Measurements of primary cosmic radiation gamma quanta from Proton I and II satellite

Grigorov, N. L.

Kalinkin, L. F.

Melioranskiy, A. S.

Nesterov, V. E.

English

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2 STUDY OF HIGH ENERGY - UANTA 
4 
3tQ 
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BEYOND THE ATMOSPHERE 
. N. L. Grigorovi 
L. F. Kalinkin, 
A. S. Melioranskiy, 
V. E. Nesterov - 
1 
. . . 4 T & - r T .  / 
(USSR) 
e 
https://ntrs.nasa.gov/search.jsp?R=19670016571 2020-03-12T11:30:56+00:00Z
. 
STUDY OF HIGII ENERGY Y -QUANTA 
BEYOND THE ATMOSPHERE* 
Izv. AN.SSSR, 
seriya fizicheskaya 
T.30,  N0.11, 1765-7, 
Izd-vo “NAUKA”, 1966. 
SUMMARY 
by N. L. Grigorov 
L. F. Kalinkin 
A. S. Melioranskiy 
V. E. Nesterov 
...... ET AL ...... 
The results of measurements are illustrated of primary cosmic radiation’s 
The translated version includes the additional 
Y-quanta, carried out from the space stations PROTON-1 and PROTON-2, designed 
for energies exceeding 50 MeV. 
results published in a later work [ 9 ] .  
* 
* * 
Work on measurement of r-quanta of sufficiently high energies in the com- 
position of primary cosmic radiation began to develop in the course of the 
last few years. 
band of registered electromagnetic radiation has been attained. 
cipate that new data will be at the same time obtained on the galactic and 
intergalactic space, and also on local emission sources [l, 21. 
By the same token a substantial broadening in the frequency 
One may anti- 
Estimates of flux of primary y-quanta with energies E, >50 Mev come up 
The greatest number of works on 
with a magnitude % 
fraction of the flux of charged particles. 
Y-ray measurements in the indicated energy range was completed during raising 
of  instrumentations on balloons. The magnitudes of the fluxes obtained u on 
Apparently, accountable factors are included in these experiments, which are 
linked with the presence of notable amount of matter ( %  3 - 5 g.cm-2), distri- 
buted over a significant height above detectors. 
tained in the Kraushaar and Clark e 
was found to be equal to 3 . 
statistical precision of the results obtained in this work is insufficient 
and the data ryquire refinement. 
cm-2-ster-1-sec-1 [l - 31, which constitutes a small 
extrapolation of data to atmosphere boundary constitute ‘L cm-2.ster- P[4-61. 
The corresponding value ob- 
eriment carried out aboard Explorer-11 
cm3.ster-l.sec-’ [7, 81. However, the 
1 --‘ 
UCIIENIYE Y-KVANTOV WSOKOY ENERGIT ZA PREDELAMI ATMOSFERY * y ‘  A
2 .  
A tlcv I c r  w a s  i ns ta l  I cd a1)oard N:S I'roton- 1 and I'rotoii- 2 w i t h  ttic view 
o f  registering y-quanta with cncrgies exceeding SO Mev. 
red t o  i n  t h e  work [ 7 ] ,  was l a i d  a t  t h e  basis  of i t s  construction so a s  t o  
make t h e  comparison of r e s u l t s  most re l iab le .  
werc introduced, of which the most substant ia l  cons is t s  i n  t h a t  the appara- 
tus  i s  adjusted Cor measurements of y-ray spectra .  
'l'lie va r i an t ,  refcr-  
A t  the  same time improvements 
1 The device cons t i tu tes  a telescope formed 
by a y-quantum converter,  which consis ts  of 
iodide disposed i n  sequence, and of a Cerenkov 
counter ~ i t h  radiator  made of lead glass ,  which 
functions a s  detector  of  energy and propagation 
d i rec t ion  of y-rays.  The te lescope 's  detectors  
a re  placed inside a iiood made of s c i n t i l l a t i n g  
p l a s t i c  materia1,shielding the telescope from 
the bachground of charged p a r t i c l e s  when sor t ing  
the anticoinicidences (Fig.1). Besides y-rays 
the device i s  usedfor  spectra  of pulses from 
other  e l e c t r i c a l  neut ra l  p a r t i c l e s  (for example, 
