Pioneer F and G Mission to Juipter

8/8/2019 Pioneer F and G Mission to Juipter

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Pioneer F and G Missions

Man's first reconnaissance ofthe giant planet Jupiter willbegin with th e launch of two

spacecraft, Pioneers F and G,in 1972 and 1973 on missionswhich are planned to last forseveral years.

These spacecra f t are expected, to be the first to go beyond the

orbit of Mars, to pass throug hthe Asteroid Belt and to use

•Jupiter 's gravity to escape thesolar system. After a t r ip ofmore than a billion m iles, eachcraf t will spend about a weekswinging around Jupiter , with

maximum scientific re turn dur -ing closest approach, to w ithi nabout 90,000 miles.

The bizarre and spectacularplanet Jupiter is potentially themost in teres t ing in the solars y s t e m . Striped in y e l l o w -orange and blue-gray like anenormous rubber ball, it has ahuge red "eye" in its southernhemisphere. Its mass is morethan twice that of all the otherplanets combined. Scientis tsrecently have raised the possi-bili ty of life on the planet. Ithas 12 moo ns and, like a small

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The Pioneer Project is managed by the National Aeronautics and Spa

Research Center, Mountain View, California, for the Office of Space Scien

Headquarters, Washington, D.C.



Spacecraft

Pioneers F and G are iden-t ical spacecr aft weighing about570 pounds apiece, including65 pounds of scientific inst ru-

ments. Each will be capableof performing 13 scientific ex-periments, and photographingJupiter in better detail thanEarth-based telescopes.

PIONEER JUPITER SPACECRAFT



Navigation, Attitude Control, and Propulsion

For navigation, the Dopplershift in frequency of the Pio-neer radio signals will be usedto calculate continuously the

speed, distance, an d positionof the spacecraft. The Dopplershift is caused by motion ofth e spacecraft and is measuredby ground t racking.

Because the planes of the or-bits of the Earth and of Jupi-

ter almost coincide, the mostefficient trajectories to Jupiter

lie in the Earth's orbital plane(the ecliptic).

Pioneers F and G will be

positioned in the ecliptic planeb y point ing their high-gain ,na r r o w -be am dish a n t e n n a scontinuously at the Ear th . The

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EARTH WILL ORBIT SUN TWICE JUPITER

COMPLETES 1/6 REVOLUTION DURING MISSION



ATTITUDE CONTROL AND PROPULSION

EARTH ORBIT

SPACECRAFT TRAJECTORY

RADIO SIGNAL PATTERN

FROM GOLDSTONE TRACKING

STATION, CALIFORNIA

CHANGE IN SPIN-RATE VELOCITYTHRUSTERS

FIRE IN UNISON

CONSTANT

EARTH-POINT

CHANGE IN a ATTITUDE

ATTITUDE 1 THRUSTERSf=» PULSE

CONSTANT

EARTH-POINT

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photopola r imete r will show theent i re planet , while at closest

approach (to within one planet

diameter, 86,900 miles) the im-age will cover abou t 25 per centof the planet 's surface. This

pic ture will show the term inator(the line between sunlit and

dark hemispheres) , which isn e v e r seen f r om the Earth.

Scanning in strips 0.03° wide,the camera will complete a pic-ture in from 25 to 110 m inutes.



Jupiter

Jupiter has a mass some 318

t imes that of the Earth. Tw oof its 12 moons, Ganym edeand Cal l i s to , are larger than

the Earth's moon.The a tmosphe re is made

up of hydrogen with minoramo u n t s of methane and am-monia , prohably hel ium, andsome water. Temperatures inthe upper atmosphere may be

near room temperature. Theseconditions could produce thebuilding blocks of life, or evenlife i tself.

