclOmtttll of TM - J.P. BRENKLE NASA-JPL crecipitatle uater with an accuracy of 5 I or better. The TM - R.H. TOLSON NASA-LARC instantmeour field of vier of the instrunent was 2 I I1 TM - C.T. STELZRIED NASA-JPL milliradians, and a stepping mirror rotated the line of fight 1M - G... BORN NASA-JPL through 15 positions to provide a roughly rectangular firkd of TM - R. REASENBERG MASS INS1 OF TECH vier of 11 I SI milliradians. Op~iationof this cxocrinrnt was terminated On August 7r 1980. BRIEF DESCRIPTION This erperinmt used the Lander S-band radio transmitter - -__-- - VIKING 2 ORBITER, rARMER------to acquire dOpplCI anr range for the lander, utilizing the sdre Deep Space Network facilities that iere used by the orbiters. lNVESTIGAllON NAME- MARS ATMOSPHERIC YATER DETECTION (MAUD) The rcsultinp data icic used to determine the lcration of the lander On the clznet's surface. They also provideo more NSSDC ID- 7:-0831-03 INVESTI~ATIVEPROGRAM precise information about the Orbital. rotational. and CODE EL-). SCIENCE precessional motion of Mars than haa rrrviaurly been available. The ti0 principal differences betieen orbiter and lander lNVESTlGATlON DISCIPLINE(S) tracking data are (1) lander trackirg ~triodsue~e newer lorgel PLANETARY ATMOSPHERES than 2 h and "ere Soaetimtr much shorter because of thermal PLANETOLOGY constraints on the duration of Lander transmitter op~..tion* and (2) landers had no X-band signals to provide the PERSONNEL ccrre~tions tc rarge data for tte interplaretary c1as.a TL - C.B. FARMER NASA-JPL effects. Consrqucntlyr Lander ranging rrriioni were scheduled TM - D.D. LAPORTE SANTA BARBARA RES ClR to be nearly riwultancour rich Crbitei ranging rhencrcr TM - D.Y. DAVIES NASA-JPL possible, so that the Orbitti 5- and X-band data could SUPP~Y these corrections. BRIEF DESCRIPTION The RAuD used an infrared grating spectrometer mountrd on the orbiter scan platform that ".a borrsiqhted rith thr telwisicn cameras ,nr the IRTR, Ihe instrument m.awed solar infrared radiation reflectid fro# the surface through the atmosphere to the ~p.~.~iaft. Spectral intervals "err .elected NSSDC ID- TI-083C-12 INWESTI6ATIVE PROCRAII rolnridrnt with thr 1a1clength of Ua1.I. 'I~DOI absorpttm lines CODE EL-$. SCIENCE ir the I.+-.i~rO.~ter band. Ihe qlrartity of wat*r vapor a1C-g the line of sight was measurrd from 1 to 1000 micromrtrrt of 1NVESTIGAlION DISCIPLINE(S) p*ecipitlblr watrr rith an accu~aor of S I 0. better. The INlERPLANETARl PHISICS instantaneous field of view of thr inatruatnt was 2 a 11 PLANETAPI ATUOSPHERES rillirwli.ns. and a stepping Sirrcr rotated the Line Oi Sight through I5 positioni to provide a mughly rectangu1.r field of PERSONNEL vier of I1 x 31 milliradians. TL - A.0.C.NICR U OF IIINNESOTA 1W - U.B. IICELROl HARVARD U __---_-VIKING 1 LANDER, N]ER------'------TU - N.U. SPENCER NASA-61 F C

INVESIIGATION NAUE- ENTRl SCIENCE AIUOSPHERIC STRUCTURE BRIEF DESCRIPTION Thr Viking entry science neutral ataoapheric ~~.p~iiti~n NSSDC ID- 15-075C-CZ INVESTI6AIIVE PROGRAP exprriment (cnc of three that were part of the entry scient. CODE EL-4. SCIENCE invrstigat+on) was designrd to provide the composition data for the rarioua neutral sp~ties that wrre nerded to deflnr the INVESTI6AIION DISClPLINE(S) present physical and chemical state of the Wartian .tmospher.. PLANETART ATUOSPHERES wountrd in an opening in the aerorh.11 rith Its .lectron-impact own ion source recessed below the SuVface Of the .*rashell. a PERSONNEL double-focusing (elrctvoatatic and magnetic) mass speCt.Om.t.i TL - A.O.C.NlLR U Of UINLESOIA was used to meawrr the conr*ntrationa of the .tmosphrrfc TR - A. SEIFF NASA-ARC %p.cir% that have mass-to-charge ratios fro. 1 to 4V. Two TU - N.Y. SPENCER NA SA -6 SF C rollrctors I.,C used. one corering the mass range fro. 1 to 1 u. and the other simultaneously covering thr range from 1 to 49 Y. R8as spectra ucre obtained by 8rcsping the ion .ccal.ration vOlt.ge and the deflection voltage acr~asthr eI.ctrostatic C1.t.s. The SI~CIP period was .ppr~~i..t~ly S s. and dynamic range of 1.E5 1.5 provided within rarh aprctrum. --__---VsllN6 1 LLNDER. yIER------

INVESTI6AllON WARE- ENTRl SCIENCE IONOSPHERIC PROPERTIES

NSSDC ID- 1s-01%-14 INWESTI6ATIVE PROCRAR CODE EL-4. SCIENCE

INVES11GAlION DISCIPLINE(S)

PERSONNEL 1L - h.O.C.NIER U Of IIIMNESOTA TI4 - Y.B. HANSOM U OF TEKAS. DALLAS TU - N.U. SPENCER NASA-61 FC URIEF DEScRIPrlON The ulking entry scient. ionospheric propeeti*= ~.p.ri.ent (one of three that "ere part of the entry science inv.ltigation) atudird the conpositionr atructurr. and trmprrature of the ionoapherr. which "err Probed during the descent of the lander rapsul* by means of a retarding potential anatyzrr (RPA) mounted flush with the front farr of the a.rosheI1. lo cons.rw battery parer. the instrumrnt was oprratid intermittently betiern 16,000 and 5.000 km altitude but cOntinuOUsly from 5.000 to 100 k.. The instrument co.priacd a current-COllrCting Platr with Sewrn giida ahead of it. A fixed p10gra. of potential', l'as .ppIi.d to the gridsr and the coIlCCt~d LuIrentS IrIC measured at 1O-ma intervals. The instrument Operated in three phase. to meaaurt energetic electrons. thermal rlectronsr and thermal iona. ______-VIK]*G * LANDER, NfEO------

INVfSllGAlION NAME- LNlRl SCIENCE NEbIRAL ATROSPHERIC INVESTI6ATION NAUE- ENTRl SCIENCE IONOSPHERIC PROPERTIES coRPoslTIoN NSSDC IO- lJ-081C-l* INVESTI6ATIVE PR06RAR NSSDC ID- 15-015C-12 INVESTIGATIVE PR06RAR CODE EL-*. SC.IENCE CODE El-.. SCIENCE INVES716ATION DISCIPLINE(S) INVESTIGATION OISClPLINE(S) IONOSPHERES QERSONUPL PLANETAR1 ATMOSPHERES TL - A.O.C.NIER U Of RINNESOTA 1L - Y.B. HANSON U Of 1EXAS. DALLAS PERSONNEL TU - N.Y. SPfNCER NASA-6SFC TL - A.O.C.NIER U OF UIMNESOTA 111 - U.B. RCELR(II HARVARD U SRIEf DESCRIPTION TM - N.Y. SPENCER HA SA-G SFC The Viking entry sricnrr ionospheric properties e~perimrnt (one of three that were part of thr rntry aricnce BRIEF DESCRIPTION investigation) studied the compnaitionr stmcturer and The Viking ertry science neutral at.Ospheiic rompoaition temprrature of the ionosphere. rhirh rrre probd during thr experiment (one of thrtt that rerr part of the entry acierrr descent of the lander caps~leby means Of retarding potential investigation) "as resigned to DIOY~~C the co.position data for snalyzrr (RPA) mounted flush with the front face of thr the various neutral species that weir needed to define the aarostrll. lo conserrr battery poucr. the Inrtrumrnt waa crtsent physical arc thrmic.1 state rf the Rattian atmoachere. cpirated int.r.ittcntly betreen lC1000 and 5.000 km altitude Mounted in an opening in the aeioihell rith its electron-impact but COntinuOUaly fro- S.000 to 100 k.. The instrumrnt open ion IOUIC~ recessed below the surfacC of thr acrorhell~a co.prlsed a rurrcnt-collecting plate rith seven grids ahead of ocublc-feeusing (elictmltatic and m.gnetir) mass Spe~trometer it. A fixed program of potrntials waa applird to thr grids. "as used to measure the roncrntrationr of thr atmoscheric .nd the collertra currents were measur.d at 10-ms intervals. s~etiei that have #ass-t0-~harg~ratios from 1 to 49. Two The instrument Opersted in three phases to .C.SY~C energetic collccto~sicic vsed. one for the mass range from 1 to 1 UI and rlcrtrons. thrim.1 electronsr and thermal ions. the other rimultar~c~rlymeasuring ir the mass range from 1 tc 49 Y. Mass spectra were obtained by sweeping the ion --_----VI)(ING 1 LANDER, MESS------acrrlrration voltape rnd the deflection YOltiQC ~CIOSSthe ritrtrostatir plates. The sleep period MIS appro.imitely 5 SI INVESll6ATIOW NAUE- IETEOROLOGl ard dyramic rarge Of I.E5 ..I DICVidld within rach SpeCtrLI.

56 NSSDC ID- 75-015C-0 INVES116AlIVE POOGRA? CODE EL-4. SCIENCE

INVESlISAlION DISCIPLINE(S) PLANETARV ATMOSPHERES MElEOROLOGV

PERSONNEL TL - S.L. HESS(DECEASED)

BRIEF DESCRIPTION This experiment ano1yr.d the meteorological environment near the planetary surface and cbtained infcrmation abcut lNVESllGAllOh NAME- MOLECULAR ANALISIS motion lysteml of various scales. The at.0spheric D.I.*Ct*lS determined Were PICSSYI*I tCWIIatUIC. rfnd Speed, and wind NSSDC ID- 75-083C-04 INVESTIGATIVE PROGRAM direction. Diurrai and .earon.i variations were of paltic~iar CODE EL-). SCIENCE importance. The smpling rates and durations for any one Nart4.n day (sol) IC~selectable by ground command. The lNVESlIGAllON DISClPLINE(S) lensors were mounted on an erected boom. 1hre1 hot-film PLANETARV ATMOSPHERES arewcmeters. thrcugh which an tlectrii current "as palled 10 PLANElARY BIOLOGV heat tu0 glass needles coated rith platinum and Overcoated rith PLANETOLOGV aluminum Oxide. were used to measure rind speed. The electric paler needed to vainlain these lrnsors at a fixed 1emPCrature PERSONNEL above the surrounding air was the me.1~1~ of rind lpeed. 1L - K. BIEMANN MASS INST OF 1ECH At.OSDheliC tempCrltuIS IaI .*.SUltd by three fine-Mire TI - H.C. UREV(DECEASED) U OF CALIF, SAW DIEGO thermocouples in p.1111-I. A thin metal diaphragm. mount*d in TU - D.M. ANDERSON USA-CRREL a v.Cuul-Sc.l.d CaII. Mal Used 10 CeaIUIe a1masph.ric DISSSUII. 18 - 1. DYEN STATE U OF HEY YORK in - J. ORO U OF HOUSlON __-----VIKING 2 LANDER, MESS------TM - L.E. ORGEL SALK INST BIOL STUDIES iv - ~.O.C.NIER U OF MINNESOTA INVESTIGATION NAME- METEOROLOGY TU - P. TOULMIN. 3RD US GEOLOGICAL SURVEV NSSDC ID- 75-083C-07 INVESTIGATIVE PROGRAM CODE EL-4r SCIENCE

INVESllGAlION DISCIPLINL(S) PLANETARY AlMOSPHERES VETEORCLOGV

PERSONNEL 1L - S.L. HESS(DECEASED) FLORIDA STAlE U in - C.B. LEOYV U OF YASHlNGlON TM - 11-11. HENRV U OF YASHINGTON TM - J.A. RYAN CALIF SI UI FULLERTON TM - J.E. TILLMAN U OF YASHINGTON

BRIEF DESCRIPlION This experiment analyzed the m~teOrOLOgica1cnuiron*ent near the planetary surface and 0ttain.d infomrtion about motion systems of various sca1.s. The atmospheric P~r~~etrrs delerained were D~CISY~~,t.aperatUier rind sCeed. mnd rind direction. Diurnal and seasonal rariations rere of particular import.nre. The saipling rates and durations for ary cne Mar1i.n day (sol) were sclert.blc by ground co.i.nd. The sensors were mounted on an erected boom. Three hot-film .re.Ometers. thiouqh which an rl*rtrir current was passed to heat tu0 glass needles coated rith rlatinua and OwrCOaten rith lNVESlIGAlIOh NAME- PHVSlCAL PROPERTIES aluminum oxide. usre used to measure rind speed. The electric power needed to maintain these i.nlors at a tined teuperature NSSDC ID- 75-083C-01 INVESTlGAllVE PROGRAM above the surrourcirg air I., ttc measure cf rind spied. CODE EL-). SCIENCE AtmOsph.iic temperature was measured by three fine-rirr thermocouples in paraIl.1. A thin metal diaphragm. mounted in INVESTIGATION DISCIPLINECS) a vacuum-scaled case. w.1 Uaed to measure at.ospheiic Pressure. PLANElOLOGV

FERSONNEL TL - R.Y. SHORTHILL SURFACE CHEMISTRY TM - R.E. HUTTON in - H.J. MOORE. II TI4 - R.F. SCOT1 ______"1KlNG 1 LANDER, BlEl~"------' BRIEF DESCRIPTION lhe purpo~eOf the physical prop~lti~~investigation was INVESTIGATION NAME- MOLECULAR ANALYSIS to determine the physical properties of the Martian surfact and environment at the landing site. primarily using engineering NSSDC ID- 75-075C-04 INVESTIGATIVE PROGRAM measurtm~ntl and scientific instruments lcquiicd to meet other CODE EL-*. SCIENCE mission objectives. In paiticul~~~it attempted to determine such prop~fti~s1% bulk density, bearing strength. angle of INVESTIGATION OISCIPLINE(S) repose, cohesion, angle ot internal friction, particle PLANElARY ATMOSPHERES characteristics. thermal parameters, eolian transportability, PLANEIARY BIOLOGY IOpographyr and certain cnvironmcntal properties such as rind. PLANETCLOGV tempLratUrer and S0I.l flu. levels. RalimU. use was made Of hardware and instruments intended far other applications. such PERSONNEL .I the mtchaniral rubryrtenr and lander cameras. Only passive 1L - K. BlElANN MASS INS1 OF TECH devices, such as mirrors and Landing leg stroke gauges, icrc TM - H.C. UREV(DECEASED) U OF CALIF, SA1 DIEGC added for this experiment. TM - D.M. ANDERSON in - 1. OYEN in - J. ORO in - L.E. ORGEL INVESllGAlION NAME- INORGANIC ANALISIS in - A.O.C.NIER U OF MINNESOlA TM - P. TOULMINr 3RD US GEOLOGICAL SURVEY NSSDC ID- 75-075C-13 INVESTIGATIVE PROGRAM CODE EL-4. SCIENCE BRIEF DESCRIPTION INVESTIGATION DISCIPLINE(S) PLANETOLOGY

57 PERSONNEL TL - P. TOULIIN, 3RD US 6EOL061CAL SUlVEV TI - A.K. BAIRD POIONA COLLEOE BIOLO61 TI - K. KElL U OF HEY MEXICO TM - H.J. ROSE US LEOLOCICAL SURVEl TI - B.C. CLARK IARTIN-IARIETTA AEROSP

BRIEF DESCRIPTION This txprrinent utilized an .nergy-dispersivt X-pay tluoresrenrc spe~tr~met~r(YRFS) In rhich tour sealed, gas-tilled p~0po.tion.l counters detected X rays emitted from sa.ple1 of Iartian rurtaer m.trrials irrbdimtcd by X rays from radioisotope SCUIC~I(iron-55 and caamiu*-I09). The Output 01 the proportional counters 18s subjected to pulse-hcipht INYESTIGATION DISCIPLlNE(S) analysis by an onboard step-scanning, single-channrl analyrrr PLANETARV BIOL061 with adjustable counting periods. This instrument was located i*siae the lander bcoy. and samples bere aelivrrrd to it ty the PERSONNEL lander surtarr S~WLCI. Calibration standards I..* an integral TL - n.P. KLEIN NUL-ARC part of the instru.ent. Rcronrtructtd Spectra yielded sur1.c~ TI - J. LEDERBER6 STANFOPD U comcoiition data with accurarirs ranging from trr tens of TI - A. RICH IASS INST OF TECH parts PCI millicn tcr trace clr.antr to 1-1 percent tor major TP - N.H. HOROYlTl CALIF INST Of TECH rle.rnts. TI - V.I. OVAIA NASA-ARC TI - 6.V. LEVIN BIOSPHERICSI INC ------VIKING 2 LANDER. TOULIlNr 3RD------BRIEF DESCRIPTION INVESTIGATION NAME- INOR6ANlC ANALISIS Thr biclagy exprrimrnt searched for thr prrsence of Iartian organisms by looklng for metabolic p.OduCts. Thrr. NSSDC ID- 75-oa3c-13 INVESTIGATIVE PROGRAI distinct inrtruarnts (pyrolytic rel*asr (PI). Labeled relrase CODE EL-). SCIENCE (LR). and gas e.change (GEY)) incubattd s.rnp1.a of thr Iartian surface under a number ot different tnvlronmrntal conditions. INVESTIGATION DISClPLINE(S) In some instances a sample was heat strrilizd and rrproc.ss.d PLANETCL061 as control. The PRr or carbon assimil8tionr instrument sought to aetrct the Photosynthetic or chrmical fixation of (02 or CO containing C-14. The I.mplCI were incubated for several days in the pr*srnCC of the *8diOaCtil* 98s mixturer 50.8 I4*Pl1s with simulated sunlight and .om* iithout. Nextr each sample "as heated to 120 C to IemOvr unreactcd (02 and CO. The roil was pYrolized It 650 C and any organic Products wrm collectd In an organic vapor trap (OvTl. Finally. the trap has heated to cOmbuSt the Or98niC m8t.ri.l to C02 and any evolwed radioactive gas I)..mrssurd. The LR rxpcrimcnt sought to detrct m~t8bokiC procrsses through r8diolcspllo.elry. Liquid nutrients libeled uith radioactive carbon were added to the s..pLes and the Ot.OlDh@lC .bow was ~OntSnuOu~LymOnitOr.d to defect any ~.dloactive 9.1.. reI..l=d 110. these nonrolatil. nutrients. The GEL measured the production andlor uptakt Ot CO2. ~2.CH~. 142. and 02 during incubation ot a roll ...pIr. Th8 18mple 18% %riled8nd purgrd by Ht; thrn 1 uixtur. 01 He. Klr and C02 was introduced as an initial incubation at.o$phlrt. Atter the aoditlcn of selected quantity Of nutrient solution (saturated with thr diagnostic gas. nron). the samplr was incubated. At certain intrrr8ls. samples ot the at.osph*re Icrr remowed and an8tYzed by 8 gas chromatagr.ph ulth a thrra.1 ronduc t ir it Y dct ec tor. ------VIKIN6 2 LANDER. KLEIN------.------

IMVESTIGITION NAIE- 0IOL061

NSSDC ID- 75-083t-03 INVESTIBATIVE PROGRAI CODE EL-4. SCIENCE

INVESTIkhllON DISCIPLINEIS) PLINETAR1 BlOLO61

PERSONNEL PERSONNEL TL - H.P. KLEIN NASA-ARC TL - R.B. HARGRAVES PRINCETOLI U TI - 1. LEDERBER6 STANFORD U TI - A. RICH 11ASS INST OF TECH BRIEF DESCRIPTION TI - N.H. HOROY1Tl CALIF INST Of TECH The magnetic Droprrtics ezpcrimcnt dcttctrd the premnrc in - Y.I.. ~~. OVAIA ..*.*.-.Ut ..-...... - of magnetic partitles in Iartiar surface material. It used TI - G.U. LEYIN BIOSPHERICS~INC three pairs of samarium-cobalt magnets. two mounted on the backhot et the rurtacc-ramDlrr coLIect01 head and one on top Of BRIEF DEICRIPTION the lander. Each Fair consisted of an Outer ring aagnrt about Thr biology elpcrimrnt semrrhcd tor the presence of 2.5 C. in diameter with an inner core magnet of ~p~o~it. martian org.nisms by Looking for met*bolic products. Thrrr polarity. The magnets "ere directly imaged by the camera distinct Instru-rnts (pyrolytic release (PR), I8brL.d rrltase system in black ara white ard in cclor. A 4-power magnifying (LR). and gas rmrhangr (6E1)) inrub8t-d samples ot the Martian iirror was used to1 aarimum resolution. rurfsct under 8 number 01 diltCrrnt rnv$ronmental cond+tionr. In some instantes ~*.pl. "as heat atCri1iz.d and ~CD~OICSS~ - __ - - - VIKING 2 LANDER, HARGRAVfs------as a control. The Plr or carbon assimilation. instrumnt sought to detect thr Photosynthetic or chrm1c.l fixation of COZ lNVESTlGATlON NAME- IAGNETIC PROPERTIES or CO ront8ining C-14. The S..Dl+S lele inrubattd for srrer.1 days in the PIII~IICC of the radioactive 9.1 mixture. so.. NSSDC ID- 15-083C-10 IMVESTI6ATIUE PROGRAC I..~Icswith simulated sunlight and 10.e without. Went. each CODE EL-4. SCIENCE Sample "8s heated to 120 C to ICmOYt unre8cted (02 and CO. The sail "as p~i01ii.d at 650 C and any otganir products were INVESTI6ITION DlSCIPLINE(S) collected in an organic vapor trap (OVT). Finally. tht trap PLANETOLOGV 111 heated to tombust thr OrglniC matrrial to (02 and any ewolved radioactive gar was me81ured. The LR experimtnt sought PERSONNEL to detect metabolic prOceIse% through radior.$piro.etly. TL - R.0. IIARGRAVES PRINCETON U Llguid nutrients labeled with radioactive r8rbon were added to the samplrs 4nd the atmOsphrIr aborr 1.1 continwously monitorrd BRIEF DESCRIPllON to detect any radioactive gases released from thrfe nonrolatilr The magnetic ropert tie^ experirrnt detected the presence nutrients. The GEX measured the Production Sndior uptake 01 01 naqnrtir particles in Martian iurtacs material. It used c02. n2. Cn,. H2, and 02 during Incubation of soil samplr. three pairs of ramarium-cobalt nagnetsr tu0 mounted on the The sample was sealed and purged by He, then a mixture Of HI. backhot Cf thr rurfaCr-Sa.plrr Collcrtor head and One On top Of ~rrand LO2 was introduced as an initial incubation atmosphere. the lander. Each pair ronrirttd 01 an Outer ring magnet about Atter the aodition Of a selectrd quantity Of a nutrient 2.5 L. in diameter with en innee core magnet of 0pr01it. solution (saturated with the diagnostic gas, neon). the I..PIC polarity. The magnets yere directly imaged by the camera Mas incubated. At Certain inttrvaLS1 S8.DLrr Ot the 8tmO'phCI. system in black 1Td white ard in CCLOI. A 4-poker ..gnifyirp ierr rem0v.a 8nd malyzrd by a gas chrom.togr.ph rith thermal airror was usrd lor mrxi.ur resolution. conductivity drtrrtor. 1NWESIlGLlION OlSCIPi.IHElS) PLANETOLOGI PLANETARV PHlSICS

PERSONNEL 1L - D.L. ANDERSON CALIF INS1 OF TECH rn - M.N. io~soz UASS lhS1 CF TECk TU - G.H. SUllON U OF HAYAII TM - R.L. UOVACn STANFORD U 111 - G.V. LATHAV U OF TEXAS, GALWESlOh 1M F. DUENNERIEP U OF HAYAII

BRIEF DESCRIPTION The seismology experiment 1.5 designed to determine the level of rcirric activity or Uars ard its interral str~cture. The re~rnolog). instrument contained three mutually orrprndicular seise~meters. Each seismometer consisted of a roving coil and fixed magnet. lhe operating lodes were (1) sel*ction of various filters for frequency content or to adjust to best reception of specific types Of data. (2) a lor rampling ratt lor general activity. (5) a high data rate for detailed examination of events, (4) end a ~Ompreii~dmedium rate for continuous monitoring of nacsquakes that “ere dormant until actiVatCd by an event. The data iLlC COnprerred for transmission to Earth by averaging the amplit~d. of noma1 ground noire over a 15-5 period. Yh.n an event ~ccurrea. a trigger activated a higher data rate mode that sampled the aLDLitUde of the ortr~llevent enveloper uhith required only one a*DlitUde sample Der second to indickte its shape. lit the Same tile. the rharqe in polarity Of the data Iisrll (caused by crorrins the zero axis) “si sampled once each second. The sham Of the envelope an6 its inrrcmcntal frequency content “a5 transmitted to Earth and reconrtructea to acpr~limattthe Original went. The Viking 1 rrislonctc. failed to uncage and could not be uf~din a leir.ir network with the Viking 2 inrtrumen1 . NSSDC ID- 75-OMJC-Cl

SEE THIS EXPERIMENI UNDER SURFACE CHEUISTRI

JUPITER

Plate 4 is a collection of press release photographs from the Pioneer 11 and Voyagers 1 and 2 missions. (A) P21631 is a Voyager 1 montage of Jupiter and its four Galilean satellites (the four largest of its 16 known moons). (B) 79HC679, a Pioneer 11 photo of Jupiter showing the north polar region as it passed over it, showing the polar region's lack of belts but with many convection cells. This is a view and aspect never seen from earth. The Great Red Spot is at the bottom. (C) P21774, a Voyager 2 photo of the nightside of Jupiter showing the sunlit atmospheric halo and the Jovian ring discovered on Voyager 1. (D) P21195, a composite of Voyager 1 photos of the four Galilean moons illustrating their relative sizes. Io (3632 km diam.) is about 200 km larger than our moon and Europa (3126 km diam.) is about 300 km smaller than our moon (3478 km diam). Callisto (4820 km diam.) is the size of the planet Mercury and Ganymede (the largest moon in the solar system) at about 5150 km is about 350 km larger than Mercury. (E) P21305, voyager 1 photo of Io showing its completely volcanic surface and an erupting volcano on the limb. Io's volcanic activity was discovered by Voyager 1. Io is the most volcanically active of any solar system body known, and the only one other than the earth known to have current volcanic activity. (F) P21266, Voyager 1 photo of part of the surface of Ganymede showing the mysterious grooved bands with their criss-cross nature and lateral slip fault movement. (GI P21758, Voyager 2 photo of Europa showing the unique linear features which have no relief, and which look as if they were painted on. Europa's icy surface has apparently flowed and filled in the fissures. (HI P21745, Voyager 1 photo of Callisto showing its crater-saturated surface and the strange multi-ringed structure, Valhalla.

62 ORIGWAT PAGE BLACK AND LVHiTE PHOTOGRAPH

ORIGINAL PAGE IS OF POOR QUALlW INTRODUCTION

Jupiter, next in line from the sun, has been visited by four U.S. spacecraft. These were Pioneers 10 and 11 and Voyagers 1 and 2. There were 41 investigations for which NSSDC has data or knows the sources thereof, and they cover seven categories, which are (1) Imaging, (2) Particles and Fields, (3) Ultraviolet, (4) Infrared, (5) Radio Science and Celestial Mechanics, (6) Atmosphere, and (7)Polarization. Both the categories Atmosphere and Polarization were obtained from photopolarimeters which are presented under Imaging. Tables 1 and 2 and Appendix A show the investigations in more detail.

65 SPACECW ...... SPOMSORING CDUNTRYlA6fNCY UNITED STATES NASA-OSSA

SPACECRAFT COMMON NAIIE- PIONEER 10 INITIAL ORBIT PARAl4ETfRS ALTERNATE NAMES- PIONEER-f. PL-7230 ORBIT TYPE- SATUUN FLVBY 01860 PERSONNEL NSSDC ID- 72-0121 PM - C.F. HALL(NLA) NASA-ARC PS P. DIAL NASA-ARC LAUNCH DATE- 03103172 YElGHT- 231. K6 - LAUNCH SITE- CAPE CANAVERALr UNlTtD SIATES BRIEF DESCR1PTIOW LAUNCH VEHICLE- ATLAS This wa the second mission to investigate Jupitrr an' the Outer solar systr.. Pioneer 11. Like Pioneer 10. used SPONSORING COUNIRYIAGENCY Jupiter's grawitational field to alter its trajectory UNITED STATES NASA-OSSA radically- It passed close to Saturn and then It fol1Or.d an escwe traicctory from the solar svstrm . The spacrcraft was INITIAL ORBIT PARAMEIERS 2.9 8 (9-5 tt) Long and contained 2.74-¤ (P-tt) diameter ORB11 IIPE- JUPIlER FLYBY high-pafn antenna of aluminum h0n.rco.b sandwich mat.rial rhos. fard 1.1 topped uith ncdium-g.in antenna. A lor-gain. PERSONNEL omnidirectional antenna "-5 m0unt.d below the high-pain dish. PM - C.F. HALL (NLA) NASA-ARC It contained tu0 nuclear elect,lc-pouer generators. which PS - P. DYAL IASA-ARC grn-rattd I44 Y at Jupiter, but declemsrd to 100 Y at Saturn. Therr were three rrfercnce sensop.: a star (Canopus) SC~SOI. BRIEF DESCRIPTION and tMo sun sensors. Ateitudt position cowld be cai~ulatrd This mission "1s the first to be sent to the Outer solat from the r-trrsnce direction to the earth and the sun, rith thr sv1te.r and after rrrcuntrring the ylanet Jupiter it assured an known direction to CanODus as backup. Pioneer 11's star lensor *sLlP* trajectory from the solar Svrten. The IplCeC,.ft body gain 8nd threshold settings were modified. baaed on rrprrlenca was mounted bchina a 2.14-a-dianctrr Darabolir dish antenna Oalnrd from the settings used on Pioneer 10. lhre. paits at that 1.1 46 CI deep. The SParerraft atrUCturC was 36-~m-deep rocket thrusters provldrd spin-1.1. control 1.t 4.8 rp.1 and 11.1 equipment cclpartment. the tcy and botto. being regular change of thr sPaceclaft wlocity. The thvustrrs could b. heiagons. Its sicrr Mere 11 rm long. One side joined rlthcr firid steadily 0. Pullrdr by command. Communications smalLcr COmPartmCnt that carried the scientific enprrimrnts. ware malntaincd via the omidir.ction.1 and m.dium-gain The high-gain antern, feed "as lit~atedan thile struts. rhirh antennaas which operated together. connected to on* receiver. projected forward about 1.2 m. This ferd wms topprd with a while the high-gain antenna was c0nncct.d to the other medium-gain antenna. A lor-gain omniditrtiional antenna rrcsiwrr. The receivers could be fntrrrhanged by command. Two rxtcnded about 0.76 behind the rquipment rompartlent and was radio transmitters. rouplcd to two traveling wave tub. mounted bclou the high-gain antenna. Power tor the sparecraft .mplifiersr PrOdUcd 8 Y poI*r each in I-band. Communic.tion "as obtained by four SNAP-I9 radioisotop. thermonur1c.r uplink (earth tO rp.rreratt) Operated at 2110 MHZ. and domllnk gen.rators (RT-5). rhirh were held about 3 rn from the center of (spacrcraft to earth) at 2292 nHz. At J~piter'~distantr. thr IGaceCraft ty tbc three-rod trusses 120 deg apart. A third round-trip communication ttme took 92 min. Data were .rcccir.d boo. ratrndcd 6.6 m from tht e.PCri.ent COID.,t.Cnt to hold the at the Deep Space Network (DSN). The spacrcraft was magnetometer a~ay from the spacecraft. The four ~16'1 t~.rcr~turr-rontrollcd to between -23 and +38 d.g c (-10 to generated .bout 155 watts at launch and decayed to 4100 dcg f). An additional erp.rimentr a lor-.~nsitirity aPprOxiIatCly 140 watts by the time the spacecraft reathe. flugate maqretometer. mas added to the Pionerr 11 p.110.d. Jupiter on DCCCaber 3- 1973- 21 months after launch. There Instruments studird the interplanetary and *lanetar)' magnrtlc were three refrrerre srnsors: a star srnsor for Canopus. and fields; sa1.1 rind ploperti*si cosmic rays; transition region tu0 sun sensors. Attitude position could be calculated from of the hrliosphere; neutral hydrcgrn abundance; dlstiibutionr the refrrcncc directions to the earth and the sun. rith the sizcr ..is* flur. and velocity of dust p.rtic1I.i Jovian known direction to Canop~ras a backup. Three pairs of rocket .urOlaCi Jovian radio Y~Y~S;tbe .tmOfpheres of plan*ts mnd thrultcrs providrd spin-rate control (aaintaincd at 4.8 rp.1 satelliteai and the surfaces of Jupitrr. S.turn. and somr of ard changed thr velocity of the apac*cratt. The%. thrusters thrir sat*llit*s. Instruments carried for them ~xperiments could be pulsed or fired steadily by coamand. Co.munications Yere .sgn*tomctrr, rlasma an.1yz.r Ifor ao1.P wind). ICI. maintained ria the omidirertional and medium-g.in, charged-particle det*ctOl. ionlzlng detectors "on-imaginp antennas- which operated together. ronnrctrd to one receiver ttLeScoPC1 rith overlapping field. of vier to drtlct sunlight rhilc the high-galn antenna .as connected to another receiver? reflected tic. Patsing aeteoroidsr iralrd Pressuriz*d cells of Thesr receiver. ccvld be intrrrhangcd by command to proride arson and nitrogen gas for measuring penrtration of mrtcoroids. some redundancy. Two radio transmitters, couplrd to tu0 UV photometre. IR radi0mrt.r. and an ieaging photOp01.rimrte.. traveling-wave tube amplifiers- ~rcduced8 watts at 2292 IHz nhirh Produced PhOtograPhs and measured the Polarllation. each. Uplink was ~ccomplishtd at 2110 MHZI while data Fvrthrr scllntific information "as obtained fro.! +.lrstial transmi=sion downlink 1.5 at 2292 MHz. The data "I.. received mchmics and 01~~Itationph.nom.na. This sparrrraft. like by N1SA.a Deep Space hetuo?k. Thr sPacecr.11 "as Pioneer IO, COnt4fnS pla~uethat has a drauing depicting man, t..p*..tUrc-cOntrOllcd between .inus 23 d.9 C and plus 38 drg .Oman. and the location of the sun and earth in the galaxy. C. Fifteen rxyrrimentr uerc carried to study the Pioneer 11 "as 36,800 k. from Jvpiter during its CtO8est interplanetary and planetary magnetic ficldsi solar rind mpproachr Decrmbrr 4. 1974. to within 43.000 kn of Its cloud PaIametCIa; rosllr rays: transition rrgion of the h.liosph.re; top¶. It Passed by Saturn on Aug. 5, 1919 at a distanc. of neutral hydrogen abundance; distribution. size. mar(. flux. and 2IrrOO km frcm Saturn*% cloud tops. velocity of dust uarticles: Jovian aurorae; ~ovianradio waves; atnosphere of Jupiter and some Of its satellites, parti~ula~ly and to photograph JUPiter and its sat.lLltes. Inrtrumrnts ...... IC; carried for these cxP+rim*ntr "eve 8.gnetometer. p1.s.. analrzerr charged particle detector. ionizing d(.tertorr SPACECRAFT COMMON NAME- V01A6ER 1 non-imaging teleaccpes rith overlapping fields of vir. to LLTERNATE NAMES- MARINER JUPITERISATURN A, OUTER PLANETS A dttect sunlight reflected irou Parsing meteoroids. sralrd lARlNER 7lAr MJS 171 prc~surized CCILS of argon and nitrogen gas for measuring the 10321 Penetration Of .CttOlOial. UV phOtDI.feI~ 111 radio.et.ir and an inaging PhotOC~laii.~tti~which rroduced PhCtOgr.phs .ne me.sured Polarization. Further scientific information IIS obtained from thr tracking and occultation data. Thr LAUNCH DATE- 09105177 YEIGHT- 700. K6 Spacecrbft achieved its ClOScrt approach on DCcembCI 3. 1915, LAUNCH SITE- CAVE CANAVERALI UNITED STATES when it reached *ForcxI.~tCI~ three JCv1.n radii (about 2103000 LAUNCH nfHIcLf- TITAN ti). The spacecraft contains ~Laquel that have draringr depicting a man. a ronanr and the location Of the sun and the SPONSORIN6 COUNlPYIA6ENCY earth in our 9oIa.y. It is leaving the solar system and UNITED STATES NASA -OSSA passing into interstellar space. INITIAL ORBIT PARAMETERS ...... ORBIT TYPE- SAlURN FLYBY P€RSONNEL SPACECRAFT COMMON NAIIE- PIONEER 11 PM - J.R. CASANI NASA-JPL ALTERNATE NAMES- PIONEER-G. PL-T33C PS - E.C. STONE CALIF INS1 OF TECH 6421 eRlEF DESCRIPTION NSSDC ID- 73-0191 The W*t8lL Objectives Of VOyageI wer. to conduct ewloratorr inrrstig*tions of the planetar), system of Jupiter LAUNCH DlTE- 04106113 YElGHl- 251. KG and Saturn and Of the interplanetary medium out to Saturn. LAUNCH SITE- CAPE CANAVLRAL. UNITED STATES Primary emehalls MIS placed On CDmparatlYe studirs of these two LAUNCH VEHICLE- ATLAS plmrt.ry lylttms by obtaining (1) measurements of the onwironmrnt, atmOsDhele. and body charactrristics at thr planet. and the s~tellitcsof rash planet. (2) studies of the nature of th. rin9s of Saturn. and (3) cxploiatlon of thr intrrplmet*rY (0. interstellar) medium at increasing distancra from thc aun. These objrrtivcs 11,. attainrd by uslng variety of Instruments and methods including imaging. a coherent S- and #-band RF rerrivcr. an infrared intertmrameter

67 Channeltron oitectors (blue bialkili I-11 phOtO~athode5and rsd 5-20 photocathodes) to resister the intmnsity in each p~liii~.ti~nromponrnt. Polarization data also includr the interplanetary region. - ---_--ploNcE# 11, sENI€LS------'------

INVESl16A110N NAB€- IMAGING PMOlOPOLARIBElEI (IPP)

MSSDC ID- 73-0191-07 INVESTlSATlk PRO6RAB SPACECRAil COMMON NAME- VOYAGER 2 CODE EL-4. SCIENCE ALTERNATE NAMES- MARINER JUPITERISATURN 01 OUTER PLANETS B BARINER 170, MJS 170 INVESTIGATION DISCIPLINE(S) iazii Asinomomv PLANETAR1 ATBOSPHERES NSSDC ID- 77-0761 PLANElOLO61

