isee3 press kit

8/8/2019 ISEE3 Press Kit

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NASA NewsNational Aeronautics and

Space AdministrationWashington. D C 20546AC 20 2 755-8370

For Release IMMEDIATE

Press Kit Project ISEE 3RELEASE NO: 78-118

Contents

GENERAL RELEASE.................................. 1-8

ISEE 3 SCIENTIFIC EXPERIMENTS.................... 9

ISEE 3 SCIENTIFIC INSTRUMENTS.................... 10-13

MISSION SUPPORT.................................. 14

ISEE PROGRAM MANAGEMENT.......................... 14

DELTA LAUNCH VEHICL E (2914).. .................... 14-15LAUNCH OPERATIONS................................ 16

LAUNCH SEQUENCE FOR ISEE 3 . . . . . . . . . . . . . . . . . . . . . . . 17

ISEE 3 TEAM...................................... 18-19


2/22

Iu/\s/\NewsNational Aeronautics and

Space AdministrationWashington. D C 20546AC 20 2 7 5 5 - 8 3 7 0

N i c h o l a s P a n a g a k o sH e a d q u a r t e r s , Wa s h i n g t o n , D . C .(Phone : 2 0 2 / 7 55-3680)

Fc Ir Release

Immedia te

J o s e p h M c R ob er tsG od dard S p ac e F l i g h t C e n t e r , G r e e n b e l t , M d .(Phone: 301/982-5566)

RELEASE N O : 78-118

T H I R D SUN-EARTH SATELLITE SET FOR LAUNCH

NASA t h i s month f o r th e f i r s t t i m e w i l l l a u n c h a

s p a c e c r a f t t o t h e S u n -E ar th l i b r a t i o n p o i n t -- t h a t p o i n t

i n s p a c e w here t h e g r a v i t a t i o n a l p u l l of t h e S u n j u s tb a l a n c e s t h a t of t h e E ar th -M o on s y s t e m -- a b o u t 1 . 6m i l l i o n k i l o m e t e r s ( o ne m i l l i o n m i l e s ) away.

ISEE 3 , t h e t h i r d i n a s e r i e s of I n t e r n a t i o n a l Sun

E a r t h E x p l or e r s p a c e c r a f t , w i l l be l a u n c h e d t o w a r d t h e

l i b r a t i o n p o i n t a t o p a D e l t a r o c k e t f r o m N A S A ' s Kennedy

S p ac e C e n t e r , F l a . , a b o u t Aug. 12.


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From its vantage point, ISEE 3 will measure the

solar wind constantly emitted by the Sun and other solar

phenomena such as sunspots and solar flares, unperturbed

by the influence of Earth, while I S E E 1 and 2 -- inlooping trajectories around the Earth since last fall --

measure the effect of these phenomena on the near-Earth

environment.

The coordinated effort is expected to result in a

better understanding of how the Sun controls the Earth's

fluctuating near-space environment, and of a variety of

solar-terrestrial phenomena, including weather and climate,

energy production and ozone depletion in the atmosphere.

Because of its unusual trajectory and target position

in space, ISEE 3 must be launched within a five-minute

time period between Aug. 12 and 1 3 or between Aug. 21 and 25.

Once the 469-kilogram (1,033-pound) spacecraft reaches

the libration point, some 78 days after liftoff, it will be

injected into a "halo" orbit by an onboard hydrazine gas

propellant system. The propellant will not only place the

spacecraft in an orbit in the ecliptic plane (the plane in


4/22

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T h e o r b i t h a s b ee n d e si g ne d t o p a s s s l i q h t l y above

an d be low t h e e c l i p t i c p la n e s o t h a t i t w i l l a v o id e x c e s s i v e

s o l a r i n t e r f e r e n c e w i t h s p a c e c r a f t c om mu nic at io ns ba ck

t o w a r d E a r t h . T o a n E a rt h- b as e d o b s e r v e r , t h e s p a c e c r a f t

w i l l a p p e ar t o be o r b i t i n g t h e Sun. I n f a c t , i t w i l l be

t r a c i n g a h a l o above t h e E a r t h . I t w i l l t a k e a p p r o x i m a t e l ys i x m on th s t o make o n e r e v o l u t i o n .