The sur face is hidden by a

JUPITER'S

NORTH POLAR

NORTH N

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SOUTH

SOUTH POLAR

dense layer of clouds whichform bright yel low-orange andslate blue bands (atm ospher ecurrents) around the planet .Jupi te r has a huge "eye" or Red

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Electric Power T

At Jupiter and beyond, so-

lar radiation is too weak to

efficiently provide power from

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RADIOISOTOPE THERMOELECTRIC

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solar cells, so four radioiso-tope thermoelectric generators(RTG's) will be used. Two

pairs of RTG's are mountedat the ends of two booms,120° apart. The RTG's.deviceswhich convert nuclear energyto electricity, provide 160 wattsof power at launch with poweroutput expected to be at least120 watts five years later. The

RTG's are fueled with Pluto-nium 238 dioxide, and their nu-clear energy (heat) is turnedinto electricity by 90 thermo-electric couples.

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MODEL OF JUPITER INTERIOR

CLOUD TOPS

AMMONIA CRYSTALSAMMONIA DROPLETS

UPPER I AMMONIA VAPORATMOSPHERE | ICE CRYSTALS

WATER DROPLETSWATER VAPOR

LIQUID AND/OR SOLID HYDROGEN

METALLIC HYDROGEN

INTERNAL ENERGYSOURCE GRAVITATIONAL

OR RADIOACTIVE

ROCKY SILICATES

METALLIC ELEMENTS

The planet p e r i o d i c a l l yemits huge surges of radionoise. It has a magnetic field

estimated to be 20 t imes asstrong as the Earth's, and ra-

diation belts estimated to bea million t imes more intensethan Earth's.

Jupiter appears to radiatethree t imes as much energy as

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PIONEER PASSAGE THROUGH

JUPITER'S MAGNETIC HELD

AND RADIATION BELTS

MAGNETIC

AXIS

CHARGED PARTICLESFROM THE SUN TRAPPED

IN JUPITER'S MAGNETIC FIELD

SPACECRAFT TRAJECTORY

AND PATH ACROSS

JUPITER'S SURFACE

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MARS

BOUNDARY OF HELIOSPHERE

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SOLAR COSMIC RAYS

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Mission Events and Operations

EARTH ATENCOUNTER

ASTEROID BELT

RADIO SIGNAL

45 MINUTES45 MIN



The flights to Jupi ter willtake from 630 to 7 95 days, withthe shorter trip times resultingfrom launches during the ear-

lier days of the 15-day launchwindows.

Mission events include: lift-

o f f , passage thr ou gh the Earth's

shadow, acqu i s i t i on of thespacecraft by the Deep SpaceNetwork (DSN) and first orien-

tation to point the spacecraftantenna toward the Ear th .V Exper iments will be tu rned

on one at a time, starting anhour af ter launch. After four

hours , the spacecraft, travelingat half-a-million miles per day,wil l have passed out of theEarth's magnetosphere into i n _ -

terplanetary space.Ground computers will con-

stantly refine calculations ofthe spacecraft trajectory. Con-trollers will correct the trajec-tory at four days and again at30 days, to precisely target th e

spacecraft for its encounterwith Jupiter hundreds of dayslater.

Attitude changes to sharpenEar th-poin t ing of the space-

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round t r ip comm unica tion t imeof 90 minutes due to l imita t ionsof light speed.

Hazards at planet encounter

include possible crippling dam-age from Jupiter 's radiationbelts.

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Data Return, Command, and Tracking

NASA's Deep Space Network(DSN), operated by the Jet

Propu l s ion Labora to ry , w i l ltrack and receive data from

the Pioneers. For early partsof the mission, tracking will beby the DSN's 85-foot (26-me-ter) antennas. W here high rates

of data re turn are required,the powerful global net of 210-foot (64-meter) antennas of the

D SN will take over. A t Jupi terdistance, th e 85's can receive128 bits per second (EP S), w hilethe larger 210-foot dishes canhear 1024 EPS. The 210's will

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te r , M ountain View, California.