LAUNCH DAlE- 08120171 YEIGHl- 700. KG PERSONNEL LAUNCH SITE- CAPE CANAVERAL, UNITED STATES PI - 1. GEHRELS U OF ARIZONA LAUNCH VEHICLE- lllAN 01 - D.L. COFiEEN NASA-GISSU OF ARIZONA 01 - J. HAMEEN-ANTTILA SPONSORING COUNTRIIAGENCY 01 - C.E. KENKNIGHT U OF ARIIOYA UNITED STATES NASA-OSSA 01 - R.i. MUBBER SANTA BARBARA RES ClR 01 - U.G. 10BASKO U OF ARIIONA INITIAL ORBIT PARABETERS 01 - 1. SYINDELL U OF ARIZOMA ORBIT TYPE- SAIURN FLY01 BRlLF DESCRIPTION PERSONNEL The Imaging Phot0pOl.rimettr (1PP) rxptrim.nt used during pn - JJ. CASANI NASA -J PL Jovian and Saturnian encounter mrdc simultanrour. two-color PS - E.C. S7ONE ClLlP INS1 Oi lECH (blue - 3900 to 4900 Ar red - 5bOO to 1000 A) polari.et,ic and r~diOmetric*casuremcntsr and moderate-resolution (about 200 km BRIEF DfSCRIPllON at best) ~pin-lcanimages of Jupiter and the Jovian ratclliter The overall objectives of Voyager 2 "ere to cond~ct and Satuin and same of its satellites. lhc p~l.ii.~t~ic and riplcratary inveitipations ot the planetary syst~rsof Ju~iterr radiometric rctk was performed using an 8- by 8-.rad field-stop saturn. Uranus, and NePtUne. and ot the interplanetary medium. ~PC~~UICIwhile the spin-scan imaging used a 0.5- by 0.5-.rad Primary emphasis uas placed on c~~pifiti~tstudies of these aDCrturr StOC. Rrlatirt radiomrtric calibration "as derived planetary syite.s by obtaining (1) m~as~rt.rnts of the using an internal tungsten Lamp. Long-term rbsotutc environment. at.OsDhCle, and bod, rhar.rtcristicr of the calibration cf the instrument us accomplished by means of a planets and one Or *ore of the satellites Of each planst. (2) sunlight dlffurorlattenuator element lOLIted in the spactrraft studies of the nature of the rings Of Saturn and Uranusr and antenna structure. Primary radiometric calibration I.$ (:> aaploration ct the interplanetary (or intcrstillar) Wedius cbtained throughout thr mission by periodically commanding the at intrcasing 0ist.nres from the sun. These Objectives icrc teL+scope to vier this diffuse backlighted (sunlight) source. met using a variety of instruments and methods including The cxperimantal train for the IPP pactage consisted of the imagingr a coherent 5- and I-band Ri receiver. an IS tollowlng .le.cntr: (1) nc.r-diffr.~tion-li.itrd 2.14-r. inf~rf~~O.eterand I.diOmetCI. a UV splrfrO.~ttrr flung.tt II.ksUtOY t.l*ssop. of 10i.l 7.tio fll.4. (2) a loc.l-~l.n. m.gnet0.CtCII. Faraday CUPSI a Lha~gCd-DaCtiCle ana1yZc.r wheel containing lield-01-vier (iOV) aper1ure.r d.pO1lril.r~. plasma detector. plasma-ravr radio ICCC~VCI. coi.ic-ray Laliblation source. et(.. (31 a Y~llastonprism to split thr ttlescopesr photocolariactrrr and a sue~p-tre~~encyradio light into two orthogonally polarized beams. (4) I 4s-deg receiver- Jupiter clort encounter "as achieved on July 91 dichromatic mirror that r~flect.6 rauelengthr of less than 5500 1919. and Saturn on August 5. 1981. A lblut be..) and transmitted all light of longer rarelrngth (red bra.), (5) a filtering-coated rrlay lens and folding *irrors tor each sprctral beam (the 110 polarizations wrrc IIVESTIGATWWIS sc~arated)r and (6) two Bend<. rhanneltron lbluc - bialkali 1BAG1HG I-llr red - 5-20) phot0Eafhodc. for each spectral beam to register the intensity in each polarlaation component. Polarii.tiOn data include the interplanetary region. ___----"OIflGER 1, SB]TH------

INVESl16Al10N YARE- 1MAG1N6

MSSOC ID- 77-0841-01 INVEST1GAlIYE PROGRA1 COP€ LL-4fCO-OP. SCIENCE

INVESTIGAIIOY DISCIPLINE(S) ASTRONOMY METEOROLOGY PLANETARY ATMOSPHERES PLANElARI ATMOSPHERES PLAMElOLOGY PERSONNEL AlBOSPHEIIC PHISICS PI - 1. GEHRELS U 06 ARIZONA 01 - D.L. COiiEEM NASA-GISS PERSONNEL 01 - 1. HAMEEN-ANllILA U Oi ARIZONA TL - B.A. sniiii U OF ARIZONA 01 - C.E. KENKNIGHT U Of ARIZONA DT - L.A. SODERBLOI US GEOLOGlCAL SURVEI 01 - R.i. HUMMER SANlA BAR0ARA RES ClR in - 6.1. BRIGGS NASA HEADPUARIERS 01 - M.G. TOMASK0 U OF ARIZONA 1M - ..A-i- . COOK~ SA0.~ 01 - U. SYINDELL U Of ARIZONA TI - G.E. DANIELSON CALIF INS1 Oi TECH in - B.E. DAVIES RAND CORP 0RlEi OESCRIPllON TM - G.E. HUN1 U COLLEGE LONDON The Imaging PhotOpOlarimetet (IPP) experiment (used also 1R - 7. OYEN SlAlE U OF NEY YORK on Pioncc~11) used durinq Jovian cnrountrr made simult.ncousr in - c. SAGAN CORNELL U tiO-cClOr (blue - :900 to 4900 A. red - 5800 10 1000 A) in - V.E. suoni U Or UlSCONSlN p01ari.etric and radionttric measurCmentsr and 111 - T.V. JOHNSON NASA-JPL moderate-rtrolution (about 200 k. at best) spin-scan imager of TB - H. BASUPSKY US GEOLOGICAL SURVEI ~~citerand ttt Jcvian satellites. The polarimetri~ and IadlOmetliC "OIL "as PCIfDllCd urinp an 8- "8- mrsd fI.ld-ltEE BRlEi DESCRlPlION apertu,~, while the spin-scan imaging used a 0.5- by 0.5-mrma Thr PhOtO9rlDhic elperimrnt used a two-camera system# epirtur~ stop. Relative radiometric r.liblation I.* dcriwed based on thc Barincr 10 systrm. This system includ*d on. using an internal tLngstcn laip. Long-term absolute calibraticr narror-angle. long-tocal-length emera and one wide-angle. of the instrument was arromplirhrd by means of a sunlight short-focal-length cmer.. lhr ...i.um resolution .Chiev.bl. diffUsellattCnUatOr elellent Located in the SpaCeCraft antenna depended on thr actual trajectory on this .ulti-rncount.r struct~re. Plillly radiomctrir ~alibration 111 obtained mission. but the resolution was *I high as 0.5 to 1.0 k. on the throughout the m~rlionby p~ri~dicall)rommandinq the ~CI~SCCLIclosest .ppro.~hei to some objects. At Jupiter and Saturn, the to vie. this diffuse backlighted (sunlight) IOUIC~. The resolution was better than 20 km and 5 km. rrspectiwly. The experimental train for the IPP package consisted of the objectives of the e.prriment were to photogr*ph global motions fcllcring rlemrnts: (1) a n..r-dittr.ction-li.it.d 2.S4-C* and cloud distribvtions on Jupiter and Saturn, gross dynamiral natsutov catadioptric tc111c0pc of focal ratio 113.4, (2) a proptrtiei. zonal rotation, orientation of spin axis. zonal focal-plane wheel containing field-of-view (FOY) apertures. shear. veitical shear, tlor instabflitirir spots. and sptctrum aepolarizers, ralitration IOUICC~ etc.. (3) a uollaston prism of scale of atmosphtric motions in time and SPICC. Additional to split light into two orthogorally polarized btamli 14) a cbjcrtives included the study Of the .Ode Of releare Of 45-dcg dichromatic mirror that reflected uawelengths shorter internal energy flu. (rearch for ronvertion rrlls and rolls). than 5500 A (hlu. beam) and transmitted all light Of greater Study Of growth, dissipation, .OrphOlOgy. and vertical wavel.ngth (red tea.). (5) io, each spectral beam (tu0 structure of cloud complcxcr. gross opti~slproperties, global polariz~tionsl a filtering-coated relay Lens and folding and IOcaiii~d scattering funrtion in the visible sp~ctwmr mirrors, an0 (6) for each spertr.l be.., two Btndi. polarinetryr nature of chromophores (their stiurt~~eand developwent). and high resolution of the Great Red spot. The PERSONNEL objectires of the satellite enco~ntersincluded the totlawing: PI - J.H. YOLFE NASA-ARC (1) gross charactiristics (size. shape. rotation. spin axis, 01 - L.A. FRANK U OF IOYA cartography. improved ephemerides and masses.) (2) geolcgy 01 - R. lUS.1 MPI-HEADQUARTERS Irmjor physiographic pro~inte~.inpact and volcanic features. 01 - D.S. INlRIL1GAlOR U Of SOUlHERN CALIF 1incl.cntSr polar Cap*. trOIi0" ~IOCCISCII and 10"- and 01 - D.D. MCKIBBIN NASA -ARC high-density satrllite co.pirative Itudiesr drtecticn of 01 - V.T. ZAVIENISEFF(hLII NASA-LRC atLOIphCres~ frosts. and limb stratifiratipn of arrosolr,) (3) 01 - F.L. SCARF TRY SYSTEMS GROUP surface properties (coloiiictryr scattering function. nature of 01 - H.R. COLLARD NASA-ARC brightness variation, and search for ncr satcllitts.) Studies 01 - Y.C. FELDMAN LOS ALAMOS NAl LAB of Saturn's rings included: (1) rrrclvtion of irdividual rirg 01 - I.A. S~IIH NOAA-StL components or clurus of material. (2) vertical and radial distribution Of material at very high resolution. (3) BRIEF DESCRIPlION scattering funttior. (41 coarse polariietiy. (5) ocrultaticr - The instruitnt (also carried on Pioneer 11) ronrirttd of Opticll dcDthr and (6) distinguishing different types 01 dual PO-deg guadrisoherical clertrortatir analyteisr one with material in the rinpr. Other abicctivcr rerc to search tor nrr 26 individual oarticle deteltorl and the Other .ith 5 current comets. asteroidsr and targets of opportunity. rollcrtors. lhr system was capable of masvring incident p1ar.a distribution parr.leterr over the energy range 0.1 to I8 LcV for protons and aDproxi.ately 1-500 eV for ~L~ltrOns.lhe high-resolution analylc.. with a constant of 9 kcVIP pep kv INVESlIGAlION NAME- ILAGING applied to the plates. had 0 mean pl.tC radius of 9 cm and separation of 0.5 cm. This analyzer. which was used to measure NSSDC ID- 7r-076~-01 INVESTIGATIVE PROGRAM ions only. had 26 channeltrons mounted on the rrmicircular COD€ EL-4. SCIENCE trit to the analyzer. lhe aperture painted through a uiet slit in the bark of the spacecraft high-gain antenna reflector and INVESTIGAlION DISCIPL~NE(S) pointed along the spin asir touard the earth (and therefore the MEIEOROLOGY sun). lhc edges of the antenna reflector limited the viewing PLANETARY ATMOSPHER€S cf the instrument to 73 deg rith rrsccrt to the spin axis. The PLANEICLOGI channeltronr Conertd a range of plus or minus 51 dcg. Each channeltran near the center covered 3 dtgr and approximat~ly8 PERSONNEL d+g war the edges Of the analyzer. lha angular width TL - 6.1. SMIlH U 0.6 ARIZONA perpendicular to the long angular ridth la* about 2 deg. In DT - LA. SODERBLOM US GEOLOGICAL SURVEI one half tht spin period. the whole cone of halt angle 51 drg. in - G.A. ~RIGGS NASA HEADPUARTERS centered on the sun. 11s svcpt out. A medium-energy analyzer 1M - A.F. COO1 SA0 rich a mean radius of 12 cm and a 1-c. piate seuaratvon 1M - G.E. DANIELSON CALIF INS1 OF TECH (constant of 6 keVlP PCI kv applied) was used to detect both TM - M.E. DAVI€S RAND CORP ions ana electrons. The detectors were tiwe flat-surtaft lll - G.E. HUN1 U COLLEGE LONDON c~rr~nt collector^. lhc three center roll~ctorseach covered in - 1. OUEN SlATE U OF NEY YORK 15 deg and covered the angular range of PLUS or minus 22.5 deg 1M - C. SAGAW CORNELL U from the spin axis. lhe 110 outside collertorr had an angular 1M - V.E. SUOMl U OF UISCONSIN width Of 41.5 acg and were located at plus or minus 46.25 dcg TM - T.V. JOHNSOH NASA-JPL trom the center of the analyzer. lhere rere a variety of TM - H. MASURSKY US SEOLOGICAL SURVLY possible operating modes for the experiment; however, the principal node Utilized during the encounter phase rai one in BRIEF DESCRIPTION which the analyzer plate potential was stepped through its The photographic elDelilCnt used a tllo-cawrs sy~te.. range evc~y one-half rcvolvtion Ot the IpacecIaftr and all based on the Mariner 10 system. This sylt~mincluded one cu~ient collectorr 01 channcltrons were read out at the peak narrow-angle. tong-focaL-tength canera and one uide-mqit. flux roll angle. The high- and medium-resolution analyzers short-focal-length C~CIS. The maximm rcroLution achievable operated independentlyr so that a cr~is-ch~ckbetween these depended grcatly on the actual trajectory on this analyzers I~Ioosrible. The dynanir range for the pa~ti~l~ multi-tncountrr mission. but "as as high as 0.5 to 1.0 tm on fluxes was from l.OE+Z to 3.OE*9/lq cm I and the proton the tlasest app~~achesto some otiectr. At Jupiter and Siturrr temperature could be ascertained down to 2.OE1.' deg K. Data the resolution that 1.1 achieved "as bettei than 20 kn and 5 include the interplanetary rcqion. kmr rcspcrtivcly. lhc objectives of the cxperi-cnt ucrc to photogr.ph slot.1 .otions an0 cloua distributions on Jupiterr ---__--PICNftR 11, YOLTE------Saturn, UraIIus~and Neptuner grOlS dynamics1 plopelti,ll rcn.1 ratation. orientation of rpln axis, zonal shear, vertical INVESTILATION NAME- PLASllA shear. flow instabilities. spotsr and spectrum of scale of atmospheric motions in tile and scact. AdditiOI.1 obitrt,v.s NSSDC ID- 13-0191-13 lNVESlltATlVE PROGRAM included the study of the mode Of release of internal energy CODE EL-+/CO-OPI SCIENCE flu' (search to, convection OLLLI and rolls), study of growth, dissipationr morphologyr and YCrtice.1 StrUCtUrC Of cloud INVESlIGATlON PISCIPLINE(S) CCllFLercr. gIOSI Cptical pl0Pertielr global and lOc.luc4 SPACE PLASMhS scattering function in the visible sp~ctrumr pol.riletry, PARllCLES AND FIELDS natuve of chromophores (their str~ctureand derrlop.cnt)r and high resolution of the 61t.t Red spot. The objertiuer Of the PERSONNEL sat*llite encounters included (1) gecss char.rteristirs (size, PI - J.H. UOLF€ NASA-ARC shape. rot.tiOnr IDin arise caltOgraphYr implOYCd ephemerides 01 - L.A. FRANK U OF IOYA and masses;) (2) g.ol0gy (major phisicg.aphi~ provinces, impact 01 - 1. LUST MPI-HEADOUARTEUS volcanic features, lineanenti, polar C~PS. erosion 01 - D.S. lNlRlLlGAlOR U OF SOUTHERN CALIF proccrrcrr and lor- and high-density sat~llitcronparativr 01 - V.T. ZAVIENTSEFF(hLA) NASA-ARC studies. detection of atmospheres. fmstsr and limb 01 - 1.A. SMITH NOAA-SEL1RY SYSlEUS (.ROUP stratification of aeros~ls;) and (3) surface properties 01 - F.L. SCARF (colorimetryr scatt.rinp functicr. nature of brightress 01 - H.R. COLLABD NISI-ARC variation. ana s~avchfov ner satellites.) studies of saturn.. 01 - Y.C. FELDMAN LOS ALAMOS NAl LAB rings U.VC carried out ana riii be far ur.nUs' rings. 01 - O.D. MC K 100 1I( NASA -An C 0tj.ctivrr included (1) resolution Of individual ring coueoncntr of CLU~PS of material; (2) vertical and radial BRIEF DESCIIFIION distribution of material at very high ~~sol~tion;(3) The instrument consisted of dual 90-6-9 ouadlispheric.1 scattering function; (4) coarse polari.rtry: (5) occultation - electrortatir analyzerlr one rith 26 individual part,rlt o~tical depth; anc (6) distinguishing different types of detectors and the Other rith 5 current rollertors. The syst*m material in the rings. other Objectives were to search for ncr 11s capable of mcarurinq incident plasma distribution comets. asteroids. anc targets of Oppoitunity. parameters over the energy range 0.1 to 16 Lev for umtoni and a~pr~ximately1-500 cv for tlrrtronr. The high-resolution analyzer rith a conitant Of 9 krY/P per kv applied to the PlStCIe had a "Can plate radius Of V C.i and rcpa,atiOn Of 0.5 PARTICLES AND FIELDS cm- This analyzer was used to measure ions only, and had 26 channeltronr iaUntCd on the smitiic~larerit to the analyzer. The apeiture painted through a viae slit in the back of the ~paccrraft high-gain antenna reflector and pointed along the spin axis tobard the earth (and therefore the sun). lhe edges of the antenna reflector limited the viewing of the instrument lNVESllGATION NAME- PLASMA to 73 atg rith ~CSPCL~to the spin axis. lhr rhanneltrons COVeIed I range of plus or minus 51 dcg. Each rhanneltron near NSSDC ID- 12-0121-11 INVESTIGATIVE PROGRAM the centep cc~cred3 acg ana approaimateiy u acg near the edges COD€ fL-4ILO-OP. SCIENCE Of the analyzer. The angular ridth CClpCndiCU1.I to the long angular width was about 2 deg. In half the pin period the INVESllGAllON DlSClPLIN€(S) rholr cone of half-angle 51 deg rrntrrcd on the run "as swept SPACE PLASMAS Out. A medium-energy analyzer rith a maan radius Of 12 cm and PARllCLES AND IlfLDS 1 cm plate secaration (constant of 6 Lev10 per kV a~plied) *.I *.I used to detect both ions and ClCctlOnl. The detCCtOIs lclc five tlat-surface current callcrtorr. The three center collcctorr each covered 15 dcg and covered the angular range of clus or minus 22.5 aeg from the rpin axis. lhe tu0 Outside

69 r~Ll.ctOrs had an arg~larwidth Of 47.5 de9 and Were 10CltCa at NSSOC IO- 77-064A-13 INVESTIEATIVE PRO6RAM PIUS01 minus 46.25 4cg from the center of the analyirr. There CODE tL-4r SCIENCE was a variety of ~ossibleoperating modes for the enparimenti hewever. the printi~almode uti1iz.a auring the encounter phase INVESTIGATION DISCIPLINEIS) I.. one in rhith the analyze, plate DOt.nti.1 "as sttpcid PARTICLES AND FIELDS through its range e~eryonr-half rrvoluti~nof the sparrrraft. MAGNETOSIHERIC PHYSICS and all current rollcttorr or rh.nn.ltron1 "ere read Out at the PLANETARY IONOSPHfRES peak flux roll angle. The high and Wediw rrrolutlon analyzers 0p~1.t.d ind.pendently. SO a cross check betueen thest PERSONNEL analyzers was possible. The dynamic range for the pavtiele PI - F.L. SCARF TRY SYSTEMS GROUP fluxes I.. from I.GEt2 to 3.06191sq cm s and the proton CI - D.A. GURNETT U OF 1011 temperature down tc 2.OEt3 aeg K cculd br asrcrt.inrd. Data include the interplanetary region. BRIEF DESCRIPTION This investigation cvoviaed continuous, sheath-independent .tisurementi of the clrrtron-density CrOtills at Jupiter and Saturn. It also gave basic intor.rtion INVESTIGATION NAME- LOY-EYER61 CHARGED PARTICLE ANALIZER AND on 101.1 waw-~article interaction required to carry out TELESCOPE cornparatire studies of the physics of the Jupiter and Saturn magnetosphtres. The instrumentation consisted of a 16-channel. NSSDC ID- 77-084A-C7 INVESTIGATIVE PROGRAM step-frequency receiver and lou-frequency raveform receiver. CODE EL-4ICO-OP. SCIENCE rith associated electronics. The frequency range for this ~nstrument I.. fro. 10 n2 to 56 kHz. This instrument shared INVESTIGATLON DISCIPLINEIS) the 10-a antennas dewelaped for the investigation of planetary COSMIC RAYS radio aitronoey. MAGNETOSPHERIC PHlSlCS PARTICLES AND FIELDS ----_-- VOyA'ER 2, SCARF------

PERSONNEL INVESTl6AllOl NAME- PLASMA .AVE 1-01-56 KHZ) PI - 1-11. KRIMIGIS APPLIED PHYSICS LAB C1 - C.Y. FAN U OF ARIIONA NSSDC IO- 77-076A-13 INVESTIGATIVE PROGRAM CI - 6. CLOECKLER U OF MARILAND CODE EL-4, SCIENCE C1 - L.J. LANZEROTTI BELL TELEPHONE LIB C1 - T.P. ARMSTRONG U OF KANSAS INVESTIGATION DISClPLINElS) CI - Y.I. AXFORD MPI-AERONOMY PLANETARY IONOSPHERES CI - C.O. nosvncn APPLIED PHYSICS LA0 PARTICLES AND FIELDS CI - E.P. KEATH APPLIED PHYSICS LA0 MAGNETOSPHERIC PHISICS PERSONNEL PI - F.L. SCARF TRY SYSlEMS 6ROUP Cl - D.A. GURNETT U OF IOUA

BRIEF DESCRIPTION This investigation provided rO"trn"O"s, rhrath-indecendent measUIe.Cnts of the .LeLtlOn density nroiiles at Ju0it.r and Saturn and rill for Uranus and NCL~Y~C. It a110 gave basic information on local uavc-particlc interactions lcquiicd to cavly out c~mparati~eStuaicI of the chyiics of the magnetospheres of these plinets. The instrumentation consisted of a 16-channel step frequency rcccive1 and a low-trrqucnry raveform receiver rith associ11cd e11ctr0ni~s. The frequency range for this instrument was from 10 HI to 56 LHz. This instrument shaved the 10-n antennas dCIelOped for the planetary radio astronomy inrartigation.

INVESlIGAl10N NAME- LOY-ENERG1 CHARGED PARTICLE ANALYZER AND TELESCOPE INVESTIGATION NARE- PLASMA SPECTRONETERS

NSSDC 1D- 71-0761-67 INVESTIGATIVE PROGRIP NSSDC IO- 77-0841-06 INVESTIGATIVE PROGRAM CODE EL-41CO-OP. SCIENCE CODE EL-). SCIENCE

INVESTIGATION DISCIPLINE(S) INVESTlbATlON OISCIPLINE(S) COSMIC RAYS PARTICLES AND FIELDS MAGNEICSPHERIC PHYTICS SPACE PLASMAS PARTICLES AND FIELDS PERSONNEL PERSONNEL PI - H.S. BRIDSE MASS INST OF TECH PI - S.M. KRIllIGIS APPLIED PHYSICS LAn C1 - J-b. BELCHER MASS INST OF TECH c1 - C.O. BOSTROM APPLIED PHYSICS LA0 CI - C.K. 60ERT1 UP1 -AERONOMY Cl - 1.P. ARMSTRONG U OF KANSAS C1 - A.J. LAZARUS MASS INST OF TECH Cl - Y.I. AKFORD MPl-AERONOMY CI - 5. OLBERT MASS INST OF TECH Cl - G. GLOECKLER U OF MARYLAND CI - V.R. VASYLIUNAS MPI-AERONOMY C1 - L.J. LANIEROTTI BELL TELEPHONE LA0 C1 - L.F. BURLAGA NASA-GSFC CI - C.Y. FAN U OF ARIZONA Cl - R.E. HARTLE NASA-GSFC C1 - E.P. NEATH APPLIED FHYSICS LA0 CI - 1.1. OGILVIE NASA -6 S F C C1 - G.L. SI SCOE U OF CALIF. LA BRIEF DESCRIPTION Cl - A.J. HUNDHAUSfN NATL CTR FOR ATROS RES The oblertive Of this experiment "1% 10 study the CI - J.D. SULLIVAN MASS INST OF TECH .agnetospheres of Jrpiterr Saturn. Urarus. ana Neptune. "sirs CI - J.D. SCUDDER NASA-LSFC 10"-cnerpy .agnrtosnheriC p..title analy2er- This dCteItDI ..de m~asurements in (1) the distant magnetosphere and bow BRIEF DESCRIPTION shock ot Jupiter. (2) the rnagnetosph~re of Saturn and possible The plasma investigation maae use of tu0 Faraday-cup vagnetosphrrr of Uranus and Nept~re. ana (3) the trapped detertorfr Ope Pointed along the earth-IPacecraft line and One radiation belts in the vicinity of these planets. at right angles to this line. The earth-pointing detector Aaditionally, this detector was able to study 1OI-ene.g~ aaterminrd the macroscopic properties of the plasma ionrr particles in the interplanetary aedium. The energy range of obtaining accurate valuer of their velocity, density, ana thls detector was IC Lev to 1.1 MeV for electrons and 10 keV to CI~SIUI~. Three sequential energy scans were ~mployedrith 150 MeV for ions. During the inttrplanrtary cruise DCriOd, (delta €)/E t9u.l 10 201 1.2. and 1.8 I, alloiing a coitrag* protons. alpha Particles. and hcaricr nuclei lz from 3 to 26) from subsonic to highly supersonic flow. The iiac-looking were separately icentified and their energies mIasUled in the Faraaay cup m~asuiedcl~rtrons in the cncrgy ranpc from 5 ev to range from 0.05 to 30 MeV. using Lou-rnergy paiti~l. 1 Lev. t* lcsropr. ------VOlAGER 2, BRIDGt------__ - - - "Oy&GEl( 1, SCARF---'------'------'------INVESTIGATION NAME- PLASMA SPECTROMETERS INVESTIGATION NAME- PLASMA YAVE 1.01-56 KHZ) NSSDC ID- 77-0161-06 INVESTIGATIVE PROGRAM CODE EL-~ICO-OPI SCIENCE

INVESTIGATION D1SCIPLINflS) SPACE PLASMAS PARTICLES AND FlfLOS

70 PERSONNEL PI - n.s. BRIDGE MASS INS1 OF TECH CI - A.J. LAZARUS MASS INST OF 1ECH CI - s. OLBERT MASS INS1 OF TECH Cl - J.Y. BELCHER MASS INS1 OF 1ECH MSSDC ID- 17-08+A-01 INVESTIGATIVE PRO6RAM CI - V.M. VASYLIUNAS MPI-AERONOMY CODE El-4. SCIENCE c1 - L.F. BURLAGA NASA-GSFC Cl - C.K. bOERlZ MPI-AERONOMY INVESTIGATION DISCIPLINEIS) C1 - G.L. SISCOE U OF CALIF, LA PLANETARh.lAGNETIC FIELD Cl - A.J. HUNDHAUSEN NATL CTR FOR ATMOS RES PARTICLES AND FIELDS CI - R.E. HARTLE NASA-66 f C IN1ERPLANETAI)V MA6NETlC FIELDS CI - K.Y. OGILVIE NASA-GSF C C1 - J.D. SULLIVAN UASS INS1 Of TECH FERSONNEL CI - J.D. SCUDDER NA SA-G S FC PI - N.F. nEss NASA-6SFL CI - M.H. ACUNA NASA-GSFC Cl - K.Y. BEHANNON NASA-6SFC CI - L.F. BURLAGA NASA-GSFC CI - R.P. LEPPING NASA-6SF C CI - r.n. NEUBAUER BRAUNSCHYEIG TECH U

BRIEF DESCRIPTION This experiment I.. designed to 1nr.stig.tr thr m.gn.tic fields Of Jupiter and Saturn. the 1ol.r-ulnd interaction with the magnrtospher*s of these planets. and the 1ntrrplan.tary magnrtir tlrld Out to the s01.r ulnd bound8ry iith the interstell.. magnetic tield and beypndr it CIOSS.~. The investigation was rwried Out ulino t*O high-lield and two 10"-tield triaxial fluxgate magnetomt.rs. Data accu?acy of the IntClplanLtaVy fields was plus or minus 0.1 nTr and thr range ot measureaents 1.5 from 0.01 nT fo 2.E-3 1.

NSSDC ID- 12-012A-01 INVESTIGATIVE PROGRAM CODE EL-), SCIENCE IHVESlIGAlION NAME- TRIAXIAL FLUXGATE MAGNETOllETERS INVESTIGAl10N DISCIPLINE(S) PARTICLES AND FIELDS NSSOC ID- 71-176A-05 INVEST IGA 1IVE PRO61111 PLANETARV MAGNETIC FIELD CODE EL-+ICO-OP. SCIENCE MAGNETOSPHERIC PHYSICS INVESTIGAllON DISCIPLINE(6) PERSONNEL PLANETARY MA6NEllC FIELD PI - E.J. swiin NASA-JPL PARTICLES AND FIELDS 01 - 0.1. COL@URN NASA-ARC lNlERPLANETAR1 MA6NETIC FIELDS 01 - P. DYAL NASA-ARC 01 - C.P. SONETT U OF ARIZONA PERSONNEL 01 - P.J. COLEMAN, JR. U OF CALIF, LA PI - N.F. NESS WAS A -65 F C 01 - 1. DAVIS, JR. CALIF INST Of TECH CI - R.P. LEPPING NASAbSFC 01 - O.E. JONES BRIGHAN YOUNG U CI - F.M. NEUBAUER BRAUNSCHIEIG lECH U CI - K.Y. BEHANNON NASA-GSFC BRIEf DESCRIPTION CI - L.F. BURLAGA NASA-65 FC The mac)n.to.etrr on Pionerr IC (also carried on Pionrer CI - M.H. ACUNA NASA-GSFC 11) is a triaiiil helium magnetometer with reven ayn.mic ranges, trom PLUS or .inus 2.5 nT to plus or minus 10 gauss. BRIEF DESCRIPTION The linearity "as 0.11. and the noire threshold was 0.011 I.. This crprriment I.* desipncd lo Investigate (1) the tor 0-1 HI. The accuracy was 0.51 01 full scale range. lbi magnttic fields 01 Jupiter. Saturn. Uranus. and Neptune; and experiment worked as planned until November 1915. rhrn the (2) the solar-rind interaction Of the magnetospheres of thesr spacecraft was at about e a". NO turthei uretul data "ere planets with thr intRvP1anctary mqnrtlc tield out to thr ottained. The eIperimcntcr has bled RlN coordinates in his solar-uind boundary with the interstellar magnetic tirld. and data analysis. In this sv'lte-r R (or a) VI radi.llv Out..rd beyond. if crossed. The invcstigatlon was carried out using from (he sun, T (0, I) is pi,.llcl to the sun's csuatorial tu0 high-field and 110 lor-firld triaxial flussat. plane an0 has its direction given by the cross product at the ma~nctooeters. Bst. ac*nr.sy of the interplanetary tieldl 1.1 sun's spin vcc~orinto the radial direction (i...,into R) ard plus or minus 0.1 nl. and the rang. ot m..surem.nts is from N (01 2) Completes the right-handed orthogonal system (positive 0.01 nT IO2.6-3 1. northrard). A detailed instrument description may be found in Seith et al.. IEEE lrans. On MagFCtics. Mag-11, p. 962. JuIy ------PIONEER 11, ACuNA------'------1975. S0.C data .(SO include the interplanetary region. INVEST1bATION NAME- JOVIAN MA6NETIC FIELD ------PlO"EZR 11. S~Il"------.------~--- hSSDC ID- 13-0191-14 INVESTISATIVE PRO61111 INVESTIGATION NAME- IIAGNETIC FIELDS CODE EL-). SCIENCE

NSSDC ID- 13-0191-01 INVESTIGATIVE PROGRAI lNVESTlGAllON DlSClPLINE(S) CODE EL-4. SCIENCE MAGNETOSPHERIC. PHYSICS PLANETARY MAGNETIC FIELD INVESllGAllON DISCIPLINE(S) IIAGNETOSPHERIC PHYSICS PERSONNEL PLANET#RV MAGNETIC FIELD PI - n.n. ACUNA NASA-GSFC PARTICLES AND flELDS 01 - N.F. NESS NASA-GSFC PERSONNEL BRIEF DESCRIPTION PI - E.J. SMITH NASA-JPL lhis instrumentr designed to .t.suit the Jovian and 01 - 0.1. COLBURN MA SA -ARC Saturnian magnetic field. ~onsisteaof a single-range 111aii.L 01 - P. DVAL NASA-ARC tlurgate magnL10mCter sensor and ~SsOcIatCdclrrt~onirs capable 01 - C.P. SONETT U OF ARIZONA Of Irasuring fields from 1.1-6 to I.€-3 1 (0.01 to 10 gaurs) 01 - P.J. COLEPAN, JR. U OF CALIf, LA along rach orthoponll axis. Use of a 10-bit A-to-D r0nrert.r 01 - L. DAVIS. JR. CALIF INS1 OF TECH yielded quantization step size of minus to plus 600 nT tor 01 - D.E. JONES BRIGHAM YOUNG U ticldr less than 2.E-4 1. Instantaneous vector m.asurements were made once CYCIY three rrvolutianr of the spa~ecraftI36 s) BRlEf DESCRIP~ION and transmitted to the ground vlth no further onboard The magnetometer on Pioneer 11 #as a trla.i.1 hcliun pro~e~~ing.nore instrumental details are given in SP. Stl. magnetometer with seven dynamic ranges- trom plus or minus 2.5 1nitrum.r 1. Ir p. 111. 1975. Prlnripal Jovian sri.ntitir nl to PLUS or minLs 1.OE-3 1. Tht lircarlty "as 0.11 aFd 1he results can be tound in J. Gcophys. Res.. Y. 81, p. 2917, 1916. noire thr=ihold was 0.01 nl rms for 0-1 HI. The accuracy I., 0.51 ot full scale range. lhc e~perimenter used RTN __--_-_PlONELp, 10. SIMPSON------'------'------caorainat~s in the data an.lvris. In this system. R (or x) is radially OUtIard from the Sun. T (or 7) was parallel to the INYESTlGATIOL NAME- CHARGED PARTICLE COIIPOSlTlON sun's equatorial plane and had its direction given by the CIOIS Product of the sun's spin YCC~OI into the radial direction NSSDC 10- 72-0121-02 INVESTIGATIVE PROGRAM (i.e., into R) ara N (or I) cc.pleted the right-hanaea CODE €1-4. SCIENCE orthogonal IyltCm (positive northrard). A detailed instrument d*iciiptinn may be tound in Smith et al., IEEE Trans. On INVESTIGATlON DISCIPLINECS) M*gneticrr V. M-llr P. 962. July 1975. Data include the PARTICLES AND FIELDS intcrplanstary rcgicn. COSMIC RAYS PERSONNEL -__--__plQhEt@ 11, "AN ALLEN------PI - J.A. SIMPSON U Oi CHICAGO 01 - J.J. O'GALLAGHER 0 OF MARILANO IWYESlILAllON NAME- JOVIAN CHARGED PARTICLES 01 - A. lU1ZOlINO U 06 CHICAGO hSSDC ID- 13-019A-11 INVfSl16A11Vf PROLRAM 0Rlfi DESCRlPlION CODE EL-4, SCIENCE This experiment lcarrita also on Pionerr 111 m~asured charged-partitl. c~r~ositionand rrtrtr'a using tour detCctSr INVESTILATION DISCIPLINf (S) systc~s: 11) the main telestope, consisting of sewen clrmcntr PARTICLES AND ilfLDS and providing energy Ipcctla 1apprOxi.atCLy 3 to 68 MeV lor MAGNETOSPHERIC Pnvsics protons and 10 to 150 MtVIN for onygrn), element rcrolution (through oxygen), ard isotope rerrlution Itor H and He); (2) FERSONNfL the lor-anergy subsystem tlltsrOPe~COnrirtlng Of tl0 elc.rntS PI - J.A. VAN ALLEN U OF IOYA and using a very small thin first element to extend the high-sensitivity prctcn .eas~re#entl telor 1 Il.V 10.3 to 9 MU) ERlEF DESCRIPIION in the prc~cncc Of a high gamma-*ay bacbgrOLnd aboard the This t.peri.cnt used seven miniature beige, tubes in s~a~t~rafti13) the electron-current detector lor ECG). threc arrays to ~C~IUIC lat ton and electron fluxes near Jupiter consisting of a beryllium-shield silicon detector operated in and Saturn. Detector 9.0upingr ".,e ar fallows: 111 a current rode to ~~~SLIChigh fluxes cf ~ltctrollsrith energies three-tlrment LA. E- and C) difterrntially shielded tclrscope. above 3 MeV; and (4) the fission cell dctectorr recordins lube C was shielded omiaircctionally ana was used tor firsion fragments from the nucleon-induceq fission of thorium background subtraction to ~rOvide,ate, Such 1% A-C (5 to 21 232 randbiched betreen tu0 large-arca silicon detcrtori to MeV tlcrtronr and 30 to 17.5 MeV protons) and 6-C 10.55 to 21 measure fluxes Of pIOtDnl (above 30 MeV) in the PteSCMLe Sf MeV elCCtrons and 6.6 10 11.5 UCV plOtOnsJi (21 a three-element high flu~es 01 rlertronr. 1hC elp.riment ramvlc time was triangular array. each clement respond-ng to el~ctronsabove 31 rynthronirtd rith the SP~CCC~~~Ispin. permitting sectorina 01 mcv and yrotoni above 11.5 Ucv; and 13) 1 thin-window tube (6) the readout of the main and Lc*-er*rgy t~lesco~~sinto tight rith 1 gOLd-PlatLd ClbOu .I tbC enIranCc apCItuIC to admit ottants about the spin azis. Data also include the scatt~red electrons above 0.06 MeV while aisciiiinating inttrplanctary region. strongly against protons. For a descriution of the sliilar experiment On Pioneer 101 Ire Van Allen ct a1.s J- GeOuhyS. - - _-- - - PIONEER 11, S1MpSON-'----'------~------'------Res.. Y. 19, P. 3395, 1974. Early rc~ults art given in Science, I. 188, p. 4591 1915. Data include the interplanetary lNVESllGAllON NAME- CHARGED PARTICLE COMPOSlTlON region.

