Survey of trapped radiation in magnetosphere interior by Relay  I satellit

Fillius, R. W.

Mc Ilwain, C. E.

English

NASA Technical Reports Server

Apri l  13, 1965 
A SURVEY OF INNER ZONE PF"0NS 
BY 
R. W. F i l l i u s  
and 
C. E. McIlwain 
GPO PRICE $ 
OTS PRICE(S) $ 
Hard copy (HC) 
Microfiche (M F) 
Department of Physics 
University of California a t  San Diego 
La Jol la ,  Cal i fornia  
N 6 5 - 2 6 4 2 3  
J (ACCESSION NUMBER1 ITHRUI ~ 
I f I 
https://ntrs.nasa.gov/search.jsp?R=19650016822 2020-03-17T01:41:26+00:00Z
Abstract 3t.7423 
This report presents detailed da ta  from a survey of 
trapped protons made by Relay I. 
1.1 t o  63 MeV a r e  analyzed t o  determine the s ta t ionary dis-  
t r ibu t ion  of trapped protons as of January 1, 1963. 
da ta  is  presented as the  observed f l u x  of l o c a l l y  mirroring 
p a r t i c l e s  plot ted as a function of /B/ on each she l l  of 
force, and i n  the form of contour maps i n  B, L space. 
interpretat ion is reserved f o r  a companion paper, it is  be- 
l ieved t h a t  t h i s  data w i l l  be useful reference material  
for s c i e n t i s t s  investigating the  trapped radiation. 
S ix  energy channels from 
This 
Although 
. .. 
i r  .' 
I. Introduction 
The S ta t e  University of Iowa - University of California detectors  
aboard Relay I have been used before t o  make selected s tudies  of t he  
trapped radiat ion i n  t h e  i n t e r i o r  of the  magnetosphere. 
of radiation in t ens i t i e s ,  including electrons of enerQy grea te r  than 
0.45 MeV and protons from 1 . 1 t o  63 MeV, emphasizing s p a t i a l  dependence, 
radiat ion damage e f f e c t s  on s a t e l l i t e  so l a r  ce l l s ,  and geomagnetic storm- 
time ef fec ts ,  was d is t r ibu ted  i n  a NASA report  BcI lwain ,  F i l l i u s ,  
Valerio, and Dave, 19g. 
magnetic storm of September, 1963 on t h e  protons counted by a 34 MeV 
threshold omnidirectional s c i n t i l l a t i o n  detector  P c I l w a i n ,  19647. 
F i l l i u s  and McIlwain used the array of e ight  energy se lec t ive  proton 
channels t o  demonstrate the s p a t i a l  dependence of t he  energy spectrum and 
t o  indicate  the i n t e n s i t i e s  encountered @ i l l i u s  and McIlwain, 19647. 
A broad survey 
1 
McIlwain exhibited the e f f e c t s  of the  major 
- 
- 
The present report  i s  a detai led presentation of da ta  from a survey 
of protons i n  s i x  energy ranges from 1.1 t o  63 MeV. 
supplement t o  a more in te rpre t ive  paper t o  be published by F i l l i u s  D i l l i u s ,  
19627. 
and because i t s  bulk was too great  t o  be included i n  the  companion paper, 
t he  co l lec t ion  i s  presented i n  t h i s  separate report. It i s  believed t h a t  
t h i s  data w i l l  be found useful by other experimenters f o r  de ta i led  comparison 
with t h e i r  work, f o r  theoret ic ians  who want more than a super f ic ia l  knowledge 
of experimental r e su l t s ,  and, i n  general, by anyone who wishes t o  refer t o  
t h e  trapped proton i n t e n s i t i e s  within the inner zone. 
This report  i s  a 
Because it w a s  desired t o  make the  complete set of data available,  
11. Instrumentation 
This report deals with two of the four  SUI/UCSD instruments on 
Relay I. 
six energy bands of data on the trapped proton fluxes. 
marizes t h e i r  character is t ics .  Previous reports have described the  
design and cal ibrat ion of these instruments qui te  thoroughly f i i l l ius ,  
1963; F i l l i u s  and McIlwain, 1964; McIlwain e t  al, 19647. - 
can be consulted f o r  a more detai led review of the instrumentation. 