The h a l o o r b i t p a t h i s t h e most u n u s u a l e v e r p ro p o s ed

f o r a NASA s p a c e m i s s i o n . The p l a n t o place I S E E 3 i n

t h i s o r b i t w a s d e v i s e d by D r . R o b e r t W . F a r q uh a r o f t h e

G od da rd S p a ce F l i g h t C e n t e r i n G r e e n b e l t , Md., who

o r g i n a t e d t h e c o nc ep t i n h i s d o c t o r a l t h e s i s .

T h e D e l t a r o c k e t i n i t i a l l y p l a c e s t h e s p a c e c r a f t i n a

t r a j e c t o r y aimed a t t h e l i b r a t i o n p o i n t , and i n 20 d a y s

I S E E 3 w i l l b e v e r y c l o s e t o t h e h a l o o r b i t a l p o s i t i o n .

B u t t h e f i n a l i n s e r t i o n i n t o o r b i t w i l l o c c u r a b o u t t h r e e

mon ths l a t e r . D ur in g t h e t r a n s f e r p ha se from E a r t h o r b i t

t o h a l o o r b i t , s e v e r a l u nu su a l t r a j e c t o r y maneuve rs a r e

r e q u i r e d to a c c u r a t e l y p l a c e t h e s p a c e c r a f t a t t h e

i n s e r t i o n p o i n t .


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A f t e r I S E E 3 h as bee n p l a c ed i n t o t h e p r op e r o r b i t ,

s m a l l s t a t i o n k e e p i n g m an eu ve rs w i l l t a k e p l a c e a t

i r r e g u l a r i n t e r v a l s . A pp ro xi ma te ly e i g h t m an eu ve rs p e r

y e a r w i l l b e r e q u i r e d of t h e s p a c e c r a f t h y d ra z in e s ys te m

t o m a in t a i n t h e s a t e l l i t e ' s e q u i l i b r iu m a lo ng t h e o r b i t a l

p a t h . ISEE 3 w i l l c a r r y e no ug h h y d r az i n e p r o p e l l a n t t o

a s s u r e a n o r b i t a l l i f e t i m e of a t l e a s t t h r e e y e a r s .

A c c or d in g t o P r o j e c t M anag er J e r e m i a h J . Madden o f

Goddard , w h o i s managing t h e I S E E 3 p ro gr am f o r NASA, t h e

u n u s u al o r b i t w as c h o se n f o r ISEE 3 " b e c au s e o f t h e

r e l a t i o n s h i p be tw een I S E E 3 a nd t h e o t h e r t wo I S E E

s a t e l l i t e s t h a t w e r e l a u n ch e d f r o m C ape C a n a v e r a l l a s t

O c t o b e r. 'I

" I n e f f e c t , " s a y s Madden, "ISEE 3 w i l l b e s o r t of a n

e a r l y w ar ni ng s a t e l l i t e f o r a c t i v i t y on t h e Sun. I t w i l l

p i c k u p s o l a r w in d o r p a r t i c l e s s p e e d i ng a way f ro m t h e Sun

a f u l l h ou r b e f o r e t h e two o t h e r s p a c e c r a f t do s o . These

s p a c e c r a f t a r e i n h i g h ly e l l i p t i c a l o r b i t s r an gi ng from a bo ut

4 8 0 k m ( 3 0 0 m i . ) t o a l m o s t 1 4 4 , 8 0 0 km ( 9 0 , 0 0 0 m i . a b o v e E a r t h .

T h i s t e l l s s c i e n t i s t s a l o t abo u t t h e Sun and how i t changes w i t h

t i m e a n d d i s t a n c e . I n f a c t , t h i s w i l l be t h e f i r s t t i m e


6/22

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ISEE 3, in addition to providing a far-out Sun--l;arth

measuring platform, will also be useful for research

activities on the origin of galactic cosmic rays a n d

recently discovered gamma ray bursts. All three

spacecraft will be closely observing phenomena at

solar maximum for the new 11-year solar cycle which beganin June, 1976.

The three-spacecraft mission involves 117 scientific

investigators representing 35 universities and 10 nations.

ISEE 3 carries 1 3 different scientific instruments, three

of them by foreign investigators in Holland, Germany and

France.

ISEE 1,managed by Goddard, and ISEE 2 , managed by the

European Space Agency (ESA), were the first set of

spacecraft designed to be used together to investigate

Earth's immediate space environment.

