Lunar-10 measurements of soft corpuscular radiatio

Grigorov, N. L.

Maduyev, V. L.

Mandelshtam, S. L.

Pisarenko, N. F.

Savenko, I. A.

Tindo, I. P.

English

NASA Technical Reports Server

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National Aeronautics and Space Administration 
Crrddard Space F1 i g h t  Csnter 
Cont tact No. NAS - 5- 12 487 
ST- LPS- PF - 10 528 
STUDY OF THE SOFT CORPUSCULAR RADIATIOK ON 
TiIE A S  "L U K A - I  0" 
hY 
N, L. Grigorov 
V, L. ?laduyev 
S. L. Mandrl'shtam 
N. F. Plscrrenko 
1. A. Savenko 
I. P, Tindo 
(USSR) 
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2 6  O C T O B E R  1966 
https://ntrs.nasa.gov/search.jsp?R=19670002879 2020-03-16T16:58:35+00:00Z
ST- LPS- PF- 10 528 
STUDY OF TilE SOFT CORPUSCULAR RADIATION ON 
THE AMS "L U N A-10" 
Doklady A.N.SSSR, 
Geof izika 
Tom 170, No. 3 ,  567 -9, 
Izdatel'stvo "NAUKA'@, 1966 
S U M M A R Y  
by N. L. Grigorov 
V.L.Maduyev 
S.L.Mande1'shtam 
N. F. Pisarenko 
I.A,Savenko 
1. P , Tindo 
This note deals with measurements of soft corpuscular radiation from 
the AMS Luna-LO. Description of the instrumentation is given. The conclu- 
sion derived uphold the probability of extension in antisolar direction of 
the Earth's magnetosphere tail over distance to 60 Earth's radii. Comparison 
is made of the observations obtained here with those of Dolginov, whose paper 
is part of these series on Luna-10. The registration of soft electrons is 
evidence that the magnetic field does not form closed lines around the Moon. 
registered by Gringauz are directed, while particles of substantially higher 
energies are quasi-isotropic, 
Attention is also dravn to the fact that the fluxes of soft electrons 
* 
* * 
The instrument package of Luna-10 included gas- ischarge counters SBT-9 
and SF, installed outside the satellite body. Their disposition is schematic- 
ally shown in Fig.1. The SBT-9 counter 
has a mica window of 0.2 cm2 area and 
1 . 2  mg cm-* in thickness. To offset, or 
decrease the effectiveness with respect 
to X-ray radiation, it was coated with a 
layer of gold 0.3mg c r 2  thick. There- 
tore, this counter could effectively mea- 
sure (efficiency close to 1) electrons 
with energies greater than 500 kev, and 
with low efficiency the X-radiation shor- 
ter than 1 0 A .  
minum foil of 0.5cm' area and 2.7 mg cm-l 
thickncqs. These counters could reRlqtct 
* IZUCHENIYE MYAGKOY KORPUSKULYARNOY RADIATS I I 
SF- I f i i : - I f l  I 
with energies greater than 40 kev, protons I 
3 
Fig. 1 The SF counters ave a window of alu- 
NA SPUTNIKE LUNY I*LUNA lo*' 
2 .  
t h e  X-ray r a d i a t i o n  s h o r t e r  than  14 A, e l e c t r o n s  with e n e r g i e s  h i g h e r  t h a n  
50 kev and protons w i t h  e n e r g i e s  above 800 kev. (Note t h a t  t h e s e  SF-counters  
were s p e c i f i c a l l y  designed for t h e  r e g i s t r a t i o n  of Moon's X-ray emission;  t h e  
corresponding in t e r i a l  is being processed and w i l l  be t h e  o b j e c t  of later pub- 
1 i ca t i on ) . 
Pulses  from t h e  SBT-9 counter  were r e g i s t e r e d  by a s c a l i n g  c i r c u i t  w i t h  
