Polar magnetic disturbances and data on charged particles in ionosphere evaluated to prove regularity of occurrenc

Afonina, R. G.

Feldshteyn, Ya. I.

English

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National Aeronaut ics  and Space Admj n i s i r a t i o n  
Goddard S p c e  F l i g h t  Centcr  
Conti-act N o .  NAS-5-12437 
S T -  GM-- FF - 10691 
POIAR MAGNETIC DISTURGANCES AID INTRUSlON OF 
CHARGED I’AT;I’ICLI:S INTO rri i~ IO~.IOSPI IriiiE 
R .  G .  Afonina, 
Y a .  I. Fel’dshteyn 
(USSR) 
F1 
In 
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N 
0 0 5 9  I 
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(PAGES) 
(NASA CR OR TMX OR AD NUMBER) 
https://ntrs.nasa.gov/search.jsp?R=19680010590 2020-03-12T08:43:55+00:00Z
ST- 01- - PF- -___ 10691 
Kosmiclieskiye Is s 1 edovaniya 
Tom 6 ,  vyp.1, 150 - 1 5 2 ,  
I zdate 1 's tvo "NNJKA" , 1965 
by R. G .  Afonina 
Yam I . F e l t  dshteyn 
The r e g u l a r i t i e s  of appearance o€ DP a r e  f u r t h e r  corroborated by a v a s t  
observation mater ia l  assembled during the IGY. 
77 bay- l ike  disti irbanccs is evaluated from da ta  of 15 observa tor ies .  
va l en t  cu r ren t  systeni i s  represented a t  i onospherc he ights  , 
p o s i t i v e  and negative DP and the  pos i t ions  of  icestern and eatsern e l e c t r o j c t s  
are discussed.  
va t ion  da ta .  
Space-time d i s t r i b u t i o n  of 
?Ilc equi- 
The appearance of 
The e n t i r e  pa t t e rn  i s  discussed i n  the l i g h t  of  s a t e l l i t e  obser- 
.j: 
Polar  inag~ietic dis turbances (DP) c o n s t i t u t e  a c h a r a c t e r i s t i c  s i n g u l a r i t y  
€ormation oC regions of  increased ion iza t ion  
of magnetic f i e l d  va r i a t ions  at high l a t i t u d e s .  
a r e  coiiditioried by two €actors :  
as a r e s u l t  of i n t rus ion  i n t o  the ionosphere of f luxes  of charged p a r t i c l e s  
(e lec t rons  and protons) and generation of e l e c t r i c  f i  e lds  of ionospheric a s  
wel l  as mgrictospheric o r i g i n  [l - 51. 
Their appearailce arid i n t e n s i t y  
According t o  observations i roin AES it was shoiim jn [GI t h a t  the  r e l a t i o n -  
sh ip  between the i n t e n s i t y  of a magnetic clisturhence on the  Ea r th ' s  sur face  and 
the f l m  of charged p a r t i c l e s  depends e s s c n t i a l l y  on l o c a l  t i m e .  I n  co l~ lcc t io i l  
wjth t h i s  it is of i n t e r e s t  t o  ascer ta in  the space-time d iq t r ibu t ion  of t he  frc- 
q~iency of appcaraiicc and i l l tensi ty  of DP, which i s  c s s c n t i A  f o r  tlie understand- 
ing o€ the  na ture  of  physical processes respons ilile f o r  the  occurrence and  devc 
lopment of DP and the v a r i a t i o n s  in  the ionosplicre and tlie magrietospl~re a t  t i i l l , .  
o€ inagile t i c  di s turbances . 
The fu1-1damenta1 s t a t i s t i c a l  regu!-xitics of  appearance of po la r  d i s tu rb -  
ances ai-e expoundcd i n  [ 7  -IO] . 
permit ted to  
and uniform iiiaterinl . 
O b s e n a t i o n s  i n  tlic per iod of  the IGY have 
md\e more prccisc the ~ i c l l  knorm regular i  t i e s  by nieaiis 01 a v a s t  
2 
Space-iirrie d i s  ir-ibuiioii 01 77 bay-l ike dis turbances was considered 011 
t he  b a s i s  of data  of 15 magnetic observator ies  of  the northern liemisphere a t  
geomagnetic l a t i t u c k s  @ > 60" €or the winter  season of the  IGY. P lo t t ed  i n  
Fig.  1 is the  frco,uenc J of appearance of p o s i t i v e  and negative 1lP with ainplitude 
g r e a t e r  than 150 y . The three-hour i n t e r v a l  containing the  c]ioseli bay, \\ras 
charac te r ized  by a p lane tary  index 3 < Kp < 5. 
uiifornily d i s t r i b u t e d  by t~co-hour i n t e r v a l s  of  the day. 