The use of three spacecraft, separated by a variable

distance, allows scientists to study the boundaries betwee?

interplanetary space and the space controlled by the Earth,

and the nature of fluctuations in the boundaries.


7/22

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T h es e b o u n d a r i e s i n c l u d e t h e p l as m a pa u se , t h e p o s i t i o n a t

w h i c h t h e r e i s a d r am a t i c d ro p i n t h e d e n s i t y of t h e m a g n e t o -

s p h e r e ( t h e m a g n e ti c e n v e l o p e w h ic h s u r r o u n d s t h e E a r t h ) ;

t h e m a gn et op au se , w he re t h e m a g n et ic f i e l d o f the E a r t h

meets t h a t o f t h e s o l a r w i nd ; t h e bow s ho c k, a sort of

bow wave c r e a t e d b y t h e m o t i o n o f t h e s o l a r w i n d p a s t the

E a r t h , and s e v e r a l l e s s o b v i o u s f e a t u r e s o f t h e Earth's

m a g n e t i c t a i l .

I S E E 3 w i l l o b t a i n n e a r l y c o nt in u ou s d a t a o n t h e

f l u c t u a t i n g s o l a r w i nd , a nd on s p e c i a l s o l a r phenom ena

s u c h as s o l a r f l a r e s an d s u n s p o t s , w h ich a r e a p p e a r i n g

m o r e f r e q u e n t l y a s t h e s o l a r c y c l e moves i n t o it s most

a c t i v e s t a t e .

I n c e r t a i n i n s t a n c e s , t h i s w i l l g i v e s c i e n t i s t s on t h e

g r o u n d t i m e t o make i n p u t s t o onboard i n s t r u m e n t a t i o n on

t h e m o t h e r- d a u gh t e r (ISEE 1 and 2 ) s p a c e c r a f t t o l o ok fo r

c o r r e l a t i n g p h e n o m e n a . A t t h e same t i m e , s o u n d i n g r o c k e t s

c an b e f i r e d fro m any g l o b a l l o c a t i o n t o i n v e s t i g a t e

:her a s i * - > c t s f o n r u sh i n g s o l a r wi nd .


8/22

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A s part of this program, ground stations, sounding rockets,

b a l l o o n s , a i r c r a f t and satellites, including the ISEE

spacecraft, will look at the same phenomenon simultaneously

from different parts of the Earth, including polar areas

and space. Data exchange offices have been established

in Meudon, France and Boulder, COlo. Meanwhile a

sophisticated Satellite Situation Center ( S S C ) at Goddard

will calculate satellite orbits which will be published

through the Boulder office. The published S S C orbits are

designed for correlation with the various IMS systems to

indicate when spacecraft data are likely to be especially

fruitful.

Although numerous other spacecraft have been separately

probing the magnetosphere since the early 19GOs, the ISEE

satellites carry instrumentation 10 times more sensitive

than previously flown. As a result, much fine detail

essential to understanding the range of Sun-Earth phenomena,

the entire environmental system of Earth and theinteractions between the two is now available for the

first time.


9/22

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N A S A i s r e s p o n s i b l e fo r ISEEs 1 and 3 , t h e D e l t a l a u n c h

v e h i c l e , t r a c k i n g a nd d a t a a c q u i s i t i o n and d a t a p r oc e s s i n g .

E S A i s r e s p o n s i b le f o r t h e I S E E 2 s p a c e c r a f t and i t s

o p e r a t i o n .

Goddard w i l l p r o v i d e o r b i t a l c o m p u t a t i o n , a t t i t u d e

d e t er m i na t io n and s p a c e c r a f t c o n t r o l s u p p o r t t o t h e ISEE

m i s s i o n s d u r i n g t h e p la n ne d t h r e e - y e a r l i f e t i m e of t h e

s a t e l l i t e s . ESA, i n c o o r d i n a t i o n w i t h G od da rd , i s

r e s p o n s i b le f o r o p e r a t i n g t h e I S E E 2 s p a c e c r a f t a n d

s o f t w a r e f o r maneuver d e t e r m i n a t i o n a n d c o m p u t a t i o n .

ISEE 3 i s b a s e d o n G o d d a r d d e s i g n s , b u t i t was

f a b r i c a t e d a nd t e s t e d by F a i r c h i l d Sp ace and E l e c t r o n i c s C o . ,

Germ antow n, Nd. Most of i t s c o m p o n e n t s e i t h e r w e r e made a t

Goddard o r s u p p l i e d b y i n d u s t r i e s a nd u n i v e r s i t i e s .