NSSDC ID- 11-019A-E2 INVESll6CllVf PROGRAM ------PlCkEfR 10, FlL~lus------'------'---- CODE EL-4. SCIENCf INVfSlI6ATION NAME- JOVIAN 1RAPPED RADlAllON INVESlIGAllON DISCIPLINEIS) PARllCLfS AND ilELDS NSSDC ID- 12-012A-05 INVESTIGAllVE PROGRAM COSMIC RAYS CODE EL-4, SCIENCE

PfRSONNEL INVCSllGATlON OISCIPLINE(S) PI - J.A. SIMPSOH U OF CHICAGO PARllCLES AND ilELDS 01 - J .J. O'GALLAGHER U Oi MARILAND I4GNETOSPHERIC PHISICS 01 - A. 1UZZOLlNO U Oi CHICAGO PERSOYllLL 0RlEi DfSCRIPlION PI - 11.11. ilLLlUS U Of CALIF, SAM DIEGO lhii experiment used two t.lescOpes to ~C~IUI~the 01 - C.E. MCILYAIN U Of CALlir SAM DltL0 composition and energy spectra of solar (and galactic) paIti~1C1 above about 0.5 MrVlnuClcon. The main telcrcopt 0RIEi DESCRIPTION renrirted ot five rollincar rlc-entr (three solid state, one This cs~crinent consisted ot an arvay of five p~lti~l~ Csli and On+ sapphire Cerenkov) Surrounded by a plastic aetectors rith electron thresholds in the range .01 to 35 MeV anticoincidence shield. The teleSCOpe had a 60-degi full-angle and proton thr~sholdsin the range 0.15 to 60 MeV. 1 Cerenkov a~ctptance cone with its axis ap~roxi.ately normal to the LOY~~CI (0 had tour output channels (CIS (2. C3, and CDC) spacecraft npin asis. permittirp I-sectorco intormatior cn sensitive to ~l~ctl~nshaving tntrriel above 6. 9, 13, and 1 patti~l~arrival direction. io". elrientf of the main MeV. IeIp~CtiYIly. An CleCtlOn-IcattCr LOuntCl (E) had three telescope IC,~ pulse-height analyzed, and (01- and high-gain output channcll lflr E2r and €3) sensitive to alcrtronr above mOIIeI could bc selected by command to DCrRit resolution of the -16. .26, and .4b MeV. A minimum ionization rounte~(I) had elements H through Ni or of the electrons of H and He aCd the three Output channels, 111 sensitive to clcttrons having iSOtOD15 of H and HC and light nuclei. A selection-priority energies 91CatCI than 35 MeV, n2 that me.rureO background. and scheme "1% included to permit sampling of leis abundant (13 that I.% ~~nsitiveto DrOtOnS having energies greater than particle sp~cic~uraer normal and sclar-flare rolditions. The 80 rev. lhe last two sensors icrc scintillator detectOPs (SP lo.-rncrgy tcle~copc "as ess~nt~allya tw-elc.ent. shielded. and Sf), both Of which had CnCrgy thresholds Of 10 Lev tor SOtid-ltatC detector with a lO-deg. tull-anglc acceptance tone. eLCCtrOnl and 150 Lev far DlOtOnS. lhe I~nSltivityOt the SE lhe first element "as pulse-height analyztdr and data "ere dctcctor 10 protons I.% about a factor of 10 lower than if% recorded by ItctCll. Data inLLUdl ttt interplanetary repior. s~nfitirity to electrons. Thus, the SEDC channel effertivtly mtaiured thr rlertron flux, which could then be subtracted 1,011 __.____PIONEER 10, VAN ALLEN------the SPDC channel ~CSPOIIIC 10 Obtain the pi0t0" tlux. Several other rhannrlrr listed above. required Corrections to Obtain lNVESllGATION NAME- JOVIAN CHARGED PARTICLES the flu~es cf the sptties indicated. Three of the channels ICDC, SPDCI and SEDCJ were lead out through a common NSSDC ID- 72-0121-11 1NVESTl6AllVE PROGRAM ~LCctcOmttel. 0°C to 1 maltunction that oLLurrc0 beticcn Launch CODE El-4. SCIENCE and Jovian cnC0untclr there three channels produced no usable encounter data. lhe detector channels could be prograamro to, INVESTIGATION DISCIPLlNE(S) readout in any one 01 four DattClnS at each 01 the clght PIRTICLfS AND ilELDS s~ac~~Iattbit rate .Odes. During encounter rhcn tht MAGNEIOSPHERIC PHISICS rpacacraft was Operating in the highest bit rate mode, the mini.". time to sample one channel was 1.5 s and the t3.e to PERSONNEL obtain 8 COePLCte scan through all channels uas 108 I. Since PI - J.A. VAN ALLEN u Of 10.1 the dir.CtiOnll dettCtDIS Pointed PelDtndiCUL.r to the spin axis and thr spin rate ras 5 ID.. pit~h-anple .easurtnentr were BRIEF DESCRIPTION Obtained. YhiLC the exD*ri.cnt waI prinarlly delignatcd for This e~perimrnt (also carried On Pionccr 11) used seven encounter studies, some data I~IC obtained at lor rates in minieture Geiger 1bt.s in three srrayr to measure proton and inttrplantlary space. A description of the instrumentation and +lcttron flu.ei in interplrnctari space and in the vicinity of initial results ids published in J. GCDD~YS. Res., 1. 79, p. Jupiter. DC~CI~OI groupings wire as tollour: 11) a 3589. 1974. three-element (Ar 01 and C) ditfcrentially shielded tclescoper rith tube C shielded o.nidirertionally an0 vied for bartgrauno ------PICNEtR 11, FILLI"S------subtraction to vrovidt directional rates such as A-C 15-21 MeV electrons and 10-71.5 MeV protons) and E-c 10.55-21 Ilsv INVfST16AlION NAME- JOVIAN lRAPPED RAOIATION elrrtronr and 6.6-17.5 MeV pr0tOnS)r 12) a thlCI-tlCICnt (D, E* and i) trirngular array. each eltiert reSpOndinq to elettrcrs NSSDC IO- 13-019A-05 IRVfSTILlllVE PROGh'AM above 31 ?lev and protons above 11.5 MeV. and 13) thin-uindoi CODE EL-4. SCIENCE tube IC) with a gold-plated rlbou as the aperture ihich aamitted scatterid clcrtro~l abowe 0.06 MeV rhilr INVESlIGAlION OISCIPLINf (5) discriminating strongly against protons. Srnqlr element and PARTICLES AND ilELDS coincidence rates HCIC telc.ctered from the tirrt two MAGNETOSPHERIC PHISICS telescopes. lhe telemetry bit rate prevailing during the PLANE TOLOGl ~~pitetencounter cermitted direrticnal sampling in intervals of about dcq Of roll about the spin asis. For tuither details, ste Baker and Van Allen- J. GeophYS. Res., 1. 81. C. 611, 1916.

12 PERSONNEL BRIEF DESCRIPTION PI - R.Y. FILLILS U OF CALIF, SIN DIEGO lhis expcrimrnt consisted of three 3-clement tetIscOpeII 01 - C.E. MCILYAIN U OF CALIFr SAN DIEGO all looking normal to the spacecraft spin axis. A bidirectional t.Lesiopr .e.sur*d 20- to 80D-RrVlnurleon 0RlLF DESCRIPTION particles with 5 to 102 ebergy resolution. Another t.tCSCOp. This experiment ronrirtcd cf an array of five p~rti~l+ measured 3- to 22-MeWlnuLllOn PaltfCIeS with 51 resolutfon. detectors with rlrctron thresholds in the rangr -01 to 35 MeV Their two telescopes m..sw*d ~8rt$rleswith 1 valurs betreen 1 and proton thresholds in the range 0.15 to 80 MeV. A Cercnkov and 8. The third telescope aeasUr.d 50-Lev to l-IcV electrons Counter (C) had fObr OUtpUt rhlrrrlr ((1, C2r (3. and CDC) and SO-kcv to 2O-Iev pIOtDnS with 2D1 rlrolution. Data include sensitive to rl.rtrons having energies above 5, 8. 12, and 1 the interplanetary +*pion. MeV, rCIpCLti~C1y. An electron sc.ttel COuntCr (E) had thlee OUtPUt channels (tlr EZI and E3) srnsitivt to electrons above .16. -26, and .4C MeV. A minimum ionization CLUIIter (M) ha0 three output channels: 111. rcnritirc to elcctronr having INVESl1GAT1ON NAME- HIOH- AND MODERATELV LOU-ENERGI energies greater than 35 MeV; 12. measuring background: and M3, COSMIC-PAY TELESCOPE sensitive to protcrs having cnrrgitr preater than 80 MeV. The Lest tu0 sen9ors usre scintillator dctrrtorr (SP and St), both NSSDC ID- 77-084A-08 INVESTIGATIVE PRObRAI of rhich had energy thresholds of 10 krV for electrons and 150 CODE rL-4. SCIENCE Lev for protons. The sensitivity of the SE detector to protons 11s about a factcr of 10 Lori, than its sensitivity to lNWESllGAllON DlSClPLINE(S) rlectronr. Thus. the SEDC rhannrl effectively .easwed the COSllIC RAlS clCrtlOn flux. rhirh could then be Subtracted from the SPDC MAGNElOSPHERlC PHISICS channel response to obtain the proton flux. Several other channels listed rbcve rcquir~dcorrections to Obtain the fluxes PERSONNEL Of the species indicated. The detector channels could be PI - R.E. VOGl CALlf INS1 OF TECH P.09,.1.Ld for readout in any one of four patterns at each of CI - J.R. JOKlPll U Of ARllONA the eight spaceoraft bit-rate modes. During encounter Yh.n the CI - E.C. StQME CALIF INS1 OF TECH Sp.rcrraft Yas Operating ir the tighest bit-rate mod.. the LI - F.B. MCDONALD NASA-GSFC minimum time to sample ont channel was 1.5 I and the time to C1 - J.H. TRAINOR NASA-GSfC obtain a complete scan through all channels was 108 I. Since CI - Y.R. YEBBER U OF NEU NAIIPSHIRE the directional detectors p~intedpirpendicularly to the spin CI - A.Y. SCHARDT NASA-6SFC axis and the *pin rate was 5 ~pm. pit~h-anglemeasurCmmts wrc obtained. Although this ~xpeiimentbas primarily designed lor BRIEF DESCRIPTION encounter studiesr some data utle obtained at lor rates in This investigation studied the Origin and acceleration interplanetary spare. A description cf the instrumentaticn ird Eroc~ss. life histor?. and dynamic contribution of interstellar init7al Pioneer 10 lCIUltl "as published in J. Geophys. Res., LOI~~Erays. the nucleorynthrris of elements in cosmir-ray V. 79rp. 3589. 1914. SOUIILSI the behavior of cosmic rays in the interplanetary mediumr and the trapped planetary enerpetic-p.clicle ------PIONEER 10, MCDQNALD------.------rnuiron.cnt. The instrumentation included Htgh-En.rgr Telescope System 1NElS) and I Lou-Enrrgy Teles10p1 System INVESTIGATION NAME- COSMIC-RAY SPECTRA (LETS). The HElS covered an energy rang. between b and SO0 L.wlnurlcon for nuclei ranging in atomic numbers from 1 through NSSDC ID- 72-0121-12 INVESTIGATIVE PROGRAM 30. In addition, electrons in tbe energy range betieen 3 and CODE EL-4ICO-OP. SCIENCE 100 MeVlnucleon were measured by this t.LlllOp~ and an electron telescope (TET). lhc LETS measured thr energy and drterminrd INVESTIGATION DISCIPLINE(S) the identity of nuclei for energies betueen SO. The PARTICLES AND FIELDS instruments also measwed the anisotropies of elCctiOni and COSMIC RAVS nuclei. In addition. elections in the energy vangc betreen 3 and 100 MeVlnUcleOn were measuied by an electron tCl.scOpe. PERSONNEL P1 - FA. MCDONALD NASA-GSFC 01 - K.G. MCCRACKEN CSIRO 01 - Y.R. YEBBER U OF HEY HAMPSHIRE INVESllGATION NAME- HIGH- AND MODERATELY LOU-ENEIGV 01 - E.C. ROELOf APPLIED PHYSICS LAB COSMIC-RAY TELESCOPE 01 - J.H. TRAINOR NASA-GSF C 01 - 0.J. TEEGARDEN NASA-GSFC NSSOC ID- 17-0161-08 INVESTIGATIVE PROGRAll CODE EL-), SCIENCE BRIEF DESCRIPTION This rxeerincnt consisted of three nulti-elclentr lNVESTlGATlON DISCIPLINE(S) solid-state teleiccpes, all lookins normal to the spa~ccraft COSMIC RAYS Spin axis. It 1.5 also carried on Pioneer 11. lhr htgh-energy llAGNElOSPHERlC PHYSICS telCicOpt (MET) rcrrirtcd cf fire rollincar senso~i, ~F(I measured sto~pingparticles (I= 1 to 8) in the energy range 20 PERSONNEL to 50 Mcvlnurlcon and p~n~tratingparticlc~ in the range 50 to PI - R.E. VOGT CALIF INS1 OF TECH 8rO Mcvlnuclcon. Charge resolution for penetrating particles CI - J.R. JOKIPII U OF ARIZONA "as p~~iiblcup to 200 MrVlnurleon. The first lou-enerqy C1 - E.C. STONE CALIF INS1 OF TECH tcleSCopc (LET-I) had four elements and measured Stopping (2 = Cl - F.B. MCOONALO NASA-GSfC 1 to U) particles in the energy range 3 to 32 Mcvlnuclcon. The Cl - J.H. TRAINOR NASA -G SF C second lo~-tne~gytelescope (LET-11) haa three rltmcntr ard CI - Y.R. YEBBER U OF NEY HAMPSHIRE measured Stopping CLCCtrOnS beteean 50 and 1000 keV and C1 - A.Y. SCHARDT NASA-GSFC StOpping protons betuccn 50 LcV and 20 MeV. For each t~ltrrop~.Fount rates were obtained far each of slrrnl sensor BRlEf DESCRIPTION raincidrnrL-.ntircircid~"~= modes. Scmr of the rates from each This investigation studied the 0rip.i" and acceleration ttlescope icrc sectorid into eight o~tsntirn thc SP.CCC*.~~ PIOC~SI, life history. and dynamic ~ontributfonof interstellar Spin plane. In addifion. thlee-sensol ~~LIC-heighf.n.lyris. cosmi~ raysr the n~cl~oiynfheiis01 tlcm.nts in eosmi~-ray with priority stheles favoring the analysis of heavier aOUrLesr the behlvior of Coslic 1.11 in the intrrplanrtari Dalticlesr 11s associated with each telescope. mediumr and the t1apped planetary energetic particle environment. The inrtrumcntition included a High-Energy McDQNALD------PlQNfER 11, Telefcope System (HETI) and I Low-Energy TILCSCOP. System (LEIS). The HElS covered an energy range between b and 50C INVESTIGATION NAME- COSMIC-RAY SPECTRA Mevlnuclcon for nuclei ranging in atomic numbrrr from I through 30. In addition, el~rti~niin the energy range betwen 3 rnd NSSDC ID- 73-0191-12 INVESTIGLT IVE PROGRAM 100 llcV IeIc measured by this teteLCOpC and an electron CODE EL-41CO-OP. SCIENCE teleicOpC (TET). The LETS measured the energy and determined the identity of nuclei for energies betrrcn .lS and IO INVESTIGATION OlSCIPLINE (5 ) Mcvlnurlcon and atomic numbers from 1 to 30. The instruments PARllCLES AND FIELDS also measured the anisotropic5 of electrons and nuclei. In COSMIC RAYS addition, electrons in the energy range betuten 3 and 100 Mew ~ercmrasurrd by an election tCLCSCDpC. PLRSONNEL PI - F.M. ~COCN#LC NASA-GSFC 01 - K.G. MCCRACKEN CSIRO 01 - U.R. YEBBLR U OF NEY HAMPSHIRE ULTRAVIOLET 01 - E.C. ROELOf APPLIED PHISICS LAB 01 - O.J. TEECARDEN NASA-GSFC 01 - J.H. TRAINOR NASA-GSFC

73 NSSDC ID- 12-012A-06 INVESTIGATIVE PROORAM CODE EL-4, SCIENCE INVESTIGATION NAME- ULTRAVIOLET SPECTROSCOPY INVESllGATlON DISClPLINElSl ASTROLCMY NSSDC ID- 11-0761-04 INVESTIOATIVE PROGRAM PLANETAR1 ATMOSPHERES CODE EL-4ICO-OP. SClENCE

PERSONNEL INVESTIGATION DISCIPLINEIS) PI - D.L. JUDGE U Or SOUTHERN CALIF PLANETARY ATMOSPHERES 01 - R.Y. CARLSCN NLSA-JPL PERSONNEL BllEi DESCRIPTION PI - A.L. 8ROADiOOT U OF SOUTHERN CALli This experiment (on both Pioneers 10 and 11) consisted at CI - A. DALGARNO SA0 a brsadband photometer sensitir. betbeen 200 and 800 A. During CI - J.C. RCCOLNELL YORK U the cruise phase of the mission, this aiperimcnt "as used to CI - R.M. GOODY HARVARD U search tor the *~p.ll~ni~-t~-s~bs~nictransition region in the CI - 7.n. DONAHUE U OF MICHIGAN solar rind. During the Jovian encounter^ this experiment MIS CI - 11.8. MCELROY HARVARD U used to look tor evidence 01 ir auroral oval on the Jovian CI - R.J.S.BELTON Klll PEAK NATL OBI dayside. to tind the ratio Of hydrogen to helium in the Jovian C1 - D.T. STROBEL US NAVAL RESEARCH LAB atmosphere. and to tind the temP*ratUre of the outer portion of CI - H.I. noos JOHNS HOPKINS U the Jovian atmosph.r*. Ewid*nce 01 helium "as found in the CI - J.E. BLAllONl CNRS-SA interpla ne ta ry reg ion indi L. t ing ir terac t ions betre en c hargea CI - J.L. BERTA~I CNRS-SA pa,ticles and neutral hydrogen. CI - S.K. ATREYA U OF MICHIGAN CI - 8.1. SANDEL U OF SOUTHERN CALIi ------PIONEER 11. JUDGE------C1 - D.E. SHEMANSKY U Of SOUTHERN CALli

INVESTIOATION NAIL- ULTRAVIOLET PHOTOMETRY BRlEi DESCRIPTION The UV spCctro.eter was designed to measure atmoipheric NSSDC ID- 73-019A-86 INVESTIGATIVE PRObRAM Pr0Certi.s and measured radiation in the uavelength range 0.04 CODE EL-), SCIENCE tO 0.16 .icrO.cter (400 to 1600 A). TI0 .Odes Of instrument operation UCIC planned: iirglow and occultation. In the INVEST16ATION DISCIPLINE(S> airqLow mode. the atmospheric raaiation "as .CasUrCd. This AsTRoLonl radiation is predominantly rrsonancc-scmttered solar radiation. PLANETARY ATMOSPHERES where the scattering is by the molecular or atomic atmospheric PLANETOLOGY constituents. such as hydrogen (1216 A) or htlium (584 A). In PARTICLES AND FlfLDS the orcultation mder runligbt was rttlected into the IPIEttO.eteI. and tbc Solar SPCCtIU. UaS TcCOldcd. AI the PERSONNEL .tmOlphel. moved betieen the Imacecratt and the run. the PI - D.L. JUDGE U OF SOUTHERN CALIi abSOlptiOn ch.ractCristirs 01 the .t.Olphcrc were obtained over 01 - R.Y. CARLSON NASA-JPL the measured ravclcnqth region. The abSorGtion SP.C~~Y. was used to idertify the absorber as rrll as to ~C~IUIC its BRIEF DESCRIPTION abundance in the line 01 sight to the run. In addition, the This rxperiment consisted ot a broadband photometer. *tmOsDhel*~l thermal ItrUCtUI* could be interred. sensitive between 200 and 800 A. During the cruise phase at the mission. this ewerimrnt I.. used to search tcr the rupc.~onic-to-.ub,ori~ transition region in the solar rind. During the Jovian encounter. this rxpcrimrnt was used to look INFRARED for evidence of an *croral 0r.L on tbe Jovian daysid.. tc fino the ratio of hydrogen to helium in the Jovian 11.oiphtrer and 10 tind the Iemperat~lt of the outer portion et the Jovian af.olph~re. Eiidence 01 helium I.. lound in the intrlplan=t.ly ,.pion. indicating int*rartions Lltbern tharged PaltltlII arm n.utr.1 hydrogen.

__-__--VOyAGLR 1, BROADTOOT------NSSDC ID- 77-0841-03 INVESIIGATIWE PROGRAM CODE EL-4, SCIENCE INVESTIGATlON NAME- ULTRAVIOLET SPECTROSCOPY lNVESTlGAllON DISCIPLINE(S) NSSDC ID- 17-084A-04 lNVESTlGATlVE PROGRAM PLANETARY ATMOSPHERES CODE EL-4. SCIENCE FERSONYFI lNVESTIGATlON DISFIPLINE(S) PI - 11.1. HANEL NASA-bSiC PLANETARY ATIOSPHERES CI - V.6. KUNDE NASA-GSFC CI - D.P. CRUIKSHANK U OF HAdAlI PERSONNEL CI - Y.C. RAGUIRE NASA-GSiC PI - A.L. BROADFOOT U OF SOUTHERN CALli CI - J.C. PEARL NASA-tSiC CI - H.Y. MOOS JOHNS HOPKINS U CI - J.A. PlRRAGLlA NASA-GSiC CI - M.J.S.BELTON KIT1 PEAK NATL OBS CI - R-E. SAMUELSON NASA-GSiC Cl - D.F. STROBEL US NAVAL RESEARCH LAB CI - P.J. OIERLSCH CORNELL U CI - 1.M. DONAHUE U Or MICHIGAN CI - C.A. PONNAMPERUMA U 06 MARYLAND CI - 11.8. WCELROY HAUVARD U CI - 0. GAUTIER PARIS 06SEPVATORY CI - J.C. MCCOhhtLL YORK U c1 - ~.n. ~LASAU NkSA-GSiC C1 - R.M. GOODY HARVARD U CI - I. KUMAR U OF SOUTHERN CALli CI - A. DALGARNO SA0 CI - B.J. CONRATH NA S A -65 i C C1 - J.E. BLAMONT CNRS-SA Cl - J.L. BERTAUK CNRS-SA BRIEt DESCRIPTION CI - S.K. AlREYA U OF MICHIGAN This investigation "as carried out wins an inlrarcd C1 - B.R. SANDEL U OF SOUTHERN CALIF radiometer ana an intcrtc.olttrr-rpcrt,~.~t~, rimiiar in design CI - D.E. SHELAhSKY U Or SOUTHERN CALli to the mariner 9 IRIS, combined into a single instrument. The investigation studied both global and local energy balancer BRIEF DESCRIPTION urinq intrircd spectral meaIurC.ents in conjunction rich The UV sPCCtI0mCtCr "as designed to measure at.0spheric broad-band .C.Sult.CntS Ol retltrttd Solar en*lgy- Atmospheric PrOPerties. and tC measure radiaticn in the rarelength range composition was also investigated. including determination of 1.0. 0.04 to 0.16 micrometers trco to 1600 A). TWO modes ot the H2lHe ratio. and the abund*nrc at CH2 and "3. Vertical instrument opelatio~bere planned, airglow and occultation. In temperature profiles itre obtained on the planets and the airplow .Ode the atmospheric radiation was me.s~red- This satellites rith .tmOapheres. Studies of the ~o.po~iti~n. radiation is preocwirantly resonance-scatterid solar Iadiaticn. thermal properties. and sile Of particles in Saturn's rings where the ICattCiinq is by molecuLar or atomic atmospheric were conducted. The intcrtrramcter had a spectral range ot 200 constituents Such as hydrogen (1216 A) Or helium (514 A). In to 4000 1Ica. rhile the radiometer rang. covered 5000 to 33,000 the OccUlt.tiCn .cde. sunlight "as retlrrtrd into the Ilc.. The instrument used single primary mirror 51 CI in sPictrOm.ter. and the solar SPIC~~Y. 1.5 r.cOided. AI the diameter rith tield of vier 01 0.25 deg. atmOspher* moved between the spictcritt and the sun. the .bsolption characteristics Of the .t.OlphelC IC,* obtained Over the .C.IuICd wartlrnpth Pegion. TIC ablOlptiOl Ip~ctrumwas used to identity the absorber 81 ucll as to .=.sure its INVESllGAllON NAME- INiRARED SPfClROSCOPY AND RADIOMETRV abundance in the line of light to the run. In addition. the atmosoherlc thermal ItlUetUIe could be interred. NSSDC ID- 11-0161-03 INVESTIGATIVE PROGRAM CODE EL-4. SCIENCE

INVESIIGATION DISCIPLINE(S) PLANETARY ATMOSPHERES

14 PERSONUEL PI - R.A. HAUEL NASA-6SF C BRIEF DESCRIPTION Cl - C.A. PONUAIPERUMA U OF MARlLAMD Thr Radio Scirnrr Team usrd the trleconaunications syatem Cl - P.J. GIERASCH CORNELL U of the Vopgrr apac*c,.ft to ~e~formits atudiea. The syatem Cl - 4.A. PIRRAGLIA NASA-SSFC Mas a roharrnt S- and I-band downlink and S-bana uplink- The CI - R.E. SAIUELSOU NASA-6SFC scirnre objrctinea of the radio scient- Inueatipmtion were (1) CI - Y.C. IAGUIRE NLSA-GSFC to determina thr Chyslral propartiea of plan*tary and satelilte CI - J.C. PEARL NASA-GSFC ionosphrres and ataaspheras by oxmining the propagation CI - W.6. KUNDE NASA-GSFC rffccts on dWl-fregU.nc7 radio *+gnat during immersion and CI - D.P. CRUIKSHANK U OF HAYAII emrraion of spacecraft Occultation by the aubjact body. 12) to CI - B.J. CONRATH N ASA-GSFC deternine planetary and a.tellitr mas#w, gravity iieldsr and CI - D. GAUTIER PARIS OBSEBYA~ORl densities by preciar trarkfng of a dual-freqwncy radio aignal CI - F.M. FLASAR NASA-GSFC from the spacrrraft during the rncounter period. and (3) to CI - 5. KUIAR U OF SOUTHERU CALIF determine the amount and sizr distrlbutlon of material In Saturn's ring. and thr ring dlmrnaions by *..mining the BRIEF DESCRIPTION Propagation rffecta on a dual-frrqurncy radio aignal that This invrrtication vas carriad Out uaing an intrarrd passea through each ring in aurrrisionr and through the 9ap radiometer and an int.rferomct+r sprct.om.ter aimi1.r in design betmeen the C ring and Saturn's surface. to thr Mariner 9 IRIS, rombinrd into single instrument. The invrstiOatian studied both global and Local energy balanr., ------V01AGER 2, llLER------using infrared spectral mrasurIvrrts in conjunction with bro4d-band .easUrCmenti of refltcttd sola. *n.lgy. Atmosph.rir IUVESTIGAllON NAME- RADIO SCIENCE TEAM coDpOiitim "as also invrstigatedr including d.trr.ination of the HZIHC ratla and the abundance of CH2 and NHS. vrrtical USSDC ID- 71-816A-02 1~YEST16AlIVEPR06RAI teSPIIatUIe pTOfi1lS were ObtDired On the pI.n.1. and CODE EL-0. SCIEYCE satellites with atnosphcrrs. Studies of the composition. thermal proocrti.sr and size of F..ti

BRIEF DESCRlFTlOl The Radio Scirnce Team Yard the trlecommuni~ationa SYStrlS Of the Voyager Spac.Craft 10 P*rform their a1udi.s. The syflrm I.% coherent S- and x-band douniink and I-band uplink. lhe acitncr oblrrtiwes of the radio science INVESTIGATION DlSClPLINE(S) investigation wtr. (1) to determine th. Dhyait.1 propertics of ASTROUOIV planrtary and sat.llit. ionorphrrea and atmospheres by PLAUElCLOGV examining th. Dropagation .ff.ctl on a dUal-fr*qurncy radio CELESTIAL MECHANICS Sinnwl during immrraion of SDscecraft Occultation by the subject body. (2) to detrrmine planefary and aatellitc mesaear PERSONNEL gravity ficlda and densitis, by pr*ciae tracking of PI - J .D. ANPERSOH NASI-JPL dual-frequency Iadio aignal from the spacacr.ft during the 01 - G.Y. NULL NASA-JPL encounttr period. and (3) to determine thr amount and sir. diatributions of ..tCIiBl in thr rings of Saturn and thr ring dinenaions by ...mining the propagation effects on a dual-fr.quanry raoio signal that pas.es through each ring in succession and through the gap b.1r.m the C ring and the .",faLC of S.t".". ----_-_PIONEER 10, ~LlORE------..------

INVES116AllON NAME- S-BAND OCCULlAllON

NSSDC ID- 72-0121-10 INVESTIOATIVE PRO61111 CODE EL-+. SCIENCE

INVESTI6AllON DISCIPLlNE(S) IONOSPHERES LND RAOIO Pnysics INVE SI IGAlIOU DISC LPLlHE 1s) PLANEIARV ATMOSPHERES PLANETOLOGV ASTRONOMV PEasonntL CELESlIAL CECHANICS PI - A.J. KLIORE NASA-JPL 01 - G. FJELDBO(NLA) YASA-IPL PERSONNEL PI - J.D. ANDERSON NASA-JPL 01 - G.Y. NULL NASA-JPL

NSSDC ID- 17-0891-02 INVESlIGATIVE PROGRAI CODE EL-4. SCIENCE

INVESTlGATlON OISCIPLINE(S) AlMOSFHERlC PHVSICS CELESllAL UECHAHICS IONOSFCERES AND RADIO PHYSICS NSSDC ID- 73-019A-IO INVESTIGAlIWE PROCRAI CODE €L-+. SCIENCE PERSONNEL IL - G.L. TYLER SlANFORD U lNVESTlGAIlON DISCIPLINE

ORIGINAL' PAGE IS OF POOR QUALITY PEISONNFL PI - A-J. RLlORE NASA-JPL 01 - 6. FJELDBO(NLA) NASA-JPL 01 - D.L. CAIN NASA-JPL 01 - B.L. SElDfL NASA-JPL 01 - 1.1. RASOOL 1811-PAR IS

IMVESlIGAT10N NAME- MULlIFILlLR ?HOTOPOLARIRfILlt~ INWES71GATlON NARE- PLANETAPY RADIO ASTRONORI 2200-1300 A

ISSDC ID- Tl-084A-10 INWESlI6AlIWf PRObRAR NSSDC ID- 17-0161-11 INVEITICATIWE PRO6RAI CODE EL-4ICO-OP. SClEYCP CODE EL-+ICO-OP* SCIENCE

INWESTIGATION DISCIPLINE(S) INWES~IGATIONDISCIPL~NE IS) MAGNETOSPHERIC PMVSICS INlfRPLANElARl DUST SPACE FLASIAS PLANflARY ATROSPHERLS

PERSONNEL RADIOPHISICS. INC PI - A.L. LANE NASA-JPI NASA-GI FC CI - C.D. PAN6 NASA-JPL U OF FLORIDA CI - J.E. HANSEN NASA-61 SI Cl - F.1. HADDOCK u OF nicniun CI - D.L. COFFfFN NASA-6155 Ct - D.H. SIAELIN MASS INS1 OF TECN Cl - L.U. ESPOSITO U OF COLORADO Ct - A. BOISCHOI PARIS 00SLPYAlORl CI - M. SATO(NLA) NISI-611s Cl - C.C. HARVEI PARIS oesEevaroav ci - 1.1. YEST U OF COLOYADC CI - I. LmLauc PARIS 08SER1110RI CI - C.U. WORD U OF COLORADO CI - U.E. BIIOUN. JR. NASA-JPL C1 - S. GULKIS NASA-JPL BRIEF DESCRIFTION Cl - I. PHILLIPS NASA-JPL This @.peri.rnt coniisttd of an 8-in. (20-rm) 111.1 Cl - J.B. PLAICE RADIOPHISICSI INC telescope that sent radiation through a polarizer and a filter Cl - A.C. RIDDLE U OF COLCRADO for one of eight bands in IhC 2200- to 7300-1 spictr.1 rcgion, Cl - I.G. PLLT1LR naniiu-nm1fiia AEROSP then on to a phOt0.ultipler tube. By study of these emission CI - R.L. KAISER NASA-GSFC Sntcnrity data, information on surface texture and composition at JUpiteVr Saturn. Uranus. and Neptune could be obtained, BRIEF DLSCRIPlION along with information of silt distribution and composition of This erp.ri.ent consisted cf sueep-freguency raaio Saturn's and Uranus' rings and information on at.OspheriC .eceiw*r oprratinp in both ~01.~12.tion states. betreen 20 kHz scattering ~i~p~ifie~and density tor all ~lantt~.Molccul~r and 40.5 RHI. The Signal I.*recelled by pair 01 OlthOgOnal scale hti0hfs for these planets could also be determines f,Oi lo-. monopole anteiiai. Study 01 the radio-.mission signals these data. from Jupiter and Saturn over this range of trrquencles yielded data concerning the physics of .agn.tcsphrric p1aS.a resonances and nontherm.1 radio emissions Tro. these plmctary rcpionr. FOLARllATlOl ------"O*&GER 2, yApyI(K------'------.------

INWLSlI6AlION NAME- PLANETARY RADIO ASlRONORY

NSSDC ID- 11-016A-IO INYESl1611IW€ PROGBAR CODE EL-4. SCIENCE

INVESTISATION DISCIPLlN€(S) MA6NETOSPHERIC PHYSICS SPICE PLASRAS

PERSONNEL PI - J.U. YARUlCK RADIOPHISICS. INC C1 - U.E. BRObNr JR. NASA-JPL CI - I. GULKIS NASA-JPL Cl - L.C. HARWLI PARIS OBSERUAlORI CI - 1. LEBLANC PARIS OBSLRWAlORI CI - D.W. SlAtLIN MASS INS1 OF TECH Cl - A. BOIICHOT PARIS OBSLRWATORI C1 - 1.D. CARR U OF FLORIDA CI - F.T. HADDOCK U OF RICHIGAN CI - J.K. ALEXADOER. JR. NASA-GSFC C1 - I. PHILLIPS NASA-JPL C1 - R.G. PELTZER MARTIN-MARIETTA AEROSP INWESTlGATlON NAME- I)ULTlFlLTER PH070POLAR1RETER~ Cl - J.B. PEARCE RADIOPHVSICS. INC 2200-1300 A C1 - A.C. RIDDLE U OF COLORADO CI - R.L. KAISER NASA-GSFC NSSDC ID- 77-am-ii

BRIEF DLSCRIPlION SEE THIS EIPERIIENT UNDER ATIOSPHERE This experiment consisted ct a s~~ep-li~quinc~racio rrttirtr optrating in bath polarization states. betreen 20 kH1 and 40.5 IHr. Ihc signal was received by a pair of Orthogonal lo-. monopolt antennal. The Physics Of .agnttOSDhCliC PlllmI resonances and ncrthrrmal radio erirricnr fro. these planetary regions 1.5 studied by investigation 01 the radio .mission signals from ~~pitiiand Saturn over this range of frrqurnrierr and rill do likcrise at Uranus and Neptune-

ATROSPHERE

16 Saturn SATURN

Plate 5. This is a collection of press release photographs from Voyagers 1 and 2 missions. (A) P23400 is a Voyager 1 montage of Saturn and some of its 23 known moons. (B) P23068 is a Voyager 2 photo showing that the rings are composed of myriads of ringlets (over a thousand in number, of which about 100 can be detected in this photo,) making it look like a playing record. (C)P23925 is a Voyager 2 photo of part of Saturn's rings showing many ringlets and the radial bands on the B-ring, discovered on Voyager 1. (D) P23099 is a Voyager 1 photo of the F-ring appearing to consist of twisted or braided rings discovered on this mission. Voyager 2 photos showed a single ring composed of at least 9 ringlets, (but not braided or twisted). (E) P23113 is a Voyager 1 photo of Dione (1120 km diameter) showing a highly cratered surface. (F) P23094 is a Voyager 2 photo of Dione showing an entirely different surface for its other hemisphere from that in (E). Here it is less cratered and splashed with light ray-like material with little relief. (GI P23956 is a Voyager 2 photo of Enceladus (500 km diameter) showing an area of smooth, craterless terrain with ridges bordering it, indicating surface movement in the past to present. (H) P23200 is a Voyager 2 photo of Mimas (390 km diameter) with an enormous deep crater with a high central peak, making its resemblance to the Death Star in Star Vdrs remarkable. (I) P23915 is a Voyager 2 photo of part of the atmospheric surface of Saturn showing bands, belts and vortices. These features are somewhat similar to Jupiter's though smaller in size and appearing more subdued because of a high-altitude haze on Saturn not present on Jupiter.