The niunbcr o f  bays is about 
I? 1Zh 
Oh Oh 
Fig. 1 
of p o s i t i v e  (a) and negat ive (b) I)P wi th  anipli- 
I so l ines  of the  frequency of appearance 
tude g rea t e r  than 150 y 
The dashed l i n e  i s  s i t u a t e d  a t  t h e  l a t i L u d e  of 
t h e  most €frequent appearance of n c g a t i v e  DP f o r  
t h e  corresponding 1 oca1 t ime.  The coord ina l .es  a r e  
t h e  c o r r e c t e d  geomagnetic l a t i t u d e  and l o c a l  geo- 
magnetic t ime [13 141 
Since the i n t e n s i t y  of disturbanccs va r i e s  with U.T. ,  the frequency of ap- 
pearance of bays a t  s t a t i o n s  w i t h  about i den t i ca l  l a t i t u d c s  were averaged scj as 
t o  diminish t h i s  ef 1cc t  . 
was coinputed as the r a t i o  01 the  number of bays w i t h  I A I I [  > 150 y t o  t h e i r  gene- 
ra l  nunlier i n  the corresponding pcr j  od of local tiiiie. 
nes i n  Fig.  1, in t e rpo la t ion  between ncigliboring values was pcrfoniicd. 
Q, < 70', wi th  maxiimun frequency Q 0 . 4  on Q, -- 65' a t  about 1800 hours L.T.  
Negative DP are observctl on a l l  l a t i t u d c s  aid a t  any time of the  day. 
quency 01 t l i c i r  appcni~~ncc decreases by more than two times from n i g h t  t o  day 
hours ,  which is determined by bay in t ens i  t y  dccrcasc i n  t h i s  s e c t o r .  
of freqrcncy maxiniuni of  negat ive IIP appearance h a s  a n  oval  shape, disposed a t  
higl-er l a t i t u d e s  i n  daytirric than i n  n ight t j inc .  
are observed simul ta~icously i n  evening hours, but a t  di  ffei-cnt l a t i t u d e s .  
t i v e  bays a r e  o b s e r l d  c lose r  t o  the lmlc. 
Ell, 121. 
than the pos i t i ve  bays by aboiit tlco t imes,  diicli i 5  a l so  condi tioiicd by a s i g n i -  
€i cantly grcatcr in t ens j  ty of ncgatilrc h y s .  
The frequency of appearance o€ bay- l i k c  di  s tulbanccs 
Il'hcn drawing the  i s o l i -  
Pos i t i ve  DP appear only i n  i n  the evening s e c t o r  during wjntertiinc, CII 
The f r e -  
The region 
Ibsi t ive  and negat ive  bays 
This ii:y)ortanl casc i s  s t r e s scd  i n  
Nega- 
Negative bays w i t h  [ A H /  < 150 y on Q Q 65" appLar  more frequcmtly 
3 
Shown i n  Fig.  2 is the equivalent cu r ren t  sys tern a t  ionosphere he ights ,  
g iv ing  a generalized rep icsenta t ion  on tile magnitude and d i r e c t i o n  of the  pe r -  
turbed vec tor  i n  the hor izonta l  plane. 
of the  per turbed vec tor  i n  thc v e r t i c a l  plane.  The equ.i.valent cur ren t  systeiii 
cons i s t s  of  two v o r t i c e s ,  night. and evening. 
near ly  the e n t i r e  po la r  cap, i s  most in tense  i n  morning hours a t  @ CL 6S0,  and 
i n  evenink hours a t  @ Q 65'. 
p r a c t i c a l l y  a l l  the  longi tudcs,  but i t s  i n t e n s i t y  depends on l o c a l  time with 
maxinium j.n n igh t  and morning hours and minirn~un i n  daytiiiie. 
s i d e ,  a t  @ 7 0 ° ,  the  current  dens i ty  is  negl ig ib ly  small as a consequence 
of absence of in tense  disturbances a t  these l a t i  tudes .  
t e  da t a  shows, t h a t  the western e l e c t r o j e t  of Fig.2 is disposed along tlie ou ter  
boundary of the radiat-ion b c l t  with 40 kev e lec t rons  [16, 1 7 1  i n  the  region 
wherc hES "INJUN-3'' obscrvcd the  I ~ I O S ~  in tense  el.ectron aurorae [lS] . 