G od da rd ma na ge s t h e D e l t a l a u n c h v e h i c l e p ro gr am f o r

NASA's O f f i c e of S p a c e T r a n s p o r t a t i o n Systems. McDonnell

Douglas A s t r o n a u t i c s Co., H u n t in g t o n B e ac h, C a l i f . , i st h e p r i m e c o n t r a c t o r .

(END O F GENE% RELEASE. BACKGROUND INFORMATION F O L L O W S )


10/22

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Instrument

ISEE 3 SCIENTIFIC EXPERIMENTS

Principal Investigator

Solar Wind Plasma S. J. Bame

Magnetometer E. J. Smith

Low Energy Cosmic Ray D. Hovestadt

Medium Energy Cosmic Ray T. von Rosenvinge

High Energy Cosmic Ray H. H. Heckman

Plasma Waves F. L. Scarf

Cosmic Ray Electrons P. Meyer

Protons R. Hynds

X-rays and Electrons K. A. Anderson

Radio Mapping J. L. Steinberg

Plasma Composition K. W. Ogilvie

High Energy Cosmic Ray E. C. Stone

Ground Based Solar Studies J. M. Wilcox

Affiliation

Los AlamosScientific Lab.,Los Alamos, N.M.

Lab., Pasadena,Calif.Max PlanckInstituteGarching, Germany

NASA Jet Propulsion

GSFC

University ofCalifornia

TRWRedondo Beach,Calif.

University ofChicago

Imperial Collegeof Science andTechnology, London

University ofCalifornia

Paris ObservatoryMeudon, France

GSFC

California Institute

of Technology,Pasadena, Calif

Stanford UniversityPalo Alto, Calif.


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I S E E 3 S C I E N T I F I C I N S T R U M E N T S

S o l a r Wind P l a s m a . T h i s i n s t r u m e n t i s d e si g ne d t o p r o v i d es o l a r wind i o n a nd e l e c t r o n p a r a m e t e rs on a c o n t i n u o u s b a s i s ,t o s t u dy t h e o r i g i n and e v o l u t i o n of s t r u c t u r e s i n t h ei n t e r p l a n e t a r y medium, a nd t o s t u d y t h e th e r m a l s t a t e of t h ei n t e r p l a n e t a r y p la sm a u n p e rt u rb e d by t h e E a r t h ' s bow s h o c k .P r i n c i p a l I n v e s t i g a t o r : S . J . B a m e , L o s A l a m o s S c i e n t i f i cL a b o r a t o r y , N . M.

Magn etometer. The magne tometer i s u se d t o s t ud y s o l a ri n t e r p l a n e t a r y p henomena s u c h a s t h e i n f l u e n c e on t h ei n t e r p l a n e t a r y f i e l d of h e l i o g r a p h i c l a t i t u d e , d i f f e r e n t i a ls o l a r r o t a t i o n , a nd c ha ng in g p h o t o s p h e r i c m a gn et ic f i e l d s .The e f f e c t s o f t h e i n t e r p l a n e t a r y f i e l d on t h e E a r t h ' sm a g n e t o s p h e r e -- s u c h a s t h e t r i g g e r i n g o f m a g n et o s ph e r ic st or ms --i s a l s o a m aj or i n t e r e s t . P r i n c i p a l I n v e s t i g a t o r : D r . E . J . S m i t h ,J e t P r o p u l s i o n L a b o r a t o r y, P a sa d en a , C a l i f .

Low Energy Cosmic Ray and G a m m a Ray B u r s t . T h i s i n s t r u m e n tw i l l m ea su re u l t r a lo w-e ne rg y c h ar g ed p a r t i c l e s a c c e l e r a t e da t t h e Sun i n t h e E a r t h ' s v i c i n i t y i n t h e i n t e r p l a n e t a r y m e d i u ma nd beyond t h e s o l a r s ys te m. P r i n c i p a l I n v e s t i g a t o r :D r . D . H o v e s t a d t , Max P l a n c k I n s t i t u t e , G a r c h i n g , G erm any.C o - I n v e s t i g a t o r s : D r . G . G l o e c k l e r a n d D r . B. Te e g a r d e n ,U n i v e r s i t y o f M a ry la nd .