INTRODUCTION

The planet farthest from the sun that has been visited and measured by planetary missions is Saturn. It has been visited by three U.S. spacecraft: Pioneer 11 and Voyagers 1 and 2. Voyager 2 is now on its way to Uranus and is expected to arrive at Uranus in January 1986. Although all investigations on these missions that flew by Jupiter obtained data also on Saturn, these data are still being reduced and analyzed and these data are anticipated for deposit in NSSDC. There are nine investigations for which NSSDC has data archived and these data cover the five categories: (1) Imaging, (2) Particles and Fields, (3) Radio Science and Celestial Mechanics, (4) Atmosphere, and (5) Polarization. Again, as in the case of Jupiter, data €or the Atmosphere and Polarization categories come from the photopolarimeter investigation and are described under Imaging. Tables 1 and 2 and Appendix A give more detail on these investigations. SPACECRAFT ...... INITIAL ORBlT PARAIETERS ORBIT 1lPL- SAlURN FLYBY

SPACECRAFI COMMON NAME- PIONEER 11 PERSONNEL ALTERNATE NAMES- PIONEER-GI PL-133C cn - J.R. CASANIINLI) NASA-JPL 6421 PS - E.C. STONE CALIF INS1 OF IECH NSSDC ID- 13-0191 nnirr oEscaipiiou The orera11 objrrtlres of VOUger urre to conduct LAUNCH OAlE- 04106113 YEIGHI- 231. KC exPloratory investigations of the plan.tary systems of Jupltrr LAUNCH SITE- CAPE CANAVERAL. UNITED SIATES and Saturn and of the int+rolanetary mrdlua Out to Saturn. LAUNCH VEHICLE- AlLIS Primary emshasis was placed on COIParatlwe studies of these two Plmrtary iystrms by obtaining (1) measur.mmts of the SPONSORING COUNlRTlAGENCI rnwironm.nt. atm~sphrr~~and body sha,acterIstlcs of thr UNITED SlATES NASA-OSSA Pl*n*tr and thr satellites of rach planet. (2) studlea of the nature of thr rings of Saturn. and (3) esptoration of the INllIAL ORB11 PARAMEIERS Intcrplmet.ry (or interstellar) mbdium at increasing distanc.r ORBIT TYPE- SATUI1N FLYBY f10m the sur. Thsse objectiuas were attalned by using a warlety of inltruments and mmthods including Imaging. a PERSONNEL coherent 5- and X-band RF receiver, an infrared int.rftrOmetrr PM - C.F. HALL(NLA) NASA- A R C and radiometer, uw spectrometer. t1ung.t. magnrtomrtrrs. PS - P. DIAL NASA-ARC Far.d.y cups. a chalged-p.rticle an.lyzer. plasm. detector. PLaa.a-u.re radio retrirrrr cOlll~-raY telescop~s~ BRIEF DESCRIPTION photopoI.rimeter, and a swrp-fr8qu.n~~ radio rece1v.r. This "as thi ICCOnd Rirsior. tc investisate Jupiter and UoYagcr 1 had its closcst .nrount.r rlth Jupiter on March SI the Outer solar system. Pioneer 11. like Pioneer IO. vied 1979. and rlth Saturn on November 12. 1980. Jupiter's gravit.tiona1 field tc alter its trajectory r.dicaLLy. It passed close to Saturn and then it follored an ...... CSC.PI trajectory Irom the solar system . lhe spacecraft us1 2.9 I (9.5 11) long and containrd 1 2.14-rn (9-ft) diameter high-gain antenna of aluminum honeycoeb srndrirh aaterial whole SPICECRAFT COMMON NAME- YOlLGER 2 fssd 1.1 topped rith a mc6ium-pain antenna. A lor-gain. ALTERNATE NAMES- MARINER JUPlTERISAlURN 8. OUTER PLANElS B omnidircction.1 antenna 1.1 mounted below the high-gain dish. MARINER 176. IJS 178 It contained ti0 nuclear electric-poier gmeratorl. which 10211 grneratrd 144 Y at Jupiter, but decieased to 100 Y at Saturn. There yere three ref.rcnre s.nsOrs: a st., (Caropul) sensor. NSSDC ID- 11-OlbA and two sun s~nsori. Attitude position could be calculated from the reference direction to the earth and the sun. rith the LAUNCH DATE- 08120171 YEIGHT- 100. 16 knorn direction to Canopus a1 backup. Pioneer 11's star senlor LAUNCH SIlE- CAPE CANAVERAL, UNIIED STAlfS gain and threshold settings "ere scdifird. based on .xperi.nre LAUNCH YEHICLE- TlIAN gained from the s.ttings used on Pioneer 10. Three pairs Of rocket thrusters prowidcd spin-axis control (at 4-8 rpm) and SPONSORING COUNlRlIIGENCI change of the spacec~aft vrloclty. lhe thruster1 could be UNITED STATES NASA-OSSA either filed steadily or pulsrd, by command. Co.munirationr uerc maintained via the omidircction.1 and medium-gain INlIlAL ORBIT PARLIIETERS antennas. which operated together. connected to on. receiver, ORBIT TYPE- SATUFIN FLYBY rhilr the high-gair antenna was rennectcd to the other receiver. The recCiv.rs could be interchanged by command. 110 PERSONNEL radio transnittersr coupled to tu0 traveling wave tube PM - J.R. CASANI(NLA) NASA-dPL mplilicrsr produced 8 Y power each in S-band. Communication PS - E.C. STONE CALZF INS1 OF TECH uplink (earth tC spacecraft) operated at 2111 MHzr and downlink lspacecralt to earth) at 2292 IHz. At JYD~~CI'S distance. BRIEF DESCRIPTION round-trip rommunirrtion tilt took 92 .in. Data "ere received The Orrrall objective1 of Woyaa.r 2 Mere to conduct at the Deep Space Network (OS*). The sp.cecraft was CxPIOratory inv*stig.tions of the planetary eysttms of Jupiter. t~mprI.t~re-rOnt10ll~dto between -23 and +$(I deg c (-10 to Saturn. Uranus. and Neptune. and of the interplanetary medium. *loo deg F). An additional experiment- low-smsitiwity Primaiy emphasis "as placrd on comparatlue studirs of thrs. fluxgate magnetometerr was added to the Pioneer 11 payload. Planetavy systems by obtaining (1) m.asurements of the Instruments sfudiec the Interplanrt*ry and pl.net.r)r mapnetir env+ronmcnt. .t.Osph.re. and body characteristics Of the fields; sola, rind pioperties; cosmic rays; trmaition region planets and one or more of the satrllites of each Planet. (2) of the h.1ioaph.i.; neutral hydrogen abundance; distribution. studies of the natur. of the rings of Saturn and Uranul. and size. mass. flux, and VCIocity of dust p.rtiiles; Jovian (3) ervlor.tion of the int.rpl.n.hry (or interstellar) ..diu. abrora~; Jovian radio uaves; the atmosphere1 of planets and at inCrtaSlng diltanc.1 fro. th. sun. These objectives Were satellites; and the rurfacrr of Jupiter, Saturn, and IO.. of oet using a variety of instruments and methods ineluding their satellites. Instrumrntr carried tor these experiments iwaging. a coherent s- md X-band Rf rrcsivrr. an In "Itt mnlQ"cto.rt.r. p1.s.. analyz.r (for SOL., rind). int~rferOmeter and radiometer. a UV lpectr~meter. fluxgate rharg.d-p.rtic1. drtector. ionizing dCttCtOl# non-im.plng mwnetoiet.rsr Faraday cups. charged-particlr ana1yz.r. telescopes rith orerlmpping fields 01 vier to detect runllght plasma detector, pla~.a-~~eradio rcc*irrrr cosmic-cay reflected from passing mrteoroids. lealed pressurized rrlll of tCl.sCOP.1~ photOpolaPimeterr and a 1I.ep-fvequency radio argon and nitrooer 5.1 for measurinp cenrtration cf mrtroroiar. receiver. Jupiter rlorc rnrounter "as arhlcved on July 9. UV photo**ter. IR r.diOmeterr and an imaging photopoI.ri.eter. 19191 and Satwn on August 5. 1981. which produced photographs and measured the polarization. Further scientific information was Obtained from cel.stlal mechanics and o~c~ltati~nphenomena. This apacecraftr like ~WvEmnOws Pioneer 10. contains plague that has a drawing depicting manr IMAGXMG romanr and the lor.tion 01 the sun and earth in the galnay. Pioneer 11 was 36r8OO km fro. Jupiter during its closeit approach. December 4. 1914, to within 431000 km of its cloud topi. It passed by Saturn On Lug. 5, 1979 at a distance of ...... 21.+00 km lrom Satvrn's rloud tops.

SPACECRAFT COMMON NAME- VOlA(rER I LLTERNATE NARES- MARINER JUPITERlSATURN A. OUTER PLANETS A MARINER 171. MJS 111 10321

NSSDC ID- 11-084A

LAUNCH DATE- 09105117 YEIGHT- 100. 16 PI - T. GfHRELS U OF ARlZONA IAUNCH SITE- CAPE CANAVERAL. UNIlED STATES 01 - 0.1. COFFEEN NASA-GI IS LAUNCH VEHICLE- TITAN 01 - J. HAMEEN-ANTTILA U OF ARIZONA 01 - C.E. KENKNIGHT U Of ARIZONA .PONSORING COUNTRYIAGENCY 01 - R.F. HUMMEIl SANlA 0AlkARA RES CTR UNITE0 STATES NASA-OSSA 01 - 11.6. TOMASXO U OF ARIZONA 01 - Y. SYINDELL U OF ARIZONA

83 NSSDC ID- 17-076A-01 INVESTIGATIVE VROGRAM CODE EL-4. SCIENCf

INWESIIGATION DISClPLINE(S1 METE OROLOG Y PLANETART ATMOSPHERES PLANETOLO6V

PERSONNEL 1L - 8.1. SUITM U OF ARIZONA DT - LA. SODERBLOM US GEOLOGICAL SURVET TI - 6.A. BRlt6S NASA hEADPUARTERS TI - A.F. COOK SA0 TI - 6.t. DAllELSON CALIF INST OF IECH Ill - M.E. DAVIES RAND COUP TM - 6.E. HUNT U COLLEGE LONDON TI - 1. OUEN STATE U OF NEU YORK TM - I:. SAGAN CORNELL U II - Y.L. SUOIl u OF usconsin TI - I.V. JOHNSON NASA-JPL TI - H. IASURSKl US GEOLOGICAL SURVEY

6RlEF OESCRIPTION The photographic rXPII1mCnt Used 1 tWO-C..CI. SYSt*mr based on the nariner 10 system. This system included One narror-.nglcr long-toc.1-length camera and one ride-angle. short-focal-length ca.er.. The ..zimum r~solutionachievable o*cendrd gl..tly On the actual trajectory On this multi-encounter mission. but uas as high as 0.5 10 1.0 km on the c10s~stIPPIO.C~II to s0.r objects. AI Jupiter and Saturn, the resolution that 11% achieved 11s better than 21 k> and 5 km, respecti.rly. The objcrti+es of the ..peri.-nt lele to ~hotagraph global motions and cloud distributions on Jupiter. IkVEST16ATlON NAMf- IMA61NG saturn. ufanus. and Nrptunc. g~ossdynaeical properties. zonal rotation, orirntation ot sp5n axis, zonal shear. r*rtical nssoc ID- TT-O~~A-O~ INVESTIGATIVE PROGRAI shtar. tlor instabilitiri. SpOtSr and sprctrum ot scale of CODE EL-4/CO-OPr SCIfNCE .t.Osph=ric motions in time and space. Additional 0b)CCtiYes included the study Ot the mode Of IeIrasC 01 internal energy INVESTIGATION DISCIPLINE(S) flux (srarth for ronrertion cells and rollsl. study of growth. MEIEOROL06Y dissipationr .OrphOlOgy. and vrrtic.1 St*uCtUII Ot cloud PLANElARY ATIOSPHERES romplcrcs, gross optical DrOpSrtirSl global and localiicd PLANETCLOG1 scattering tLnctiOn in the visible spectrum^ polarimetry. ATMOSPHERIC PHYSICS nature of chromopho~es(their struct~e~and dCV~LOp.tnt1. and high ~esolution ot the Great Red Spot. The objertircr of the PERSONNEL ~atellite encounters included I11 9101s ch*racteristics (size. TL - B.A. SMITH U OF ARIZONA shape, rotation. Spin anis, cartO9laphy. improved *ohe..lidel OT - LA. SODERBLOM US SEOLOGICAL SURWEI and .asses;> 121 geo1ogy Ima~orph,siogr.phic provinces, impact IM - 6.A. 811665 NASA HEADPUARTERS and uolranir fratures. lineaments. polar caps. erosion 1M - A.F. COOK SA0 CIOCIISCS. .pa lor- and high-density satellite co.uar.tiv* TI - S.E. DANIELSON CALIF INST OF TECH studies, detection of atmosphe,esr frortrs and limb TI - I.E. DAVIES RANb COUP stratification 01 ~rrorolsil and (3) surtacc properties TI - G.E. HUNT U COLLEGE LONDON Icoloiimctry. scattering tunction. nature of brightnrss IM - 1. OUEN STATE U OF NEY YORK r.ri.tion. anc search tar nrr sat~llitcs.1 Studies ot Saturn‘s TU - c. SAGAN CORNELL U rings iert carried out and rill be tor Uranus. rings. 111 - W.E. SUOII U OF d1SCONS1M Objertirrs included (11 resolution ot individual ring 111 - T.V. JOHWSON MA SA-J PL co.ponents ot clumps ot matrriali (2) veitic.1 and radl.1 TM - H. IASURSUI US 6fOLOGlCAL SURVEI distribution ot material at scly high lCIOLUtioni (3) scattering tunrtioni (4) co.,se polati.ctry; (51 occultation - BRIEF DESCRIPTION Optical depth; and I61 distinguishing ditttrent types of The photographit cxpcri..nt usrd 1 tiO-c*.rra systr.. .aterial in the rings. other Objrttivts ICI~ to search tor new based on the Marinrr 10 system. Thtr system included on* co.*ts. .steroids. ana targets ot opvoitunity. narrow-angle. long-focal-length caa.ra and one wide-angle. short-tocal-lrnpth camera. The ma.i.u. rirolution achirvabl. dipended On the actual trajectory on this aulti-cncountrr missionr but the resolution was as high as 0.5 to 1.0 km On thr PARllCLfS AND FIELDS rlorest .ppIO.ch~S 15 s0.C objects. Lt Jupiter a66 Saturn. the rrsolution .as batter than 20 km and I tmr ,elp=CtlWe~Y- Ihe objectivrs 01 the ripiiiment were to photogwaph QlObaI motions and .loud distribut$onr on J~pi1-land Siturnr gross dynsmiral __--_-_PIONEER 11, uoLFE--‘-‘------~roperti.sr zonal rotation. oriertation 01 spin axis. zonal shear. vrrtic.1 shear, flor instabilitir.. SDO~S. and sp.ct,~m IkVESTlGATION NAME- PLASMA of scale ot at-oschrric motions in ti.. and space. Additional objectives included the study 01 the eode ot rel.ase 01 NSSOC ID- 73-0191-15 lNVESTIGATlVE PROGRAI internal rnrrg, flLx (search tor rrrvrction cells and rolls). CODE EL-+/CG-OP. SCIENCE study Of gVOuth, dissipation. morphology, and rcrtir.1 structure of cloud ~o.ple..t, gross optical pro pet tie^, global INVESIIGATION OISCIPLlNE(S) ard localiltd scattiring tunction in the visible spectru.r SPACE PLASMAS polarimetryr nat~re 01 ChrOrOphCt~s (their struCtuII and PARTICLES AND FIELDS derelop.ent). and high resolution 01 the 6rt.t Red Soot. The objectives 01 the s~t~lliteencounters included the tollOring: ?ERSONNEL 11) gross charact~ristics tsizr. sbapr. rotatien. spin asis. PI - J.H. UOLFE NASA-ARC caltOgr.phYr ilpc0l.d ephr.Crides and marrrrr) (21 geology 01 - L.A. FRANK U OF IOYA (majar physiographic pr~~inc~~,i.Flct and ~olcanicteaturerr 01 - R. LUST MPI-HEADOUARTELS ltncmcntrr polar ZWS. erosion piocessesr and lor- and 01 - D.S. INlRlLIGAlOR U OF SOUTHERN CALIF high-drnsity satellite ~~.paratiie studies. detection ol 01 - V.T. LAVIENISEFF~NLAI NAS1-ARC atmotpheresr trOstsr and 1l.b stratitication ot ariosols,) (31 01 - 1.1. SIITH NOAA-SEL surface properties l~010ri.etry. scatt*iing tunrtion. nature ot 01 - F.L. SCARF TRY SYSTEMS GROUP brightness variaticn. and search fcr ner s.tellitei.) Studies CI - H.R. COLLLRD NASA-ARC of Saturn’s rings included: I11 resolution of individual ring 01 - U.C. FELOMAN LOS ALAIOS NAT LAO CO.PO~~~~Sor clumps ot material. (2) vertical and radial 01 - D.D. MCKIBOIN NASA -ARC distribution ct material at very high rrsolutionr (31 scattering function. (41 coarse p~(ari..tiy, (51 oerult.tion - ORlEF DESCRIPTION octical depth. ana 161 distinguishing ditterent types ot The instrument consisted ot oual 90-deg qUadrisphCiicz.1 material in the rings. Other objectives ICI~ to search tor nrr ~I~ctr~stati~ana(yicrrr one rith 26 individual particle comttl. asteroids, and targets Of ODpOrtYnity. dettctors ~PCthe Other rith 5 currrnt rollactors. Ihe system “as capable ot me.ruring incident plasma distribution ---_---vOY&GER 2, S(llTH------”------para.~te,s 01-1 the energy range 0.1 to 18 kcV +Or plOtOnS and approximately 1-500 eV tor electrons. The high-resolution INVESTIGATION NAME- IMAGING an.ly2er rith a Constant Of 9 LeVIP per kV .DOlird to the plates. had mean plat. radius Ot 9 CI and scuarltion Of 0.5 cm. This analyzer 11s used to ICasuIe ions only, and had 26 ch.nnrltrOns mounted an the rcliCircu1.r enit tO the analyzer. Vhe aperture pointed through .lid- Slit in the bask Of the sp.cecratt high-gain antenna ritlrctor and pointed along the spin exis toward the earth (and ther.for. the sun). The edgrs PERSOWNEL 01 the bntenn. r.tlertor Limited the virwing of the instrumtnt PI - F.B. ICDOWALD YASAdSFC to 13 deg rith rtspect to thr #pin axis. The channeltrcns 01 - 1.6. ICCRACKLN CSIRO coverrd a range of plus 0, minus 51 del. Tech ch.nn.ltron near 01 - Y.R. YEBBEI U OF WEY IIAMPSHIRE thr center cOw.red 3 drg and aDorOx4rnatelv 8 drg near the Sdgts 01 - E.C. ROELOF APPLIEO PHISICS LAB of the analyzer. The angular vidth perpmnalrular to the lcng 01 - B.J. lEI6ARDtN NASA-6SFCNASA-LSFC.. .-. angulbr ridth was about 2 dog. In half the pln period the 01 - J.H. TRAINOI NASA-CSF C rhole Cone 01 half-angle 51 dog centered on tht sun "as swgt Out. A mcdium-cn=rpy analyzer iith mean radius 01 12 I. and a 1 cm plate separation (constant rt 6 Lev10 per kv applied) was urd to detect both ions and electrons. lhe detectors *ere fiut flat-surtace rurtrnt coIl.ctors. lhe three center collectors each colertd I5 de0 and ccvered the anpu1.r range of plus or minus 22.5 deg fro. the spin axis. The two outside rollcctDrs had an angular ridth of 41.5 dsg and .IS,. locb1.d bt plus cr minus 46.21 0.g fro. the center of tht analy1.r. There was a varitty of possible operating modes for tbe e.mtrimenti hOu*vtr~ the principal aade utiliz*d during the encounter phase 1.9 on. in which the analyler plat. pottntial was stepped through its rangt eiery one-half re~cIutionof the spb

85 POLARIZATION

86 Interplanetary Investigations by Planetary Probes INTERPLANETARY INVESTIGATIONS BY PLANETARY PROBES

Plate 6. This is a collection of press release images of typical planetary spacecraft that conducted investigations in interplanetary space. (A) Mariner 4 was one of the first spacecraft to conduct planetary (Mars) and interplanetary exploration. (B) Pioneer 10 investigated the interplanetary medium, the nature of the asteroid belt, and conducted exploration of Jupiter and its environment. (C) Voyager 1 was designed to conduct investigations of the Jupiter and Saturn systems and to study interplanetary space.

88 Mariner 4

Pioneer 10 Voyager 1 INTERPLANETARY INVESTIGATIONS BY PLANETARY PROBES

INTRODUCTION

Six planetary probes carried instruments specifically to make investigations in interplanetary space. These were Mariners 4 and 5, Pioneers 10 and 11, and Voyagers 1 and 2. There were 11 investigations for which NSSDC has data or knows the sources for obtaining data. These cover three categories which are (1) Particles and Fields, (2) Ultraviolet, and (3) Interplanetary Particles. Table 1 and Appendix B show the investigations in more detail.

91 SPACECRAtl ...... PERSONNEL PM - C.F. HALL(NLA> NASA-ARC PS - P. Q?AL NASA-ARC SPACECRAFT COMMON NAME- MARINER 4 ALTERNATE NAMES- 00942 BRIEF DESLRlPTlON lhir mission was the first to be sent to the outer solar NSSDC IO- 64-0711 syste.r and after cnrount*ring thr planet Jupit-r it assumed an escape trajectory from the solar systrm. The spacrcraft body LAUNCH DATE- 11128164 YEIGHT- 262. 16 was mounted behind a 2.74-m-diamrter parabolic dish antrnna LAUNCH SITE- CAPE CAMAVERAL. UNITED STATES that was 46 cm deep. The .p.~e~~aftstyurtur. I.. a 36-cm-drep LAUNCH VEHICLE- ATLAS flat equipment compartaent. thr top and bottom berng regular hrmgons. its sidrs yere 71 cn long. One side joined a SFONSORING COUNTRVIAGENCY smaller CompartRtnt that carried the scientific .xp~riments. UNITED STATES NASA-OSSA The high-g8ir antrnna feed was situated on th,.. struts. uhich projrrtcd toward about 1.2 m. This feed "as topped with a lNlTlAL ORBIT PARAMETERS atdium-gain 4ntenna. A low-gain omnidir.ction.1 antenna ORBIT TIPE- MARS FLlBY rxtendod about 0.16 rn behind the eguipment rompartm.nt and was mounted brlor the high-gain antenna. Power for the spacecraft PERSONNEL us Obtainea by four SNAP-19 radioisotope thrr.onurl*ar PM - J.N. JAMES NASA-JPL g.neiatOla (RTG). which were held about 3 fro. the center of PS - R.K. SLOAN(NLA) NASA-JPL the Ipacrcraft by tYO three-rod trusses 120 d.g .part. A third boom cxtrndrd 6.6 from the rrperimrnt compartment to hold the BRIEF DESCRIPTION ~agnttometer away from the ap.c.craft. The four RTG's Mariner 4 IDS the fourth in a series of spacecraft used generated atOUt 155 watts at Launch and decayed to tor planetary cxplcration in a flyby mode. It was designed to aPproximat*ly 140 watts by the time the spacecraft reached conduct CIOSCUPscientific observations of the planet and 4uDitcr on Drcembcr 3. 1973. 21 months after launch. Them to transmit these observations tc earth. Cther aissicn were thrre reference sensors: a star smsor for Canopus. and objectives were to perform field and DII~~CICmeasur~ment~ in ti0 sun SinsOIS. Attitude position could be calculated fro. interplanetary SP~CC in the vicinity of Mars and to provide the rrfrrrnci directions to the earth and the sun. with the c.~erirnce in ard krcblrdge of the er(ineering crpabilities fer known direction to Canopus as a backup. Three Pairs of rocket interplanetary flights Of long duration. After 7.5 months of thrusters pvovidrd spin-rate control (maintained at 4.8 rp.) flight. the soacecraft flcr by Mars on Iuly 14. 1965. and and changed thr velocity of the spacecraft. Thesr thrusters returned 21 pictures plus 21 lines rf picture 22. The tios*st could be pulsed or fired steadily by rommand. COmmunic.tions approach ins 9,846 kn from the Martian surface. The rparccraft ucre maintained via the omnidirectional and medium-gain performed all Drogrammsd activities successfully .t the proprr ontcnnasr uhith Operated togethrr. connected to one rrceirer. tiler and returnem LICfUl data fro. lsunrh until October 1965, rhilr the high-gain antrnna was connected to another receiver. when the dirtancr from eaith 8nd its antenra orientation Thesr rcreirrra could be interrhangrd by command to provide temporarily halted the signal acauisition. Data acquisition some rrdundancy. 110 radio tlansmittcrsr r0upl.d to two resumed in late 1961 and continued until December 20, 1967. trarrling-wave tube amplitiersr ~roduc~d8 watts at 2292 MHz each. Uclirk was arcoaplish*d at 2110 MH1. rhilr dsta ...... transmirsion dornlink "as at 2292 MHz. The data "ere receiwed by NASA's Deep Spnre Network. The rpacrcraft was te~p~~it"~e-~ontrOlledbrtrem minus 23 drg C and PIUS38 deg SPACECRAFT COMMON NAME- RARINER 5 C. Fifteen ~lptriments wrr earrird to study the ALTERNATE NAMES- MARINER VENUS 67. 02845 interplanetar, and planetary magnetic fisidri solar rind VENUS-67 PaIamCterS; ros*ic rays; transition region of the hrlfosphem; rrutral hydrcgen abundance; distribution. size. massr flu.. and NSSOC ID- 67-0601 uelocity of dust particles; Jovian ~UIOI~L; ~orianradio "awes; atmolpherc of Jupiter and some of its satellitcsr partic~larly LAUNCH DATE- 06/141C7 YEIGHT- 245. KG Io; and to photograph Jupiter and its satellites. Instruments LAUNCH SITE- CAPE CANAVERALI UNITED STATES carried for these riprrimrnts YCIC magnetom.terr plasma LAUNCH VEHICLE- ATLAS analyicr~ charged particle detrctotr ionizing drtector. non-imaging tclesroprs with owcrlapping fields of ricu to SPONSORING COUNlRY/AGENCY detect sunlight refltcted fro. passing mettoroids. .rated UNITED STATES NASA-OSSA Pressuiized Celts of argon and nitrogen gas tor measuring thr penetration of mrtroroids. Uv phatomrter. In rad4Omter. and an imaging photopotarimettl. which produced phOtOgr.phs and PERSONNEL me.sured Dolarilation. Further scientific information was PI1 - D. SCHNEIDERMAN NASA-JPL obtained tic. thr trarklng and orrultation data. The PI - T.V. PARKfR(NLA) NASA-JPL spacecraft achieved its closest aPPrOach on December 31 1973. PM - G.A. REIFf(NLA) NASA HEADPUARTERS when it reached aPproximtcIy thrre Jovian radii (about 210r000 PS - C.Y. SNYDER NASA-JPL La). The spacecraft contains plawes that have drawings depicting a man. a r0.m. and the 'lotation of the sun and the BRIEF DESCRlPTlON earth in our 9aia.y. It is leaving the solar system and The Mariner 5 ~pi)~ecraft*.I the fifth in a series of pasring into intrrrtellar SP.IC. Spacecraft "Sed for planetary ciploration in the flyby mode. Marircr 5 rar a Ielbrtished backup s~.~ecraftfor the Mariner 4 ...... miision and was converted from a Mars mission to VC~YS mission. The spacecraft Mas fully attitude stabilized. using the sun and Canopus as rcf~rmrts. A central computer ana SPACECRAFT COMMON NAME- PIONEER 11 sewtnce~ subsystem supclied timirs se~utncesand computirg ALTERNATE IAPES- PIONEER-6. PL-733C services tor other spacecraft subsystems. The spacecraft 6421 Gassed 4,CoO km from Venus On October 19, 1967. The ~pi~~~ritt instruments measured bath interplanetary and Vcnuriin magnetic NSSDC ID- 73-0191 fieidsr fhal9Ca particlc~~and p1.1ma11 8s r.11 a. the radic CCfractivitY and UY rliirioni of the Vrnurian atmosphere. The LAUNCH DATE- 04106113 YEIGHT- 231. KG liIIiDn was termed a IUCCCSS. LAUNCH SITE- CAPE CANAVERAL. UNITED STATES ...... LAUNCH VEHICLE- ATLAS SPONSORING COUNTRVlAGENC? UNITED STATES NASA-OSSA SPACECRAFT COMMON NAME- PIONEER IC ALTERNATE NAMES- PICNEER-Fr PL-723D INITIAL OR811 PARAMETERS 05860 ORBIT TYPE- SATURN FLIBV

NSSDC ID- 72-0121 PERSONNEL PM - C.F. HALL(NLA) NASA -lR C LAUNCH DIT€- O3lC3172 bEIGHT- 231. KG PS - P. OVAL NASA-ARC LAUNCH SITE- CAPE CANAVERAL, UNITED STATES LAUNCH VEHICLE- ATLlS BRIEF DESCRIPTION This was the stcond mission tn inwestigate IUpiter and SPONSORING COUNTRYIAGENCY the outer solar system. Pioneer 11, like Pionerr 10, Used UNITED STATfS NASA-OSSA Iupiter's qraritational firld to alter its trajectory radic.11~. It Passed cloir to Saturn and then it followd an IhllllL ORBIT PARAMETERS escape trajectory from the solar system . The spacecraft was ORBIT TYPE- JUPllER fLYBV 2.9 (9.5 tt) long and contained a 2.74-¤ (9-ft) dimeter high-gain antenna of aluninum honeycamb sandrich material "hose feed was topped with a medium-gain antenna. A low-gain. Omnidiicctionil antenna was mounted bclor the high-gain dish. It contained tu0 nuc1rc.r electric-power genrratars. which genei*tcd 144 Y ot Jwittr. but decreased to 100 Y 4t Saturn. There YC~C thrrs ~C~CII~CCsrnsors: a star (Canopus) sensor. and two run sensors. Attitude position could be calculated from the reference directinn to the eerth and the fun. with the

PRECEDING PAGE BEARX NOT FILMED krobr direction tc Caropus .I backuc. Pioneer 11's star senior SPCNSORING COLNlRIlA6ENCV gain and thmshold settings were -0diticdr based on ezperirnte UNITED STATES NASA-OSSA gainrd fro. the settings used On Pioneer IO. Three pairs of rocket thrusters proiidrd spin-.sir COntCOi (It 4.8 Cp*> and INITIAL ORBIT PARAIETERS change cf the SplCrCr.ft Yelocit). The thrulteis could be ORE11 TYPE- IATURN FLYBI either fivrd steadily 01 pulsed, by command. Communications were maintained via the oinidi,ectional and m.diu.-g.in PERSONNEL .ntenn.s, rhich Cclrated together. Connected to One rccrir*rs PI1 - J.R. CASANIINLA) NASA-JPL while the high-gain antenna was conrutted to the Other PS - E.C. STONE CALIF INS1 OF TECH recrirrr. The rtciive~scouid be interchanged by ro..and. 110 radio tranlmitteii. coupled to two traveling wave tube BRIEF DESCRIPTION ..piifiris. picau~r~8 Y OOI~I eact in I-tand. Co..unic.tion The over.11 objcrtivcs of Yoyag*r 2 were to conduct uplink (earth to S~~CCII.~~) ~pe,.t~d at 2110 UHI~ and dornlink e.eloratory investigations of the planttary syste.s of ~upiter, Ispaccc,aft to eavth) at 2292 UHz. At Jupiter's distance, Saturn. Uranus. and Neptune. and of the interplanetary medium. round-trip communication time took 92 .in. Data were received Primary r.ph.sis was plactd on camparatire studies 01 thtse st the Deep Space Nttrork IDSN). Thr spac.craft bas tlanetary systems by obtaining (1) measurrmentr of the t~.p~ritu.~-cont.oll.~ to betllCCn -23 and t38 dcg C (-10 to enrironm+ntr atmosohtie. and body characteristics of the +loo dCg f). An additional experimtntr a l01-sensitiiity &lanets and one 0. more of the satellites of each planet. 12) flusgate m.pncto,rtcrr I.. aadea to the Pioneer 11 payload. studies 01 the nature Of the rings Of Saturn and Uranus. and Instruments studird thr intrrpldnrtary and planetwy magnetic 13) exDloration ot the interplanetary (or intrrstellar> medium fields; solar wind pioprrties; cosmic rays; transition region at increasing aistanrcr fro. the sun. These objtctircs were of the hcliospher.; neutral hydrogen abundance; distribution, met using wariety of instruments and methoas including sillr .ass. flu.. and YrlOrity ct dust pa~ticl~s;Jovian imaging. a coherent 5- and X-band RF receiver. an 11 .UIOIIC; Jovian radio waves; the atmOspher1s of pl.nct~ and inteifeio-eter and r.dio.rterr a UV spectrometer. fluxgate s.tellite~; and the surfares of JUpittl. Saturn, and some of ma9netOmetersr Faraday CUDS. chargd-particl. analyze^. their satellites. Inrtrumerts carried for these experimerts ~11s.a aetector. ~lasma-~ave radio receiver. cos.ic-ray wire magnctometrr. plasma analyztr (for solar rind). ttlescones, ohotopolarimrtrrr and a sirrp-frequency radio charged-particle cetertorr ionizinp detectorr non-imaging rrreivcr. JYpitCI Close CnCOYnter 1.5 achieved On July 9, telescopes iith OwerlapDing fields of vir" to detect sunlight 19191 and Saturn on August 5. 1981. reflected from carsir9 meteoroids, sealed orrrsurizec cells cf argon and nitrogen sal for measuring prnetration Of meteotoids~ uv photo.ctrl. IR radiometer. and an $.aging phOtOpol.iimeterr IMsTIGIzITww(SnvtSIWImS rhith producedpr0du1.d phctcgraehfphctcgraehs and *e.sured the p~larization.Polarization. FARTICLIS AND FIELDS Furthtr scirntifir inform.tion 11% obtained fro. celestial mechanics and occultation nhrnomena. This roarrrr.ft- like

Pioneer 11 was 36.800 km 1.0. Jupiter during its r101elt .pproachr Otcembll 4. 1914. 10 within 43rOOO k. Of its cloud INVEST1GATION NAME- INTERPLANETARY ION PLASUA PROBE FOR topi. It oaised by Satuir on Aus. 5, 1919 at a distance of TIP 01 40 TO 94CC VOLTS 71.400 tm from Situvn'l cloud tons.

INVEST16ATION DISCIPLINE(S) SPACECRAFT CORRON NAUE- V01A6ER 1 PARTICLES AND FIELDS ALTERNATE NAUES- MARINER JUPITERISATURW Ar OUTER PLANETS A INTERPLANETARY PHISICS RARINER IlAr UJS 11L 10321 FERSONNEL PI - H.S. BRIDGE UASS INST OF TECH NSSDC ID- 11-0841 01 - C.Y. STNDER NASA'JPL

LAUNCH DATE- 09105111 YEIGHT- 100. KG ERIEF DESCRlPllON LAUNCH SITE- CAPE CANAVERALI UNITED STATES This thi~r-s~ctio~al-coll~ct~~80dulatrd-grid Faraday cup LAUNCH VEHICLE- TITAN ..asured positive ions from +O to 9400 cVlP in eight appiOxi.at.1~ Logarithmically tquiipired energy rindorr. AI SPONSORINS COUNlRYlA6ENCl the instrument always pointed toward the sun. vector data UCIC UNITED STATES NASA-OSSA obtained by romp.ring the relative signals from the thrre 120-de9 pie-shaoed rollrctor sections. Ouring each telemetry INITIAL ORE11 PARAMETERS sequence, the instrument was stepped forward and barkward ORBIT TYPE- SATURN FLYBY through thr eight rindows to mraturc the sum of thr currents lr0. the three plates. Then it Was Stepped forrard and PERSONNEL backrard to .easure. for each voltage Settinpr the currents to PM - J.R. CASANIINLA) NASA-JPL the three plates in rurcrsiion. The entire 32 steps in voltmge PI - E.C. STONE CALIF INS1 OF TECH iindoi per t.l..etry sequence Produced 64 CUrIrnt measurements. These measurem*nts were repeated every 5 .in. The instrument BRIEF DESCRIPTION operated nominally throughout its mission. The overall objectives of Voyager "ere to conduct raplcratory ini.stigations 01 the clanrtary syste.~ of Jupiter ------RARlhER 4, sIRpsoN------'------and Saturn and of the intcrp1anct.r~ medium Out to Saturn. Primary emphasis "as placed on comD1vatirr studies of these two INUESlISAllON NARE- COSUIC-RAl TELESCOPE planetary systems by obtaining (1) .easure-ents of the enriron.rntr at.osther~~ ard too) tharacteristici of the LSSDC ID- 64-011A-O* INVESTIGATIVE PROGRAR planets and the satellitts of each planet. (21 studies of the CODE EL-*. SCIENCE nature of the rirgs of Saturnr and (3) explor.tion of the intcrplanctary (or interstellar) acdium at increasing distances INVEST1GATION DISCIPLINE(S1 fro. the sun. Ttesc objectives bere attained ty using COSIIIC RAYS variety of instruments and methods including imaging, 1 coherent I- and I-band RF receiver. an infrared intrrfcranst*r PERSONNEL and radiometer. UY se.rtrOletCr, fluxgate mrgnctometersr PI - J.A. SIUPSON U OF CHICAGO Faraday cups. cha1ged-particle analyzerr 01.1.. detertcr. 01 - J.J. O'GALLAGHER U OF UARYLAND ptasma-wavc radio receivers COI.~ c-ray t clcicores s photOpOlali.CtCr, and a sweep-frrqucnry radio receiver. BRIEF DESCRIPTION vcyagcr I had its closest rnrountlr rith Jupiter on Rirch I, A set cf three silicon surfare barrier detectors was used 1979, and eith Saturn on NOvembCI 121 1980. in the form of 1 dEldx VI range teles~oveto drttrminr the flus of protons in the energy interYalI 15 to 10 Rev and 10 to 170 ...... UCVI alpha p.rtitlts in the energy ranges IS to 10 R~Vlnucleon and above IO ?.Ulnucleonr and protons and alpha particles in the energy interval 1.2 to 15 Rcvlnucleon. The detector was SPACECRAFT COURON NAUE- VOIAGER 2 mounted on the spac~craft so as to point always in the ALTERNATE NAUES- PARIhER JUPITERISATLRN 0. OUTER PLANETS e antisolar direction. A 128-channel pulse-height analyzer was UARINER 17E. UJS 110 used to SamtIe the cncrgy LOSS in the top deterto? elrmrnt of 10211 the telescope. It "as ooiiible to pul~e-hripht anilire protons and alpha particlef tro. 15 to 10 UcVlnucLeon. protons from 70 NSSDC ID- 11-076A to 110 MeV, and alpha particles with energies above 70 UeWlnucleon. fro count rates ana tu0 pulse height an.1ys.c~ LAUNCH DATE- 08120111 YEIGHT- 100. KG icrc Obtained every 12 or 18 I according to whether the LAUNCH SITE- CAPE CANAVERAL, UNITED STATES spa~ecrift transmission rate was 8-113 or 33-113 bps. lhr LAUNCH VEHICLE- TITAN rapsrimcnt eerforwd n~iiallyfrom launch until October 1965. -hen the space~raft"as turned Off to conservt power. Yhtn the spacecraft .as turned on again at Liter time. the dettctor did not respond. For further details. ICC 0'6allaghClr AD. J.. *. 1501 e. 615. 1967.