Using pulse height discrimination, these detectors  generate 
!Fable I sum- 
These referencqs 
The output of the detector  is  d ig i t a l ,  w i t h  d i g i t a l  telemetry and 
data handling. The discriminators and spalers  are $inear f o r  the  counting 
ra tes  experienced by these detectors and a redundant readout i n  the  
telemetry frame guards against  transmission errors. The l i n e a r  amplifiers 
have a temperature coeff ic ient  whic\h causes the  discrimination leve ls  t o  
change by as much as 20$ i n  the  operating temperature range of -5  t o  
+30° C. The data presented here has been compensated f o r  t h i s  change by 
calculating, f o r  the observed spectrum, the  counting rate that would have 
been observed at the cal ibrat ion temperature. Furthermore, radiat ion 
damage caused the gain of detector  B t o  drop t o  504 of i t s  i n i t i a  value 
i n  the  period from April  10 t o  m y  10, 1963. 
by a similar correction. 
given by Fi l l ius  p9627. 
data rarely amounts t o  as much as .b$ and is generally less than 20% 
This data has been recovered 
A complete descr ipt ion of t h i s  correction i s  
The temperature correction t o  the B detector  
That t o  the C detector data is ra re ly  more than 30$ and generally l e s s  tham 
15$. The radiation damage correction t o  detector  B increases from zero t o  
I 
1 
c 
' /  3 
as much as a f ac to r  of t e n  at the highest. 
selves va l id  by reducing the sca t t e r  i n  the points, and, furthermore, the 
These changes have proved them- 
data recovered by the damage correction has made it possible t o  perform 
operations on the computer which, without it, had t o  be done by hand. 
It may be noted that previously published data DcIlwain,  e t  8.1, 1964; 
F i l l i u s  and McIlwain, 19647 does not include the  temperature correction 
t o  detector  C o r  the  addi t ional  detector B data gained by the damage cor- 
r ec t  ion. 
111. Data Reduction 
- 
The complex data analysis program used fo r  t h i s  survey was developed 
by McIlwain DcIlwain,  19637 f o r  Explorer XV data. 
reviewed here as it has been applied t o  Relay I. 
The method w i l l  be - 
The r a w  satel l i te  data consists of counting rates f o r  t h e  several  
detectors  versus time. 
time is  provided by NASA and added t o  the  data. 
i n  magnetic coordinates, o r  B, L space. Fc I lwa in ,  19617. 
obtained the counting ra tes  versus B and L. 
in terpolates  the  da ta  t o  selected magnetic shel ls  [L = 2.0, 2.05, 2.1, e tc .7  
wherever the o r b i t  crosses them and data are usable. 
are grouped according t o  L value and sor ted i n  order of B. 
data, one can then p lo t  the counting rates as a function of B f o r  any 
selected L. 
The posit ion of the sa te l l i t e  as a function of 
Posi t ion i s  calculated 
From t h i s  is - 
Next a computer program 
- 
The interpolated data 
With adequate 
Usually there  is  a strong B dependence. 
A s  each crossing of a magnetic she l l  occurs a t  a d i f fe ren t  time, the 
For proton data it i s  typ ica l ly  t i m e  dependence has so f a r  been l e f t  out. 
qui te  small. When the  time dependence is steady and not a function of B, 
._ 
one can fit the flux on a l i n e  of force w i t h  the function, 
N-2 (1) 
+ A ( E )  Bo + Ab ($J2+. . + A N  (id 
where 
- is t he  value of t h e  magnetic f ie ld  at  t h e  
BO L3 
equator for that L, 
< < 3 . - N - 8 is selected by t he  computer o r  by the  
programmer f o r  the  best f i t .  
G is  the  geometric f a c t o r  i n  cm2 - s t e r  f o r  the detector.  
t is numbered i n  days and f rac t ions  of a day, beginning w i t h  
1 on January 1, 1963. 