Medium Energy C o s m i c Ray. The MECR i n s t r u m e n t w i l l s t u dy t h ec o m p o s i t i o n of s o l a r c o sm ic r a y s f r o m h y d r o g e n t h r o u g h i r o no v e r a n e n e rg y i n t e r v a l f ro m 0 . 5 t o 5 0 0 MeV/nucleon. I t w i l la l s o s t u d y e l e m e n t a l ab un da nc e o f g a l a c t i c c os mi c r a y s w i t hs p e c i a l e m ph as is o n t h e r e g i o n fro m z = 1 6 - 2 6 and t h e i s o t o p i c

c o m p o si t io n f r om h y dr og en t o n i t r o g e n , a nd w i l l be u s ed t oo b t a i n a c o m p r e h e n s i v e u n d e r s t a n d i n g o f g a l a c t i c and s o l a rcosmic r a y s by me a su r in g t h e i r s t r e a m i n g p a t t e r n s o v e r a b r o a dr a n g e of 0 . 5 t o 1 5 0 M e V. P r i n c i p a l i n v e s t i g a t o r : T . von Rosenvinge( a l s o P r o j e c t S c i e n t i s t ) GSFC.


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P l a s m a Waves ( I S E E 3 ) . I t w i l l s t u d y t h e b e h a v io r of t h e so la rwind an d d e t e r m i n e t h e r o l e s t h a t plasma waves p l a y ati n t e r p l a n e t a r y d i s c o n t i n u i t i e s ; a l s o p h y s i c a l e f f e c t 8 associatedw i t h w a ve -p a rt ic l e s c a t t e r i n g i n t h e s o l a r wind . PrincipalI n v e s t i g a t o r : F. L . S c a r f , TRW Systems Group, Redondo B e a c h ,C a l i f .

C o s m i c Ray E l e c t r o n I n s t r u m e n t . T h i s i n s t r u m e n t w i l l measu re

t h e e ne r gy s p ec tr um o f e l e c t r o n s i n t h e r a n g e f r o m 5 t o 400 MeV.T he se p a r t i c l e s a r e known t o o r i g i n a t e i n t h e Sun , come fromJ u p i t e r a nd t h e g a l a x y , w i l l i n t e r f e r e w i t h t h e Gamma Ray Burste x p e r i m e n t ( H o v e s t a d t ) . P r i n c i p a l I n v e s t i g a t o r : P . Meyer,U n i v e r s i t y of Chicago .

P r o t o n s . T h e i n s t r u m e n t w i l l s t u d y t h e t r a n s p o r t o f lo w-e ne rg y

s o l a r p r o to n s t h r ou gh i n t e r p l a n e t a r y s p ac e and t h e i r t r a n s p o r tf ro m t h e f l a r e s i t e ; t h e c o - r o t a t in g i n t e r p l a n e t a r y p r o t on ss t r eams a s s o c i a t e d w i t h s p e c i f i c s o l a r a c t i v e r e g i o n s ; t h ee f f e c t s of s h o c k waves a nd o t h e r t y p e s o f i n t e r p l a n e t a r yd i s c o n t i n u i t i e s on l ow -e n er gy p r o t o n p o p u l a t i o n s .l o w e n e r g y p r o t o n s a l s o w i l l be e x p l o r e d .D r . R . H yn ds , I m p e r i a l C o l l e g e , L on do n.

Q u i e t - t i m eP r i n c i p a l I n v e s t i g a to r :

X-Rays, E l e c t r o n s and G a m m a Ray Bur s t s .c o n s i s t s of two s e p a r a t e s e n s o r s y st em s and t h e i r a s s o c i a t e de l e c t r o n i c s .t i m e v a r i a t i o n of t h e s pe ct ru m o f 6 t o 2 2 8 k e V X-ray emi s s ionf rom s o l a r f l a r e s w i t h a t i m e r e s o l u t i o n of 1 s econd . Ex t r eme lys h o r t ( 1 0 s e co n d s) b u r s t s of gamma r a y s f r o m b e y o n d t h e s o l a rs y s t e m w i l l a l s o be o b se r ve d . T h e e l e c t r o n s e n so r i s d e s i g n e dt o s tu d y e l e c t r o n s i n t h e e n e r g y r a n g e b e tw e en s o l a r wi nd a n dg a l a c t i c cosmic r a y s . B e tween t he se t w o p a r t i c l e p o pu l a t i on st h e en e r g y s p e ct ru m , a n i s o t r o p y, a nd p r o p a g a t i o n c h a r a c t e r i s t i c sof t h e p a r t i c l e s c ha ng e d r a s t i c a l l y f ro m b u l k p la sm a t o s ingle ,p a r t i c l e c h a r a c t e r i s t i c s . T h i s i n s t r u m e n t w i l l i d e n t i f y andm ea su re t h e f l u x of e l e c t r o n s f ro m 2 t o 800 k e V. T h e s e lowe ne rg y p a r t i c l e s a r e p a r t i c u l a r l y s e n s i t i v e t o t h e a mount o fm a t t e r t r a v e r s e d i n terms of e n e r g y loss.