94 BRlEf DESCRIPTION This experiment (on both Pioneers 10 and 11) consisted of broadband Chotometer sensitive betreen 200 and 800 A. During the Cruise phase of the mission. this r.perim.nt was used to search for the supersonic-to-subsonic trensltion region in the NSSDC ID- 17-084A-08 INVESTIGATIVE PROGRAM solar ~ind. Dwinp the Jovian encounterr this efiperiment was CODE EL-4, SCIENCE used to look for evidence Of an auroral oval on the Jovian dayside. to find the ratio of hydrogen to helium in the Jorlan INVESTIGATION DISClPL1NE(Sl atm0spher.r aid to find the temperatur. of the out., portion oi COSMIC RAYS the Jovian .tmosph.fe. Evidence ot-,h.lium I.. found in the MAGNETOSPHERIC PHYSICS interplan*tary region indicsting interactions betreen charg.d partitles and neutral hydrogen. PERSONNEL PI - R.E. VOGl CALIF INST Of TECH --_---_PIONEER 11, JUDGE------'------CI - J.R. JOKIPII U Of ARIZONA C1 - E.C. STONE CALIF INS1 Of 1ECH INVESTIGATION YARE- ULTRAVIOLET PHOTOMETRY CI - F.B. MCDONALO.. NASA-GSFC. .. . CI - J.H. TRAINOR NASA-GSFC NSSDC ID- 73-019A-06 INVfST16ATIVE PROGRAM CI - Y.R. YEBBER U OF NEW HAMPSHIRE CODE EL-+. SCIENCE CI - A.Y. SCHARDT NASA-GSFC IMVESTIGATIDNASTRONOMV DISCIPLlNF(S) BRIEF DESCRIPTION This inv.stigation studied the origin and a

NSSDC ID- 17-0164-08 INVESTIGATIVE PROGRAM CODE EL-4. SCIENCE INTERPLANETARY PARTICLES

INVESTI6LTION DISCIPLINE(S) COSMIC RAYS MAGNETOSPHERIC PHYSICS ------PIONEER 10, SOBERMAN------

PERSONNEL INVESlIGATIOY NAME- ASTEROIDIMETEOROID ASYRONOMY PI - R.E. VOGT CALIF INST OF 1ECH CI - J.R. JOKIPII U OF ARIZONA NSSDC ID- 72-012A-03 INVESTIGATIVE PROGRAM Cl - E.C. STONE CALIF INST OF TECH CODE El-4. SCIENCE C1 - F.B. MCDONALD NASA-GS f C CI - J.H. TRAINOR NASA-GSfC INVEST16ATION DISCIPLINE(S) CI - Y.R. YEBBER U OF NEW HAMPSHIRE ASTRONOMY CI - A.M. SCHARDT NASA-GSFC INTERPLANETARY DUST

BRIEF DESCRIPTION VERSONNEL This investigation studied the origin and acceleration PI - 1.1. SOUERRAN GENERAL ELECTRIC CO process. life history. and dynaaic contribution of intrrrtcLLa. 01 - H.A. ZOO1 NASA-JSC cosmic rays. the nutl.osynthrsis of elements in cosmic-ray sourcesr the behavicr at ror~lr ray$ in the interplanetary BRIEF DESCR1111ON medium, and the trapped planetary energetic paiticle The orerall objective of this r.p.riment (also carried on environment. The instrumentation included a Hlgh-Energy Pioneer 11) was to investigate dust particles and meteoroids in T.lescope System (HETI1 and Lor-Energy Telescope System intrrDl.n.1.rl SD.C.=. It I.. eSS.nti.LLy tu0 ..pe,i.*ntSr (LETS). The HETS cowrrd an enrrsy range betreen 6 and 500 usinn two different terhnigues. One method was to detect MeVlnurl*on tor nuclei ranging in atomic numbers from 1 through Pirticles by the refl*ction of light from them. and the 0th.r 36. In addition. elections in the energy range betreen 3 and method was 10 detect them by their impacts. lh. objec1iv.s IC0 MeV were reasurcd by this t.lescOp. ord an .Lectron were to determine distanre. trajeztory. velocity. relative ttlescops (1ET). The LETS acasured the energy and determined size. and flus of particles ranging in sizr fro9 minute fht identify of nulL.1 for energies betreen -15 and 30 P.itic1.s fer *.t.rs from the t.LescOp. 10 distant asteroid.. MrYlnurleDn an0 atomic nu.berS fro. 1 to 3D. lht instruments Th- Cquip-ent fov the d.I.Ctlon 01 refl.rtion ronsi.1.d 01 tour ~LSO .Casuied the anlsatropies cf electrons ard nuclei. In "on-imaging Ritchey-Chrttiin 1eL.scOp.s with primary mirror. of addition. electrons in the CneIgy tangs betreen 3 and 100 I4-u 20-rm (8 in.) diameter. and 25-1. (10 in.) fora1 Lrnpth, fields Mer. measured by an electron tel*scope. of view (TOY) of 0.2 rad (8 dog) each, secondary Optics, and a photO.ultlpLier tube. The 1.tt.P d.t.ets the ref1.Ct.d Light COllCcted by thr teLe8r.OPe. An event was recorded rhrn at least three of the four tel~scopessaw the Obleet. Entry and ULTRAYIOLEl departure times of thr light enabled determination of range and velocity. The equipment fop the impact mode consisted of IS panels each containing 18 se.Led re1111 pr.ssur1z.d "4th argon and nitrogen gas, coverlng 0.65 sq (6.9 sq tt) Of the back of the ..in entcnn. dish. Pcn.tration by partiel. IesULted in Loss of gas at a rmt~proportional 10 the sizs of the hole, rhich would be r.1at.d 10 the paitlcle mass and w.lOcity. Penetrations icrc registered from particles as small as 1.E-8 NSSDC ID- 72-0121-16 INVESTI6ATIVE PROGRAM 9. CODf EL-4. SCIENCE ------PIONEER 11, SOBERMAN------"------lNVESTlCATlON DISCIPLINE(S1 ASTRONOMY INVES11GATlOL NAME- ASTEROIDIMETEOROID AS11ONOMl PLANETARY ATMOSPHERES NSSDC ID- 73-019A-03 lNYESTlGATIVE PRO6RAR PERSONNEL CODE EL-). SCIENCE PI - D.L. JUDGE U Of SOUTHERN CALIF 01 - R.Y. CARLSON NASA-JPL INVESTIGATION DISCIPLINE(S) ASTRONOMY INlERPLANETARY DUST

ORlGlNAC PAGE IS OF POOR QUALITY PERSONNEL PI - 1.1. SOBERMAN GENERAL ELECTRIC CO 01 - HA. 1001 NASA-JSC

BSlEf DESCRlPlION The orcr.11 0b)CCtiwe af this expctimrnt was to investigate dust ~arti~lesand meteoroids in interplanetary INVESTI6ATION NAME- ZODIACAL-LIGHT TYO-COLOR space. It "as rstcntially two txpcrimcntsp using two different PHOTOPOLARIMETRI techniques. One techad "as to crtrrt particles by the reflection of light from the., and the other method 11% to NSSDC ID- 72-012A-14 lNVESTlGATIVE PROGRAR detect the. by their impacts. Tht VbjcCtiVts icrc ta determine CODE EL-4, SCIENCE distance. trajectory. ve10city. relative size. and flux of p.rtiClcS ranging in size ftom minute particles fer meters INVESTIGATION OISCIPLINL(S) from the tCteSCDpC to distant artrroidl. The equipment for the ASTROHOMI detection of ~eflection consisted of four non-imaging PLANETARI ATMOSPHERES sitthey-ChletitP te1esraGes rith clirary sirrcrr of 20-r. (8 IODIACAL LIGHT in.) diametet. 25-C. I10 in.) local length. fields of rlrr (FOV) Of 0.2 rad (8 deg) carhr SCLOndary Optics, and a PERSONNEL photomultiplier lute. The latter oitects the reflected light PI - J.L. hEINBERG U Of fLORIDA coll~~ttdby the filescapes. An event "as recorded uhrn th*ee 01 - n.s. MANNER NASA-JPL of the four 1eLescopcI sa" the ctjcrt. Entry and departure timer of the light enabled dct+rmination of range and velocity. BRIEF DESCRIPTION The equipment fcr the impact tcae ranristcd at 13 canelr The liarling PhOtopo1ari.eter IIPP) cxperimcnt 1al.o containing 18 sealed ~111s~~ICSSYII~~~ rith argon and nitrogen carried On Pioneer 11) 11s used to obtarn mavs of the zodiacal 9.1- covering 0.65 SQ .(6.9 sq ft) of the back of the main light distribbtion in two rolorr~blue (39PO to 4900 A) and red antenna dish. Peretration by a ~arti

INVESTIGATION DISCIPLINE

96 to.m.ttCd to produce a sky map. 360 deg in clock angle by 1)l dcy in cone angle. The cxp.rimtntal train tor the 1PP package consisted of the tollorinp .lemcntsr 11) a n.ar-diftr.rtion-li.itcd 2.54-rm Uatsutov catadicptric telescopt (fl3.+); (2) a focal plane wheel containing field-of-vier ap~rtures~depolarizelf. calibration 10urcc1 ctc.; (3) a Yollarton pris. to split the light into twc orthogonally polarized beams. (4) a 45-drp dichromatic mirror thmt reflected wavelengths less than 5500 A (blue beam) and transmitted all light Of greater warelength (red beam). 15) fer each sp~ctral beam (two polarixationr) a filtering, coated relay lens and folding mirrors. and (6) tot each spectral brame ti0 Bcndix rhanntltron d.tCctOrs (blue - bialkali S-11 phOtOCathOdel. rea - S-20 phetocathcaes) to register the intensity in each polarization component. (Note: a riai1.r experiment #as also aboard Pioneer 10.) Data include the interplanetary regicn.

91 Interplanetary Investigations

PRECEDING PAGE BUNK NOT FILMED up~uIw))uILLxtluwg INTERPLANETARY

Plate 7. This is a collection of press release images of typical spacecraft designed solely to conduct investigations in interplanetary space. (A) Pioneer 5 investigated particles and fields in ciscytherean space, including solar flares and the solar wind. (B) Pioneer 6 investigated interplanetary phenomena in ciscytherean space to within about 0.814 AU of the sun. (C) Pioneer 9 collected scientific data on the electromagnetic and plasma properties of the interplanetary medium. (D) Helios-A investigated the properties and processes in interplanetary space in the direction of and close to the sun.

100 Pioneer 6

Pioneer 5

Helios A

Pioneer 9 INTERPLANETARY INVESTIGATIONS

INTRODUCTION

There were seven missions which were designed solely to make investigations in interplanetary space. These were Pioneers 5, 6, 7, 8, and 9, and Helios-A and -B. There were 54 investigations for which NSSDC has data or sources for obtaining data. These cover three categories which are (1) Particles and Fields, (2) Radio Science and Celestial Mechanics, and (3) Interplanetary Particles. Table 1 and Appendix C show the investigations in more detail.

10 3 PRECEbrKG PAGE BLANK NOT FILMED ...... appropriate tC the satellite distance fro. the earth...... SPACECRAFT COMMON NAME- PIONEER 5 ALIERNATE NAMES- 1960 ALPHA Ir 00027 SPACECRAfT COPMON NAUE- PIONEER 1 NSSOC ID- 60-001A ALTERNATE NAMES- PIONEER-8. 02398

LAUNCH DATE- (13/11/60 YEIGHT- 43. KG NSSDC 10- 66-0151 LAUNCH SITE- CAPE CANAVERIL. UNITED STATES LAUNCH VEHICLE- THOR LAUNCH DATE- 08/17/66 YEIGHT- 138. KG LAUNCH SITE- CAPE CANAVERAL, UNITED STATES SPONSORING COUNTRYIAGENCY LAUNCH VEHICLE- DELTA UNITED STATES NASA-OSSA UNITED STATES DOD-USIF SPONSORING COUNIRYIALENCY UNITED STATES NASA-OSSA lNlIlAL OR011 PARAMETERS ORE11 IYPE- HELIOCENTRIC EPOCH DAlE- 03111160 ORBIT PARAMETERS ORB11 PERIOD- 311.6 DAYS INCLINATION- 3.35 DIG OR011 TYPE- HELIOCENTRIC EPOCH DATE- 02/12/76 PERIAPSlS- 0.1061 AU RAD APOAPSIS- 0.9931 AU RAD ORE11 PERIOD- 402.9 DAYS INCLINATION- O.OY& DIG PERIAPSIS- 1.009 AU RAD APOAPSIS- 1.125 AU WAD PERSONNEL PM - C.F. HALL(NLA) NASA-ARC PERSONhEL PM - C.F. HALL(NLA) NASA -ARC BRIEF DESCRIPTION PS - J.H. YOLFE NASA-ARC Pioneer 5 (1960 alpha 1) "as a spin-stabilized space probe used to investigate intrrtlanetary IPaCI brtrrrn the 0RIEf DESCRIPllON orbits of earth an0 Venus. The spacecraft mCaSuICd magnetic Pioneer 7 "1% the second in a series of solar-orbitrngr field phenomena. solar flare particlesr and ionization in the spin-stabilized, solar-cell and battery-powered 1lt~L1it~s interplanetary regicn. The digital aata were trarsmitted at Ir oerigned to obtain measurements of intcrplanrtary phenomena 6. and 69 boss depending on the distance of the sps~~c~lttfrom tram ridtly separated points in space on a continuing basis. the earth and the size Of the lecelving antenna. Yeight The spacecraft Carried txperincntr to study positive ions ana Limitations on the solar cells pr~venf~dcontinuous operation cLcctrons in the solar wind. the interplanetary electron of the telemetry transmitters. About four operations of 25-nin density (radio propagation e~periment)r solar and galactic duration were scheduled per day with orrasional inrrrasrr caraic rays, and the interplanetary magnetic field. Its main during times of special interest. A total of 138.9 h of antenna "as a high-gain directional antenna. The spacecraft operation "as ~omplited~and over 3 million binary bits of data uii spin-stabilized at about bo rp.. and the spin axis was were received. Ihe major portion of the data 111s racaircd at perpendicular to the ecliptic plane and pointed aopr~~imately the Man~h~sterand Hadaii tracking stations because their torard the south ctliptrr pol?. by ground commndr one of five antennas provided gric IeCCptiOn. Pioneer 5 performed normally bit rates, one Of four data formats, and one Of four Opclatlng until April 30. l9CCr after which telemetry transsission Cecame modes could te selected. The five bit rater iert 512, 2561 64, too infrequent for any significant addition to the data. The lbr and 8 bps. Three Of the four data formats contained spa~ecraft established a c~mm~nicati~nslink with the earth bcimarily scientific data and consisted of 32 seven-blt uords from a record distance of 22.5 millicn miles On June 26, 1960- per frame. One scientific data format was used for the two which 1.9 the last dry of tranrnirsion. highest bit rates. Another was Used for the thlee lorrrt bit rater. The third contained data from only the radio ...... prOp.g.tiOn experiment. The fourth data format contained mainly engineering data. The four operating modes were (1) real time, 12) telemetry store, (3) duty cycle store. and (4) SPACECRAFT COMMON NAME- PIONEER 6 memory readout. In the real-time eode. data i~rtsanplcd and ALTERNAIE NAMES- PIONEER-Ar 01041 transmitted directly (without storage) as specified by the data format and bit rate IClCCtCd. In the tCLemCtly Store node, NSSDC ID- 65-1D5A data "ere stored and transmitted simultaneously in the format and at the bit rate selcctcd. In the duty cycle store mode, a LAUNCH DATE- 12/16/65 YEIGHT- 146. KG single franc of scientific data "as TOLLFC~C~ana stored at a LAUNCH SITE- CAPE CANAVERAL, UNllED STATES rate of 512 bpi. The time period betieen which ~~cccssive LAUNCH VEHICLE- DELTA frames *ere ~OLl~ctedand stored could be rarlcd by ground comaand brtrrcn 2 and 17 min to provid~partial data coverage SPONSORING COUNTRYIAGENCY for periods up to 19 hr as limited by the bit ItOlagt Capacity. UNITED STATES NASA-OSSA In the mrmory readout mode, data "ere read out at whatever bit rete "as appropiiat~to the satellite distance from the earth. ORBIT PARAMETERS ORE11 TYPE- HELICCENTRIC EPOCH DATE- 07/15/75 ...... ORBIT PERIOD- 311.1 DAYS INCLINATION- 0.168 Dtb PERIAPSIS- 0.613 AU RAD APOAPSIS- 0.983 AU RAD SPACECRAFT COMMON NAME- PIONEER 8 PERSONNEL ALTERNATE NAllfS- PIONEER-C, 03066 PM - C.F. HALL(NLA) NASA-ARC PS - P. DYAL NASA-ARC NSSDC 10- 67-123A

BRIEF DESCRIPTION LAUNCH DATE- 12/13/67 YEIGHT- 146. KG Pioneer 6 111 the first in a series of rclar-orbitire, LAUNCH SITE- CAPE CANAVERALI UNITED STATES spin-stabilized, solar-cell and battery-powered satClLit#*l LAUNCH VEHICLE- DELTA deliyncd to ObtaiP measur~ments an a continuing basif of inicrplanctary phenomena from ridely sevarat~dpoints in space. SPONSORING COUNTRV/AGENCI Its e.periients st~aiedthe positive ions and clertrcns in the UNITED STATES NASA-OSSA solar rind, the intcrplanctary electron density (radio propagation crptri*rnt). solar and gala~ticcosmic rays, and OR811 PARAMETERS the inttrplsnctary magnetic field. Its main antenna "as a ORBIT TYPE- HELlOCENTRIC EPOCH DATE- 09/11/75 high-gain d,rcctional antenna. The s~acecrift 1.11 OR011 PERICD- 317.5 DAYS INCL1NATION- 0.057 UEG spin-stabilized at about 60 rpmr and the spin iris id5 PERIAPSIS- 0.992 AU RAD APOAPSIS- 1.088 AU RAD prrpcndirular to the CtliCtir plane and pointed toward the Scuth ecliptic pole. 0y ground ramrrndr one of five bit rates. FERSONNEL One Of four data formatrr and one of four Operating modes could PM - C.F. HALL(NLA) NASA-ARC be Selected. The five bit rates uere 512, 256, 64. 16, and 6 PS - J.H. YOLFE NASA-ARC bp~. Three of the four data formats contained primarily scientific data anc consilted of 32 seven-bit woidl per frare. BRIEF DESCRIPTION One scientific data format "as for use at the fro highest blt Pioneer R was the third in a rtrirs of solar-orbiting, rates. Another uas for use at the three larcrt bit rater. The ~pin-stabilized~ sola~-ccll and battery-pOICled satelliter third contained aata from orly the radic DrOoagatiOn designed to obtain nealurrments of interplanetary phenomena enperiment- The fourth data format contained mainly from widely separates points in spare an a continuing basis. engineering data. The four operating modes icrc real time, The spacc~raft carried ~ip~iimtnt~to study the positive ions telemetry store. duty cycle store. and mmory readout. In the and el~ctronr in the solar rind, the interplanctaly tl~ctron real-tine mode, data "ere ranplro and transmitted directly density (radio propagation cxprrincnt>r solar and galart-c Idithout storaye) as specified by the data format and bit rate cosmic raysr the interplanetary magnetic field, COSIIL dust, s~lect~d. In the telemetry Itore mode, data #ere stored and and electric field.. It1 main antenna rar a high-gain transmitted simultaneously in the format and at the bit rate directional antenna. The ICactclaft "as Sp(n-ltabiliZcd at ~elected. In the dUty-Cy~lC store .Odes a Single frame Cf about 60 rtar and the Spin axil was perpendicular to the scientific data was colle~t~dand stored at a rate of 512 bps. ecliptic plane and pointed torard the south ecliptic POLC- by The time interval between the collection and storage of ground command, one of five bit ratel, one Of four data r~rcersivr frames could be varica ty ground command batweer 2 forllatsr and one of four Operating modes could br Selected. and 17 mi" to PrDIidC partla1 data coverage for periods UD 10 The five bit rates "ere 512, 256, 64, 16, and & bpl. Three Of 19 hr as limited by the bit itorage capacity. In the me.101)l the four data formats were used primarily for scientific data readout WOdtr data were Pead Out at uhrtrvcr bit late IaS and conri%tcd of 22 seven-bit rords per trine. One scientific

10s

PWECEDCNG PAGE BLANK NOT FILMED ...... ORB11 PARAMETERS ORBIT 17PE- HELIOCEMTRIC EPOCH DATE- 01116l15 ORBIT PERIOD- 190.15 DAWS INCL1MATION- 0.U DES PERIAPSIS- 0.3095 AU RAD APOAPSIS- 0.985 AU RAD

PERSONNEL PM - A. KUlZER 6ES FUR YELYRAUMFORSCH PI - 6.Y. OUSLEY NASA-6SFC PS - H. PORSCHE DFVLl PI - J.H. YRAINOR YASA-6SFC BRIEF DESCRlPl10N ThIs spacecraft ".a one of 8 pair of deep apace probe. derrloprd by thr Federal Republic of 6rrm.n~ (FRG) In 8 coopirative program with NASA. Experiments I-,.provided by sri.ntists fro- both FR6 and the U.S. NASA sYppli.d the TitanlCentaur Launch YehitLC. Thr SpaC.

106 in the iournal Raunfahrttorsrhunpr v. 19. n. 5, 1975. PERSONNEL PI - G.S. LEVY NASA-JPL mmnows BRIEF DESCRIPTION PARTICLES AND FIELDS This experiment utilized m~as~rementsof the polarization of the IPaCeCPaft teLCietiy signal to obtain measurements 01 the relative taraday rotation due to the interplanetary medium and the earth's ionosphere.

INVESTIGATION NAME- SUPERIOR CONJUNCTION FARADAY ROTATION

NSSDC ID- 66-075A-08 INVESTIGATIVE PROGRAM CODE EL-). SCIENCE INVESTIGATION DISCIPLINE(S) PARTICLES AND FIELDS lNVESlIGATlON D1SCIPLINE(S) SPACE PLASMAS HIGH ENLRGY ASTROPHYSICS

PERSONNEL PERSONNEL PI - H.S. BRID6E MASS INST OF TECH PI - 6.5. LEVY NASA-JPL 01 - A.J. LAZARUS MASS INST OF TECH 01 - F. SCHERB U OF YISCDMSIN BRIEF DESCRIPTIDN This exprrinent utilized rn~as~~ementiof the polarization BRIEF DESCRIPTION Of the SpaCcCr.tt telemetry Signal to Obtain IeaIYTCmentS Of A multigrid Faraday cup with two s~mlcircular. co~lanar the relative Faraday rotation due to the interplanetary Medium CollectOrs was used to study solar rind ions and cl.rtrons. and the earth's ionosphere. The instrument had 14 rontiguous, energy-per-charge (EIP) rhanrcls brtuccn 75 and 9485 Y tcr po~ltivcions. and fcur ------pIg*E(R $3, "OLff----'------en~igy-per-ch.rgt channels bcturen PO and 1580 v tor rlrrtrons. The instrument vier asis "as perpendicular to the space~raft lNVESllGATION NAME- SOLAR PLASMA DETECTOU spin axis and parlll~l to the ecliptic plane. The line separating the tu0 collectors lay in the ecliptic clar'e, NSSDC IO- 6b-1001-02 INVESTIGlllVE PROGRAM enabling a rough determination 01 sol., rind bulk tlor CODE EL-4. SCIENCE peipendi~ular to the ecliptic plane. During every second SFarrcraft rotation and at one voltage level, the sum of the INVESTIGATION DISCIPLINE(S) cuii.nts fro. the collectors was obtained in 28 rontigucvr SPACE PLASMAS 11.25-drg angular Srctois (fro1 -45 dcg to 270 degr with 0 de9 PARTICLES AN0 FIELDS being the spa~tcraft-sunline). The eight ~~a~urementsabout the sun-earth line (-45 dcg to t45 dtg) urre telemetrred. hut PERSONNEL only the Largeit IC~SUIC~C~~in each succeeding 45-de9 intcrr.1 PI - J.H. YOLFE NASA-ARC (45 dcg to 270 deg) "as te1emeter.d. In addition. during this 01 - D.D. MCKlB81N NASA-ARC rotation. the current tro. one 01 the rollrrtorr I.% aeasured in all twenty-ciqht 11.25-deg sectors, and the largest was BRIEF DESCRIPTION identified and telZmeteied lboth magnitude and sector). A A truncated hemispherical tlectrortatic analyzer (12o-deg romplctc set of positive ion ..asUcements and one energy tatel p~r.ll~l-pl~t~CUIV~~UIC> with three contiguous c~rrent channel of electron measurements icrc completed every 32 s. collectors was used to study the directional intensity ot the The timr betreen each 52-r group ct neasurea~ntsvariec bith electran. ana positive ions in the solar rind. lanr were the bit rate. For a more ~0ipl.t. descriptions see 1. Geophys. detected in SQ iagarith.ically r~uispared energy per unit RCS.. ". 71. p. sin-mi. ;Lugust 1966. charge 1ElP) steps tram 150 ta 15.000 v. rhtre was an rlrrtron mode of operation in rhirh electrons were measuled in 14 ------PIONEER 7, BRIDGE------logrrithnically cguispaced EIP steps ranging from 12 to loo0 V. There #as a110 8 zero EIP. or background. step. The three lNVESTIGATION NAME- SOLAR MIND PLASMA FARADAT CUP rollrctors measured particles incident tram three diftcrrnt rtntiguous angular intervals relative to the IPILCCII~~ NSSDC ID- 66-075A-02 INVESTIGATIVE PROGRAM eeuatorial plane Crane as the ecliptic plane). Two rollertors CODE EL-4. SCIENCE mcasurcd flux from 10 to 85 deg on either side of the ID~Cecratt e~uatorial plane. and the third ICaSUred tlux in a INVESTIGATION DISCIPLINE(S) 20-de9 interval rcntcrrd On the spacecraft ~~~it0ii.1piane. PAUTICLES AND FIELDS As the spa~ecratt *as spinning, fluxes YCII IC.TUIC~ in 25 passible 2-13116-deg-ride alilluth.1 angular sectors. Seventeen PERSONNEL 01 these sectors were contiguous and bracketed the solar PI - H.S. BRIDGE MASS INS1 OF TECH dirtrtion. The remaining six s~ctorsicrc widely spared. The instrument had three .Iodes Of data cOllectiOn: polar scan. BRIEF DESCRIPTlON azimuthal scan. and maairnun flux. At the two highest bit rates A multigrid Faraday cup with two se.fcirrul.rr coplanar (512 and 256 bpi). the polar-scan modc was alternated with the roilrrtorr "as used to study solar rind ions and elertrcns. azimuthal scan mode at each EIP step. In the polai-~ianrnt7.de. The instrument had 14 contiguous energy-per-charge channels all three roll~ctorrmere Observedr and the peat flux obtained brtrrrn 75 and 94.55 V tor positive ions and tour and the azimuthal direction (to 2-15116 deg) of the observation en.rgy-per-charpt channels betwren 115 and 1600 V tor IC?* reported for each rollertor. In the azimuthal Scan mode. electrons. The instrument view axis MIS ~erpendicularto the the Dcak tlui abserved in the 25 azimuthal s~itorswas recorded spacecraft spin axil and parallel to the ecliptic plane. The for the central collector at each EIP step. At the IOU bit Line separating the two COILCT~O~I lay in the ecliptic plane, ratel (64. 16, and 8 bps)r the marinurn flu. mode 1.1 used at enabling a rough determination ct solar rird bulk tlcr each EIP step followed by either (1) tar ions. a polar scan and PCrDendiLULar to the ecliptic plane. During every second an azimuthal scan at that EIP step rhere the peak tlui SCaCeCratt rotetion and at one voltage level, the sum of the measurement during the marinurn tlux mode was Obtainear or (2) currents from the collectors was Obtained in 20 contigucus for clectransr a polar scan and an azimuthal scan at LIP = 100 11.25-drg angular SectO~s(1101 -45 dcg to 270 degr with 0 de9 V. In the aaximum flux iode. only the central collector was being the space~raft-~unline). The eight meas~r~mentsabout obrcrvrdr and the peak tlux obtained and the azimuthal the IUn-ealfh line (-41 dcp to e45 dcg) were tCIe.Cfered~ but direction (to 2-13116 dcg) Of the ObLCrYation Icre rrLorfed. A only the Largest meaiuremcnt in each rurreraing 45-6-9 inttrual COSplSt* 5-1 of ~~ISUIC~CI~S ranrirtcd ot reven sets of ion (45 deg to 270 deg) -as telemetered. In addition. during this meaIUrCment1 11t each El9 step> and one set 01 electron rotation the current tr0. one 01 the collrrtors was measured in measurrmrnts (at each EIP step). At the high bit rates (512 all twenty-eight 11.25-de9 sectcrlr and the largest bas and 256 bpr) one let ot ion measurelents took 62 s and one set identified and te1emetCIed (both magnitude and sector). A of ~lectronncarureltntrr 38 s. At the lor bit rates (64. 16. tOmPlCte set Of sositiwc ion measurements and one electron and 8 bpr). one set of ion rne.surerents tO~k37 I and One %el .raaUrrment were completed every 32 I. The time between each of elcctrDn measuICm~nlSr28 S. At 64 bplr a Co.lplctc Set Of 52-l group of mc~s~r~.~cntlvariea with the bit rate. The ~ea~urem~nts(seven ions plus one electron) was taken and e#periment worked r.11 from launch until it became inoperable teltmetertd rrery 402.5 s. At 16 bPs* (t took l6lD SI and. at in November 1972. For sore COIP~C~C intormationr Ice J. 8 bps, it took 5220 I. Geophys. Ues.. V. 71. PP. 3767-5791. August 1966. ------"ELI0S-A. ROSENBA"Ee------PIONEER 6, LEVY------INVESTIGAIION NAME- PLASMA DETECTORS INVESTIGATION NAME- SUPERIOR CONJUNCTION FARADAY ROlATlON NSSOC ID- 74-097A-09 INVLSllGATlVE PROGRAM NSSDC ID- 65-105A-US lNVESlIGATlVE PROGRLM CODE EL-*ICO-OP, SCIENCE CODE EL-4. SCIENCE INVESTIGATION DISCIPLINE(S) INVESTIGATION DISClPLINE(S) PARTICLES AND FIELDS HIGH ENERGT ASTROPHYSICS SPACE PLASMAS

107 PERSONNEL sampling rate of the spectrum data in this mode was 14.2 PI - H.R. ROSEN0AUER MPI-hERONOMI samples per S for elch ChDnnrl. One half of the dipole antenna 01 - H. PELLKOFER MPI-EXTRATERR PHIS failed to extend pIOpCILy and was short Cilcuited to the 01 - J.H. YOLFE NASA-ARC spacecraft ground. The resultant configuration was that of a monopole rhich 11s calculated to hare an rffective lmpth of BRIEF DESCRIPTION aoorozimatcly 8 m. The primary detriment81 effects we,* the This experiment (€1) employed three plasma analyzers fcr loss of 6 d0 in E field sensitivity due to the shortened positive ions and one for electrons. All detectors "ere antenna and the increase in the 178 LHz ch8nn-1 by 25 dB. mounted nor.al to the spin *.is. Positive ions with energy per solar cell and sheath effects caused interference in the Lo..st charge within the range 0.155 to 15.32 keVlP were me.sured in 6 channel5 (Which 1CSS Seucrr with inCrO.sing channel ti0 IngUlaI dimmrions using a ro.binrtion of a hemispherical, frequency). For nore details. see J. Gcophyl. Res., Y. 82. p. a quadrisoherical. and a sinUIoidllly Shaped el.ctr~statii 632. 1975. 8nd p- 245-247 Of RaUmf.hrffOrSchUnQ. V- 19, n. 51 analyzer. Electrons rith energy from 0.5 to 1660 cv #ere 1915. measured with a ht.isphtrica1 electrostatic aralyzer in one dimension. The experim~nt operated in several modes, .ith ------HEL1OS-B. GURNETT------differing time rriolution depending in detail on telemetry format and satellite bit rate. Tycical time rcrclvtion #as cn INVEST1GATION NAME- SOLAR UIND PLASMA YAVE the order of a minute. Also. wheneve? the special shock alar. mode ras triggpred by erprrimrntr -04 or -01. NSSDC ID- 16-OOJA-04 INVESTIGATIVE PROGRAM high-time-resolution plasma data for a pii7od before and after CODE EL-4ICO-OP. SCIENCE the event was recorded into rcarerratt m~mory for later transmission. BCCIYIC the sparerraft body 11s dielectricr INVESl1GATION DISCIPLINE(S) sheath potentials of up to 100 cv degraded the usefulness of PARTICLES AND FIELDS data taken in tPe lower electrcr-energy channels. This IONOSPHERES AND RAD10 PHISICS phenomenon 11% judged to hare minimal effects on the uicfvlncrr of the ion data. for mort detailed infor.ation see p. 226 of PERSONNEL Rauafahrtforrrhung, Y. 191 n. 5, 1915. PI - D.A. GURNETT U OF IOWA 01 - P.J. KELLOGG U OF MINNESOTA _--_---HELI0S-B. ROSENBAUER------01 - S.J. BAUER 6RAZ U 01 - 1.6. STONE NASA-6SFC INVESTIGATION NAME- PLASMA DElEClORS BRIEF DESCRIFTION NSSDC ID- 16-003Ai-09 INVESllGATlVE PROGRAM This expcrimrnt lE5a) shared the "2.r tip-to-tipr CODE EL-4ICO-OP. SCIENCE electric antenna "4th caprrimcnts -05 and -06. lhe instrument ronrirtcd of a 16-channel sotctrum enalyzrr with aporoaimately INVESTlGATION DISCIPLINEIS) logarithmically CquiSPaCed renter frequencies. 16 lop PARTICLES AND FIELDS LO~DICSSO~~~16 R-C integrators for 8vcraging the Iag-cOmprriSedr electric field amplitude between readouts. and PERSONNEL 16 peak detectors uhich Yere reset after readout. lhe 16 PI - H.R. ROSENBAUER *PI -AE RONOMI averages ana 16 peak log values were sampled almost 01 - H. PELLKOFER MPI-EXTRATERR PHlS simultaneously. The channels rovered thc frequency range of 01 - J.H. UOLFE NASA-AR C about 20 HI to 200 kHzr with four channels per decade of frequency. The log COmpreSsOrs bad a dynamic range Cf 100 d0. BRIEF DESCRIPTlON Sa.ollng rate depended in detail on the ipa~~craltbit pate and This experiment (El) employed fhrcr plasma an.lrzcrr lor teIeme11y format. The fastest real-time ttlCmetelCd cafe uas positive ions an0 one for electrons. All detectors #ere for 16 averages and 16 peak values to be sampled every 1.12s s. mounted normal to the spin axis. Positive ions rith energy e-, Yhenever a very strong signal was detected in a ~11-se1~cted charge within the range 0.155 to 15.32 kcVIP were measured in channel, the shock alarm data mode "8s initiated in rhirh the two angular dimensions using a combination Of a hemispherical, tl~ctric field sp~ctru.r magnetic field. and p1.s.. data were a quadiis~h~rical,and a rinuroidally-shaped eliitrostatic rocoided into spacecraft memory for a period atarting before analyzer. Elcctrons uith energy fro- 0.5 to 1660 eV "ere and terminating after the triggering sign81 time. The m8rimum mtai~red with a hemispherical alectrostatir analyzer in one sampling rate of the spectrum data in this mode was 14.2 dimension. The excerimtnt operated in srueral modes rith ~a.plt~ per I for each channel. Interference. caused by solar differing time 1e101ution depending in detail on telemetry cctl noise. occurred ~ri.*rily in the lorest six channels. and format and satellite bit rate. Typical time rcrolvtion "as on harmonics wre related to the spin frequency 8nd the spacecraft the order of a minute. Also. rhcnercr the special shock alarm sheath. HOI~YCI. a combination of factors. including the .=de was triggered by axcsrimentr -04 or -01. FIOD~I deployment of the dipole antenna and the COndurtivI high-ti.e-resOlutiOn plasma data for period starting before spacecraft Coating. rcsultcd in data from this spacecraft being and ending after the event "ere recorded into spacecraft .emery of higher quality than data from Helios-A. For further fcr later transmission. Because the spacearatt body was coated details, IC- pp. 245-241 of Rau.fah,tforschung. I. 19. n. 5. with a conductive coating, the sheath potentials "CIS atout 5 1915. CV. causing far less degradation in the uScfuln~ssof data taken in the loier electron energy channels than on the ------PIONEER 8, SCARF------HeIiCS-A ~pa~e~raft.and almost no affect on the ion oat*. fcr nore detailed intarnatran ICC p. 226 of Raumfahrtforirhvngr v. INVESllGATlON NAME- PLASMA WAVE DETECTOR 19. n. 5, 1975. NSSDC ID- 67-1231-07 INVESTIGATIVE PROGRAM - - __ - - - HEL1OS-A. GURNElT------CODE EL-4. SCIENCE lNVESTlGAllON NAME- SOLAR YIND PLASMA YAVE INVEST16Al10N DISCIPLINEIS) PARTICLES AN0 fIELDS NSSDC ID- 74-0911-04 INVESTIGATIVE PROGRAM CODE EL-kICO-OP, SCIENCE PERSONNEL PI - F.L. SCARF TRY SISTERS 'GROUP INYESTlGATlON DISCIPLINEIS) 01 - 1-11. GREEN TRY SYSTEMS GROUP IONOSFPERES AND RADIO PHYSICS PARTICLES AND FIELDS BRIEF DESCRIPTION Electrostatic and ekCCtI0.8glletiC p1.1.. waves were PERSONNEL measured in the solar wind near 1 AU using an unbalanced dipole PI - D.A. GURNEll U OF 1011 antenna. The 423-MHz Stanford University antenna. rhich served 01 - P.J. KELLOGG U Of MINNESOTA as the ~enscrr was capacitiv~ly coupled to three channels. 01 - S.J. BAUER bRAl U Channel 1 111 I 15 Z bandpars filter centered at k00 Hzr a 01 - R.G. STONE NAS A-GS F C typical intcrplanctary ~lectroncyclotron frequency. Channel 2 uas a 15 1 bandpass filter centered at 22 kHzr a typical BRIEF DESCRIPTION interplanetary electron plasma frequency. The broadband This erpcrinrnt IE5a) shared the 32 mr tip-to-tip channel from 100 Hz to 100 kHz was fed into a count rate meter electric antenna with czpcrimcntr -05 and -06. The instruacnt that measured the number of positive going pulrrs per unit time Conitsted 01 a 16-channel SDCctru. aralyzcr with appr~iimately having amplitudes large enough to cross the present trigger lagarithnically rquirparcd center frequenciesl 16 log level. The trigger lcrel was varied in 16 steps PCI telemetry COIDICSlOlSr 16 R-C integrators for averaging the log sequence. The trigger lrvtlr together rith the count rate at (CDcreSSed clcrtrir field amplitLaC between readouts. and 16 each level gave a leasure of the broadband ooicr sp~ctiu.. peak detectors rhirh icrc reiet after readout. The 16 averages Alm~st all of the time this measurement amounts to the powel and 16 peak log valuer were saapled almost rimultanrourly. The spectrum at near 100 Hi. At the highest telemetry rate at channels co~ccedthe frcqucncy range 01 about 20 HZ to 2OC kHz, Pioneer 8. this sequence I.. repeated cvcry 1.41 .in. uith four rhanrelr prr decade of frequency. The IC? CO~~ICSIOII had a cynam1c range of loo ds. Sampling rate ------PIONEER 9, SCARF------depended in detail on the space~raltbit rate and telemCtry fcrnat. The faltcst real-tire telemetered rate was for 16 INVESlIGAllOh NAME- ELECTRIC FIELD DETECTOR a~cragcs and 16 peak ualurs to be sampled every 1.125 I. lhenever a very strong signal was detected in a pie-sel~ct~d channel, the shock alarm data mode "as initiated in rhirh the electric field scictruir magnetic field. and plasma data "ere recorded into SpaCCclaft memory for a period starting before and terminating after the triggering signal time. The maximum

108 NSSDC ID- 68-1OOA-OT IhVESllGAlIVE PROGRAM NSSDC ID- 66-0751-03 lNVESllGATlVE PROGRAM COOE EL-4. SCIENCE CODE EL-4, SCIENCE

lNVESlIGAllON DISCIPLINE(S) lNVESTlGAlION DISCIPLINE IS I PARTICLES AND FIELDS PARTICLES AND TlELDS SPACE PLASMAS SPACE PLASMAS