a l o g a r i t h m i c  s c a l e ;  t h o s e  from SF-counteres were r e g i s t e r e d  by t h r e e  indepen- 
d e n t  l o g a r i t h m i c  i n t e g r a t o r s .  
rogated t h e  measuring channel o u t p u t s  once every  two minutes. 
During measurement s e s s i o n s  t h e  te lemet ry  in te r -  
The readings  of t h e  c o u n t e r s  a r e  schemat ica l ly  represented  i n  F i g . 2 .  
CP&F- I I I 
F i g . 2 .  Headings of t h e  counters  f o r  t h e  per iod from 3 Apri l  t o  13 May; 
t h e  l e n g t h  of t h e  s t r o k e s  is  p r o p o r t i o n a l  t o  pulses / sec .  Radial  dashes  
i n d i c a t e  t h e  r e g i o n s  of t-he assumed e x t e n s i o n  of t h e  magnetosphere t a i l .  
. 
3. 
The 'background of t h e  SBT-9 counter  c o n s t i t u t e d  2 0 -  23 p u l s e s  i n  t h e  
cour se  of t h e  per iod  from 3 t o  23 A p r i l ,  bu t  from 23 A p r i l  t o  1 2  May, it 
f e l l  p r a c t i c a l l y  t o  t h e  l e v e l  of cosmic r a d i a t i o n .  We re la te  t h e  count ing  
ra te  i n c r e a s e  over  t h e  cosmic background dur ing  t h e  f i r s t  p a r t  of t h e  opera-  
t i o n a l  per iod  t o  t h e  r e g i s t r a t i o n  of Sun's X-ray r a d i a t i o n .  Besides t h e  in -  
d i c a t e d  f l u c t u a t i o n s  of t h e  background, i ts increase t o  50 pu l ses .  sec-1 was 
observed dur ing  t h e  per iod  from 8 t o  13 A p r i l ;  i t  was a p p a r e n t l y  due t o  
s o l a r  cosmic r ays ,  f o r  at t h e  beginning of April . .several  f l a r e s  were observed 
on t h e  Sun. 
The SF-counters were switched on only  on 8 A p r i l .  
2 May they were p a r t i a l l y  oFf-sca le ,  g i v i n g  p a r t i a l l y  t h e  l e v e l  of cosmic back- 
ground. The SF-111 coun te r  gave over t h e  e x t e n s i o n  of t h i s  per iod  a modulated 
s i g n a l  w i th  maximum near 300 pu l ses  .set" , which w a s  due t o  s a t e l l i t e  s p i n -  
ning. A t  t h e  same t i m e ,  t h e  s i g n a l  minimum corresponded t o  cosmic background 
( t h e  l i m i t s  of r ead ing  v a r i a t i o n s  of t h i s  coun te r  are shown i n  Fig. 2 by dashes) .  
The o f f - s c a l e  r ead ing  of coun te r s  SF- I and SF-I1 is a p p a r e n t l y  expla ined  
Between 8 A p r i l  and 
by t h e  f a c t  t h a t  Sun's X-ray r a d i a t i o n  a l s o  h i t  t h e s e  coun te r s .  
During measurement time, LUW.10 crossed  t h e  assumed e x t e n s i o n  of t h e  
Ea r th ' s  magnetosphere boundary four t imes  ( r e s p e c t i v e l y  on 4 A p r i l ,  8 t o  9 A p r i l ,  
2 t o  4 May and 7 May). I n  a l l  those  c a s e s  t h e  coun te r s  d e t e c t e d  a c l e a r  rise i n  
t h e  count ing  r a t e .  P a r t i c u l a r l y  i n t e r e s t i n g  a r e  the  concomi t tan t  measurements 
by SBT-9 and SF-counters f o r  t h e  period from 2 t o  5 May. 
Beginning w i t h  2 May, a l l  t h e  coun te r s  revea led  c l e a r l y  and s imul t aneous ly  
a n o t a b l e  increase of t h e  counting r a t e  ( t h e  SF-I counter  reamining o f f - s c a l e )  ; 