One sees t h a t  the  given function can produce a st rong B dependance and 
a weak t dependence as recpired. Good f i t s  are obtained with t h i s  
function without cross t e r n  or  higher powers i n  t h e .  
have been obtained on a Sa t i s fac tory  coeff ic ients  A1, - - -, 
gr id  of L values f o r  each of t he  s,ix data channels of t h i s  survey. 
coeff ic ients  are l i s t e d  i n  Tables 2 through 7, algng with the  limits of 
B ( i n  gauss) over which the  fit i s  s a t i s f a c t o r y  and t he  number of data 
points  on the  l i n e  of force. 
difference between the  logarithm of the  data and t h e  logarithm of the  fit. 
These 
The last column gives 100 times the  rm6 
I n  the approximation of a good fit t h i s  is j u s t  the rms e r r o r  i n  per  cent. 
This measure of qua l i ty  ranges from 5 t o  75 4, and i s  
typ ica l ly  between 10 and 254. 
i 
5 
During a s t ab le  o r  slowly changing epoch a counting r a t e  a t  time 
t can be projected t o  a reference time t 
exp (A2 (t - tref)) . The r e su l t  is the in t ens i ty  that would presumably 
have been measured at  the  reference time. The figures accompanying t h i s  
paper represent such presumed in tens i t ies ,  projected t o  January 1, 1963. 
Data i n  the  three ranges of detector  B were taken during the in t e rva l  
from December 14, 1962 t o  May 10, 1963; i n  the  three  ranges of detector  C, 
from December 14, 1962 t o  September 22, 1963. 
by multiplying by ref 
Figures 1 through 21  exhibit  log 2 vs log  B measured i n  t he  six 
energy ranges of detectors  B and C. The next th ree  f igures ,  Figures 22 - 24, 
show the  sum of the  de tec tor  C channels, o r  the flux of protons from 18.2 
t o  63 MeV. 
t o  day 1, and the l i n e  i s  the ana ly t ica l  f i t  according t o  equation (1). 
The points represent the  individual measurement projected 
All of the information from an individual channel can be displayed 
by a map of in t ens i ty  contours. 
B, L space f o r  t he  seven energy ranges named above. Although the  former 
p l o t s  a r e  more accurate, contour maps a re  convenient and make a pleasing 
summary of a s e t  of data. 
F @res 25 through 31 a re  contour maps i n  
N. summary 
Over 6000 da ta  points have been presented which show the  fluxes of 
trapped protons i n  the  inner radiat ion zone. Discussion of the  data  w i l l  
be made i n  a separate paper f i i l l i u s ,  19657. 
of t h i s  data w i l l  supplement other experimental work, and w i l l  s t imulate 
t h e o r e t i c a l  s tudies  of the  origin, t ransport ,  and l o s s  of these par t ic les .  
It i s  hoped that d i s t r ibu t ion  - 
6 
Acknowledgment 
The authors are indebted t o  Mr. D. Enemark of the University of 
Iowa f o r  the e l e c t r i c s l  design of the instrument package, and t o  
Dr.  A. Hassitt of the University of California, San Diego f o r  much of the  
computer programming. 
This work w a s  supported i n  part by M A  contracts W5-1683, ~ ~ ~ r - 1 1 6 ,  
and NSG-538. 
BIBLIOGRAPHY 
I 
F i l l i u s ,  R. W., "Sa t e l l i t e  Instruments Using Sol id  S t a t e  Detectors", 
Research Report SUI 63-26, Department of Physics and Astronomy, 
The S t a t e  University of Iowa, Iowa City, Iowa, 1963. 
F i l l i u s ,  R. W., "The Trapped Protons of t he  Inner Radiation Bel t ,"  
PhD. Dissertation, The Sta te  University of Iowa, Iowa City, Iowa, 
1965 9 
F i l l i u s ,  R. W., and C. E. McIlwain, "Solid S ta t e  Detectors f o r  Inner 
Zone Protons", Space Research 111, Proceedings of t h e  Third COSPAR 
Symposium, Washington, D. C., April-May, 1962, pp 1122-1128, 
North Holland Publishing Company, Amsterdam. 