PERSONNEL PERSONNEL PI - F.L. SCARF TRU SYSTEMS GROUP PI J.H. YOLFE NASA-AR C 01 - I.M. GREEN TRY SYSTEMS GROUP 01 - R.Y. SILVA TRY SYSTEMS GROUP 01 - 6.1. CROOK GAINES n. CROOK ASSOC 01 - R.Y. FREDERICKS TRY SVSlEMS GROUP BRIEF DESCRIPTION A quadrispherical electrostatic analyzer with eight BRIEF DESCRIPTION rontiguoua current collectors was used to study the directional Electrostatic and electromagnetic plasma wwes "ere intensity of the electrons and positive ions in the solar rind. reasured in the solar rind near 1 AU using an unbalanrcd Ions weir detected in 16 logarithmically Cquispaced energy per electric dipole antenna. The 423-MHI Stanford University unit charge (EIO) steps from 200 to l01000 V. There was an antenna. rhirh served as the sensorr "as capacitivrlv ~o~plcd electron mode of operation in rhich elections were measurea in to three telemetry ch8nnclr. Channel 1 "as 15 I bandpass eight logarithmically equispaced energy per charge steps filter centered at 400 HI. and charnel 2 "as a 15 1 band&asr ranging from 0 to 500 V. The eight c01l~ct0rsmea~urtd filter centered at 30 kHI. These channels were tach sampled 6q particles incident from eight different contiguous angular times per telmetry sequence. Channel 3 #as a broadband 100-HZ intervals relative to the SPICCCI.~~ equatorial plane (same as to 100-LHz channel. The broadband channel was fed into a the ecliptic plane). lhere "ere four 15-de9 intervals, tu0 count-rate meter that ne*surcd the number of FOS~tiw-gcirg 20-drg inttrvalrr and two 30-drg intervals. AI the SP.LCCI.~~ pulses per unit time having amplitudes large enough to cross uas spinning. fluxes weit measured in 15 azimuthal angular the present trigger level. The trigger level was varied sectors. Eight of the these ICC~OIS iclc 5-518 dcg wide. were through eight stecs, tight tises cer teleaetry sequinre. lhe rontiguourr and bracketed the solar direction. The remaining trigger levrisr together with the count rate at each lruel~ Seven Sectors LCIC 45 dcg wide. lhrcr different model Of data gave a measure of the broadband power IPCC~~U.. Que to ambient collection were used. At the highest bit rate (512 bps). the conditions. these data usually represented the POYC~at about full scan mode was alternated with the laxinun flux iode at 100 HI. The telemetry sequence "as 1e0e4t-d over time each EIU step, In the full scan lode. the maximum flux intervals 1.0. 7 .in 28 s to 472 min 52 s. observed in each of the 15 azimuthal sectori as the spacecraft rotated was iecorded for a given single collector at a given ____--_PIONEER 6. YQLFL------E19 step. During 24 IUCCCSIIYC operations of the full scan mode 08 fpac=cI.ft rrvOlutiOnl). the 16 ion El9 steps and INVESTIGATION NAME- ELECTROSTATIC ANALYZER eight rlcctran €19 steps were excrriscd 10, a given collector. During tight zucrsssive such periods. each Of the eight NSSOC ID- 65-105A-P6 INVESTlGAlIVE PROGRAM CalleCtOrl was exercised. The full cycle of full scan mode CODE EL-4. SCIENCE data required 400 Spa~eclaftr~~Dl~tiDnr labout 400 SI. Such cytle~were repeated without interruption at the high bit rate. INVESTIGATION DISClPLINE(S) In the nanimu. flux .ode. for the EIY step used in the PARTICLES AND FIELDS preceding revolution of full scan mode op~ration. all CQLICC~OIS Obrerrtd for onr rcrolulionr and the maxinun PERSONNEL flux observed 1.3 reported along rith the number of the PI - J.H. YOLFE NASA-ARC collrrtor that Observe0 it and the angular direction (2-13116-6.9 resolution) Of the observation. At the next BRIEF DESCRIPTION highest bit rate 1256 bpi), the short scan mode "as alternated A qUadlifphlliLa1 electrostatic an.Lyzcr with eight every splce~raft revolution rith the maxinu. flux mode. The CDntiguouS current c~lle~t~rl1as usid to study the directional short scan mode Y~Ithe same as the full scanr c~reptthat only intensity Of rlcrtrms and p~iitiirions in the solar wind. the peak flux in each Of the eight 5-518-deg-ride azimuthal Ions icrc detected in 16 l~garithmically equispaccd sectors LI.S recorded, thus, this cycle also took 400 spacetraft energy-per-charge (E19) steps fro. 200 to lO.000 v. There was rtvOlutionS. At the lor bit ratel (64. 16, and 8 bpS)r the an electron mode Of operation in which electrons were measured maximum flux mode alone was used. Thus, no azimuthal in right logaiithmically e~uispacedEIP steps ranging fro. 1 to distributions UCIC measured. At the lor bit rates. it took 32 500 V. The eight collectors mcasurrd partic1.i incident ftom I for complete Set of ion mtaSuICi%~ntS and 16 5 lor a eight differmt contiguous angular intrrvala relative to the COmPletF Set Of electron mcarureacntl. At 64 bpls the ion and spacecraft equatorial plane (sane as the ecliptic plarc). electron IeasUIemCnts were taken and telemetered every 64 I. There Mere four 15-deg intervals. ti0 20-des interwals, and ti0 At 16 bPI, they were taken and t~lemet~redewe~y 36 I. At 8 IC-dcg intervals. As the spacecraft was spinning. fluxes were bpsr they were taken and telenetered every 672 I. measured in 15 aiiruthal angular sectors. Eight of these sectors "ere 5-510 deg ride. were contiguous. and bracketed the ------PLQNEER 8, YOCFE------solar direction. The remaining seven sectors were 45 de9 ride. Three different modes of data collcrtion iert used. At the lNUESlIGATlON NAME- ELECTROSTATIC ANALYZER highest bit rate (512 bpi). the full scan mode was alternated with the narimu. flu# .ode at each EIP I~CP. In the tull stan NSSDC IO- 67-1231-02 INVESTIGATIVE PROGRAM mode, the marimurn flux observed in each of the 15 azimuth.1 COOE LL-4, SCIENCE sectors as the sp.cerr4ft rotated was recorded for 1 given single collector at a given El9 step. During 2+ sucrrsriue INVESTI6ATlON DISCIPLINE(S1 Oper*tions of the full scan mode (48 space~r~ftrcrolutions). PARTICLES AND FIELDS the 16 ion TIP Steps and eight clrctron EIP steps ltre SPACE PLASMAS exercised foc given c011ect0r. During eight ~urrcssircruth periods. each of the eight collectcrs was rrrrtisrd. The full PERSONNEL cvcle of full scan mode data rewired 400 spacecraft PI - J.H. YOLFE NASA-ARC revolutions (about 400 5). Such rvrlcr were repeated without 01 - D.D. 1CK1881N NASA-ARC irterruption at the high bit rat.- In the .a.i.um flux Ioder for the EIP step used in the preceding revolution of tull stan BRIEF DESCRIPTION lode Operationr ell COLlCLtOIS icrc Observed for one A tiuncittd hemispherical el~~trostatic.nalyrcr (120-drg IevOlUtion. and the maximum flu. ObsrrVCd "1s repoitedr along total parallel plate curvature) with three contiguous current rith the number of the r~llertcr that Observed it and the collectors was used to study the directional intensity of the angular direction (2-13116-drg resolution) of the Observation. elcrtronr and positive ions in the solar wind. Ions icrc At the next highest bit rate (256 bps). the short-scan mode was detected in 30 logarithmically eqvirparcd energy psi unit alternated every rparrtraft revolution with the m.xi.un-flux charge (EIPI StCpS from 150 to 15.000 V. There "as an electron mode. The short-scan mode was the same as the full-scan mcde, mode of Operation in which electrons were measured in I4 except that only the peak flux in each of the eight logarithmically equispaced El9 steps ranging from 12 to lo00 V. S-518-dcg-uide azimuthal Sectols "as recorded. Thus, this lheie IDS also a zero ElP. or backgroundr step. The three Cycle also took 400 IPlrCLratt r~rolutionS. At the lor bit c0111ct0rl measured partic1~1 incident 110. three different rates (64. 16. and (I bes)r the maximum flux mode alone #as contiguous angular intervals relative to the spacecraft used. Thus. no azimuthal diitributicnr ICI~ measured. At the quatorial plane (same as the ecliptic plane). 1r0 rollertors lor bit rates, it took 32 s for a complctc 1-1 of ion measuied flui from 10 to 85 dcg on either side Of the measurementi and 16 s for a rcnplctc set of elertrcn spacerraft equatorial plane. and the third measured flux in a me.SUICments. At 64 bpsr the ion and electron mcarurtmrntr 20-dcg interval centered On the spacec~aftequatOrla1 plane. "ere tbken and telsmettred t'l~fy84 S. at 16 bpsr they were AI the spac~cinft was spinning. fluxes icvc measured in 23 taken and t*lemetered every 336 I. At 8 bps. they "ere taken possible 2-1sli6-dag ride azimuthal angular sectors. seventeen and trlemetered every 612 I. of these sectors were cOntigu0~1 and bracketed the solar direction. lhc remaining si. ~ertorf"ere widely spared. The _------PIONEER 7, "OLFE------instrument had three modes of data ~~11~1tionipolar scan. azimuthal scanr and maximum flus. At the two highest bit rates INVEST1GATlON NAME- ELECTROSTATIC ANALYZER (512 and 251 bps) the polar scan mode MIS altrrnsted with the azimuthal scan mode at each EIP step. In the polar scan moat. all three collectors icrc obscrwcd, and the peak flu. obtained and the azimuthal direction It0 2-13116 dcy) Of the observation WCII re~ortedfor each collector. In the azimuthal scan node, the peak flux observed in the 23 azinuth.1 sectois ids ~ecoided for the central col~ccto~at each ZIY step. At the lor bit

109 NSSDC ID- 66-8151-01 INVESTIGATI~EPROCRAM CODE EL-4. SCIENCE

INVESTIGATION DISCIPLINE(S) PARTICLES AND FIELDS

PERSONNEL PI - N.F. NESS *A SA -6 SFC

INVESl1GATION DISCIPLINE(S) PARTICLES AND FlELDS

PERSONNEL PI - E. KEPPLER MPI-AERONOMY 01 - 8. YILKEN nPi-&ERouonY 01 - D.J. WILLIAMS NOAA-ERL

BRIEF DESCRIPTION The Oblective of the rrprrimrnt (€8) #as to study the origin and the distribution mechanism of lor-energy ~l~rtronl NSSDC ID- 61-123A-01 INVESlI6AlIVE PRO6111 and protons. The instrument. magnetic spectrometers CODE EL-4ICO-QPr SCIENCE consisted of six serirondurtor ditectcrs with the field of ricr in the plane of the ecliptic. Species separation I).% athitied INVESTIGATION DISCIPLIWE(S) by an inhomogcneoui m.gnctir field oriented perpendicular to PARlICLLS AND FIELDS thr particle path. Four electron and two proton detrctorf measured electrons from 20 tC I000 key and PrOtCnS from 80 to PERSONNEL 1coo Lev. The proton me.iurcments "eve mad. rith PI - N.F. NESS NASA-6SFC tio-defectol telescOpC C.pLOring roinridcnr. mnd 01 - S.C. CANlARANO CUR. SPACE PLASMA LAB anticeintid.nce logic. Both particle specie. lele .t.surld in 01 - F. MARIAN1 U OF ROME 16 energy rhmnels through pulse-height .nalylis. Far further information Ire pp. 261-263 of Raumfwhrttorsthung. v. 19. n. 5. 1915. ------"ELIQS-8, IEppLER------lNVESTIGAlION NAME- ENERGEllC ELECTRON AND PROTON DETECTOR

NSSDC ID- 16-0031-10 INVESllGAllVE P106RAM CODE EL-4ICO-W. SCIENCE

INVESlIGAlION DISCIPLINE(S) PARTICLES AND FIELDS

PERSONNEL PI - E. KEPPLER IIPI-AERONOMY 01 - 8. WILKEN MP1-AERONOMY 01 - D.J. YILLIAMS NOAA-ERL NSSDC IO- 68-1001-01 INVESTIGAlIVE PROGRAM BRIEF DESCRIPIION CODE EL-4s SCIENCE The objective of the experiment (Ea) was to study the origin and the distribution mechanism at lor-rncrgy clectrona lNVESTlCATION DISCIPLINE (5) and protons. lhe instrusent. I aagnetic specti~.et~rr PARTICLES AND FIELDS consisted of six se.irondurtor detectors with the field of rier in the plane of the ecliptic. Species separation 1.1 achieved PERSONNEL by an inhomogeneous magnetic field oriented DIIPCndicUIaI to PI - C.P. SONE11 U OF.AR1ZONA the partirl~path. Four tlertrcr and tu0 prcton detectcrs 01 - D.S. COLBURN NASF-ARC measured il~rtrons 1.0. 20 to ID00 Lev and protons tram 80 to 1000 Lev. The proton measurements "ere mwde with a BRIEF DESCRlPllON two-detector telescope employing Coincidence and A bOo.-mOunt.d. triixi.1 fluxgat. m.gnct0mct.l was Usid antiroincidencr Icgics. Both partrcie species usre measured in to study the interplwnctwry mIgn*tir field wnd Its 16 energy channels through pulse height analysis. for further fluctuations. lht srnsors were Orthogonwlly mounted "4th one information see pp. 261-263 of Raumtahrtforsthung. V. 19, n. 5, wsir p.r.ll*l to the spacecraft spin .ais. Upon command. 8 1915. motor fnt.rrhangrd a scnsor in the spin plan. with the smlor along the spin axlsr enabling inflight d.ter.in.tion of ZClO - - _-- - - p1ONEER 6, NESI------LIYLII. Every 24 hours. the instrument was rommwndtd into a self-~alibiat~sequence. and this usoften reprated after the INVESTIGATION NAME- UNIAXIAL FLUXGATE MAGNETOMEIER sensors urre flipped. The instrument. which had 8 dynamlr range of PIUS01 minus 200 nl rith resolution of plus or NSSDC ID- 65-105A-01 INVESllGAT1VE PROGRAM minus 0.2 nT. was Capable of inflight derodulation of the CODE EL-4. SCIENCE signals rereired fro. the two s*nsoii in the spin p1.n.. Ewrh mapnrtir field component "as digitizrd into 8 IO-bit t.lemttry INVESTIGATION DISCIPLINE(S) word. Ninr magnetic field componrntsr com~rising three PARTICLES AND FIELDS magnetic field vectors, rere transmitted in rich spacecraft te1e.etry tr*.r. PERSONNEL PI - N.F. NESS NA SA-G S F C

BRIEF DESCRIPIION INVESlIGAllON NAME- fLUKGAlE MAGNETOMETER FOR AVERAGE FIELDS A single, bCOm-.Ounted uniaxial fluxgate m*gnsto.etrlr rith a dynamic range of plus or minus 64 nl and plus or minus NSSDC IO- 14-0911-02 INVESTIGATIVE PROGRAM 0.25-nl resol~tion, obtained a complete vrrtor magnetic field CODE EL-4ICO-OP. SCIENCE .eaSYIC.C(It by means of three .eaSurCmtnts taken at equal time interrais during each space~raftsrin period (acpr~iim.tely 1 INVESllGAlION DISCIPLIWE(S) I). At telemetry bit rates lesi than or equal to 16 bus. PARTICLES AND FIELDS averages yere CO.~Y~C~on board for transmission to earth. The instrument roited well from launch to July 6, 1910. NO useful data itre obtalnec after that date. For further details. See

110

c'.4! PERSONNEL variations ct the ambient magnetic ticldr a PI - N.F. NESS NASA-GSFC shock-idrntiticitian EO.PUtCI triggered the storage of 01 - F. MARIAN1 U OF ROME rapid-rate data. in the spacecratt memory. Two measurement 01 - L.F. BURLAGA NASA-GSFC ranges #.IC used, plus or minus 100 and 400 nT with rcsolutionr 01 - S.C. CANTARANO CNRr SPACE PLASMA LAB ot plus or minus 0.2 and 0.8 nT. respectively. The instrument was e~uipped rith flipper mechanism, which re-oriented each BRIEF DESCRIPTION sensor by 90 drg periodically. For detailed information. see This e.prri.int (E3) conlilted at a boom-mounted. p. 232 at Rwmtahrtforschung. Y. 19, n. 5, 1975. triailal-tluigite magnCtOneter. An automatic intlipht range sritch system lelected the optimum of tour ranges that uece -----__PIONEER 5, GREENSTADT------ninul to plus 16. 48. 144. and 432 nl per SenSol. These had carresoonding digitization resoluticns ot minus to PLUS 0.03, lNYESlIGAlIOh NAME- SEARCH-COIL IAGNETOMETER 0.09, 0.28. and 0.84 nl. A sen so^ t1ipp.r "as actwttd every 36 h to assist ih sensor zero Lertl determination. For NSSDC ID- 60-0011-02 INVESTIGATIVE PROGRAM telemetry bit ratcs above 256 bcs. w.ctor mealurrments usre CODE EL-kr SCIENCE ..de at rates betieen 1 and 16 Per I. depending On bit rates. At lorer bit ratel. IVCI~~CI and variances rere c~mp~tedon INVESTIGATION DISCIPLINE(S) board tor transmission to earth. PARllCLES AND FIELDS

------HELIOS-0, NESS------PERSONNEL PI - E.Y. GREENSTAD1 TRY SVSTEMS GROUP INVESTIGATION NAME- FLUXGATE MAGNETOMETER FOR AVERAGE FIELDS 01 - D.L. JUDGE U OF SOUTHERN CALIF 01 - C.P. SONETT U OF ARIZONA NSSDC ID- 16-003A-02 lNVESTlGATlVE PROGRAM CODE EL-4ICO-OP, SCIENCE BRIEF DESCRIPllON This search roil magnetometti. which 11% similar to those lNVESTlGAllON DISCIPLINEIS) tlorn on Pioneer 1 and Explorer 6. was designed to study the PARTICLES AND FIELDS interplanetary magnetic tield. The detector consisted ot a ringla search coil that was mounted on the SD*CeCraft so that PERSONNEL it meas~r~dthe magnetic field per~mdi~u1.rto the spaceciaft PI - N.F. NESS NASA-GSFC spin .air. The magnetometer could measure tieldr trom 1 01 - F. MARIAN1 U OF ROME microgauss IC 12 nilligaurs. No intlight calibration was 01 - L.F. BURLAGA NASA-GS F C Provided tor. The c.pcrimcnt had both digital and analog 01 - S.C. CANTARANO CNRr SPACE PLASMA LAB Outputs. The magnetoieter amplitude and phase were sampl~d continuously tor analog transmission and intermittently (every 96, 12, and 1.5 s. depending on satellite bit rate) tor digital transmission. App~~x~mateLy2Ir000 digital readings 01 the magnetic ticld amplitude were Obtained. The last data were taken on May 6, 1960. HOUCYC~~no intOrmation was obtained on the phase angle of the tirld about the spin axis. See Colrnan, J. GeOphy*. Rei.. Y. 69. p. 3051. 1964. tor further details. ------HELI0S-A. NEUBAUER------'------

INVESTIGATION NAME- SEARCH COIL llAGNElOMETER

NSSDC ID- 74-097A-03 INVESllGATlVE PROGRAM CODE EL-4ICO-OP. SCIENCE

INVESTIGATION DISCIPLINECS) PARTICLES AND FIELDS INVESTIGATION NAME- FLUXGATE MAGNETOMETER FOR FIELD FLUCTUATIONS PERSONNEL PI - FA. NEUBAUEY u OF KOLN NSSDC ID- 74-097A-01 INVESTlGAl1VE PROGRAM 01 - 6. DEHMEL BRAUNSCHUEIG TECH U CODE EL-4ICO-OP~ SCIENCE BRIEF DESCRIPTION INVESTIGATION DISCIPLINE(S) This cxpcrimcnt (E+) "as designed to inleitigate the PARTICLES AND FIELDS iagnttic component ot electromagnetic uwes in the solar wind trom 0.3 to 1.0 AU. By naanr of its raretar. channel (YFC) the PERSONNEL rapid variations 01 the magnetic field icrc measured up from PI - F.M. NEUBAUER U OF KOLN plus or minus 8.75 nT to plus or minus 275 nT in thrcr 01 - A. MAIER BRAUNSCHYEIG TECH U Orthogonal directions from 4 to 128 Hz. A spectrum analyzcr observed the field components in the ecliptic plane and BRIEF DESCRIPTION perpendicular to it, to obtain the power spe~traldensity and The instru-ert (E2) consisted of a triaxial tluxgate peak YILYCS tor eight 1ogarith.icaLLy spaced channels in the magnetometer mounted on a 2.75-1 boo. to make magnetic field range from 4.7 to 2200 HI. BCI~USC at the large amount of data ~easurements up tC 4 Hz. Data tram each axis *ere first sent produced by this experiment, an adaptive data reduction was through a lor-pars filter with the 3 dB attenuation point at 4 applied. For interesting time intervals selected by the Hz. Dep.nding On the telemetry tor*at and bit rate. the data tlurgate nag~etomet~r114-097A-01r hCUbaUCr) or Gulnett (-04). ieit ttd either into a tilt-averaging LOmDUtCI or directly ravetorn data Could be read into an On-board memory at a repid connected to telemetry. A shock identification computer rate tO be transmitted slorly atterrards. For more detailed triggered the stcragc ot rapid-rate data in tht soacecratt intor-ation see p. 241 in ua~mfahittorschungrV. 1P. n. 5, memois "hen there were discontinuities in the variations ot the 1975. ambient magnetic field. TWO mCaSUre.ICIIt ranger IC,. Used. DLUS or minus 100 and 400 nl with resolutions ot plus or minus 0.2 ------HEL1OS-B. NEUBAUER------and 0.8 "TI rtspIctivrly. The instrumrnt was equipptd with a tlipprr mechanism, uhith rtorientsd each IC~SOI by 90 deg lNVESTlGAllON NAME- SELRCH COIL MAGNETOMETER ptriodi~.lly. FEI detailed intar-rtionr see p. 232 ot Raumtahrttorsrhungl Y. 191 n. 5, 1015. NSSDC ID- 76-DD3A-03 lNVESllGAlIVE PROGRAM CODE fL-4ICO-OP, SCIENCE ------HELfO*-B, NEUBAUEI------INVESTIGATION DISCIPLINE(S) INVEST IGATION NAME- FLUXGATE MAGNETOMETER FOR FIELD PARllCLES AND FIELDS FLUCTUAlIONS PERSONNEL NSSDC ID- 76-0034-01 INVESTIGATIVE PROGRAU PI - F.M. NEUBAUER u OF KOLN CODE EL-4ICO-OP. SCIENCE 01 - 6. DEHMEL BRAUNSCHYEIG TECH U I NVE Sl]GAT ION DISC I PL INE < 5) BRIEF DESCRIPTION PARllCLES AND FIELDS This experiment lE4) #as designed to investigate the magnetic ronyonent of Llectromagnetic waves in the solar rind PERSONNEL trom 0.3 to 1.0 AU. By means of its wi~ctorichannel 1rFC). PI - F.M. NEUBAUER U OF KOLN the rapid variations ot the magnetic tirld were measured up 01 - A. MAlER BRAUNSCHYEIG TECH U trom plus or minus 8.75 nl to plus or minus 275 nl rn theee orthogonal directions from 4 to 128 112. A SPCC~~U~analyzer BRIEF DESCRIPTION OblelvCd the tield ranpontntr in the ecliptic plane and The instrument (E2) consisted ot a triaxial Il~xqate perpendicular to it, to obtain the poiel sp~ctialdensity and magnCtometCr mounted on a 2.75-1 boom to make magnetic field peak valuer top tight logarithmically spaced channels in the measurements UP to 4 Hz. Data from each axis wcrc tirst rent ranae trOm 4.7 to 2200 HI. Because Of the large amount Ot date through a lor-pair filter with the 3 dB attenuation point at 4 produced by this experim~nt. an adaptive data reduction was HI. D~p~ndingon the telemetry format and bit rater the data applied. For interesting tine intervals selected by the were tcd either into a time-averaging co~puteror directly tluxgatt maqnCtOieter (Ncubaucr) 76-003A-01, or Gurnett (-09). connected to tele#etry. rhcn there bere dilcontirUitiel in the 1aYet0rm data Could be read into a0 Onboard IICIOIy at D rapla

111 rite to be transaittrd slorly afterwards. For more detailed NSSDC IO- 66-0751-Ob INVEST16ATIVE PRO61111 irformation IC. F. 241 in RaumfatrtfOrs~h~ngrY. 191 n. 5. CODE EL-** SCIENCE 1915. INVESTIGATION OISCIPLlNE(S) ------PIONEER 5, YINcKLER------PARTICLES AND FIELDS cosnic RAVS INVESTIGATION NAME- ION CHAMBER AND GM TUBE PERSONNEL NSSDC ID- 69-001A-03 INVESTIGATIVE PROGRAM PI - J.A. SIMPSON U OF CHICASO CODE EL-4. SCIENCE 01 - C.V. FAN U OF ARIZONA 01 - J.E. LAnponT U OF CHICADO INVESTIGATION DISCIPLINE(S1 PARTICLES AND FIELDS

PERSONNEL PI - J.R. YINCKLER U OF MINNESOTA 01 - R.L. ARNOLDV U OF NEY HAMPSHIRE 01 - R.A. HOFFMAN NASA-GSFC

BRIEF DESCRIPTION This rxperi.ent consisted cf a Nther-type integrating ionization chamber and an Anton 502 Geiger counter. The Geiger counter "as mounted normal to the spacecraft spin axis. Due to the romple.. nonuniform shielding of the detectolsr the ion chamber responded q~.li-~.nidil=(ticn.lly to prOtOnS prcater than about 25 MeV while the 6.19.1 counter responded gu.ii-o.nidir~ltion.lLy to plot~nsgreatti than about 35 MeV. Energy thresholds for uuari-~.nidir~rtionil responses to INvESTI6ATION NAME- COSMIC-RAY GRADIENT DETECTOR electrons were ap~roximately 1.6 and 2.9 Me1 for the ion chamber and Geiger counter. respecti~*eLy. Counts fro. the NSSDC ID- 67-123A-06 INVESTIGATIVE PRO6RAM Gcipcr countel and CYLSLS from the ion chamber were accumulated CODE EL-), SCIENCE in sepacate registers and trlcmctercd by both analog and digital ryrteal. The experiment p*rtcrmrd normally fro. launch INVESTIGATION DISCIPLINE(S1 through nay 17. 1960. Telemetry noire Limited the timespan of PARTICLES AND FIELDS useful data to the period from la~nchthrough April 29. 1960. COSMIC RAVS

-_____-PIONEER 5, sInpsQN--'------'------PERSONNEL PI - Y.R. YEBBER U OF NEW HAMPSHIRE INVESTIGATION NAME- PROPORlIONAL COUNTER TELESCOPE BRIEF DESCRlPTlON NSSDC ID- 60-001A-01 INVESTlGAIlVE PROGRAM This experiment utiliicd 1 tcLcscopc comprised Of fire CODE EL-4, SCIENCE solid-state sensorsr a CerInCov dcteCtOrr and an anticoincidence shield. The telescope axis I.. pc~pindicular INVESTIGATION DISCIPLINE(S1 to the Soarccraft Spin asis. As determined by two roinridcnrc MAGNEIOSPHERIC PHVSICS .Odes and el~rtronlo dirrrimination Of *ensor output pulsrsr PARTICLES AND FIELDS particles measured icrc CICL~IO~Iin three centiguous energy intervals bctrrcn 0.34 and 8.4 MeV, protons in si. contiguous PBRSONNEL energy intervals betieen 5.49 and 64.3 MeV (one of fine count PI - J .A. SIMPSON U OF CHICAGO cites "ai due to the sum of counts in tu0 nonrontigueus energy 01 - C.Y. FAN U OF ARIIONA intrrr.ls)r and alpha 01rticlei in tour cOnti9uOus energy 01 - P. MEIER U OF CHICAGO intrrrall betiren 6.64 and 64.1 McVlnuClron (one of three count rates was due to the sum of counts in two noncontiguous energy BRIEF DESCRIPTION intervalsl. A third coincidence mode measured the sum of A triple coincidence amnidirertional proportional counter counts due to cLect10Ds above 0.6 MeV and nuclei above 14 telescope "as used to obscrvc terrestrial trapped radiation and Mwlnurl*on. A fourth coincidence *Ode measured the sum of solar particles IprOtOnl E)75 MeV# electrons E)13 MeV). nuclei above 42 Mevlnurleon and electrons above 5.1 MeV. Me.sui~itnts obtained for about 2 months during which a Sp.cecraft spin-intcglatcd dirertion.1 fluzcs were measured in reek of quiescent magnetic field conditions follorcd by two the v~iious modes. Arcu.ulation times and reidout interr.ls geomagnetic storms closcly spaced in time occurred. The date itre dependent on the tClCwCtP). bit rate and icce typirally in of trrnamirrion cf the tart usetcl informaticn was May 16. tens of seconds. In all castir they WC~Clonger than the 1960. rpactrraft Spin period. At 101 tclc.etry bit rates .CCumuIator Saturation rendered Sole COunting moddl to be Of no value. For -______PIONEER 6, PIMPSON------further details. SCC J. GcOphyS. ICs.. Yr 16. p. 1605. 1971.

INVESTIGATION NAME- COSI11C-RAY TELESCOPE ______PIONEER 6, MCCRACKEN------

NSSDC ID- 65-1051-03 INVESTlGATlVE PROGRAM 1NVEST16AT1ON NAME- COSMIC-RAY ANISOTROPV CODE EL-+. SCIENCE NSSDC ID- 65-1051-05 lNVESTIGATIVE PROGRAM lNVESTIGATlON DISCIPLINE(S1 CODE EL-4ICO-OP. SCIENCE PARTICLES AND FIELDS cosnic RAYS INVESTIGATION DISC1PLlNE(Sl PARTICLES AND TIELDS PERSONNEL COSMIC RAVS PI - J.A. SIMPSON U OF CHICAGO 01 - I.E. LAMPORT U OF CHICAGO FERSOUNEL PI - K.G. IlCCRACKEN CSlRO BRIEF DESCRIPTION 01 - Y.C. BARTLEI DOE HEADQUARTERS This crperimcnr used a ch4rged-partitlc telescope 01 - U.R. RAO ISRO SATELLIIE CENTER comp~itd of four silicon solid-state detectors to stuay the anisotropy and fluctuations of IOlaI protons and alvh. BRIEF DESCRIPTION particles. lhe proton energy ranges sampled were 0.6 to 13.9 This c.Dtrimcnt was designed pri..iily to aeasure the MeV. 13.9 to 73.2 MeV. 73.2 to 115 MeV, and €)IT5 MeV. The directional rhararterirtics of galactic and solar cosmic-ray alpha particle energy range1 saIplCd "ere 2.4 to 55.6 MCV. 55.6 fluxes. The particle detector was a CsI (TI) srintillator to 293 Mcv, and E1294 MeV. The time resolution ranged from crystal that was set into an anticoincidence plastic atout one .IC~SUIC#~~~PCI 0.4 f to atout one 1~81urement per 28 scinti Llator collimator CUP. Separate photomultiplier tubes I depending on the tCle.Ctry bit rat?. The detector was riered the tu0 scintillators. Pulsc~ fro. the CII crystal mounted 10 that it made a 36D-dcg Scan in the eCliptiC plane unicco.panied by PULICI 1.0. the plastic srintiLl.tor WIC about once PCI I. Pulse-height analySiS Of detector Dl DUtDUt sorted by. a three-rindor pulse-height analyzer. the windous (128 channel) aOd D3 Output (32 charnel) "as 1~COlpliShed101 rorrcsp~ndlng to cncrgy depositions Of 7.4 to 44.0, 44.0 to tne last event prior to each telcmrtry readout for the 77.1. and 123.8 to 303.8 MeV. Counts in the two louer energy experiment. For further details. see Fan et at., J. Geophys. rindorr were due mainly to protons with the rindor enerpirrr Res.. Y. 73. P. 1555r 1966. while only particles of 1 greater than or equal to 2 contributed to the highest energy rindor count rate. (Protons ______7, SIMPSON------"------above 90 MeV gave anticoincidence pulscs.1 FOI each energy .indor# counts were separately arcumul.ted in each of four INVESTIGATION NAME- COSMIC-RkY TELESCOPE angular sectcrs as the s~8c.c~ift spun. Each angular sector lis normally 89.5 deg in width, with the sun in the middle of One sector. HOICYCI, when 1aIgC fluxes icic entounteredr each angular seitol was reduced to 11.2 dcg. with the sun near the midpoint between ti0 sectors. A spin-integrated (isotropic) mode. in uhich all particlei depositing 1.4 MeV in the csl ~iystal(no anticoinridenrc tequircaentl itre counted. "ifalso Used. Accumulation timer for each at the 12 directional lodes

112 and for the omnidirectional aode varied betiein 14 s and 112 s (sDac.Claft spin period ear about 1 s) depending on the t~lemetrybit rate. Set Bartley et s1.r Rev. Sci. Instrum., Y. 38. p. 266. 1961. for a more detailea experiment description. ------PIONEER 7, MCCRACIEN------

lNVESTlGAlION NAME- COSMIC-RAY ANISOTROPY lNVESTIGATION DISCIPLlNE(S1 PARTICLES AND FIELDS NSSDC ID- 66-015A-05 INVESTlGAllVE PROGRAM COSMlC RAVS CODE EL-4. SCIENCE PERSONNEL INVESTIGATION DISCIPLINELS) PI - Y.R. UEBBER U Of NEY HAMPSHIRE PARTICLES AND FIELDS COSUIC RAYS BRIEi DESCRIPTION This cxpcri.cnt utilized a telescope comprised of five PERSONNEL solid-state sensors. a Cerenkov detector. and an PI - K.G. MCCRACKEN CSIRO anticoincidence shield. The tel~~copeaxis was p*rprnaicular 01 - U.C. BARTLEY DOE HEADOUARTERS to the acecr craft spin axis. As determined by two coincidence 01 - U.R. 110 lSR0 SATELLITE CENTER node1 and electronic discriaination of scnsoi Output DULSCII Eartitles measured were rlectrons in three contiguour energy BRIEF DESCRIPTION intervals brt.cen 0.34 and 8.4 MeV, protons in six contiguous This experiment was delipned primarily to measure the energy intervals betreen 3.49 and 64.3 MeV (one of five count dirrrtional characteristics of galactic and solar cosmic ray rates was due to the sum of counts in two noncontig~o~senergy fluxes. The particle deterto, 111s Csl (11) scintillator intervals)# and alpha partirlcr in four contiguous ent~gy crystal that was set inta an antiCOinCidtnCI plastic intervals bCtrccn 6.64 and 64.1 MeYlnuClcOn (one Of three count rcintillator colli.ator CUP. Sep.r.1~ photomultiplier tubes rates "as due to the sum of counts in two noncontiguous energy viewed the two scintillatorr. Pulses from the Csl ~ryrt.1 that intervals). A third caincidcnre mode IC~IUIC~ the sum of lele not accosparieo by pulses frC* the plastic scintillator counts due to electrons above 0.6 MeV and nuclei above 14 were sorted by a three-*indow wlse-height analyirrr the MeVlnucleOn. A fourth roinridcnrr made Irarurcd the sum of rindorr Corresponding to energy depo~itionsof 7.2 to 47.4, nuclei above 42 MLVInutlcOn and electrons above 5.1 MeV. 41.4 to 64.5- and 64.5 10 81.2 MeV. No DOIitiYC IpCcieS Spacecraft spin-integrated directional fluxes rere measured in identification was ..as. although most of the counts in each the various modes. Artunul.tion timer and readout interval5 rindor *ere usually due to protons iith the rindor energies. Yere dependent on the telemetry bit rate and were typi~allyin For each CnCIgy windo.. counts **IC s~paratelyacruaul.tcd in tens of seconds. In all carer, they icrc longer than the each of four argLlar sectors as the roarerratt spun. Each spacecraft spin period. At Lou tetemetiy bit rates accumulator angular sector "ai norially 89.5 deg in width, iith the run saturation IerdCrCa some counting lades to be 01 no value. For either near a sector boundary or in the middle Of a ~ector. further details, See J. Grophys. Res.. Y. 16, p. 1605, 1971. depending on the operating mode. However. "hen large fluxes itre encounteredr each angular ILltcr was reduced to 11.2 degr ------FICNEER 9, uEBBER------rith the sun *ithe, in a sector 0. near the midpoint brtrern tu0 sectoil. A rpin-integrated (isotropic) iode, in which all 1NVESTIGATlON NAME- COSMIC-RAY GRADIENl pirti~les depositing 1.2 UeV in the Csl crystal (no a~tiroincidenc. rea~irrmrnt) were counted. was also UICO. NSSDC IB- 68-1001-06 INVESlI6AlIVE PROGRAM Accu.ulation times for each Of the 12 directional modes and for CODE EL-4, SCIENCE the 0.nidirectional mode varies betieen 14 and 112 I (spac.Craft spin period "as about 1 I) depending on the INVESlIGAllON DISCIPLINElS) telmetry bit rate. See Bartley et a1.e Rev. Sci. 1nrtrur.s Y. PARTICLES AND FIELDS 38, p. 266. 1961, for a more detailed enperimrnt description. COSMlC RAYS

__-____PIONEER 9, M(CRA(IEN------.------PERSONNEL PI - Y.R. YEBBER U Of NEY HAMPSHIRE INVESTIGATlON NAME- COSMlC-RAY ANISOTROPY BRlEi DESCRlPllON NSSOC ID- 68-1001-05 1NYESllCAlIYE PROGRAI This twerimsnt utilized s telcsropc CO~P~~SC~of five CODE EL-4ICO-OP. SCIENCE Solid-State ICnlOrSr a Cerenkov dCtertoPr and an anticoincidence shield. The teles~op~axis *as perpendicular lNVESllGAlION DISCIPLINE(S) to the spacecraft spin axis. 1%determined by two roinridrnre PARTICLES AND ilELDS modes and electronic discrimination of sensor output pulrrrr COSUlC RAYS particles measured rere (1) electrons in three contiguous energy intervals beticen 0.31 and 5.1 MeV- (2) protons in five PERSONNEL contiguous energy intervals brtrcrn 2.2 and 42 MeV, and (3) PI - K-G. MCCRACKEN CSIRO alpha particles in contiguous energy intervals between 5.b and 01 - U.R. 110 ISRO SATELLllE CENTER 42 McVlnurleon. A third coincidence mode rneasur~dthe sum of 01 - Y.C. BARTLEY DOE HEADOUARTERS counts due to rlcctronr above 0.6 MeV and nuclei above 14 Mcvlnutleon. A fourth coincidence mode measured the sum of BRlEF DESCRlPIlON nuclei above 42 MeVlnuclron and rlcctranr above 5.1 MeV. This ex~crinentconsisted of a CII rrintillator and three SplCcClaft %bin-integrated directional fluxes bere mca~uredin solid-state telesco&er. The Csl scirtillator "1% ~ollimitedby the various modes. Accumulation tines and readout intervals an anticoincidence plastic ~cintillator and had a conical "ere dcpendert on the telemetry bit rate and were typically in aperture rith a 38.2-deg half-angle. The rrintillatar look tens of seccnds. In all carer, they icrc longer than the direction was centered in the ecliptic plane. Thrrt rpacrrratt Spin period. solid-state dctettcrs "ere oricntsa in a fan arrangement rith rcscLct to a fourth ~olid-statedefecforr such that each Of the ------"EL[OS-A, TRAINOR------first three dCtCctOrs formed a telescope rith the fourth aetector. Each of the three tilescopes thus formed had an 1NYESlIGATIOh NAME- GALACTIC AND SOLIR COSMIC RAYS acc~ptanc~cone of 23-6-9 half-angle. The mean v~ering directions of the telc~copcsYere in the ecliptic plane and 48 NSSDC io- i4-09i~-oa lNVEST1GA7lVE PRO6RAM deg above and below that planer respectively. TWO con~u~rent CODE EL-4ICO-OP. SCIENCE mCder of counting ULIC cm~loyed. In the first ~OOCI counts illC arCu.ul.tcd in eight separate 45-dtg intervals during the INVESl1GAlION DISCIPLINE(S) spacecraft spin. while. in the second, rpin-integrated counts COSUlC RAYS I~IC acquired. In the first mode. the scintillator separately PARTICLES AND FIELOS IC~SYIC~ particles bith energies in the ranges 1.4 to 21.5 MeVlnurlcon and 19.1 to 63.0 MIVlnYclcOn (no sprcicr PERSONNEL disclilination) while each solid-state ~~LCICOPC s~parately PI - J.H. TRAINOR NASA -GSit mrarured protons ir the energy ranges 3.3 to 3.6 MeV and 3.6 to 01 - E.C. ROELOF APPLIED PnvsIcs LAB 6.1 MeV. In the scrand mode, the scintilletor ScparatelY 01 - B.J. TEEGARDEN NASA-GSFC measured particles in si, contiguous energy intervals betieen 01 - F.U. UCDONALD NASA -65 i C 4.5 and 40 Mrvlnurlron (interval Lower limits at 4.5. 1-01 9.6, 01 - K.G. MCCRACKEN CSIHO 13, 21, and 28 MtV1nutleon)r while each Of the solid-state telescopes separately measured p.otans in the energy ranges 1 BRIEF DESCRIPTION to 81 1 to 5, 1 to 3, and 4 to 6 MeV. and alpha particles in The detector coapltncnt of this experiment (El) consisted the energy range 4 to 8 MeV. During each 224-bit main cf three se~arate delta Eldelta x YS E tCLesCOpCI and a telemetry frame, tu0 firrt-mode 9-bit arrumulatorr and One proportional counter for monitoring solar I-rays in the ranqe recond-.od~ 9-bit acc~m~lal~r"ere read out. lnflight 2-8 kcV. The high-energy telescope had a geometric factor of calibration of the scintillator ana cf some of the ClectiOniCs 0.22 Iq cm-Ir and mCaIuICd clcctrans in three ranger between 2 was performed daily. See Bukata et 11, IEEE lranf. NUL. Sci., and 8 MeV, and PrOtOnl and alpha PartitlCI in three ranges ~~-11.PO. 18-24, 19~0. for a nore detailed experiment between 20 and 56 NeVln. Plotens above 230 MeV are also description. measured. The first Lou-energy teltscOpe (g*onctric factor vas 0.155 59 cm-sr) measured protons and I >1 particles in three ranger betreen 3 and 21 MeVln. The second low-energy tclerrope (geometric fartor 111 0.015 14 cm-sr) measured protons in rcrrral ranges betreen 0.12 and 2.1 Rev, alpha particles in the

113

881GlMAL PAGE IS OF POOR QUALITY ranges 0.6-2.1 and (-21.2 nevIn. and electrons in four ranges PERSONNEL betreen 0.12 and 2 MeV. For ruwber Of coincidence .Odesr PI - H. KUNOY U OF KIEL counting-rate data sect0,ed into tight 45-de9 sectors "ere 01 - G.H. UIBBERENI U OF KIEL obtained. The aata cycle time was dependent on the spacecraft 01 - 6. GREEN U OF KIEL telemetry rate lrariable betreen 4096 and 8 bitsls) and format. 01 - n.I- IIIFCLER-MELLIN~~ELLE~-~ELLIN U OF KIEL Under optimum conditions. tire events PCI second wri 01I - 1. YlTTE..IE U OF KlEL DULse-ht~ght analyzes and the rate data cycle was of the order 01 - H. HEMPE.E U OF KIEL of 5 .in. At the slorest combination of bit rate and format, a complete data cycle required about 2.5 h. See IEEE Trans. en BRIEf DESCRIPTION NUL. Sci., NS-22, 0. 570. 1975, and Rau.f.hrtforsthungr 1. 19. The objective of the experiment (€6) Was to Stud7 n. 5. Pp. 258-2601 1975. for further details. high-eneegyr charped. coamic-ray articles of solar. planetary, and a*l.ctic orlQin in int*rplanetarv soace. Protons and alpha ------HELI0S-B. TRAINOR------Carticlei rith en*rgirs D1.3 MrVlnurlron. and el.ctrons >0.3 MeV were measured within int.rpl.net..y space over the range INVESTIGATION NAME- SALACTIC AND SOLAR COSMIC RAYS fro. 0.3 to 1.0 AU. The instrument. a particle telescope with 5s-dcg field of view. consisted of fire semiconductor NSSDC ID- 76-0031-OB INVESIlGATIVE PROGRAM dCtectOrl. one sapphire Cerenkov counter. and one scintillation CODE EL-4ICO-OP. SCIENCE counter. all enclosed by an 8nticoinridrnc* cylinder. The telescope 1.5 calibrated prior to launch using radioactive INYESTIGATION DISCIPLINE(SI COUIC*S. p.rticle ~ccelcrators. 4nd gmund-iev.l muons. It PARTICLES AND flELDS measwed protons and aloha PartiCLeI in six channels 11.3-3.3. cosnic RAYS 3-3-13, 13-21, 21-31. 37-45. and ~45Mcvlnuclrnn) and elrctrons in tire energy channels (0.3-0.8. 0.8-21 2-1. 3-4. and >4 MeV). PERSONNEL For more details aee PO. 253-2S7 of Raumfmhrttorschuns. v. 19. PI - J.H. TRAINOR NASA-GSFC n. 5, 1975. 01 - E.C. ROELOF APPLIED PHYSICS LAB 01 - B.J. TEEGARDEN NASA-6 SFC 01 - 6.0. ~CDONALD NASA-GS FC 01 - K.G. MCCRACKEN csrao RADIO SCIENCE AND CELESTIAL MECNANICS

BRIEF DESCRIPTION The detector roepicmrnt of this experiment (€1) consisted of three separate delta Eldelta x VI E tclescopeI and piop~rti~nilcounter for monitoring solar I rays in the range 2-8 ktY. The high-energy telescoce haa a gtometric factor of 1NVEST1GAT1ON HARE- CELESTIAL MECHANICS 0.22 so cm-sr and aeasured +lrctronr in three ranges betreen 2 and 8 MeV. and yrotons and alpha particl~~in three ranges NSSPC ID- 65-105A-01 INVESTISATIVE PROSRAM between 20 and 56 MCVln. Protons above 230 MeV we,. also CODE EL-4. SCIENCE measured. The first lor-energy telescope lgrometric factor 11s 0.155 Iq cm-sc) ~C~SYIC~protons and I >I particles in three INVESTIGATION DlSClPLlNE (I) ranges between 3 and 21 McVln. The second lor-energy tllClCDpC CELESTIAL MECHANICS lgecmetiic factor was 0.015 19 cm-sr) mcasurrd PlDtOnf in several ranger bCtleCn 0.12 and 2.1 MeV, alpha particlcl in the PERSONNEL ranges 0.6-2.1 and 6-21.2 McVInr and slrCtrOnr in four vangel PI - J.D. ANDERSON NASA-JPL betreen 0.12 and 2 MeV. For 1 number Of coincidence .Odes, counting data SectCrCd into eight 45-dcg sectoii ..re Obtained. BRIEF DESCRIPTION The data cycle tire -11 dependent On the Sparrcraft telemetry The eurpose of this tzperimrnt "as IO use the tracking lvariable between 4196 and U bitsls) and format. Under 0pti.U. data tram the mission to obtain primary detrrmlnatians of the conditions. five events per I are cblse-height analyzed and the wassrs of the earth and moon. the astronomical unit. and the rate data ryclr .as on the ordcc of 5 .in. At the sloiest oscillating elemrnts of the orbit of the eapth- This was ro.bination Of Dit rate and fOl*atr COmpletC data cycle appraprlatc berDuse Of the absence of midcourse o~bit rcqui~cd about 2.5 h. For further c~tailsICC IEEL Trans. on Cotrections and near-planetary cnrounters. Also, solar NU'. Sti.. 18-22. P- 510, 1915. and PO. 258-260 Of radiation P~C~IUIC effects were small. The ~x~erimentused the Raulfahrtfoiichungr V. 19. n. 5, 1915. onboard receiver and transmitter equipment in conjunction rith Deeo Spire Network station equipment to obtain Doppl~i -_----- nEL1oS-A. Iu*oy------.e.s"re.e"tl.