I n c o m i n g telemetry data

from the spacecraft will be re-

ceived at the DSN stations,and imm edia te ly fo rm at ted forhigh-speed transmission to the

SFOF computers. These com-puters will check for criticalchanges and provide data foranalysis by specialists on the

spacecraft , on the experiments,and on ground systems. Theiranalyses will be used immedi-

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The Experiments-What They Tell

Magnetic Fields

Magnetometer — will m apthe in te rp lanetary magnet ic

field beyond the orbit of Mars,Jupiter 's magnetic fields, andthe modulation of Jupiter's

magnetic fields by its innermoons.

The Interplanetary SolarWind and the Heliosphere

Plasma A n a l y z e r — w i l lmapth e density an d mechanismsof

th e solar wind (ions and elec-t rons f lowing out from theSun) beyond the orbit of Mars;will determine solar wind in -teractions with Jupi ter , includ-ing the planet ' s b ow shockwave; and will look for theboundary at which the solarwind and solar atmosphere(the heliosphere) end and in-terstellar space begins.

Cosmic R a y s , Jupiter'sRadiation Belts and RadioSignals

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electrons) w i t h Jupiter and

w i t h i n Jupiter 's radiation

belts.

Jupiter's Charged Particles

Geiger Tube Telescope,

Trapped Radiation Detec-

tor — These tw o experimentswill a t tempt to learn the con-

tents and mechanisms of Jupi-ter's radiation belts by mea-suring the intensities, energies,and distr ibution of energeticelectrons and protons in the

belts, and will study Jupi ter 'shuge, periodic radio signals.

Asteroids, Meteoroids,Interplanetary Dust, and

Celestial Mechanics

Asteroid-Meteoroid Detec-tor — consists of four opticaltelescopes which can detect as-

teroids and meteoroids as smallas 1/100,000th gram by mea-suring sunlight reflected fromthem. The instrument can mea-sure particle concentrations,

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MAGNETOMETER

COSMIC RAY TEL

INFRARED RADIOM

CHARGED PARTIC

TRAPPED RADIATI

ULTRAVIOLET PHO

GEIGER TUBE TEL

IMAGING PHOTOP

PLASMA ANALYZE

METEOROID DETE

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Celestial Mechanics — Ex-perimenters will use precisionDoppler tr ackin g of the Pioneerradio signals to improve calcu-lations on: the mass of Jupiter,character of the Jovian gr avityfield, mass of Jupiter's 12moons, Earth's orbit, and othersolar system data.

Interplanetary Hydrogen,

Helium, and Dust;

The Heliosphere; Jupiter's

Atmosphere,Temperatures,Auroras, and Moons

Ultraviolet Photometer —

will determine the density ofneutral hydrogen in interplan-etary space, will attempt tofind the limits of the helio-sphere by measurements o fh y d ro g e n d i s t r i b u t i o n , w i l lmeasure the hydrogen-heliumrat io in Jupiter's uppe r andlower atmospheres, will lookfo r Jovian auroral activity

near both poles, and for phe-nomena resulting from pas-sages of the moon, lo. Mea-surements of light in the farultraviolet given off by hydro-

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the hydrogen-helium rat io inthe atmosphere.

Occultation Experiment —will measure effects of Jupiter's

a tmosphe re on the Pionee rradio signals as the spacecraftdisappears behind the planetand reappears aga in . These

changes will show th e refrac-

tive index of the planet's at-mosphere, add to knowledge ofit s hydrogen-helium rat io , andshow electron densi ty in theionosphere.

Imaging Photopolarimeter

—wil l measure intensities andpolarization of visible light. Itsmeasurements of reflected light