b l l l i h i d f

T h i s i n s t r u m e n t

T h e o b j e c t i v e o f t h e X-ray sys tem i s t o s t u d y t h e

Thus t h e y can b e u s e d


13/22

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Radio Mapping. The direction (two angles) of type I11 solarbursts at several frequencies will be measured. When using a

second spacecraft similarly instrumented or relying on solarrotation, one can obtain the 3-D map of the magnetic lines offorce which guide the electrons which produce type 111's from10 solar radii to 1 AU in or out of the ecliptic. PrincipalInvestigator: J. L. Steinberg, Paris Observatory, Meudon,France.

Plasma Composition. The relative abundance of ions in the solarwind at a distance of 1 AU and the relative population of theircharge rates will be measured. The relative abundances arerelated to the solar abundances and the charge states to thecoronal temperature structure since the interplanetary medium iscollisionless. The abundance measurements will yield informationabout the mechanism of fractionation in the corona andacceleration into the solar wind; the charge state measurementswill also provide information on the acceleration of heavy ions

from the corona into the solar wind. The "shock piston"phenomenon will be further explored, and used as an indicatorof the processes in the lower corona. The composition of themagnetospheric plasma will be simultaneously measured by anotherinstrument, so that a comparison may make the phenomena governingthe entry of plasma to the magnetosphere clearer. PrincipalInvestigator: K. W. Ogilvie, Goddard Space Flight Center.

High Energy Cosmic Rays. The isotopic abundances of all elementsfrom Li ( 1=3) to Ni ( 2 = 2 8 ) and their energy spectra in a rangefrom several MeV/nucleon to several hundred MeV/nucleon, outsidethe Earth's magnetosphere, will be determined. The Heavy IsotopeSpectrometer Telescope (HIST) will determine the isotopicabundances of solar and galactic cosmic ray nuclei in the 2 to200 MeV/nucleon energy range for all elements from lithium tonickle. This unique instrument complements the Hechman experiment.Principal Investigator: E. C. Stone, California Institute ofTechnology.

Ground-Based Solar Studies. Real-time observations of large-scale solar magnetic and velocity fields made with the Stanford


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Since solar flares have been shown to be most likely to occurnear a solar sector boundary, it is very possible that anunderstanding of the large-scale solar magnetic field improvesthe physical understanding of the flare mechanism and thecauses of solar activity may a l s o improve. The mean solarfield that will be observed with the Stanford Solar Telescopeis usually very similar to the interplanetary magnetic fieldobserved with spacecraft near the Earth. In particular, whenthe polarity of the mean solar field changes sign, a sectorboundary is usually observed near the Earth four or five dayslater. This prediction capability could enhance the spacecraftobservations of sector boundaries, and in particular newlyformed boundaries which may contain interesting magnetic loopstructures. In addition, the preference of large solar flaresand shock waves for positions near boundaries can be utilizedin the day-to-day planning of the spacecraft observations. TheStanford Solar Telescope will a l s o have the capability to ob-serve the average amplitude of the photospheric velocity fieldswithin an area near the center of the visible solar disk. Sometheories of the solar wind suggest that the solar wind velocityshould be related to the amplitude of these photospheric velo-city fields, and therefore, to the flux of wave energy goingup into the corona. Continuous correlative observations overmany solar rotations will be necessary to test these theoreticalideas. Principal Investigator: Dr. J. Wilcox, StanfordUniversity.


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MISSION SUPPORT

GODDARD NETWORK SUPPORT

The Goddard Space Flight Tracking and Data Network (STDN) isresponsible for all tracking and data acquisition for theISEE 3 spacecraft.