Taken i n t o  account was also the si.gn 
The night. vortex,  enc.ompassing 
The e l ec t ro j e t .  of wester ly  d i r e c t i o n  engul-fs 
On the daytiirie 
60 
Coinparison with s a t e l l i -  
Oh 
Fig. 2 Equivalent current  system 01 UP i n  win ter  season 
a t  high l a t i t u d e s  o f  the northern hemispliere during I G Y  
The l i n e s  are  drawn through 20000 a. Account w a s  t a k e n  of 
c u r r e n t s  induced i n  the ground. The c o o r d i n a t e s  are  t h e  cor -  
r e c t e d  geoinagnetic l a t i t u d e  and the e c c e n t r i c  d i p o l e  time [15] 
Thereforc the  western e l e c t r o j  e t  is s i t u a t e d  i n  the  rcgion of  hot plasma 
runoff from the  iringnetosp1i:~rc t o  j oiiosphcrc heights ,  whi cli determined tlic ap- 
peai-;~iicc i n  tlic ionosplicrc of  a ~ I i o l e  series of geopliysical c i f e c i  , including 
the  w s t e i n  e l c c i r o j c t  . ?'he ccceritrical disposj  tiori of the liestel-n elect TO- 
j e t  r e l a t i v e  t o  tlic pole  is conditioncd by the  asylmcti-ical shape O€ the  mngne- 
tosplicre, contracted on the  daytime side by the s o l a r  wind. The cu r ren t  systein 
o r  Fig.  2 agrces 1\7clI w i t  11 tlie p i -~~scn t - chy  represcntat ions 011 tlie structure of 
tlic gco,ii;i~;nct i c' f i e l d  \ v i  t h i n  t h \  l>oiimls of thc  iiingiictosplici-e, and i n  pa r t i cu l  ar 
wi t11  tlic Ionilnti 011 of the gcnmag,ietic tail. 
4 
The eastei-j-1 e i ec i lv j e t  i n  t he  evciiing scctor on @ % 65" is scve ra l  times 
l e s s  in tense  than tlie Icestern one. 
l e n t  cu r rcn t  system, brought out  i n  Fig.2 we u t i l i z e d  DP a t  a l l  hours U.T. ,  
the  small value of the eas t e rn  e l e c t r o j e t  i n  evening hours cannot bc explained 
by the absciice o€ observa tor ies  r eg i s t e r ing  p o s i t i v e  DP, as i s  done i n  [19]. 
I t  may be assumed t h a t  thc s i g n i f i c a n t l y  lower i n t e n s i t y  o i  the  e a s t e r n  e l ec -  
t r o j e t  r e l a t i v e  t o  thc  western i s  a c h a r a c t e r i s t i c  p e c u l i a r i t y  o i  the winter  
season o€ the Icly [ZO] . The eas t e rn  e l e c t r o j c t  closes mainly through middle 
l a t i t u d c s  . 
na tu re  of p o s i t i v e  and negative disturbcmccs [20, 21j. In  p a r t  cular ,  it i s  
assumed i n  [22]  t h a t  t he  appearance of the  eastcrn e l e c t r o j e t  is conditioned 
by the  e l e c t r i c  f i e l d ,  emerging as  a consequence of the  d iv i s ion  o€ charges 
in t rvding  i n t o  the. ionospherc during evening hours. 
Since f o r  the computation of the equi1.a- 
Its sepal-ation from the l i e s t em e l c c t r o j  c t  presupposes a di  f i e r e n t  
I n  the  l i g h t  of l a t c s t  s a t e l l i t e  obsc~-vat ions it i s  iinpossible t o  explain 
S a t e l l i t e  da t a  i n  
the  lower i n t e n s i t y  o€ negat ivc UP on the daytimc s i d e  of the Earth by conipari- 
son with thc  nighttime s i d e  by a smaller f lux  of p a r t i c l e s .  
po la r  o r b i t  a t  340 hi1 a l t i t u d e  Iiavc shown [6] t h a t  jn daytime the energy of 
in t iud ing  e lec t rons  with E > 0.  OS kcv i s  grcatcr than i n  n ight t  imc, while the 
v a r i a t i c n s  01 the inagnztic i i e l d  ;re smaller i n  dq-time than i n  nighttimc. In 
the  course 01 the exq~eriment tlie ionosphere was 1 i t  a t  a l l  a l t i t u d e s  during 
the  completc 24 hours a t  an iclcntjcal  zen i tha l  angle and t h i s  is  why the efCect- 
day- - n i ~ h t  cannot be explained by the  d a i l y  v a r i a t i  oils of  physical  paramctcrs 
of t he  ionosphcre. I t  was noted  above t o  what ex ten t  011 
of rnagnctic di s twbances  was sinall. 
i n t iud ing  e lec t rons  i i i t l i  E > 40 kev i n  the ncar-noon hours a t  thcse  l a t i t u d e s  
i s  more than by one order Iiigher than on thc ni:l':t sick [16]. Therefore,  sa- 
t e l l  i t e  observations are e\ridence t h a t  the  i n t i  
on the  daytimc side of  the Earth induces the rc  
o i  the  rnagnctic f i c l d  than i n  night  hours. 
re1 a t i v e l y  s m a l l  e l e c t r i c  f i e l d  o€ rnagnctospheric o r i g i n  i n  daytime. 
