Proton flux measurements onboard lunar prob

Grigorov, N. L.

Lutsenko, V. N.

Maduyev, V. L.

Pisarenko, N. F.

Savenko, I. A.

English

NASA Technical Reports Server

I 
National Aeronaut i cs and Space Administration 
Coddard Spacc I:1 ight  (:enter 
Contract No. NAS - 5 - 124 8 7 
ST- DF- SCR- 10684 
REGISTRATION OF S O W  COSMIC RAYS ON TIE AMs "LUNA-11" 
by 
N. L. Crigorov 
V. N. Lutsenko 
V. L .  Maduyev 
N.  F. Pisarenko 
N .  A. Savenko 
(CODE) 
Y 
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fUl(;ISTKAI'ION OF S O W  COSMIC RAYS ON TIE &IS "LUNA-11" 
("1 
Kosmi ches k i  ye I ss ledovaniya 
Tom 5 ,  vyp.6, 
st r .  946-948, 
Izda te l ' s tvo  "NAIM",  1967 
by N.  L. Grigorov 
V. N.  Lutsenko 
V. L. Maduyev 
N.  F. Pisarenko 
I .  A. Savenko 
S m m Y  
Protons fluxes were measured on LUNA-11 during t h e  l a t e  summer 1966 
and their r e l a t i o n s h i p  with powerful solar flares is established. The results 
obtained are compared with those on AES "PKOTON-3", making it possible to 
evaluate t h e  spectrum of  solar protons at time of measurement. 
* 
* *  
'Yhe ; l y t i f i c i a l  Moon's s a t e l l i t e  (AMs) ''LUNA-11'' was plrlced in to  a sele- 
Ilocentric;ll o r b i t  011 28 August 1960 with the following parameters: aposelion 
a t  1 2 0 0  !ai; pcr i se l ion  a t  133 km, o r b i t  i nc l ina t ion  t o  the lunar equator ia l  
plaiie 10'. The comniunication sessions with the s a t e l l i t e  were conducted t o  
1 October 19bb. The apparatus was described i n  a preceding paper ( r e f . [ l ] ,  
page 891 of the cur ren t  issue and ST-PF-IPS-10083). I t  was operational 
only a t  time of communication sessions which were conducted once a day a s  an 
average arid had a duration from 2 t o  40 min. 
?'his work considers the par t  of the  r e s u l t s  of measurements having t o  do 
with the  gcncral var ia t ion  i n  time of proton flux i n  two energy in te rva ls :  
1.8 -100  MeV (3rd threshold of the s c i n t i l l a t i o n  counter) arid Ij, > 50 Mev 
(STS-5 countcr).  Note t h a t  f o r  s o l a r  protons having a s teeply dropping spec- 
t run, these in t e rva l s  correspond p rac t i ca l ly  t o  two points  of the  in tegra l  
spcctrun: Tlie in tens i ty  01 ga lac t i c  cosmic 
ray protons i n  the 1 . 5  - 100 Mev range is too low for i t s  r eg i s t r a t ion  by our 
apparatus. 
J:l > 1.8 Mcv arid E2 > 50 Mcv. 
Fig.1 next page i l l u s t r a t e s  the var ia t ion  i n  time of the in tens i ty  o f  pro- 
~ O I X  !*[it!! Ell > 50 MCV a i d  > i. 8 biev jnielui vaiuc f o r  ~ a c h  scssioJ1) . n e  g3- 
l a c t i c  cosini c r:rys , whose in tens i ty  const i tuted according t o  OUI. rneasurcmeIlts 
.3.8 C I I I - ~  scc-l, entei. the First group (Ep > 50 MeV). 
(*) RT~(;ISTRi\TSIYA SOLNEaWKIl KOSMICfESKIKH LUGEY NA ISL "LUNA-11" 
2 
.-4 
I 
k 
. -  - 
ID0 q ,  , , , , , ,-+,j, ,- , , , , , , , , , , , , , , , , , * , , 
Absorpt icn inpolar 1-1- - 
I 
o c  
k l7OP. 
3u f 5 
August 1?b6 September 1966 
Fig .1  
l ' lotteci above i s  t h e  i n t e n s i t y  of protons with E > 1.8 Mev and 
lCp > 50 MeV. I n  t h e  middle a r e  t h e  moments and !he h e l i o c e n t r i c a l  
coordir ia tes  of t h e  most powerful f l a r e s  of  f o r c e  lB, 2B, 3B and 