(zodiacal light) will be used tocalculate the amount , d is t r ibu-tion, an d origin (from asteroidsand comets) of interplanetarydust. A t Jupiter, experimenterswill use the data to at tempt tofind the structure and compo-

sition of the Jovian clouds an datmosphere, data on the plan-et's thermal balance, and to

retrieve close-up pictures. Theinstrument also will at tempt to

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t Team

1ATOMIC ENERGY

COMMISSION

Space Nuclear Systems Division

D. S. GabrielSpace Nuclear Sys tems Office

G . A . N e w h y

Isotope Power Systems Project

Branch — H . Jaf feSNAP-19/Pioneer Project

1

Teledyne Isotopes

NASA HEADQUARTERS PROGRAM M A N A G

OSSA— Dr.J.E.Naugle

Planetary Programs —R. S. Kraemer

Pioneer Programs Manager— F. D. Kochendorfe

1

NASA-AMES RESEARCH CENTER (ARC

PROJECT MANAGEMENT

Director — Dr. Hans MarkDirector of Development — J. V . Foster

Pioneer Project Office

Project Manager— C. E Hall

Project StaffManagement Control — J. R. S pah rMission Analysis & Launch Coordination — R. U. Hofstett

Project Support

Reliability & Quali ty Assurance— J . R. Mulk emR. O . Convertino

Magnetics — E. J. lufer

27





Experiments and Experimenters

Instrument

1. Imaging Photo Polarimeter

2. Helium Vector Magnetometer

3. Plasma Analyzer

4. Charged Part icle Instrument

5. Geiger-Tube Telescope

6. Cosmic Ray Telescope

7. Trapped Radiation Detector

8. Ultraviolet Photometer

Principal Investigator

Dr. Thomas GehrelsUniversity of Arizona

Dr. Edward J. Smith

Je t Propulsion LaboratoryDr. John H. WolfeNASA-Ames Research Center

Dr. John A. SimpsonUniversity of Chicago

Dr. James A. Van AllenUniversity of Iowa

Dr. Frank B. McDonaldNASA-Goddard Space F light Center

Dr. R. Walker FilliusUniversity of California at San Diego

Dr. Darrell L. JudgeUniversity of Southern California

29



,

Instrument

9. Infrared Radiometer

10. Asteroid-Meteoroid Detector

11. Meteoroid Detector

12 . The spacecraft radio trans-mitter used fo r S-Bandoccultation experiment

13 . The space craft and the

Deep Space Network Dopplerradar used fo r celestialmechanics exper iment

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Pioneer Accomplishments

Pioneers 6 to 9 continue to op-erate in solar orbit, and some oftheir accomplishments are:

1. The most precise determinationso far of characteristics of thesolar atmosphere (the helios-phere) .

2. Determinat ion of solar cosmicray and solar wind flow pat-terns, an d magnetic an d electricfield mechanisms in the solaratmosphere.

3. Longest-lived operational inter-planetary spacecraft (Pioneer6, launched December 16 , 1965).

4. Pioneers 6 to 9, by the end of1971, had achieved 230 months ofday- to-day t racking and dataacquis i t ion . Almos t 20 bill ion

data bits had been received , pro-cessed, analyzed, an d reportedto the scientific comm uni ty . Atotal of 26,000 commands hadbeen transmitted to these fourspacecraft.

8. Fon

9. Fin

5. First use of telecomm unicationscharacter is t ics fo r spacecraf torientation.

6. First gathering of space we atherdata for operational use.

7. First spacecraft to use convolu-tional coding/sequential decod-in g (Pioneer 9).

10 .

11 .

31



12. Most distant intelligible telem-etry data from Earth, an d mostdistant use of command func-tions, 170 million miles (Pio-neer 6 ).

13. First spacecraft to define char-acter of Earth's magnetic tail(Pioneers 6 and 7).

14. First spacecraft to use linearlypolarized S-band antenna andtherefore only spacecraft able toconduct Faraday rotation expe-riments durin g solar occultation(Pioneers 6 and 9).

15. First spacecraft equipp ed with

a t e lecommunica t ions range-adaptive telemetry system.

16 . First major spacecraft systemdesigned, developed, and deliv-ered on a fixed-price incentive-fee contract.





The Pioneer spacecraft havea record of reliabili ty and per-formance which makes themcand ida t e s f o r f u t u r e d e e pspace missions.



National Aeronautics and Space AdministrationAmes Research Center

Moffett Field, California 94035

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Pioneer F and G Mission to Juipter

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