-
F i l l i u s ,  R. W., and C. E. McIlwain, "The Anomalous Energy Spectrum of 
Protons i n  the  Earth 's  Radiation B e l t " ,  Phys. Rev. Let ters ,  12, 
609-612 (1 June, 1964). 
-
McIlwain, C. E., "Coordinates f o r  Mapping the  Distr ibut ion of Magnetically 
Trapped Part ic les" ,  2. Geophys. Res 66, 3681-3691, 1961. -.' 
McIlwain, C. E., "The Radiation Belts, Natural and A r t i f i c i a l " ,  Science, 
- 142, 355-361, October, 1963. 
McIlwain, C. E., "Redistribution of Trapped Protons During a Magnetic 
Storm", Paper delivered a t  t h e  1964 COSPAR Symposium, Milan, Italy. 
I 
McIlwain, C. E., R. W. F i l l i u s ,  J. Valerio, and A. Dave, "Relay I 
Trapped Radiation Measurements", NASA Technical Note NASA TN D-2516, 
National Aeronautics and Space Administration, Washington, D.C., 
December, 1964. 
8 
Table I -- 
Summary of Detector Character is t ics  
Detector B 
Sensor: S i l icon  surface-barr ier  diode w i t h  depletion depth 
2 of 25 mg/cm . 
2 Geometric factor:  .0136 cm - s t e r  (d i rec t iona l ) .  
Shielding: 8.5 p/cm brass i n  s ides  and back. 1.115 mg/cm 
2 2 
(air equivalent)  nickel  l i g h t  sh ie ld  over look cone. 
Electronic discrimination levels :  
Bcu - 0.87 &v 
BB - 1.41 MeV 
BY = 2.11 MeV 
3.84 MeV - B6  
Proton energy ranges: 
Range one: 1.1 t o  1.6 MeV and 
7.1 t o  14  MeV 
1.6 t o  2.25 MeV and 
4.75 t o  7.1 MeV 
Range three:2.25 t o  4.7 MeV 
Range two: 
Detector C 
Sensors: Two s i l i c o n  L i -d r i f t  diodes w i t h  ac t ive  depths of 
2 
ster (d i rec t iona l ) .  
107 and 132 mg/cm , operated i n  coincidence. 
2 Geometric factor :  0.22 cm 
9 
Electronic  1 
Table I (Continued) -- 
iscrimination levels :  
- Cia, - 
c1 B - 
C 1 Y  - 
c2a - 
c2B - 
C 2 Y  - 
 
 
- 
- 
- 
Proton Energy Ranges : 
Range one: 
Range two: 
0.75 MeV 
1.71 MeV 
2.84 MeV 
1.14 MeV 
2.04 MeV 
3.53 MeV 
18.2 t o  25 MeV 
25 t o  35 MeV 
Range three:  35 t o  63 MeV 
Direct i o  na l  it y 
These detectors  are mounted perpendicular t o  the  s a t e l l i t e  spin 
axis and are  gated by a magnetometer t o  record data only when they point 
+ 
within - 10 degrees of t:ie plane perpendicular t o  the  l o c a l  magnetic f i e l d  
vector.  Thus they measure j, , the f l u x  of l oca l ly  mirroring pa r t i c l e s .  
v) z 
0 
c 
0 
Q. 
a 
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I: 
0 
rl 
0 
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11 
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Figure 
Nos 
1 - 4  
, 
FIGURF: CAPTIONS 
5 - 8  
9 -  2 
13 - 15 
16 - 18 
Protons 1.1 t o  14 MeV. 
v8 B f o r  28 l i n e s  of force from 
The f lux of mirroring pa r t i c l e s  
L = 1.5 t o  L = 4.2, 
on January 1, 1963. 
Protons 1.6 t o  7.1 MeV. The flux of mirroring pa r t i c l e s  
vs B f o r  28 l i nes  of force from 
L = 1.5 t o  L = 4.2, 
on January 1, 1963. 