a l s o  the  graphs of a c t i v e  r eg ions '  motion along t h e  Sun's  d i s k .  
S t i l l  f u r t h e r  below a r e  c e r t a i n  geophysical  parameters i ir iked with 
t h e  s o l a r  a c t i v i t y  
3 
A s  may be seen from Fig.1, most of t he  time the in t ens i ty  of protons 
Two s i g n i f i c a n t  in-  with % > 50 MeV corresponds t o  ga l ac t i c  background. 
t e n s i t y  increases were reg is te red  only on 28 August and 2 September. 
lat ter case the in t ens i ty  exceeded the background by two orders.  As t o  t he  
in t ens i ty  of protons with EP > 1.8 MeV, it underwent la rge  f luc tua t ions ,  
emerging a t  times beyond the l i m i t s  of device 's  dynamic band, whereupon the  
m a x i m u m  values of i n t ens i ty  were observed with a l ag  from a few hours t o  1 . 5  
days by comparison with the m a x i m a  of protons with Ep > 50 MeV. 
Plot ted a t  the center  of Fig.1 are graphs of  motion of ac t ive  regions 
according t o  the  v i s i b l e  d isk  of the Sun (longitude as a function of time) 
and the  coordinates of the most powerful f l a r e s .  
regions d id  not p r a c t i c a l l y  vary i n  the course of two consecutive passages. 
Two in t e rva l s  with high s o l a r  a c t i v i t y  were observed during measurement time: 
from 28 August t o  4 September and from 17 t o  2 1  September. These increases 
i n  a c t i v i t y  were caused by the passage alvng the  Sun's d i sk  of three long- 
l ived  ac t ive  regions with l a t i t u d e s  N 22', N 07' and N 23". 
apparently s p l i t  i n t o  two p a r t s  a f t e r  the first passage. 
reg is te red  f l a r e s  of force  l B ,  2B and 3B took place i n  these regions,  whereupon 
the most ac t ive  was the  region N 23'. I t  may be see from the graph t h a t  the 
increases i n  in t ens i ty  of protons with % > 50 MeV followed on 28 August and 
2 September f l a r e s  of force 3 B i n  the ac t ive  region N 23'. 
ments of 28 August were conducted 3 hours a f t e r  the  commencement of op t i ca l  
f l a r e ,  while on 2 September they were conducted only after 1 4  hours. Newer- 
theless i n  the second case the in tens i ty  of protons was was by one order 
grea te r .  The s i g n i f i c a n t l y  g rea t e r  e f f e c t  from the second f l a r e  may be ex- 
plained by the f a c t  t h a t  the disposi t ion of the f l a r e  of 2 September (W 60") 
r t x s  more favorable f o r  the  a r r i v a l  of protons i n  the neighborhood of the system 
k r t h  bloon. 
In the  
The l a t i t udes  af ac t ive  
The l a s t  region 
More than 90% of the  
Note t h a t  measure- 
I n  the  lower p a r t  of the same Fig.1 we  brought out the values of the Kp- 
irides and the readings of the neutron monitor (Moscow, three-hourly averages) 
and we noted the magnetic storms and radiowave absorptions i n  the polar  cap. 
I t  may be seen t h a t  the  flares of 28 August and p a r t i c u l a r l y  t h a t  of 2 Septem- 
ber Ityere attended by powerful geomagnetic disturbances and Forbush-drops, which 
c o r r e l a t e  qu i t e  well with the in tens i ty  var ia t ions  of protons i n  the v i c i n i t y  
of the Moon. 
The t h i r d ,  q u i t e  as s t rong a f l a r e  took place a t  the limb on 4 September 