neutrons) ,  and a l so  the fluxes of charged p a r -  
t i c les ,  of which the energy exceeds the  threshold 
of luminance i n  the r ad ia t io r  of t he  Cerenkov counter. 
The d e t a i l s  concerning t h i s  device and the character-  
ist ics of its operation a re  presented i n  the work [9] .* 
layers  of p l a s t i c  s c i n t i l l a t o r  and caesium i 
The processing of  information arr ived a f t e r  4 
the  launching of Proton-1 allowed us t o  obtain pre-  
liminary data  on rad ia t ion  in t ens i t i e s  beyond the  Fig.1. Block-scheme 
limits of the  atmosphere. The device's  spectra  of the device: 1) 
from y-quanta and neutral  p a r t i c l e s ,  measured f o r  p l a s t i c  s c i n t i l l a t o r  
40 hours of f l i g h t  a r e  p lo t t ed  in  F i g . 2 .  The in-  (' 'hood") ; 2) laminar 
c l ina t ions  of these spec t ra  a re  d i f f e ren t ,  which c r y s t a l ;  3) Cerenkov 
is evidence of the d i f f e ren t  nature  o f  radiat ions counter (Lead glass)  ; 
connected with them. 4) e lec t ronic  c i r c u i t s .  
spectrum of  y-rays a f t e r  correct ion f o r  accounting 
of the e f f ec t ive  r eg i s t r a t ion  and of device 's  geome- 
t r ic  f ac to r  (E = F l ~ 2 =  0 . 3 ) ;  here z1=0.43 i s  the  
pro1)ability of y-ray convers ion;~2  x 0 . 7  is the probabi l i ty  determined by the 
cffcct iveness  of neutron and y-ray f i s s ion ;  ref%7 cm2.ster [9 ] .  
of y-quanta with enerqies E 
agrees w e l l  with the data obtained in  measurements on balloons,  and a l so  with 
those of Kraushaar 'and Clark for  the case when the device 's  o r ien ta t ion  i n  
spncc i s  not taken in to  account [8 ] .  The basic contr ibut ion t o  the in tens i ty  
thus determined is  conditioned by y-rays of albedo from the atmosphere. This 
conclusion i s  corroborated by the close cor re la t ion  i n  the var ia t ion  of the 
countins r a t e  of charged pa r t i c l e s  on account of l a t i t u d e  e f f e c t  with the 
counting r a t e  of neutral  p a r t i c l e s  ( y-quanta, as w e l l  as  neutrons). The 
value of the cha rac t e r i s t i c  index of the y-ray spectrum y = 1 . 6  is a l so  not 
i n  contradict ion with the assumption, t ha t  the y-quanta regis tered by the device 
a r e  fundmental ly  conditioned by by decay of neutralTO-mesons formed i n  the 
atmosphere matter by primary cosmic rays.  
* 
The same f igure shows the  
The f lux  
5 50 MeV, equal t o  'L 2 cm-2*ster-1 -sec- l ,  
[Some of the data from t h i s  work and Figs . l ,4*  and 5"were borrowed from 
t h i s  l a t e r  work] 
. 
5 .  
Thc orientation magnitude of the f l u  of primary y-quanta may be deter- 
mined by introduction of data on satellite orientation obtained on the basis 
of readings of thc SEZ-device entering into the complex of scientific appa- 
ratus of Proton-1 [ l o ] .  
Fig.2. Integral spectra of 
radiations beyond the atmo- 
sphere: 1) device's spectrum 
of pulses from y-quanta,y' = 
= 1.5; 2) same from neutral 
particles, yn' = 1.3; 3) 
normalized spectrum of y-rays 
y' = 1.6 
Fig.3. Counting rates of y- 
quanta with energies E, > 15  
and > 50 MeV, averaged for 
eight satellite revolutions 
(T = 1 corresponds to the re- 
volution period; the time of 
measurement at each point is 
At = 48 min) : 1)- N ( > S O  MeV) 
2) N (>15 MeV) 
According to these data it was found to be possible to choose the time 
interval when the angle between the axis of the telescope, measuring quanta 
and the direction toward the center of the Earth was sufficiently great. 
The counting rate of y-quanta with energies E > 15 Mev and i 50 Mev, including 
the indicated time intervals, is shown in Fig.3. In the region 0.6 - 0.8T 