Only three stations (Madrid, Orroral and Goldstone) arepresently planned for use for the ISEE 3 during the orbitalphase where a 26-m (85-ft.) antenna is needed to receive tele-

metry.of spacecraft data during the 36-month initial mission life isset as a goal.

A data acquisition objective of 90 per cent recovery

ISEE PROGRAM MANAGEMENT

The memorandum of understanding between the European SpaceAgency and NASA, dated March 17, 1975, divides the project

responsibilities and provides for an international managementorganization. NASA is responsible for the ISEE 1 and 3spacecraft, Delta launch vehicle, tracking, data acquisitionand data processing. ESA is responsible for the ISEE 2spacecraft and its operation.

NASA's Office of Space Science is responsible for overalldirection and evaluation of the NASA portion of the program.The Office of Tracking and Data Acquisition has overall

tracking and data processing responsibility.

Goddard Space Flight Center has management responsibility forISEE 3 and is directly responsible for tracking and dataacquisition and data processing.

ISEE 3 is a Goddard-designed spacecraft with all its componentssupplied by United States industry.was done by Fairchild Space & Electronics Co.

Goddard directs the Delta rocket program and McDonnell DouglasAstronautics Co., Huntington Beach, Calif., is the primecontractor.

Integration and testing

DELTA LAUNCH VEHICLE (2914)


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F i r s t S t a q e

The f i r s t s t a g e i s a M cD on ne ll D o u g l a s m o d i f i e d T h o r b o o s t e ri n c o r p o r a t i n g n i n e s t ra p - on T h io k ol s o l i d - f u e l r o c k e t mo to rs .T h e b o o s t e r i s powered by a R o c k e t d y n e e n g i n e u s i n g l i q u i do xy ge n an d l i q u i d h y d ro c ar b on p r o p e l l a n t s .i s g im b al -m o un te d t o p r o v i d e p i t c h a nd yaw c o n t r o l f ro ml i f t o f f t o main e n g in e c u to f f ( M E C O ) .

The ma in eng ine

S e c o n d S t a g e

T h e s e c o n d s t a g e i s powered by a TRW l i q u i d f u e l , p r e s s u r e- f e de ng in e t h a t a l s o i s g imba l -moun ted t o p r o v i d e p i t c h a n d y a wc o n t r o l t hr ou gh t h e s ec on d s t a g e b u r n .u s e s e i g h t f i x e d no z z le s f o r r o l l c o n t r o l d u r i n g pow ered a ndc o a s t f l i g h t a s w e l l a s p i t c h a nd yaw c o n t r o l d u r i n g c o a s t an da f t e r s ec on d s t a g e c u t o f f (SECO). Two f i x e d n o z z l e s , f e d b yt h e p r o p e l l a n t t a n k he li um p r e s s u r i z a t i o n s y s te m , p r o vi d er e t r o t h r u s t a f t e r t h i r d s t a g e s e p a r a t i o n .

A n i t r o g e n g a s s y s t e m

T h i r d S t a g e

The t h i r d s t a g e i s t h e TE-364-4 s p i n - s t a b i l i z e d , s o l i d p r o p e l l a n tT h i o k o l motor.s e c o n d s t a g e .f i x e d t o t h e s p i n t a b l e ac co m pl is he s s pi n- up o f t h e t h i r d s t a g es p a c e c r a f t a s s e m b l y .t h i r d s t a g e m oto r .

I t i s s ec u re d i n t h e s p i n t a b l e mounted t o t h eThe f i r i n g of e i g h t s o l i d p r o p e l l a n t r o c k e t s

Th e I S E E s p a c e c r a f t a r e a t t a c h e d t o t h e


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LAUNCH OPERATIONS

Delta 144 with the ISEE 3 spacecraft will be launchedunder the direction of the Kennedy Space Center's ExpendableVehicles Directorate from Pad B , southernmost of the twolaunch pads at Complex 17, Cape Canaveral Air Force Station.

The Delta first stage and interstage were erected onPad B June 23. Mounting of the nine strap-on solid rocketmotors around the base of the first stage was accomplishedJune 26-27 and the second stage was erected June 2 8 .