i n  the  considered region N 23'. The nearest  communication session after tha t  
flare was only on 7 September; however, comparison of our measurements with 
the geophysical da t a  allows us to  assume t h a t  the effect from protons of t h a t  
f l a r c  was lesser than during the f l a r e  of 2 September. ,Just a s  f o r  the f l a r e  
of 28 August, t h i s  case agrces w e l l  with the representations on the  in te rp la -  
nc ta ry  magnetic f i e l d ,  of- which thc l i n e s  of force a r e  curved along the Archime- 
des ' sp i ra1. 
Siiniiltaneously with the incasllrements on LUNA-11, others  were conducted 
aboard X S  "I'KOTON-3" and concentrated on protons with Ep > 400 MeV. 
s i t y  incrcasc above the  cosmic background (% 10% of background) was observed 
i n  t h e  period a f t e r  the  f l a r e s  of  28 August and 2 September. 
No inten-  
Comparing these 
4 
&t;i l i i th  the r e s u l t s  obtained on LUNA-11, it is  possible  t o  evaluate the  cha- 
r ac t e r  of the  spectrum of s o l a r  protons a t  time of measurement. 
fo r  the in tegra l  spectrum of protons the law N(E) % E T ,  we s h a l l  obtain f o r  y 
the values y1 > 1 and y, > 1 . 7  f o r  the 28th of August and 2nd Scptcmber respect-  
ively. 
I f  we assume 
The in t ens i ty  of protons w i t h  E$ > 50 Mev from the f l a r e  of 2 September 
t-3.4 (the t i m e  is counted from the commencement of the op t i ca l  var ied a s  N 
l l a r e ) .  The estimate of the in tegra l  flex cf protons based upon t h i s  depend- 
ence on t and on various assumptions on the  times of flux maximum, f luc tua te s  
from 108-to l o 9  cm-2, which corresponds t o  the absorbed dcse of protons 
with Ep > 50 MeV from 10 t o  100 rad. 
thc S u i  t hc  g rea t e s t  a c t i v i t y  was reg is te red  i n  the  period from 1 7  t o  2 1  Sep- 
tember. 
ac t ive  regions N 22' and N 07". 
f l a r e s  a re  c lose t o  the f l a r e s  of 28 August and 2 September, t h e i r  proton e f -  
fect iveness  is  subs t an t i a l ly  l e s se r .  We observed an in t ens i ty  increase only 
fo r  protons with Ep > 1 . 8  Mev [ l ] .  The in t ens i ty  of protons w i t h  Ep > 50 MeV 
was close i n  a l l  sessions t o  the  g a l a c t i c  background. 
neutron monitor and the geomagnetic data  a l s o  a t tes t  t o  the lesser effect iveness  
of the f l a r e s  of 17  -21 September. 
Ihr ing thc  second passage of ac t ive  regions through the  v i s i b l e  disk of 
A t  t h i s  t i m e  the most powerful f l a r e s  (3 B) were obscrved i n  the 
Although by t h e i r  power and disposi t ion these 
The readings of the 
The authors express t h e i r  grat i tude t o  L. I .  Dorman and h i s  coworkers 
f o r  supplying the da t a  of the superneutron monitor. 
Received on 25 May 1967 
RWERENCES 
[ l ] .  N .  L .  GRICOROV, V. N.  LULSENKO ET AL. CURRENT ISSUE. (ST-PF-IRS-10683). 
[ 2 ] .  .J. J .  O'CALLAGIER, J. A. SIMPSON. Phys. Rev. Letters 16, 1 2 1 2 ,  1966. 
CONI'RACT NO. NAS-5-12487 
VOLT TECf iN I CAL COWORAT ION 
1145 - 19th St.NW 
WASHINGTON D.C. 20036. 
Telephone: 223-6700 (X-36) 
Translated by ANDRE L. BRICHANT 
on 4 March 1968 


Registration of Solar Cosmic Rays on the AMS ''luna-11''

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