sharp minima were observed on the curves of Fig.3 (rise to the left and to 
right explainable by the fact that in respective regions the device begins to 
register mainly y-rays of albedo [ S I ) .  
minimum, three y-quanta were registered for the 48 minutes, of which the ener- 
gies exceeded 50 MeV. The magnitude of the flux, estimated on the basis of 
-thee data, was found to be (5 2 3) - 10- km-2 ster- 1 sec- 1, and agreeing w e l l  
with [7, 81 within the limits of measurement errors. The precision of this 
result may be considered only as tentative. 
sing will allow more substantial conclusions on the fluxes and also on spa- 
tial and energetic distribution of primary y-rays. 
the 
In the interval corresponding to the 
It is hoped that further proces- 
* * * 
(The following has been borrowed from the work ref. [ 9 ] )  
'Ilw s;l)cct i.orii(\ t r I c' ptmpcrt i c~ o I t lic d c i v  i cc liavc- I w c ~ i  iiiadc : i p p  wii t i 11 
atmosphere matter.  (Fig.4") . The experimental r e s u l t s  were normalized, 
taking into account the geometrical charac te r i s t ics  of the  device : 
I c.xpc>riinciits a t  SC;I lcvel by way of mcasureincnt of' spectra  of y-quanta in the 
re f f  = 6 cm2 .sterad,4kff = 22 
and the r eg i s t r a t ion  eff ic iency E . Y 
Plot ted in  Fig.5" a re  the cha rac t e r i s t i c  r e s u l t s  of measurements of char- 
and of the e lec t r ica l ly-neut ra l  radiat ion ( y-quanta and neutons) gcd p a r t i c l e  
as functions of  time f o r  the Idwest energy threshold (measurements car r ied  out 
on Proton-?).  
of the The asymme- 
trJ- of t h e  maxima 2 and 4 is  due t o  the  increased in tens i ty  i n  the  region of 
the Brazil ian anomaly. 
The per iodici ty  of the curve a reflects the l a t i t ude  e f f e c t  
dependence of p a r t i c l e  in tens i ty  of crimary cosmic rays.  
'I'he cor re la t ion  between the curves a - and - b is evidence 
l i ig .4*  ( f i g . 3  of 91) Fig.5" (Fig.4 of [9]) 
Intensi ty  var ia t  ion of charged p a r t i c l e s  
(a) , and of e l ec t r i ca l ly -neu t r a l  radia- 
t ion  ( b ) ,  t ha t  is y-quanta and neutrons 
as ru~ictioiis of time. The scales oi the  
d i f f - r en t  . 
curves - a m d  b i n  ordinates  a re  
of the chief  contr ibut ion t o  the counting r a t e  of y-quanta and neutrons of 
elect r i ca  1 1 y - lieu t r a l  rad i  a t ion of secondary or ig in  (from sat e l  1 i t e  cons t ruc  - 
t ion components and, p r inc ipa l ly  from the  atmosphere "albedo") . 
\ 
5.  
1 .  V. L. GlNZ13\JRG7 S. I. SYROVATSKIY. ZIEETF, 46, 1865, 1964. -
E .  V. L. [;lNZBURG, S. I. SYROVATSKIY, IJFN, 84, 201, 1964. 
3. . J .  B. POLIACK, G. G. FAZIO. Phys. Rev. , 131, 2684, 1963. -
4. T. , J .  CLINE. Phys. 1,ett. 1. 109, 1961. - 
5. 
6 .  
7. 
8. 
9 .  
10. 
*J. G .  DUI'HIE, E. €1. HAFFNER, E. M. KAPLAN, G. G. FAZIO. Phys.Rev.Letters 
10, 364, 1963. -
G .  b l .  FRYE, L. H. SMITH. Bul. Am.Phys.Soc. 10, 705, 1965 - 
W .  I,.  KRNJSIlMR, G .  W. CLARK. Phys. Rev.Lett. 8, 106, 1962 - -- 
G .  GAIVIIRF,, W. I,. K R A U S W .  Space Sci.Rev. 4, 123, 1965. - 
N. L. GRIGOROV, N. L. KALINKIN ET AL. Kosm. Issl., T . 5 ,  N O . l ,  1967. 
N. N. VrOI,0(7DICIEV, N. N. GRIGOROV, N. L. NESTEROV ET AL. 
-. 
Curr.volme p.1763, 
1966. 
D I STRI BUT I ON 
same as ST-CR-10550. Add Dr.Pieper GSFC Code 600 
as permment addressee, effective Jan.1, 1967 
Contract No.NAS-5-12487 
VOLT TECIINICAL CORPORATION 
1145 19th St.", 
D.  C. 20036. 
Telephones: 225-6700 and 223-4930. 
Translated by ANDRE L. BRICHANT 
on 13 March 1967 


Study of High Energy Gamma-Quanta Beyond the Atmosphere

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