t h e  s i g n a l s  of a l l  coun te r s  are not modulated. The r ead ings  of a l l  of them 
v a r i e d  e n t i r e l y  synchronously,  r evea l ing  small d e c r e a s e s  and i n c r e a s e s ,  i n  par -  
t i c u l a r  on 5 May, when a l l  coun te r  r ead ings  showed a dec rease  t o  n e a r l y  t h e  l e v e l  
of cosmic background. The counting ra te  niaximum i n  t h a t  per iod  c o n s t i t u t e d  (upon 
s u b t r a c t i n g  t h e  cosmic background) : 50 p u l s e  .cm-2 s e c - l s t e r .  f o r  SBT-9 and 
GO pulse  .cm-2 sec -1ster. f o r  t h e  SF-counters ,  A f t e r  7 May t h e  r ead ings  of a l l  
coui i tc rs  decreases t o  t h e  level of cosmic background. 
7 May may be n a t u r a l l y  i n t e r p r e t e d  a s  t h e  r e g i s t r a t i o n  of a p p a r e n t l y  i s o t r o p i c  i n  
d i r e c t i o n  f l u x e s  of p a r t i c l e s , m o s t p r o b a b l y  e l e c t r o n s  wi th  ene rg ie s  E 
i n  t h e  r eg ions  of t h e  presumed magnetosphere boundary. These e l e c t r o n  f l u x e s  are  
c o r r e l a t i n g  w e l l  w i t h  f l u x e s  of s o f t e r  e l e c t r o n s  w i t h  E > 7 0 e v ,  measured by K. I. 
Gringauz - ET AL 
t h e  Ea r th ' s  magnetosphere t a i l  a t  t h e  d i s t a n c e  up t o  6 0 E a r t h ' s  r a d i i .  I t  should  
be noted, however, t h a t  t h e  measurement by Sh. Sh. Dolginov ET AL of t h e  magne- 
t i c  f i e l d ,  which are a l s o  published i n  t h e  c u r r e n t  j o u r n a l  (ST-LPS -PF- 10530) ,  
a p p a r e n t l y  f a i l  t o  g i v e  d i r e c t  i n d i c a t i o n  on the c r o s s i n g  by t h e  Moon of t h e  
r e g i o n  of magnetosphere t a i l ,  though on 4 Play t h e r e  w a s  observed a sma l l  i n c r e a s e  
i n  t he  a b s o l u t e  v a l u e o f  t h e  magnetic f i e l d  by comparison w i t h  t h e  per iod  7-11 
and 18- 2 1  Apr i l .  I t  should be a l s o  noted t h a t  t h e  r e g i s t r a t i o n  of e l e c t r o n s  
wi th  e n e r g i e s  40-  50 kev and, t h e  more SO, of e n t i r e l y  s o f t  e l e c t r o n s ,  is e v i -  
dence t h a t  t h e  magnetic f i e l d  does n o t  form c losed  l i n e s  around t h e  Moon. 
The i n c r e a s e s  coun te r  readings  on  3 and 8 - 4  A p r i l  and a l s o  on 2- 3 and 
> 40 kev 
and publ i shed  i n  the same j o u r n a l  (ST-LPS-PF- 10529) .  
These d a t a  make q u i t e  probable t h e  e x i s t e n c e  i n  t h e  a n t i s o l a r  d i r e c t i o n  of 
. 0- , 
* 
- 
4. 
Attention is also drawn by the fact that the flues of low energy electrons 
(E > 7 0 e v )  
quasi-isotropic. 
are directed, while particles of substantially higher energies are 
Institute of Physics 
in the name 
of P. N. Lebedev 
of the 
USSR Academy of Sciences 
Manuscript received 
on 28 June 2966 
Contract No.NAS-5-12487 
VOLT TECHNICAL CORPORATION 
1145 19th st.NW 
D.C. 20036. Tel: 223-6700 
Translated by ANDRE L. BRICHANT 
on 26 October 1966 
D I S T R I B U T I O K  
same as ST - LPS - PF - 10 526 


Study of the soft corpuscular radiation on the AMS ''Luna-10''

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