Protons 2.25 t o  4.7 MeV. 
vs B f o r  25 l i nes  of force f r o m  
The flux of m-rroring pa r t i c l e s  
L = 1.5 to L = 3.9, 
on January 1, 1963. 
Protons 18.2 t o  25 MeV. 
vs B f o r  18 l i n e s  of force f r o m  
The flux of mirroring pa r t i c l e s  
L = 1.3 t o  L = 3.0, 
on Jsrmary 1, 1963. 
Protons 25 t o  35 MeV. 
vS B f o r  14 l i n e s  of force from 
The flux of mirroring pa r t i c l e s  
L = 1.6 t o  L = 2.9, 
on January 1, 1963. 
FIGURE CAPTIONS 
( Continued) 
Figure 
Nos. 
19 - 21 Protons 35 t o  63 MeV. 
vs B f o r  12 l i n e s  of force from 
The flux of mirroring par t ic les  
L = 1.8 to L = 2.9, 
on January 1, 1963. 
Protons 18.2 t o  63 MeV. 
vs B for 12 l i n e s  of force from 
22 - 24 The flux of mirroring par t ic les  
L = 1.8 t o  L = 2.9, 
on January 1, 1963. 
25 - 31 Contour maps i n  B, L space f o r  the f l u  of trapped protons. 
FOR EACH L VALUE 
THE REFERENCE LINE 
IS to4 sec-' cm-2 sterl 
0 0  
0 00 
000 
I I I 1 I I I I (  I I j I I  1 1 
.05 ,I -2  .OI .02 
8, GAUSS 
Figure 1 
I . 
I '  
FOR EACH L VALUE 
THE REFERENCE LINE 
IS lo4 sec-' cm-* ster-' 
I 1 I I l l I I  J J j J  I I I 1  
* I  .2 .02 .05 001 
B ,  GAUSS 
Figure 2 

FOR EACH L VALUE 
THE REFERENCE LINE 
I S  IO' se? cmi2 ster-' 
B ,  GAUSS 
Figure 4 
I 
I '. 
DIRECTIONAL INTENSITY 
RELAY I DEC. 14,1962 TO MAY IO, 1963 
PROTONS 1.6 TO 7. I MEV 
8, GAUSS 
Figure 5 

Figure 7 
Figure 8 
DIRECTIONAL INTENSITY 
PROTONS 2.25 TO 4.7 MEV 
RELAY I DEC. 14,1962 TO MAY IO, 1963 
6 ,  GAUSS 
Figure 9 
FOR EACH L VALUE 
THE REFERENCE LINE 
IS  10' s e c l  cm-2 s t e i '  
Figure 10 
. 
\ x  
FOR EAC VAL 
x i 
x 
I -3 
L L L- L- L--L_LL 
20 I -02 .05 . I  .2 
B ,  GAUSS 
Figure 11 
f= I 1 I - I I I I I  1 1 1 1  I I 1 -  - DIRECTIONAL INTENSITY - - 
PROTONS 2.25 TO 4.7 MEV 
RELAY I DEC. 14,1962 TO MAY IO, 1963 
- 
t- 
1 
x 
FOR EACH L VALUE 
THE REFERENCE LINE 
IS lo4 sec-' cni2 s ter '  
io I .02 .05 .I .2 
B,  GAUSS 
Figure 12 
OIRECTIONAL INTENSITY 
PROTONS 18.2 TO 25 MEV 
RELAY I DEC. 14, I962 TO SEPT. 22, 1963 
i 
FOR EACH L VALUE 
THE REFERENCE LINE 
IS lo2 sei' cmi2 ste? 
I I . I  I I I l l 1  I l l l l  1 I 1 1  
.01 .02 .0;5 .I .2 
B ,  GAUSS 
Figure 13 
I .  