= 60 - 70" t he  valuc 
Hoivevcr , according t o  Injun- 3 the  f l u x  of 
CJII of in tense  p a r t i c l e  €luxes 
s t a i i t i a l  l y  smal lc r  va r i a t ions  
Tlic l u s s i b l e  c isc o f  t h i s  is the  
Tlie equivaleiit curl-ent system reprcscntcd i n  F ig .2  may serve a s  a bas i s  
€or tlie coiiiputation of  e l e c t r i c  f i e l d s  of planetary s c a l e ,  rvhich e x e r t  a sub- 
s tant ia l  i n h u e n c e  upon the flow of c~iargcci p a r t i c i e s  i n  &e niagnctosp~iere 
[23, 241.  
&$:$:A T H E E N D A A A : ~  
blanuscript reccivcd on 
1 Ju ly  1967 
COX"TR\CT KO. NAS - 5 - 1248 7 
1145 - 19t11 St.hlIr 
VOLT TECHiLTlCiU CORP'OitYJION 
i,xmiC;ms D.C. 20036. 
l'elcpiione : 2 2 3 - 6 7 0 0 (S- 3 6) 
on 25 hIarch 196s 
liefcrencos To1 lo!:. . , 
5 
R E F E R E IJ C E S 
[l 3 . 
[ 2 ] .  T .  NAGATA. P l a n e t .  Space S c i e . ,  11, No.12, 1395, 1963. 
B .  E .BRYUNEI,LI. Geomagiietizm i Areonomiya , 2 , KO, 5 , 801 , 1962. 
. K. D .  COLE. Space Scie.Rev. 5, PJo.6, 699, 1966. 
. S.  I .  AKASOFU. I b i d . ,  6 ,  No.1, 21,  1966. 
. T .  OBAYASHI. 
[6]. H. M. MOR07,LCldI. Plan.Space Sei., 1 4 ,  87, 1966. 
[TI. H .  3 3 .  SILSREZ, E.  H. VESTII!E. 
[8]. H .  FUKUSIiiru'fl. J. Fac. S c i .  Univ. Tokyo, Sec 11, 8, p t .  5, 1953. 
[9]. N .  P. BEN'KOVA. 'J!rudy NIIZ!d ,  vyp. 10 (20), 1953. 
[ l o ] .  0 .  A .  BURDO. Trudy AANII., 223, vyp. 3, 21 , 1.960. 
[I-11. I,. €IARANG. Terr.Magn. , 51, No.1, 353, 1946. 
[12]. S .  I .  AIiLlSOFU, S .  CHAPMAN, C .  I. ?.!EiLTG. 
[13]. B .  HULTQUIST. Ark. Geophys. 3 ,  63, 1958. 
[14]. Y .  HAFXJRA. Rep. Ion. Space Res. Japnn, 20 ,  Mo.2, 1966. 
[15]. IC. D. COLE. 
[16]. L .  A .  FRAWK, J .  A.  VAN ALLEN, J .  D .  CRAVEN. 
[17]. I .  B .  McDIAW,IIT), I .  R .  BURROWS. Can. J .  Piiys. , 42, NO.4, 616, 1964. 
[18]. B.  I .  O'BRICM, 11. TAYLOR. J .  Geophys. Res. 69, 4 5 ,  1964. 
E191 . 
[20]. YA. I .  FEL' DSHTEYN, A .  N. ZAYri'S2V. Geom. i Aerozcwiya., 5, 6 ,  1123, 1965. 
[21]. R .  G .  AFONIBA. I b i d . ,  5, 4 ,  772, 1965. 
[22]. Y .  I .  FELDSTEIN, A .  N .  ZAITZEY. Tel lus  5 ,  1968. 
[23] . V .  I .  KRASOVSKiY. Sb. I s s l  .Kosi-?icheslrogo P ros t r zns tv t  , NAUICA, 11- , 1965. 
[21+]. H .  E .  TAYLOR, E .  14. HONES. 
The i n t e r a c t i o n  o f  s o k r  plasna w i t h  t h e  geomagnetic f i e l d .  
l3 1 1; 1 
Belgrade. August 1966. 
T e r r .  Iilagn. 47, i'To.3, 195, 1947. 
J .  Atm E .  Terr.Phys.  , 27, l l " 1 2 ,  
1275, 1965. 
r k t u r e ,  199, No.bgc10, 1279, 1963. 
J.Geopys.Rcs. , 69, 4 ,  616, 1964. 
J .  P.  HEPPNER. High Lat i tude  :;egnetic Dist.\wbences. GSFC Pub1 .~-61.2-66-h;5 
1966. 
J .  Geophys. Res . ,  70 ,  No.15, 3605, 1965. 
i 


Polar magnetic disturbances and intrusion of charged particles into the ionosphere

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