INVESTIGATION NAME- COSMIC-RAY PARTICLES - - _--- - p]ONEER 6, ESnLEIIA"------

NSSDC ID- 74-C97A-07 INVESllGITIVE PROGRAM INVESTISATION NAME- TWO-FREPUENCV BEACON RECEIVER CODE EL-41CO-OPI SCIENCE NSSDC ID- 65-105A-04 INVESTIGATIVE PROSRAM INVESTIGATION DISCIPLINE(S) CODE EL-4. SCIENCE PARTICLES AND FIELDS COSMIC RAVS INVESTIGATION DISCIPLINE(S) IONOSPHERES AND RADIO PHlSlCS PfRSONNEL PARTICLES AND FIELDS PI - H. KUNOU U OF KIEL 01 - G.H. UIBBERENZ U Of KIEL FERSONNEL 01 - 6. GREEN U OF KIEL PI - V.R. ESHLEMAN STANFORD U 01 - M. MUELLER-IELLIN U OF KlfL 01 - 1.1. CROFT SRI INTERNATIONAL 01 - M. UlTIE U OF KIEL 01 - R.L. LEADABRAND SR1 1NTERNAIlONAL 01 - H. HEMPE U Of KIEL 01 - O.K. GIRRlOTl NASA-JSC 01 - A.M. PETERSON STANFORDu BYIEF DESCRIPTION The objertiur of the ezperi.ent (€6) .as to study eiiEr DESCRIFTION Both 423.3-MHI and its 2117 subharmonic 49.8-nHz signals icIe transmitted fro. 46-. Steerable parabolic antenna at Stanford Unirsrsity to the tio-fre~uency radio receiver on the rpacrcr.ft. The high-frCQuency signal served as a reference signal sinre its propagation ti.c "1% not app~eriably lengthened by clcctrons alonp the path. The low-freq~~ncy signal was delayed in proportion to the total electron content in the prOpag.tiOn path. On the spacecraftr ohase-locked receiver counted the beat frcquenry zero crossings of the received signals to obtain .easurements of phasc-path diffrrenrrs. Differential delay of the group velocity 1.5 also observed, and these u.lu=s icre telenetered to the ground station. Frc. calculated total electron content ralucs. the ionospheric effect lup to s.ltcted altitude obtained from other t.pcrimantal techniques) could be subtracted to produce data describing the intrrplanetary electron content of the solar rind ana its variations. For similar experiments covering othrr time oeriods see 68-1OOA-03r 61-123A-03. INVESTIGATION NAME- COSMIC-RAY PARTICLES 66-0151-04. and 61-0601-02. More detailrd descrlptionf of the experiment can be found in 1. Geophys. Ira.. 1. 71. DD. NSSDC ID- 16-0031-01 INVE STIGAlIVf PROGRAM 3325-3521. and in Radio SCi.. 1. 6, OD. 55-63. CODE EL-4ICO-OP~ SCIENCE

INVESIIGAIION DISCIPLINEIS) PARIICLES AND FIELDS COSMIC RAVS

114 BRIEF DESCRlPTlOh Both 423.3-MHz and its 2117 subharmonic 49.0-MHZ signals YIlC tr*nSnitttd from a 4.6-m rtcerablc parabolic antenna at Stanford University to the tro-frrqurncy radio receiver On the NSSDC ID- 66-0751-04 INVESllGATIVE'PROGRAI ~pa~eciaft. The high-frequency signal served as a ieferen~e CODE EL-4. SCIENCE signal, since its propagation time was not appreciably delayed. The 101-frcquency signal vas delayed ~n piop~rti~n10 the total INVESTIGATION DISCIPLINE(S) cLec1ron content in the piopagation path. On the sDDctciaftr a IONOSPHERES phaIL-LOckCd receiver counted the beat frequency zero crollings PARTICLES AND FIELDS of the received signals to obtain ncasurencnts of Phalc-Path diffcrrnccr. Differential delay of the group velocity was also PERSONNEL obscrvcd. ana these values were te~ernet~redto the ground PI - V.R. ESHLERAN STANFORD U station and used 10 calc~Latcthe total election content- The 01 - T.A. CROFT SRI lNTERNATlONA1 ionarphcrir contribution IYP10 a selected altitude obtained from other c~perimrntal techniques) could be subtracted to BRIEF DESCRIPllON produce data describing the interplanetary ele~troncontent 01 Both 423.3-PHZ and its 2/17 subharmonic 49.8-MHz riqnals the solar rind and 11s variations. nore detailed delCrlptlOns "ere transmitted from a 4.6-m steerable paraboli~antenna st Of the experiment can be found in J. GCOPhyI. Res., Y. 11. pp. Stanford University to the two-frequency radio receiver on the 3325-3327, and in Radio Sti., Y. 6, pp. 55-63. spacecraft. The high-frequency signal served as 1 referenre signal since its propagation time was not appre~i.bly delayed. -_----- HELIOS-A, '"RNETl------The Lor-frequency signal was delayed in p10p0ition to the total electron content in the plopagafion path. On the rparccraft~a INVESlIGATIOh NAME- FIkE FRLPUENCY. COARSE TIME RESOLUTION phase locked receiver counted the beat frequency Zero crorrlngr SPECTRUM ANALYSIS Of the received signals IO obtain mCaIUICmCnts Of pharr-path differences. Differential delay of the qroup velocity was also NSSDC 10- 74-OP7A-05 INVESTl6ATIVE PROGRAM otrervcd, and these values "ere tele.etCICd to the grcunc CODE EL-~ICO-OPI SCIENCE station. From ralculatcd total electron content iilucsI the ionospheric effect IUD to a ~el~ctedaltitude obtained trow INVESTIGATION DISCIPLINE(S) other cxptrinental techniques) was subtracted to DlOdUcC data IONOSPHERES AND RADIO PHYSICS describing the intcrplanctary electron content of the solar PARTICLES AND FIELDS rind and it5 variations. The .%prriaent Operated no.in.lLy iron Launch to May 20, 1969. For similar eapcrimrntr covering PERSONNEL other time periods. See 68-1001-03. 67-123A-03, 65-1051-04. and PI - D.A. GURNETT U OF IOYA 61-0601-02. More detailed aescr(ctionr of the exp~iimtrtcar 01 - P.J. KELLOGLI U OF MINNESOTA be found in J. GCODhYS. RtS., Y. 11. p. 3325-3321. 1966, and in 01 - S.J. BAUER GRAl U Radio SLi.0 Y. 6. p. 55-63. 1911. 01 - R.G. STONE NASA-(.SFC ------PIONEER 8, fSHLEMAN------LlRlEf DESCRlFTlON This e~periment (E5b) share0 the 32 mr tip-to-tip. INVESTIGATlON NAUE- TYO-FREQUENCY BEACON RECEIUZR electric dipole antenna with e~~~rirnents-04 and -06. InstrYmcntation consisted Of three tunable plasma ~avc NSSDC ID- 67-1231-03 INVESllGlllVE PROGRAR receivers. I fi%rd-frrqurncy rideband receiver, and a ravetorn CODE EL-.. SCIENCE sawl~r. The tunable rcrciverr and rideband receiver provided data 10, airert trlcnrtry IO earth. Each of the tunable INVESTlGCTION DISCIPLINE(S) receivers Covered a different frequency band in the range 1 Hz IONOSPHERES AND RADIO Pnvsics to 200 kHz. The high-frequency receiver had 96 frequency PLANETARY ATMOSPHERES settings rcearated by about 4 1, and CQII~C~ the frcqurnry PARTICLES AND FIELDS range 6.4 tHI 10 205 kHz. The mid-range rcrcivrr had 48 lNTE#FLANElARY DUST frrqucnry stttings separated by about 6 2, ana covered the range 208 Hz to 6.01 kHz. The lor-fieqUency receiver had 24 PERSONNEL rtttingr uith 15 I ~eparati~nrand covered the range 11 H1 to PI - U.R. ESHLEUAh STANFORD U 309 HI. The response tine of the low-frrqucnry receiver was 01 - T.A. CROFT SI1 INTERNATIONAL apProiimately 1 I, ncrerritatinq the inclusion of the rideband 01 - n.1. HOYARD .Cl.US"P0...... I,. rcccivcr to Obtain infarnation about the angular diltributim 01 - 0.L. LEADABRAND SRI lNTERNATlONAL of illwef appearing in the low-frequency band. This ~CCCIV~~ 01 - R.A. LONG SR1 INTERNATIONAL covered the IreQucncy range 1 HI to 200 Hz. The t~me 01 - A.M. PETERSON STANFORD U rrsaluticn depended in detail on the ~pa~ctrafttelemetry fornafr bit rates ana experiment operational mode. uhcn the BRIEF DESCRIPTION shock alarm mode became activated. data from the ~aveform Both 423.3-UHz and its 2/11 rutharronir 49.8-MHz signals sampler rere read into spac~craftmemory for a period startrng iClC transmitted from a 46-n rtcerablc parabolic antenna at before and ending after the triggertng event. In this nodcr Stanford University to the two-frrguency radio receiver on thr the instantaneous voltage across the antenna #as parsed through r~arrrraft. The high-frcqucnty IisnaL Served 8% a reference a IOW-PaSS f1lttr rith Cornel tIcqucnCy dcprnaent on the signal since its DlOpagafion time was not appreciably dtleytd. SallPllng rater and measured at discrete intervals, the most The lor-frequency signal "as delayed in proportion 10 the total rapid being 2.2 IS. One halt of the electric dipole fa7Lea IO clcCtCDn tontent in the PCOPagatiOn path. On the IP.CCFlaftr a deploy properly, and became short-circuited IDground. The PhaIC-lOCkCd receiver counted the beat flcquency Zero rrarrirpr resulting configuration was that of a monopoLc with an of the received signals to obtarn ~C~IUIC~CII~Iof pha~e-path operational effrctiue length of about 8 I. This rtrultcd in a differences. Differential delay of the (~~OUOv11ecity "as elso 6-dB tori in Sensitivityr and an increased receiver noire Otlervcdr and these values wcrc tclc.etcrrd to the ground levels part?cularly at lor frequencies- In additions the station. From calculated total electron contert YIIUCI.the high-gain telemetry antenna ~ioduccdadditional intrrftrcnrr- ionospheric effect (UP to a s~lecfedaltitude obtained from FOP a more detailed discussion. scc p. 248 of other cxperiicntal techniques) could bc subtracted to pr~d~~cRaumfahrtfoischung~ V. 19, n. 5, 1975. deta describing the interplanetary ~Lectron content cf fhr solar eind and 11s wariafioni. For s*niLar ~~p~~?rntnts------HELIOS-B, GURNETT------covering other tire peliodlr see 68-1001-03, 66-0151-011 65-105A-04, and 61-0601-02. A more detailed description at the INVESTI(.ATION NAME- FINE FREPUENCVr COARSE TIME RESOLUTION experiment can be found in J. Geochys. Res.. Y- 11, c. SPECTRUM ANALYSIS 3325-3121, and in Radio Sti., Y. 6, p. 55-63. NSSDC ID- 76-003L-05 INVESllGAllVL PROGRAM - - ---_- PIONEER 9, ESHLEMAN------CODE EL-~ICO-OPI SCIENCE

INVESTlGATlON NAME- 1YO-FREPUENCY BEACON RECEIVER INVESTIGATION DISCIPLINE(S1 PARTICLES AND FIELDS NSSDC ID- 68-1001-03 INVESTlGATIVE PROGRAM IONOSPHERES AND RADIO Pnysics CODE EL-4r SCIENCE PERSONNEL INVESllGLTlON DISCIPLINE(S1 PI - D.1. GURNETT U OF IOUA PARllCLES AND FIELDS 01 - P.J. KELLOGG U OF MINNESOTA IONOSPHERES AND RADIO PHYSICS 01 - S.J. BAUER GRAZ U 01 - R.G. STONE NASR-GSf C PERSONNEL PI - V.R. ESHLEMAN STANFORD U BRIEF DESCRIPTION 01 - 1.A. CROFT 511 INTERNATIONAL This experiment (~5b) shared the 32-a, tip-to-tip, 01 - H.T. HO~ARD STANFORD U clertrir dipole antenna rich rxpcrinentr -D4 and -06. 01 - R.L. LEADABRAND SRI INTERNATIONAL Insfruntntali0n ranrirtcd of thice tunable plasma-wave 01 - R.A. LONG SR1 INTERNATIONAL rccciucrr, a fired-frequency iidcband receiver. and a ~avcform 01 - A.M. PElERSON STANFORD U ~ampler. The tunable receivers and rideband receiver provided data for direct t~l~metryIO earth. Each 01 the tunable receivc~s covered a different frequency Dana in the range 1 hi to 200 kH2. The high-frequency rccriucr had 96 frequency s~ttingr ~cpa~atcdby about 4 1, ana co~crcathe frequency ranqe 6.4 kbz lo 205 LHz. The mid-range receiver had 4b

115 frequency settings separated by about 8 percent and cowered the range 208 Hz to 6.07 kHz. The lcb-fr~quency receiver hid 24 settings rith 15 I, separation and cowred the range 11 HI to 309 Hz. The responst time of the low-frequency receiver mas --_----HELZOS-A, FEcnT1G----'------a~proxi.ateLy 1 SI nercssitatrng the inclusion 01 the rideband rerc~vcr to obtain information abcut the angular diitributicr INVESTIGATION NAME- MICROMElEOR01D DITECTOR AND ANALlZER of 11~sappcaiinq in the lo#-frcqurnry band. This receiver covered the frequency range 1 HI to 200 HI. The time NSSDC ID- 74-0971-12 INVESTIGATIVE PRO6RAM rrsolution dcpandec in detail cr the sparerraft telemetry CODE EL-4lCO-OPe SCIENCE formbt. bit rate. and experiment operational mode. when the shock alarm .ode became sctivated, dit. tram the rarelor. INVESTIGATION DISCIPLINE (5) sampler weit read into soi~tciaftmemory for period starting INlERPLAMETARl PHYSICS bef0.e and maing alter the triggering event. In this .oder 1NTERPLANElARY DUST the $nstantineous voltage across the antcnnb ..I passed through a low-pass filter with cornel frequency dependent an the PERSONNEL sa*pling rate. anc measured at aisrrrte intcrvllr. the most PI - H. FECHTIG UPI-NUCLEAR PHYS rapid being 2.2 .I. For I more detailed discussion see F. 24.5 OI - J. wEInRAucn npi-pnvs ASTROPHYS of Rrumfahrtforschung, 1. 19, n. 5, 1975. BRIEF DESCRlPllON ------HEL1OS-A. 6"RNElT------'------The PUIPOS~ of the e.piii.ent (110) was to invcstioate 10.e theories about the interplanetary dust including whether INVESTIGATION NAME- 26.5-KHZ 10 3-UHZ RADIO YAVE or not (1) the number Of partiCllS inrrtslts 101.16 the sun. (2) the cutoff for small particles is drpendcnt on the distance NSSDC ID- 74-097A-t6 I NVE S TI G A TI WE PROGRA U from the sun. becaune solar prtssura increaser IIC~ICI the sun. CODE EL-+/CO-OP. SCIENCE and 13) the number dcnsitics Of p.lti~1~~chanpt near the orbits of planets. The kinetic energy of dust partitles lNVESTlGLlION DISCIPLINE(S) hitting a target with high velocity (sew1r.l kalrl caused the RADIO PHYSICS material to vaporize and become p.lti.lly ionized. The PARTICLES AND FIELDS generated plasm. Cloud was then ICparat~d by apprOpriatt SOLAR PHYSICS voltages into its negative (electron) part and into positive ions. lhc .ass and the energr of the dust partic1.a was PERSONNEL determined from the i.pulsr heights. A time-of-flight mass PI - D.A. GURNETT U OF IOYA sp~trometer in ronnrrtion with the target atlored the small 01 - P.J. KELLOGG U OF UINNESOlA ion cloud to be analyzed. In this wayr the invertigbtion Of 01 - I.R. YEBER NASA-GSFC the chemical composition of the dust partitles became possible. 01 - R.G. STONE NASA-GSFC The threshold for the detection of p.iti~1~w.1 about I-E-15 9. Mass and energy determination was possible for partitles BRIEF DESCRIPTION larger than about 1-6-14 9. For particLes larger than 1.E-13 This experi.ent (E5r) shared the 32-m~ tip-tc-tip. 9. *ass s~~ctrumwas gathered. For further dqtails. see pp. electric dipole antenna with experiments -04 and -05. A dual 268-269 of Raumtahrtfoischung, 1. 19. n. 5r 1975. (redundant) 16-frequen~y rhbnnrl radiometer, with approximately l~gaiith~icallyspaced channels. bas used to detect lyre 111 ------HEL1ES-A. LEI*ERl------radio ~mis~ionsassoriatcd with 101al flare events in the frequency band 26.5 LHI tO 3 UHZ. lhe cxperi.rnt Sampling rate INVESTIGATION NAME- ZODIACAL L16Hl PHOTOMETER was synchronized such that each spi~eciatt rerolution "as aiviaed into 32 settors. The ~ccuencc ana frequency 01 NSSDC ID- 74-097A-11 lNVESlIGlTIVE PROGRAM sampling depended on the instrument OpClatiOnal .Ode lone of CODE EL-4ICO-OP. SCIENCE four) and the s~ac~craftbit rate. The most rapid sampling possible for a singlc-fiequ~ncychannel I.% once every 1132 of INVESTIGATION DISCIPLINEIS) a satellite spin ceriodr or about .03 I. A tyFira1 sa*plirg INTERPLANETlRV PHYSICS ICQY~~OC"as for one frcguenci channel to be Sa.0L.d for 16 ZODIACAL LIGHT sectors (112 rr~olution)~1ollor.a by the next. One-half Of the 32-• eipolc failed to titcnd prop~rlyduring deploymentr FERSONNEL and was shorted to ()round. The resulting antenna configuration PI - C. LElNERl UPI-ASTRONOMIE was that of a monopole with an operational effective length of 01 - E. PITI UP1-ASlRON0M1E about 8 I. lhis shoiter configuration resulted in increased radio-frequency interference IRFl) of from 3 to 30 dB abfve BRIEF DESCRIPTION CXptctCd levellr and a LOSS of 6 dB in gbin. Another problem This t.peri.cnt (E9) consisted of three photometers "as unexpected interference rith the high-gain telemetry Looking at 15 degr SO deg. mnd 90 deg from the ecliptic. These antenna. This .aced 60 dB RFl at 27.5 LHz, decreasing rith photometers ObsCrYCd the intensity and pol.rization of the increasing frequency. so that .bCIC 200 kH2 it produced no zodiacal light in UYI blur, and visual bands. The purpose of detectable interference. For -01- details about the instrument this experiment was to obtain information about the spati.1 and modes of OplratiOn. See 0. 250 Of RaumfahrtfOisChUngr I. distribution. size. and nature of interplanetary dust 191 P. 5, 1975. p.rtic1~1. for further detiilsr Ice pp. 26r-267 of Raum1.hrtforsrhulgr 1. 19. n. 51 1975. ---_-_-HELIOS-B, GURNETT------'------'-----

INVESlltATlON NAME- 50-KHZ TO 2-UHI RADIO YAWL INVESll6ATION NAME- ZODIACAL LIGHT PHOTOMETER NSSDC ID- 76-0051-06 INVESllGATlVE PROGRAM CODE EL-4lCO-OP. SCIENCE NSSDC ID- 76-003A-11 INVESTIGATIVE PROGRAM CODE EL-41CO-OP~ SCIENCE lNVES7lGATION DISCIPLINEIS) SOLAR PHYSICS lNVESTl6ATlON DISCIPLINEIS) RADIO PHYSICS INTERPLANETARY PHYSICS PARllCLES AND FIELDS ZODIACAL LIGHT

PERSONNEL PERSONNEL PI - D.A. GURNElT U OF IOWA PI - C. LElNERl MPI-ASTRONOMIE 01 - P.J. KELLOGG U OF MINNESOTA 01 - E. PITI MPI-ASTRONOMIE 01 - R.R. WEBER NASA-GSFC 01 - R.G. STONE NASA-GSFC BRIEF DESCRIPTION This experiment (E9) consisted of three photoeeters BRIEF DESCRIPTION l00king at I5 dcg. 30 degr and 90 de9 from the rrliptic. These This eipcri.ent (E5c) shared the 32-rn. tip-to-tior photo.ete~s observed the intensity and pol.ri~.tion 01 the clcctric dipole antenna with experiments -04 and -05. A dual mdiacal Light in UV. blue. selected risu.1 bands. and ihite IredundanO 16-frrqcrnc~channel raoi~mere~.with appr~.i.itely light. lhe purpose of this ewperimrnt I.$ to Obtain logarithmically spared channels. "1% used to detect type Ill information about the spatial distr$bvtionr size. and nature of radio cnirrionr .ssOCiated rith solar-flare cvents in the interplanetary dust particl~~. For further details. see pp. fccqucncy band 26.5 LHz to 3 IHz. The cxpcrimcnt sampling rate 264-267 of Raumtihrtforschunp. Y. 191 n. 5r 1975. "as syncmronizcd such that each spactcraft rcvoluticn "as divided into 32 sectors. The sequence and frcqucncr of sampling depended on the inrtrwent opcrational mode (one of fcur) and the spacecraft bit rate. The most ,*pia sa*plirg possible for a single frequency channel "as Once every 1132 01 a sat~llite spin period, or about .03 I. A typical smpling SC~U~~CC11% for one frequency channel to be sampled for 16 sectcrs I112 rcrolutionl. follorec by the ncxt. For .Cre details about the instrumcot and modes Of operation, see p. 250 of Raumtahrtforrchungr v. 19, n. 5, 1975.

INTERPLANEllRl PARTICLES

116

Appendixes APPENDIX A

INDEX TO PLANETARY INVESTIGATIONS WITH DATA AVAILABLE AT NSSDC

:NVESTIGATION CATEGORY ID MISSION BRIEF NAME PRINCIPAL PAGE INVESTIGATOR

MERCURY

:maging 73-085A-01 Mariner 10 TV Photography Murray 19

'articles and Fields 73-085A-03 Mariner 10 Scan. Elect. Analyzer Bridge 19 73-08%-07 Mariner 10 Energetic Particles Simpson 20 73-085A-04 Mariner 10 Flux. Magnetometer Ness 19 rltraviolet 73-085A-05 Mariner 10 EW Spectrometer Broadf oot 20 infrared 73-085A-06 Mariner 10 IR Radiometer Chase 20 ladio Science and !elestial Mechanics 73-085A-02 Mariner 10 Radio Science Howard 20

VENUS imaging 73-085A-01 Mariner 10 TV Photography Murray 29 78-051A-06 Pioneer Venus 1-orb. Cloud Photopolarimeter uansen 30 75-050D-01 Venera 9-Desc. Pan. Telephotometer 30 75-054D-01 Venera 10-Desc. Pan. Telephotometer 30 8 1-1 06D-0 1 Venera 13-Desc. Pan. Telephotometer 30 81-llOD-01 Venera 14-Desc. Pan. Telephotometer 30

'articles and Fields 62-041A-06 Mariner 2 Elect. Analyzer Neugebauer 30 73-085A-03 Mariner 10 Scan. Elect. Analyzer Bridge 30 78-051A-13 Pioneer Venus 1-orb. Electric Field Detector Scarf 31 62-041A-07 Mariner 2 Particle Detector Van Allen 32 73-085A-07 Mariner lr\ Energetic Particle simpson 32 78-078A-02 Pioneer Venus 2-Bus. Ion Mass Spectrometer Taylor, H. A. 32 78-051A-17 Pioneer Venus 1-Orb. Ion Mass Spectrometer Taylor, H. A. 32 78-05111-07 Pioneer Venus I-Orb. Ret. Pot. Analyzer Knud s en 31 78-051A-18 Pioneer Venus 1-Orb. Solar Wind Plasma Analyzer wolf e 31 62-041A-03 Mariner 2 3-axis Fluxgate Magnetometer Coleman 31 78-051A-12 Pioneer Venus 1-Orb. 3-axis Fluxgate Magnetometer Russe 11 32 73-085A-04 Mariner 10 Fluxgate Magnetometer Ness 31 67-0601-05 Mariner 5 Helium Magnetometer Smith 32 62-041A-04 Mariner 2 Cosmic Ray Ionization Anderson 33 78-051A-05 Pioneer Venus 1-Orb. Gamma Ray Burst Detector Evans 33 78-051A-03 Pioneer Venus I-Orb. Gas and Plasma Environment Croft 35 fltraviolet 73-085A-05 Mariner 10 EW Spectrometer Droadf oot 33 78-051A-15 Pioneer Venus 1-Orb. W Spectrometer Stewart 33

A- 1 IUDEX TO PLANETARY I?NES?ICA?I~NS WITH DATA AVAILARSE A? NSSDC (contiqued) - - ;NVESTlGATlON CATEGORY ID MI S S 1ON BRIEF UAYE PSINCIP4L P4GE INVEST I24TC P

VENiJS (continue4) nfrared 62-04 1A-02 Mariner 2 IR Ralznmeter %eu qe ha12 e r 73-085A-06 mriner 10 IR Ra.iioneter Ihase 79-0 5 1A- 16 Pioneer Venus 1-orb. Temperature Soiinm-ler Tivhr 78-078D-05 Pioneer Venus-Lge. IR Ra4iometer Boese 78-078E-04 Piorleer Venus Sm. 1 IP Radiometer Suomi 78-078F-04 Pioneer Venus Sm. 2 19 Radiometer Suom I 78-n78~-04 Pioneer Venus Sm. 3 Slloml

!adio Science and :elestial Mechanics 62-04lA-Of3 Wriner 2 Celestial Yec%anics Anderson 35 67-360A-07 mriqer 5 Celest ral Yechanics Anne r s 011 35 78-051A-21 Pioneer Venus I-orb. ?e 1est i a 1 Yec h a n i c s Shaplr7 3i 73-085A-02 "lariner 10 Ralin Science YOWd f 3 35 57-060A-02 '4ariner 5 2-Frenuency Seacon Cr?ft 35 78-051A-02 Pioneer Venus 1-Orb. jar Altimeter Pettengill 36 78-051A-20 Pioneer Venus 1-Orh. Kliore 35 70-05 1A-23 Pioneer Venus 1-orb. Internal Density Dist. IIDD Philllos 36 itmosphere 78-078A-06 Pioneer Venus 2-Bus Atx. Circ. Pat. 3LR L ) Cou n se 1man 37 78-07AD-09 Pioneer Venus L;JF? At?. 3irc. Pat. DLAI 1 Tou ns e 1Ta n 3Q ~EI-o~EE-~~Pioneer Venus Sm. 1 Atn. 3irc. Pat. 3LBL ) Zounselman 37 78-078F-03 Pioneer Venus-Sm. 2 4tm. 71rc. Pat. DLRI ) ZQunselnan 37 78-078G-0 3 Pioneer Venus-Sm. 3 4tn. 7irc. Pat. 3LRI ' 3?

78-051A-01 Pioneer Venus 1-Orb. Electron Tempera 'Jrd Probe Srace 36 78-051;\-11 Pioneer Venus 1-Orb. Yeut. Part. Yass 5pecEr 3neter l'ie-tann 36 78-078A-03 Pioneer Venus 2-Bus Yeut. Part. Mass Spectrgmeter Von Za\q 36 78-078D-06 Pioneer Venus-L ge . Yeut. Part. Yass Spectrometer Hoffman 36 78-051A-19 Pioneer Venus 1-Orb. Atmosp'Ieric Drag (OADl Yeat in9 36 78-051A-22 Pioneer Venus 1-Orb. Atm. Sol. Cor. Turh. ('TU?) YO0 37 78-078D-02 Pioneer Venus-Lge. Cloud Extent. Struct,ire Ragent 37 78-078E-02 Pioneer Venus-Sm. 1 Cloud Extent. Structure Raqent 37 78-078F-02 Pioneer Venus-Sm. 2 Cloud Extent. Structure Raqent 37 78-078G- 02 Pioneer Venus-Sm. 3 Cloud Exteqt. Structure Raqent 38

A- 2 INDEX TO PLANETARY INVESTIGATIONS WITH DATA AVAILARLE AT NSSDC (continued)

IWESTIGATION CATEGORY ID MISSION BRIEF NAME PRINC I PAL %PAGE IVVESTIGATOR 1 VENUS continued) I Atmosphere 78-078D-01 Pioneer

(continued) 'lenus-Lqe. Atm. Structure seiff 33 ~ 78-0786-0 1 Pioneer I Venus-Sm. Atm. Structure Serf€ 33 , 78-07QF-01 Pioneer I 'Jenus-Sm. 2 Atm. Structure Seiff 38 1 78-0786-01 Pioneer I Venus-Sm. 3 4t?. Structure self€ 3R 79-0780-94 Pioneer Venus-Lge. Gas Chromatog. Oyama 49 1 78-078E-04 Pioneer I Venus-Srn. 1 Sas Chromato?. suorni 34 ' 79-078F-04 Pioneer Venus-Sn. 2 Gas :hrornatog. suomi 34 9- 0 78G- 0 4 1 ' Pioneer Venus-Srn. 3 Gas ^hromatoq. suomi 70-0703-03 Pioneer 34 I Venus-Lge. '310~4Part. Size Snectrometer Knol lenberq 40 I 79-0783-'?7 Pioneer Venus-Lge. 1 Solar E?erqy Peqetrdtion Tomask 7 40 I 79-07PD-11 Pioneer I Venus-Lge. 4t.n. Pr3oaqation ?r?€r 39 1 1

YARS

64-077A-01 'lariner 4 Television Le i yhton 48 I 69-014A-01 Plariner 6 Mars Surface TV Camera Le ighton 48 69-03OA-!I 1 %riner 7 Mars Surface TV Camera Le i gh ton 49 I '1-95 1A-04 %riner 9 'l"ele.iision Photoqraphy YaSJr5k:t 49 7 5-07%-9 1 Viking 1-Cro. Imagery Tarr 43 75-'393A-91 Vikiqq 2-'3rb. Iwqery zarr 43 ' '5-375:-96 'Jikinq 1-tan?. Lander Imaqi?q YUtCh 50 ' 75-393C-06 Viking 2-Land. San3er Imagi?q uut-l? 50 I I Particles and Fields 64-377A-02 %ri?er 4 %laqne c mete r Smith 50 1 1 Vltraviolet 59-914A-94 Mariner 6 :Iv Spectrometer Sarth 50 ' 63-330A-94 Variner 7 YV Soectrometer Barth 51 I 71-35 1A-02 Uariner 7 Soectrmeter Barth 51 I I

A- 3

QWEGINWL PAGE IS OF POOR QUALITY INDEX TO PLANETARY I'TVESTI~~ATI'7NS WITY DATA AVAILARLE 4T VS53C crontinue?)

IWESTIGATION CATEGORY ID YISS ION 3RIEF VAME Pa I *JCI PRL P4;E INVEST IGATSP -- - 7 MARS (continue?)

[nfrared 6J-014A-02 F4ariner d Spect. 1.5-15 Yicrorn. Pinen te: 69-03OA-02 Nariner 7 Spect. 1.5-15 ~icrom. Pimentel 69-014A-03 ariner 6 Chan. 19 Radio.neter Vel;geSaier 69-030A-03 Mariner 7 :*an. I9 Qadrorneter Yeuqebauer 71-051A-01 Xariner 9 I9 Radiometer V ell a e 5 a u e f 7 5-075A-0 2 Vikinq 1-qrb. IQ Radionarer Kiecfer 75-083A-02 Vikinq 2-Orb. I9 Radinmeter Kieffer 71-O51A-03 '4ariner J 19 ITterfereTce Spectrqrne'er Hanel ladio Science and :elestial Yechanics 64-077A-09 Chriqer 1 le ?est:al Yechanics Anderson 59-014A-05 Yariner 6 ,?elestial Yechanics Anderson 69-0 30A-05 Yariqer 7 Celestial Yechanics Anderson 59-'31JA-96 Yariner 6 +Band occult. Yliore 69-030~-06 Chriner 7 S-Band ,?CCU1C. Yliore 7 1-95 1A-00 'lariier 9 S-Band Occult. Klinre 75-075A-04 Vikiqq 1-9rb. Fladio Scieice wichael 75-583A-04 Viking 2-Orb. Qdio Science Michael 75-O75C-11 Vikinq 1-Lan3. Qadi0 Sc:ence Yic9ael 75-083C-11 Viking 2-Land. Qdio Science Yichael itmosphere 75-075A-03 Vikino 1-Orb. Spect rame ter Fdrner 7 5-083A-0 3 Viking 2-Orb Spectrometer Farmer 75-07%-02 Vikiqg 1-Land. Atm. Structure Vier 75-083C-02 Viking 2-Land. Atm. Structure Vier 7 5-07%-12 Viking 1-Land. Atm. Comp. Vier 75-083C- 12 Vrkiqq 2-Land. 4tm. Comp. Vier 75-0752-14 Viking 1-Land. IQnospher. Prop. Vier 75-083C-14 Viking 2-Lan?. Lonospher. Prop. Vier 56 1 75-075C-0 7 Vikinq I-land. Yeteo r rjlo ay Yes5 57 7 5-08 3C -0 7 Viking 2-Land. Yeteo r o 1o qy Yess 57 1

;urface Chemistry 75-083C-0 1 Viking 2-Land. Physical ?rop. Shorthill 75-075C- 10 Viking I-Land. %vet. ?rop. war Traves 75-083C- 10 Viking 2-Land. Yapet. Prop. 4aroraves 7 5-0 7 5C-04 Vikinq ?-Land. yo lecu 1a r Ana 1. 3 lend 71 75-083C-04 Viking 2-Land. rolecular Anal. 9 i eidn? 75-075C-13 Viking 1-Land. Iqorgan. 3emistr:r 7ou lrni 1 75-083C-13 Viking 2-Land. Iiorqan. ;hemistry :oul?in

3iology 7 5- 0 7 5C-0 3 Viking 1-Land. BiOlOqy Klein 75-083C-03 Viking 2-Land. Bioloqy Klein 7 5-075C-04 Viking 1-Land. Yolecular Anal. giemann 7 5-08 3C-0 4 Vikinq 2-Land. %lecular Anal. 91 emdnn je i smoloqy 75-083C-0 8 Viking 2-Land. Sei smo loqy hderson

JUPITER

L magi ng 72-012A-07 Pioneer 10 Imaqe Photopolarimeter Gehre1 s 7 3-0 19A-07 Pioneer 11 Image Photopolarimeter Gehrels 77-084A-01 Voyager 1 Imaging Smith, 8. A. 77-076A-01 Voyager 2 Imaging Smith, 8- A.