The ISEE 3 spacecraft arrived at KSC June 29 and under-went initial processing at Hangar AE at Cape Canaveral AirForce Station. It was moved into the Spin Test FacilityJuly 21 and mated with the third stage Aug. 1. The space-craft/third stage assembly was moved to the pad and erectedatop the second stage Aug. 3 . The spacecraft was scheduledto be encapsulated Aug. 9 within the payload shroud whichwill protect it during its flight through the atmosphere.

countdown are conducted from the blockhouse at Complex ly bya joint government-industry team.

All launch vehicle and pad operations during the launch


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E v e n t

LAUNCH SEQUENCE F O R I S E E 3

T i m e A l t i t u d eK i l o m e t e r s / m i l e s

L i f t o f f 0 sec . 0 0

S i x S o l i d Motor B u r n o u t 3 8 s e c . 6 4

T h r e e Solid M o t o r I g n i t i o n 39 sec . 6 4

T h r e e S o l i d Motor B u r n o u t

N i n e S o l i d Motor J e t t i s o n

1 rnin. 1 8 s e c . 2 1 1 3

l m i n . 2 7 s e c . 26 1 6I

Main Eng ine Cu to ff (MECO) 3 min . 45 s e c . 9 1 56

F i r s t /S e c o n d S t a g e S e p a r a t i o n 3 min. 54 sec . 9 6 60

S ec on d S t a g e I g n i t i o n

F a i r i n g J e t t i s o n

S ec on d S t a g e C u t o f f #1 (SEC #1)

B e g i n C o a s t P h a s e R o l l (1 rpm)

End C o a s t P h a s e R o l l

S e c o n d S t a g e I g n i t i o n # 2

Second S t age Second Cu t -Off 2(SECO 2 )

T h i r d S t a g e / P a y l o a d S p in -u p

J e t t i s o n S t a g e I1

T h i r d S t ag e I g n i t i o n

T h i r d S t a g e B u r n o u t

P a y l o a d S e p a r a t i o n , A c t i v a t eR e t r o S y s t e m .

3 min. 56 s e c . 99 61

4 min. 56 s e c . 1 2 6 7 8

8 rnin. 4 4 s e c . 157 97

9 min. 2 3 s e c . 1 5 7 9 7

4 4 min. 23 s e c . 27 5 17 1

53 min . 31 s e c . 28 5 1 7 7

53 rnin. 52 sec .

54 min. 50 s e c .

54 min. 5 2 s e c .

5 5 min. 33 s e c .

56 min. 1 7 s ec .57 min. 30 s e c .

2 87

327

1 7 8

20 3


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ISEE 3 TEAM

NASA Headquarters

Dr. Noel S . Hinners

Andrew J. Stofan

Dr. Adrienne Timothy

T. Bland Norris

Dr. Harold Glaser

Frank Gaetano

Dr. Erwin R. Schrnerling

John F. Yardley

Joseph B. Mahon

Peter T. Eaton

William C. Schneider

Goddard Space Flight Center

Dr. Robert S . Cooper

Robert E . Smylie

Robert Lindley

Don Fordyce

Associate Administratorfor Space Science

Deputy Associate Administrator

Deputy Associate Administrator(Science)

Director, AstrophysicsPrograms

Director, Solar TerrestrialPrograms

ISEE Program Manager

ISEE Program Scientist

Associate Administrator forSpace Flight

Director of Expendable LaunchVehicle Programs

Manager, Delta Program

Associate Administrator forTracking and Data Acquisition

Director

Deputy Director

Director of Projects

Associate Director for Projects


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Goddard Center (cont d.~

James 0. Redding

John A. Hrastar

Martin A. Davis

David W. Grimes

William R. Russell

Robert Goss

E. Michael Chewning

Thomas C. Moore

Kenneth McDonald

K

Lee Scherer

Gerald D. Griffin

Dr. Walter J. Kapryan

George F. Page

W. C. Thacker

Wayne McCall

David Bragdon

Financial Manager

Mission Operations Manager

Scientific Instrument Manager

Delta Project Manager

Deputy Delta Project Manager,Te hn ca

Chief, Mission Analysis andIntegration Branch, Delta ProjectOffice

Delta Mission Integration Manager

Mission Operations Manager

Network Support Manager

Director

Deputy Director

Director, Space Vehicle Operations

Director, Expendable Vehicles

Chief, Delta OperationsDivision

Chief Engineer, Delta Operations

Spacecraft Coordinator

CONTRACTORS


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