- - X X  - - - 
- - - 
-  
f FOR EACH L VALUE - 
1 THE REFERENCE LINE - 
Z IS IO* sec-' c~~ ster'  - 
I 1 1 I I I I I  I l l l l  I 1 I I  
- 
- 
t - I I I I l I I I - 1  1 1 1 1  - - - 
- 
DIRECTIONAL INTENSITY 
PROTONS 18.2 TO 25 MEV 
RELAY I DEC 14,1962 TO SEPT. 22 , 1963 
\ 
t I D '4
I I 
I .  - - - - I 1 I I l l 1 1  1 1 1 1  I - - 
- 
DIRECTIONAL INTENSITY 
PROTONS 18.2 TO 25 MEV 
RELAY I DEC. 14, I962 TO SEPT. 22,1963 y 
E- \ 
E- 
€ 
\ b V 
\ A 
k- c FOR EACH L VALUE 
!I THE REFERENCE LINE 
- IS lo2 s e c '  mi2 s t e t '  c 
3 
I 
7 
I 1 I I I l l l  I I I I I  I 1 I I i  
-0 I .02 .05 . I  .2 
B, GAUSS 
Figure 15 
DIRECTIONAL INTENSITY 
PROTONS 25 TO 35 MEV 
RELAY I DEC. 14,1962 TO SEPT. 22,1963 
Figure 16 
- I I 1 ;  - DIRECTIONAL INTENSITY 
PROTONS 2 5  TO 35 MEV 
RELAY I DEC. 14,1962 TO SEPT. 22,1963 
- - - - 
- - - 
E- 
I 1 
i \ D D FOR EACH L VALUE x = THE REFERENCE LINE I S  lo2 s e c '  cni2 ster 'x  I X X I 1 I I I l l +  1 I I l l  I I 
10 I .02 .05 .I 82 
8, GAUSS 
Figure 17 
- 
RELAY I DEC 14,1962 TO SEPT. 2 2  , 1963 
- - DIRECTIONAL INTENSITY - - - PROTONS 25 TO 35 MEV - 
L +t+ 1 
E 
[. t "I, ; 7 
-* ; 1 
FOR EACH L VALUE 
THE REFERENCE LINE 
IS lo2 sec-' cm-* s t e r '  
L - l - L L U L L J  
. 02  .05 . I  . 2  .Ol 
B , GAUSS 
Figure 18 
I .  
E ,  GAUSS 
Figure 19 
I 
~~~ ~ 
DIRECTIONAL INTENSITY 
PROTONS 35 TO 63 MEV 
RELAY I DEC.14, I962 TO SEPT.22,1963 
FOR EACH L VALUE + + + 
IS lo2 sec' ste? + 
THE REFERENCE LINE + +  
B, GAUSS 
Figure 20 
' .  
x 
I 
x 
x 
FOR EACH L VALUE D x  X t 
THE REFERENCE LINE 
I S  to2 secl  ster' 
B, GAUSS 
Figure 21 

DIRECTIONAL INTENSITY 
PROTONS 18.2 TO 63 MEV 
RELAY I DEC. 14,1962 TO SEPT. 22, 1963 
FOR EACH L VALUE 
B, GAUSS 
Figure 23 
F I I I 1 I I . 1  1 1 1 1  
" '7 7 1  DIRECTIONAL INTENSITY PROTONS 18.2 TO 63 MEV RELAY I DEC. 14,1962 TO SEPT. 22,1963 
t 
E 
I- A 
i t  I - 3 c -  + \ "  1 -r-- L - L . V 7  \ 
I- 
? 
t 
+- I  
c x i -  
- . /  
c 
\ . k \ 3  
\ 
\ 
vDY 
x X -  
E FOR EACH L VALUE = THE REFERENCE LINE X I  
- - IS IO* sec-' cm-2 ster-' 
8, GAUSS 
Figure 24 
I I I " '  I I I 1 I 
m e  / 
I I /  I l l  I I I I 1 I 
0 0 0 9 
0 cv - cu 
ssnws 'a 
I I I "  I '  I I 1 I 
i -- 
I I 1 1 1 1 ,  I I 1 1 
v) cu - - cu 
0 0 9 0 9 
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0” 
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I '  
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- 
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I I 1 1 1 1  I I I I 1 - 
0 cu m N 0 0 9 9 
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0 - ln N 0 N 0 0 0 
ssnw ' 0  
n 


A survey of inner zone protons

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