A- 4 INDEX M PLANETARY INVESTIGATIONS WITH DATA AVAILABLE AT NSSDC (continued)

INVESTIGATION CATEGORY ID MISSION BRIEF NAME PRINCIPAL PAGE INVESTIGATOR

JUPITER (continued) i articles and Fields 72-012A-01 Pioneer 10 3-axis Helium Mag. Smith, E. J. 71 i I 73-01911-01 Pioneer 11 3-axis Helium Mag. Smith, E. J. 71 73-0 19A- 14 Pioneer 11 Fluxqate Magnetometer Acuna 71 77-084A-05 Voyager 1 Fluxgate Magnetometer Ness 71 i 77-07611-05 Voyager 2 Fluxga t e Magnetometer Ness 71 I 77-084A-06 Voyager 1 Faraday Cup Bridge 70 77-0766-06 Voyager 2 Faraday Cup Rridqe 70 77-084A-13 Voyager 1 Plasma Wave Scarf 70 77-076A-13 Voyager 2 Plasma Wave Scarf 70 72-012A-05 Pioneer 10 Trapped Particles Fillius 72 7 3-0 19A-0 5 Pioneer 11 Trapped Particles Fillius 72 72-0 12A-02 Pioneer 10 Charged Particles Simpson 71 73-019A-02 Pioneer 11 Charged Particles Simpson 72 72-012A-11 Pioneer 10 Charged Particles Van Allen 72 73-019A-11 Pioneer 11 Charged Particles Van Allen 72 72-012A-12 Pioneer 10 Charged Particles McDonald 73 73-019A-12 Pioneer 11 Charged Particles Mc Dona 1 d 73 72-012A-13 Pioneer 10 Quadrasphere Anal. Wolfe 69 73-019A-13 Pioneer 11 Quadrasphere Anal. Wolfe 69 77-08431-07 Voyager 1 Particle Anal. Telescope Krimigis 70 77-07631-07 Voyager 2 Particle Anal. Telescope Kr imigis 70 77-084A-08 Voyager 1 Cosmic Ray Telescope vast 73 77-076A-08 Voyager 2 Cosmic Ray Telescope vast 73

ltraviolet 72-012A-06 Pioneer 10 'JV Photometer 200-800A Judge 74 73-019A-06 Pioneer 11 CTV Photometer 200-800A Judge 74 77-084A-04 Voyager 1 W Spectrometer Broadfoot 74 77-076A-04 Voyager 2 IN Spectrometer Broadfoot 74 nfrared 77-084A-03 Voyaqer 1 IR Interferometer Hanel 74 7 7-076A-0 3 Voyager 2 IR Interferometer Hanel 74 adio Science and elestial Mechanics 72-012A-09 Pioneer 10 Celestial Yechanics Anderson 75 73-019A-09 Pioneer 11 Celestial Mechanics Anderson 75 72-0 12A- 10 Pioneer 10 S-Band Occultation Kliore 75 73-0 19A-10 Pioneer 11 S-Band Occultation Kliore 75 '7-084A-02 Voyager 1 Cober. S- + X-Band Esh leman 75 77-076A-02 Voyager 2 Coher. S- + X-Rand Eshleman 75 77-084A-10 Voyager 1 LF, QF Receiver 'rlarw'ick 76 77-076A-10 Voyager 2 LF, W Pec.eiver Xa rwi ck 76

tnosphere 72-012A-10 Pioneer 10 S-Band gccultation Kliore 75 7 3-0 19A- 10 Pioneer 11 S-Band Occultation Kliore 75 72-012A-07 Pioneer 10 Imaq. Photopolarimeter Gehrels 64' 73-01911-07 Pioneer 11 Imaq. Photopolarimeter Gehrels 68 j 77-076A-11 voyager 2 Photopolarimeter Lane 76 i Polarization 72-012A-07 Pioneer 10 Imag. Photopolarimeter Gehrels 68 73-019A-07 Pioneer 11 Imag. Photopolarimeter Ge hre 1s 68 I 77-076A-11 Voyager 2 Photopolarimeter Lane 76

SATURN

1 magi n9 7 3-0 19A-07 Pioneer 11 Imag. Photopolarimeter Gehrels 83 77-084A-01 Voyager 1 Imaging Smith, 8. A. 84 77-076A-91 Vgyaqer 2 Imaging Smith, B. A. 84

A- 5 INDEX TO PLANETARY INVESTIGATIONS WITH DATA AVAILABLE AT USSDC (concluded)

INVESTIGATl9N CATEORY ID MISS ION BRIEF YhqE PPIVCIPkL INVEST IGXTni: I

SATURN (conclude?) I

Particles and Fields 73-019A-02 Pioneer 11 charqerl Particles Simpson 72 73-019A-12 Pioneer 11 Cha rged Particles ‘+Dona13 75 73-019A-05 Pioneer 11 Trapped Particles CLllLlS 75 73-019A-13 Pioneer 11 Quadrasphere Anal. dolfe 84 73-019A-14 Pioneer 11 Fluxgate Yaqnetometer Acuna 75 7 3-0 19A- 1 1 Pioneer 1 1 Charqcd Particles Van Allen 72 Radio Science and Zelestral Mechanics 73-019A-09 Pioneer 11 Celestial Mec5anics Anderson 85

4tmosphere 73-019A-07 Pioneer 11 Imaqe Photopolarimeter Gehre 1s

A-6 APPENDIX B

INDEX TO INTERPLANETARY INVESTIGATIONS (FROM PLANETARY MISSIONS) WITH CATA AVAILABLE AT NSSDC

1 1I INVESTIGATION CATEGORY ID MISS ION BRIEF NAME PRINCIPAL PAGE I INVESTIGATOQ t

Particles and Fields 64-077A-04 Yariner 4 Cosmic Ray Telescope Simpson 34 67-06OA-03 Mariner 5 Faraday Cup Br idqe 34 77-084A-08 Vovaqer 1 Cosmic Ray Telescope vogt 95 I 77-076A-08 Voyager 2 Cosmic Ray Telescope VOgt 95

~ u 1 t raviolet 72-012A-06 Pioneer 10 rm Photometer Judse 35 I 73-019A-06 Pioneer 11 'JV Photometer Judqe 35

73-019A-15 Pioneer 11 Zodiacal Liqht Photometer Weinber q 96 I J

B- 1 APPENDIX C

IYDEX TI) INTERPLANETARY SIISSIONS :iITH DATA AVAILABLE A? NSSDC

INVESTIGATION CATEGORY In YISSION BRIEF UAMF. PP INCIPllL P4CE -- I*XESTISAT?P

Particles and Fields 65-105A-02 Pioneer 6 Faraday Pup Rri14e 10i 66-075A-02 Pioneer 7 Faraday ?up 3r :due 107 65- 1 OSA-08 Pioneer 6 Superior Cony. Faraday Pot. Levy 107 66-075A-08 Pioneer 7 Superior Con]. Faraday Rot. Levy 107 68-100A-02 Pioneer 9 Solar Plasma Detector :io 1€e 107 74-097A-09 He110s-A Plasma Detector RoseTbauer 107 76-003A-09 Helios-B Plasma Detector Rosenbauer 108 74-097A-04 Hellos-A. Solar Wind Plasna Wave ;ur ?e t t 108 76-003A-04 Hellos-B Solar Wind Plasma Wave 31r net t 108 67-123A-97 Pioneer 8 Electric Field Detector Scarf 108 68-100A-07 Pioneer 9 Electric Field Detector Scarf 109 65-105A-06 Pioneer 6 Electrostatic Analyzer Wolfe 109 66-075~-03 Pioneer 7 Electrostatic Analyzer Wolfe 109 67- 123A-02 Pioneer A Electrostatic Analyzer Wol€e 109 74-097A-10 Hellos-A Snergetic Elect., Proton Det. Kepp 1e r 110 76-003A-10 He110s-9 Energetic Elect., Proton Det. Keppler 110

65- 105~-ni Pioneer 6 Uniaxial Yaqnetometer Yess 110 66-075A-0 1 Pioneer 7 fJnid x i a 1 Ya qne t ome t e r Ness 110 67-123A-01 Pioneer A Uniaxial Yaqnetometer Uess 110 68-100A-01 Fioneer 9 Triaxial SIaqnetomater Sonnett 110 74-097A-02 He1 ios-A Triaxial Fluxqate Yaqnetometer Ness 110 76-003A-02 Ye1 ios -B Triaxial Fluxgate Yaqnetometer Ness 111 74-097A-01 He1ins-A Triaxial Fluxgate Yaqnetometer Neu5auer 111 76-003A-01 Hellos-R Triaxial Fluxgate Yaqnetometer Yeubauer 111 60-00 1A-02 Pioneer 5 Search Coil Yametometer Greenstadt 111 74-097A-03 Hellos-A Search Coil Maqnetometer Neubauer 111 76-003A-03 Hellos-B Search Coil Yaqnetometer Neubauer 111

60-001A-03 Pioneer 5 Ion Chamber and GM Tube !iinckler 112 60-001A-01 Pioneer 5 Coincident Cosmic Prop. Ctr. Simpson 112

65- 105A-0 3 Fioneer 6 Cosmic Ray Telescope Simpson 112 66-075A-06 Pioneer 7 Cosmic Ray Telescope Simpson 112 67- 123A-06 Pioneer 9 Cosmic say Telescope Webber 112 65-105A-05 Pioneer 7 losmic Ray Anisot. YcC r a cte ? 113 66-075A-05 Pioneer 8 cosmic Ray Anisot. YcCracke? 113 68-l00A-05 Pioneer 9 :osnic Ray 4nisot. YcCracken 113 67- 123A-06 Pioneer 8 Cosnlc Ray Grad. 3et. Webber 113 68-100A-06 Pioneer 9 cosmic 9av Sral. De:. Webher 113 65-105A-05 Pioneer 6 cost-i 3 Ray 9etector YcC r a c 4 e n 112 74-097A-08 He1ios-A Cosmic Rav Detector Trainor 113 76-003A-08 He1 ios-B ~OSrnlCRay Detector Trainor 114 74-097A-07 He110s -A Cosmic Ray Particles Kunow 114 76-003A-07 Hellos-B Cosmic Ray Particles Kunow 114

-die Science .s 65-105A-07 Pioneer 6 Celestial Mechanics An der s on 114 :elestial Mechanics 65-105A-04 Pioneer 6 2-Frequency Beacon Receiver Eshleman 114 66-075A-04 Pioneer 7 2-Frequency Beacon Receiver Eshleman 115 67-123A-03 Pioneer 8 2-Frequency Beacon Feceiver Eshleman 115 68-100A-03 Pioneer 9 2-Frequency Beacon Receiver Eshleman 115 74-097A-05 He110s-A Fine-Wave Spectrometer Gurne t t 115 76-003A-05 Hellos-B Fine-Wave Spectrometer Gurne t t 115 74-097A-06 Hellos-A 27 KHz - 3 MHz Qadi0 Wave Gu rnet t 116 76-003A-06 He110s-B 27 KHz - 3 YHz Radio Wave Gur net t 116

:nterplanetary Particles 74-097A-12 Hellos-A Micrometeoroid Det. Analyzer Fechtig 116 74-097A-11 qelios-A Zodiacal Liqht Photometer Leinert 116 76-0034-11 Iielios-B Zodiacal Light Photometer Leinert 116

c- 1 APPENDIX D - DEFINITIONS

Investigation Discipline - The subject to which an investigation pertains. The possible entries are limited, and the NSSDC information files can be searched using this field.

Investigative Program - Code of the cognizant NASA Headquarters office, or name of other sponsoring agency program. "CO-OP" added to a code indicates a cooperative effort with another agency or foreign country.

NLA - No Longer Affiliated. Used in the spacecraft personnel section and occasionally with investigations to indicate that the person had the specified affiliation at the time of his participation in the project, but is no longer there.

NSSDC ID - An identification code used in the NSSDC information system. In this system, each successfully launched spacecraft and experiment is assigned a code based on the launch sequence of the spacecraft. Subsequent to 1962, this code (e.g., 72-01211 for the spacecraft Pioneer 10) corresponds to the COSPAR international designation. The experiment codes are based on the spacecraft code. Forr example, the experiments carried aboard the spacecraft 73-019A (Pioneer 11) are numbered 73-019A-01, 73-019A-02, etc. Each prelaunch spacecraft and experiment is also assigned an NSSDC ID code based on the name of the spacecraft. Prior to launch, for example, the approved NASA launch, Solar Mesosphere Explorer, was coded SME. The experiments to be carried aboard this spacecraft were coded SME -01, SME -02, etc. Once a spacecraft is launched, its prelaunch designation is changed to a postlaunch one; e.g., Pioneer-G, which was launched April 6, 1973, was given the NSSDC ID code of 73-019A, and the NSSDC spacecraft common name of Pioneer 11.

01 - Other Investigator.

PI - Principal Investigator.

PM - Project Manager.

PS - Project Scientist.

TL - Team Leader.

TM - Team Member.

D- 1 TRF - Technical Reference File. A computerized space-investigation-oriented bibliographic reference list maintained by NSSDC. Journal publications and other documents are cited, and can be retrieved by author name, title, or NSSDC ID of relevant investigation. Used to keep track of descriptive and documentation material, as well as to produce bibliographies of certain spacecraft. The TRJ? accession number begins with the letter B and contains five digits; for example, B10851.

D- 2 APPENDIX E INDEX OF SPACECFWT AND INVESTIGATIONS BY SPACECRAFT NAME AND PRINCIPAL INVESTIGATOR

PAGE NO. *

1960 ALPHA 1 SEE PIONEER 5

1962 ALPHA RHO 1 SEE MARINER 2

HELIOS 1 SEE HELIOS-A

HELIOS 2 SEE HELIOS-B

HELIOS-A FED REP OF GERMANY BMWF 12/10/14 HELIOCENTRIC 14-09lA 106 UNITED STATES NASA-OSSA FECHTIG MICROMETEOROID DETECTOR AND ANALYZER 14 -0 9lA-12 116 GURNETT SOLAR WIND PLASMA WAVE 14-097A-04 108 GURNETT FINE FREQUENCY, COARSE TIME RESOLUTION 14-09lA-05 115 SPECTRUM ANALYSIS GURNETT 26.5-KHZ TO 3-MHZ RADIO WAVE 14-09lA-06 116 I KEPPLER ENERGETIC ELECTRON AND PROTON DETECTOR 14-09119-10 110 KUNOW COSMIC-RAY PARTICLES 14-097A-01 114 LE INERT ZODIACAL LIGHT PHOTOMETER 14-097A-11 116 NESS FLUXGATE MAGNETOMETER FOR AVERAGE FIELDS 14-09lA-02 110 NEUBAUER FLUXGATE MAGNETOMETER FOR FIELD 14-09lA-01 111 FLUCTUATIONS NEUBAUER SEARCH COIL MAGNETOMETER 14-09lA-03 111 ROSENBAUER PLASMA DETECTORS 14-097A-09 101 TRAINOR GALACTIC AND SOLAR COSMIC RAYS 14-09lA-08 113

HELIOS-B FED REP OF GERMANY BMWF 01/15/16 HELIOCENTRIC 1 6-003A 106 UNITED STATES NASA-OSSA GURNETT SOLAR WIND PLASMA WAVE 1 6-003A-04 108 GURNETT FINE FREQUENCY, COARSE TIME RESOLUTION 16-003A-05 115 SPECTRUM ANALYSIS GURNETT 50-KHZ TO 2-MHZ RADIO WAVE 16-003A-06 116 KEPPLER ENERGETIC ELECTRON AND PROTON DETkCTOR 16-003A-10 110 KUNOW COSMIC-RAY PARTICLES 16-003A-01 114 LEINERT ZODIACAL LIGHT PHOTOMETER 16-003A-11 116 NESS FLUXGATE MAGNETOMETER FOR AVERAGE FIELDS 16-003A-02 111 NEUBAUER FLUXGATE MAGNETOMETER FOR FIELD 1 6-003A-01 111 FLUCTUATIONS NEUBAUER SEARCH COIL MAGNETOMETER 16-003A-03 111 ROSENBAUER PLASMA DETECTORS 16-003A-09 108 TRAINOR GALACTIC AND SOLAR COSMIC RAYS 76-003A-08 114

MARINER 2 UNITED STATES NASA-OSSA 08/21/62 VENUS FLYBY 62-041A 21 ANDERSON COSMIC-RAY IONIZATION 62-041A-04 33 ANDERSON CELESTIAL MECHANICS 62-041A-08 35 COLEMAN, JR. FLUXGATE MAGNETOMETER ,62-041A-03 31 NEUGEBAUER INFRARED RADIOMETER 62-041A-02 33

E-1 PAGE NO.

NEUGEBAUER SOLAR PLASMA ANALYZER 62-041A-06 30 VAN ALLEN PARTICLE DETECTOR 62-041A-07 32

MARINER 4 UNITED STATES NASA-OSSA 11/28/64 MARS FLYBY 64-077A 47 ANDERSON CELESTIAL MECHANICS 64-077A-09 54 LEIGHTON MARS Tv CAMERA 64-077A-01 48 SIMPSON COSMIC-RAY TELESCOPE 64-077A-04 94 SMITH HELIUM MAGNETOMETER 64-077A-02 50

MARINER 5 UNITED STATES NASA-OSSA 06/14/67 67-06019 21 ANDERSON CELESTIAL MECHANICS 67-060A-07 35 BRIDGE INTERPLANETARY ION PLASMA PROBE FOR 67-060A-03 31 E/Q OF 40 TO 9400 VOLTS ESHLEMAN TWO-FREQUENCY BEACON RECEIVER 67-060A-02 35 SMITH TRlAXIAL LOW FIELD HELIUM MAGNETOMETER 67-060A-05 32

MARINER 6 UNITED STATES NASA-OSSA 02/24/69 MARS FLYBY 69-014A 47 ANDERSON CELESTIAL MECHANICS 69-014A-05 54 EARTH W SPECTROMETER 69-014A-04 50 KIIORE S-BAND OCCULTATION 69-014A-06 54 LEI GHTON MARS Tv CAMERA 69-014A-01 48 NEUGEBAUER TWO-CHANNEL IR RADIOMETER MARS SURFACE 69-014A-03 52 TEMPERATURE PIMENTEL IR SPECTROMETER 69-014A-02 52

MARINER 7 UNITED STATES NASA-OSSA 03/27/69 MARS FLYBY 69-030A 47 ANDERSON CELESTIAL MECHANICS 69-030A--05 54 BARTH W SPECTROMETER 69-030A-04 51 KLIORE S-BAND OCCULTATION 69-030A-06 54 LE IGHTON MARS Tv CAMERA 69-03OA-01 49 NEUGEBAUER TWO-CHANNEL IR RADIOMETER MARS SURFACE 69-030A-03 53 TEMPERATURE PIMENTEL IR SPECTROMETER 69-030A-02 52

MARINER 9 UNITED STATES NASA-OSSA 05/30/71 AREOCENTRIC 71-051A 47 EARTH ULTRAVIOLET SPECTROMETER (WS) 71-051A-02 51 "EL INFRARED INTEXFEROMETER SPECTROMETER 71-051A-03 52 (IRIS) KLIORE S-BAND OCCULTATION 71-051A-08 54

MASURSKY TELEVISION PHOTOGRAPHY 71-051A-04 49 NEUGEBAUER INFRARED RADIOMETER (IRR) 71-051A-01 53

MARINER 10 UNITED STATES NASA-OSSA 11/03/73 MERCURY FLYBY 73-085A 19 BRIDGE MEASUREMENT OF PLASMA ENVIRONMENT 73-085A-03 19 BROADFOOT EW SPECTROSCOPY 73-085A-05 20 CHASE, JR. TWO-CHANNEL IR RADIOMETER 73-08549-06 20 HOWARD S- AND X-BAND RADIO PROPAGATION 73-085A-02 20 MURRAY TELEVISION PHOTOGRAPHY 73-085A-01 19 NESS FLUXGATE MAGNETOMETERS 73-08549-04 19 SIMPSON ENERGETIC PARTICLES 73-08514-07 23

MARINER 73 SEE MARINER 10

MARINER 77A SEE VOYAGER 1

MARINER 77B SEE VOYAGER 2

E-2 PAGE NO.

MARINER JUPITER/SATURN A SEE VOYAGER 1

MARINER JUPITER/SATURN B SEE VOYAGER 2

MARINER MARS 69A SEE MARINER 6

MARINER MARS 69B SEE MARINER 7

MARINER MARS 71 SEE MARINER 9

MARINER R-2 SEE MARINER 2

MARINER VENUS 67 SEE MARINER 5

MARINER VENUS/MERCURY 73 SEE MARINER 10

MARINER-I SEE MARINER 9

MARINER-J VENUS/MERCURY SEE MARINER 10

MJS 77A SEE VOYAGER 1

MJS 77B SEE VOYAGER 2

OUTER PLANETS A SEE VOYAGER 1

OUTER PLANETS B SEE VOYAGER 2

P 38 SEE MARINER 2

PIONEER 5 UNITED STATES NASA-OSSA 03/11/60 HELIOCENTRIC 60-001A 105 UNITED STATES DOD-USAF GREENSTADT SEARCH-COIL MAGNETOMETER 60-001A-02 111 SIMPSON PROPORTIONAL COUNTER TELESCOPE 60-001A-01 112 WINCKLER ION CHAMBER AND GM TUBE 60-001A-03 112 I

PIONEER 6 1JNITED STATES NASA-OSSA 12/16/65 HELIOCENTRIC 65-10514 105 ANDERSON CELESTIAL MECHANICS 65-105A-07 114

BRIDGE SOLAR WIND PLASMA FARADAY CUP 65-105A-02 107 ~ ESHLEMAN TWO-FREQUENCY BEACON RECEIVER 65-105A-04 114 LEVY SUPERIOR CONJUNCTION FARADAY ROTATION 65-105A-08 107 MCCRACKEN COSMIC-RAY ANISOTROPY 65-105A-05 112 NESS UNIAXIAL FLUXGATE MAGNETOMETER 65-105A-01 110 SIMPSON COSMIC-RAY TELESCOPE 65-105A-03 112 WOLFE ELECTROSTATIC ANALYZER 65-105A-06 109

PIONEER 7 UNITED STATES NASA-OSSA 08/17/66 HELIOCENTRIC 6 6-075A 105 BRIDGE SOLAR WIND PLASMA FARADAY CUP 66-07514-02 107 ESHLEMAN TWO-FREQUENCY BEACON RECEIVER 66-075A-04 115 LEVY SUPERIOR CONJUNCTION FARADAY ROTATION 66-075A-08 107 MCCRACKEN COSMIC-RAY ANISOTROPY 66-075A-05 113 NESS SINGLE-AXIS MAGNETOMETER 66-075A-01 110 SIMPSON COSMIC-RAY TELESCOPE 66-075A-06 112 WOLFE ELECTROSTATIC ANALYZER 66-075A-03 109

PIONEER 8 UNITED STATES NASA-OSSA 12/13/67 HELIOCENTRIC 67-123A 105 ESHLEMAN TWO-FREQUENCY BEACON RECEIVER 67-123A-03 115 I NESS SINGLE-AXIS MAGNETOMETER 67-123A-01 110 I

ORIGINAL PAGE 6 E-3 OF POOR QUALITY PAGE I * PRINC.INVEST.NAME INVESTIGATION NAME * NO. *

SCARF PLASMA WAVE DETECTOR 67-123A-07 108 WEBBER COSMIC-RAY GRADIENT DETECTOR 67-123A-06 112 WOLFE ELECTROSTATIC ANALYZER 67-123A-02 109

PIONEER 9 UNITED STATES NASA-OSSA 11/08/68 HELIOCENTRIC 68-100A 106 ESHLEMAN TWO-FREQUENCY BEACON RECEIVER 68-100A-03 115 MCCRACKZN COSMIC-RAY ANISOTROPY 68-100A-05 113 SCARF ELECTRIC FIELD DETECTOR 68-10014-07 109 SONETT TRIAXIAL MAGNETOMETER 68-100A-01 110

~ WEBBER COSMIC-RAY GRADIENT 68-100A-06 113 WOLFE SOLAR PLASMA DETECTOR 68-1OOA-02 107

PIONEER 10 UNITED STATES NASA-OSSA 03/03/72 JUPITER FLYBY 72-01 2A 67 ANDERSON CELESTIAL MECHANICS 72-012A-09 75 BARNES QUADRISPHERICAL PLASMA ANALYZER 72-012A-13 69 FILLI US JOVIAN TRAPPED RADIATION 72-012A-05 72 GEHRELS IMAGING PHOTOPOLARIMETER (IPP) 72-012A-07 68 JUDGE ULTRAVIOLET PHOTOMETRY 72-012A-06 73 KINARD METEOROID DETECTORS 72-012A-04 96 KLIORE S-BAND OCCULTATION 72-012A-10 75 MCDONALD COSMIC-RAY SPECTRA 72 -0 12A-12 13 SIMPSON CHARGED PARTICLE COMPOSITION 72-012A-02 71 SMITH MAGNETIC FIELDS 72-012A-01 71 SOBERMAN ASTEROID/METEOROID ASTRONOMY 72-012A-03 95 VAN ALLEN JOVIAN CHARGED PARTICLES 72-012A-11 12 WE INBERG ZODIACAL-LIGHT TWO-COLOR 72-012A-14 96 PHOTOPOLARIMETRY

PIONEER 11 UNITED STATES NASA-OSSA 04/06/73 SATURN FLYBY 73-01914 67 ~ ACUNA JOVIAN MAGNETIC FIELD 73-019A-14 71 ANDERSON CELESTIAL MECHANICS 73-01 9A-09 75 BARNES QUADRISPHERICAL PLASMA ANALYZER 73 -0 19A-13 69 FILLIUS JOVIAN TRAPPED RADIATION 73-019A-05 72 GEHRELS IMAGING PHOTOPOLARIMETER (IPP) 73-019A-07 68 JUDGE ULTRAVIOLET PHOTOMETRY 73-01914-06 74 KINARD METEOROID DETECTORS 73-019A-04 96 KLIORE S-BAND OCCULTATION 73-019A-10 75 MCDONALD COSMI C-RAY SPECTRA 73-01 9A-12 73 SIMPSON CHARGED PARTICLE COMPOSITION 73-01914-02 72 SMITH MAGNETIC FIELDS 73-0 1 9A-01 71 SOBERMAN ASTEROID/METEOROID ASTRONOMY 73-019A-03 95 VAN ALLEN JOVIAN CHARGED PARTICLES 73-019A-11 72 WE INBERG ZODIACAL-LIGHT TWO-COLOR 73-019A-15 96 PHOTOPOLARIMETRY

PIONEER VENUS 1 UNITED STATES NASA-OSSA 05/20/78 VENUS ORBITER 78-051A 27 BARNES SOLAR WIND PLASMA ANALYZER (OPA) 78-051A-18 31 BRACE ELECTRON TEMPERATURE PROBE (OETP) 78-05119-01 36 CROFT GAS-PLASMA ENVIRONMENT-DUAL FREQUENCY 78-051A-03 35 EXPERIMENT (OGPE) EVANS GAMMA BURST DETECTOR (OGBD) 78-051A-05 33 KEATING ATMOSPHERIC DRAG (OAD) 78-051A-19 36 KLIORE RADIO OCCULTATION (ORO) 78-051A-20 35 KNUDSEN RETARDING POTENTIAL ANALYZER (OFQA) 78-051A-07 31 NIEMA" NEUTRAL MASS SPECTROMETER (ONMS) 78-051A-11 36 PETTENGILL RADAR MAPPER (ORAD) 78-051A-02 35 PHILLIPS INTERNAL DENSITY DISTRIBUTION (OIDD) 78-051A-23 36 RUSSELL MAGNETOMETER (OMAG) 78-05144-12 32

E-4 PAGE * PRINC.INVEST.NAME INVESTIGATION NAME * NO. * *

SCARF ELECTRIC FIELD DETECTOR (OEFD) 78-051A-13 31 SHAP IRO CELESTIAL MECHANICS (OCM) 78-051A-21 35 STEWART PROGRAMMABLE ULTRAVIOLET SPECTROMETER 78-051A-15 33 (oms) , TAYLOR INFRARED RADIOMETER (OIR) 78-051A-16 34 TAYLOR, JR. ION MASS SPECTROMETER 1-60AMU (OIMS) 18-051A-11 32 TRAVIS CLOUD PHOTOPOLARIMETER 78-051A-06 30 WOO ATMOSPHERIC AND SOLAR CORONA TURBULENCE 78-051A-22 31 WUR)

PIONEER VENUS 1918 SEE PIONEER VENUS 2

PIONEER VENUS 1978 SEE PIONEER VENUS PROBE LRG

PIONEER VENUS 1978 SEE PIONEER VENUS PROBE SM1

PIONEER VENUS 1918 SEE PIONEER VENUS PROBE SM2

PIONEER VENUS 1918 SEE PIONEER VENUS PROBE SM3

PIONEER VENUS 1978 ORBIT SEE PIONEER VENUS 1

PIONEER VENUS 2 UNITED STATES NASA-OSSA 08/08/18 VENUS PROBE 78-018A 21 TAYLOR, JR. ION MASS SPECTROMETER (BIMS) 78-078A-02 32 VON ZAHN NEUTRAL MASS SPECTROMETER (BNMS) 78-078A-03 36

PIONEER VENUS ORBITER SEE PIONEER VENUS 1

PIONEER VENUS PROBE LRG UNITED STATES NASA-OSSA 08/08/78 VENUS PROBE 78-078D 28 I BOESE INFRARED RADIOMETER (LIR) 78-078D-05 34 COUNSELMAN DIFFERENTIAL LONG BASELINE 18-078D-09 39 INTERFEROMETER (DLBI) CROFT ATMOSPHERIC PROPAGATION (MPRO) 78-018D-11 38 HOFFMAN NEUTRAL PARTICLE MASS SPECTROMETER 78-078D-06 36 (LNMS) KNOLLENBERG CLOUD PARTICLE SIZE SPECTROMETER (LCPS) 18-018D-03 40 OYAMA GAS CHROMATOGRAPH (LGC) 70-078D-04 40 RAGENT NEPHELOMETER (LN) 18-078D-02 31 SEIFF ATMOSPHERIC STRUCTURE (LAS) i8-078~-01 38 TOMASKO SOLAR FLUX RADIOMETER (LSFR) 78-0181)-07 40

PIONEER VENUS PROBE SM1 UNITED STATES NASA-OSSA 08/08./18 VENUS PROBE 18-0783 28 COUNSELMAN DIFFERENTIAL LONG BASELINE 18-018E-03 39 INTERFEROMETER (DLBI) CROFT ATMOSPHERIC PROPAGATION (MPRO) 78-0783-01 39 ' RAGENT NEPHELOMETER (SN) 78-0783-02 31 SEIFF ATMOSPHERE STRUCTURE (SAS) 78-0703-01 38 SUOMI NET FLUX RADIOMETER (SNFR) 78-018E-04 34 WOO ATMOSPHERIC TURBULENCE (MTUR) 18-018E-06 31

2IONEER VENUS PROBE SM2 UNITED STATES NASA-OSSA 08/08/78 VENUS PROBE 78-018F 28 COUNSELMAN DIFFERENTIAL LONG BASELINE 78-018F-03 39 INTERFEROMETER (DLBI) CROFT ATMOSPHERIC PROPAGATION (MPRO) 78-018F-01 39 RAGENT NEPHELOMETER (SN) 78-078F-02 31 SEIFF ATMOSPHERIC STRUCTURE (SAS) 18-018F-01 38 SUOMI NET FLUX RADIOMETER (SNFR) 78-018F-04 34 WOO ATMOSPHERIC TURBULENCE (MTUR) 78-018F-06 31

E-5 PAGE * PRINC.INVEST.NAME INVESTIGATION NAME * NO. * t

PIONEER VENUS PROBE SM3 UNITED STATES NASA-OSSA 08/08/78 VENUS PROBE 78-078G 28 COUNSELMAN DIFFERENTIAL LONG BASELINE 78-078G-03 39 INTERFEROMETER (DLBI) CROFT ATMOSPHERIC PROPAGATION (MPRO) 78-0786-07 39 RAGENT NEPHELOMETER (SN) 78-078G-02 38 SEIFF ATMOSPHERIC STRUCTUFE (SAS) 78-078G-01 38 SUOMI NET FLUX RADIOMETER (SNFR) 78-078G-04 34 WOO ATMOSPHERIC TURBULENCE (MTUR) 78-0786-06 37

PIONEER-A SEE PIONEER 6

PIONEER-B SEE PIONEER 7

PIONEER-c SEE PIONEER 8

PIONEER-D SEE PIONEER 9

PIONEER-F SEE PIONEER 10

PIONEER-G SEE PIONEER 11

VENERA 9 DESCENT CRAFT U.S.S.R. SAS 06/08/75 VENUS LANDER 75-050D 29 UNKNOWN PANORAMIC TELEPHOTOMETER FOR SURFACE 75-050D-01 30 IMAGERY

VENERA 10 U.S.S.R. UNKNOWN 06/14/75 VENUS ORBITER 75-054A UNKNOWN PANORAMIC CLOUD CAMERA 75-054A-01

VENERA 10 DESCENT CRAFT U.S.S.R. UNKNW 06/14/75 VENUS LANDER 75-054D 29 UNKNOWN PANORAMIC TELEPHOTOMETER FOR SWACE 75-054D-01 30 IMAGERY

VENERA 13 DESCENT CRAFT U.S.S.R. SAS 10/30/81 VENUS LANDER 81 -1 06D 29 UNKNOWN PANORAMIC TELEPHOTOMETER FOR SURFACE 81-106D-01 30 IMAGERY

VENERA 14 DESCENT CRAFT U.S.S.R. SAS 11/04/81 VENUS LANDER 81-11 OD 29 I UNKNOWN PANORAMIC TELEPHOTOMETER FOR SURFACE 81-llOD-01 30 IMAGERY

VENUS 9 SEE VENERA 9

VENUS- 67 SEE MARINER 5

VIKING 1 LANDER UNITED STATES NASA-OSSA 08/20/75 MARS LANDER 75-075C 48 ARVIDSON LANDER IMAGING 75-075C-06 50 BIEMA” MOLECULAR ANALYSIS 75-075C-04 57 HARGRAVES MAGNETIC PROPERTIES 75-075C-10 58 IUEIN BIOLOGY 75-075C-03 58 MICHAEL, JR. LANDER RADIO SCIENCE 75-075C-11 55 NIER ENTRY SCIENCE ATMOSPHERIC STRUCTURE 75-075C-02 56 NIER ENTRY SCIENCE NEUTRAL ATMOSPHERIC 75-075C-12 56 COMPOSITION NIER ENTRY SCIENCE IONOSPHERIC PROPERTIES 75-075C-14 56 TILLMAN METEOROLOGY 75-075C-07 57 TOULMIN, 3RD INORGANIC ANALYSIS 75-07 5C-13 57

VIKING 1 ORBITER UNITED STATES NASA-OSSA 08/20/75 AREOCENTRIC 75-075A 47

E-6 PAGE * PRINC.INVEST.NAME INVESTIGATION NAME * NO. * t

CARR ORBITER IMAGING 75-075A-01 49 FARMER MARS ATMOSPHERIC WATER DETECTION (MAWD) 75-075A-03 55 KIEFFER INFRARED THERMAL MAPPING (IRTM) 75-075A-02 53 MICHAEL, JR. ORBITER RADIO SCIENCE 75-015A-04 54

VIKING 2 LANDER UNITED STATES NASA-OSSA 09/09/15 MARS LANDER 75-083C 48 ANDERSON SEISMOLQGY 75-083c-oa 59 ARVIDSON LANDER IMAGING 75-083C-06 50 BIEMA” MOLECULAR ANALYSIS 15-083C-04 57 HARGRAVES MAGNETIC PROPERTIES 75-083C-10 58 KLEIN BIOLOGY 75-083C-03 58 MICHAEL, JR. LANDER RADIO SCIENCE 15-083C-11 55 NIER ENTRY SCIENCE ATMOSPHERIC STRUCTURE 15-083C-02 56 NIER ENTRY SCIENCE NEUTRAL ATMOSPHERIC 75-083C-12 56 COMPOSITION NIER ENTRY SCIENCE IONOSPHERIC PROPERTIES 15-083C-14 56 SHORTHI LL PHYSICAL PROPERTIES 15-083C-01 51 TILLMAN METEOROLOGY 15-083C-07 51 TOULMIN, 3RD INORGANIC ANALYSIS 75-083C-13 50

VIKING 2 ORBITER UNITED STATES NASA-OSSA 09/09/15 AREOCENTRIC 15-083A 48 CARR ORBITER IMAGING 75-083A-01 49 FARMER MARS ATMOSPHERIC WATER DETECTION (MAWD) 75-083A-03 55 KIEFFER INFRARED THERMAL MAPPING (IRTM) 75-083A-02 53 MICHAEL, JR. ORBITER RADIO SCIENCE 15-083A-04 55

VIKING-A LANDER SEE VIKING 2 LANDER

VIKING-A ORBITER SEE VIKING 2 ORBITER

VIKING-B LANDER SEE VIKING 1 LANDER

VIKING-B ORBITER SEE VIKING 1 ORBITER

VIKNG-A SEE VIKING 2 ORBITER

VIKNG-B SEE VIKING 1 ORBITER

VOYAGER 1 UNITED STATES NASA-OSSA 09/05/71 SATURN FLYBY 77-084A 67 BRIDGE PLASMA SPECTROMETERS 11-084A-06 IO BROADFOOT ULTRAVIOLET SPECTROSCOPY 77-08414-04 14 HANEL INFRARED SPECTROSCOPY AND RADIOMETRY 77-08444-03 74 KRIMIGIS LOW-ENERGY CHARGED PARTICLE ANALYZER AND 77-084A-01 IO TELESCOPE NESS TRIAXIAL FLUXGATE MAGNETOMETERS 11-084A-05 71 SCARF PLASMA WAVE (.01-56 KHZ) 11-O84A-13 IO SMITH IMAGING 77-084A-01 68 STONE HIGH- AND MODERATELY LOW-ENERGY 77-084A-08 73 COSMIC-RAY TELESCOPE TYLER RADIO SCIENCE TEAM 17-084A-02 15 WARW ICK PLANETARY RADIO ASTRONOMY 11-084A-10 76

VOYAGER 2 UNITED STATES NASA-OSSA 08/20/11 SATURN FLYBY 11-01 6A 68 BRIDGE PLASMA SPECTROMETERS 11-01 6A-06 IO BROADFOOT ULTRAVIOLET SPECTROSCOPY 77-076A-04 74 “EL INFRARED SPECTROSCOPY AND RADIOMETRY 77-076A-03 74 KRIMIGIS LOW-ENERGY CHARGED PARTICLE ANALYZER AND 77-076A-07 IO TELESCOPE

E-7 PAGE * PRINC.INVEST.NAME INVESTIGATION NAME * NO. * * *

LANE MULTIFILTER PHOTOPOLARIMETER, 11-Ol6A-11 16 2200-7300 A NESS TRIAXIAL FLUXGATE MAGNETOMETERS 11-016A-05 71 SCARF PLASMA WAVE (.01-56 KHZ) 11-016A-13 70 SMITH IMAGING 77-Ql6A-01 69 STONE HIGH- AND MODERATELY LOW-ENERGY 11-016A-08 13 COSMIC-RAY TELESCOPE TYLER RADIO SCIENCE TEAM 17-Ql6A-02 75 WARW I CK PLANETARY RADIO ASTRONOMY 17-016A-10 16

ORtlGIMAL PAGE IS OF POOR QUALITY