Relationship between geomagnetic activity parameters and energy density of quiet solar wind flu

Kovaleskiy, I. V.

English

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National Aeronautics and  Space A h i n i s t r a t i o ~ ~  
Goddard Spacc Fl ight  Ccritcr 
Cont r a c t  No. NAS- 5 - 124 57 
NL.4TIONSI IIP I3EIIEIN 'I'lE GEOMAGNETIC ACTIVITY AI11 
Tllli IJNERGY DENSITY OF QUIET SOLA1 WIND FLUX 
bY 
I. V .  Kovalevskiy 
(USSR) 
Y 
https://ntrs.nasa.gov/search.jsp?R=19680007323 2020-03-12T09:18:23+00:00Z
ST- IMF- CSI- 10072 
MLA'~IONS1 IIP BETWEEN RE GEOMAGNETIC ACTIVITY AND .- -
11-IE ENERGY DENSITY OF QUIET SOLAR WIN11 FLUX 
by I .  V .  Kovalcvskiy 
12ccoiding t o  da ta  of IMP-1 on the  s e c t o r i a l  st i-ucture of t he  in te rp lanc-  
t ; i ry  I-L ;:lietic f i e l d ,  apparent ly  representing a q u i e t  s o l a r  wind, es t imates  
are m:dc 01' c i i c r , ~  f luxes  of d i r ec t ed  motion of theqnal arid electromagnetic 
encrgy inciclcrit upon the  c ros s - sec t ion  of the magnetosphere. 
I t  is  shown t h a t  t he re  are enough energy f luxes  of each k in3  sepa ra t e ly  
even for  the  c r e a t i o n  of the  e n t i r e  complex of geophysical events  i n  a per iod 
o f  rnotlernte magnetic s tonn.  'The charac te r  is inves t iga ted  of the  1 ink between 
thc thrce-hou1-1y values  of the  E; -index of  geomagnetic a c t i v i t y  o r  the  amplitu- 
des aI, equivalent  t o  them, with !he flux d e n s i t i e s  of the  var ious  forms of 
energy. 
* 
* * 
l'lic s e c t o r i a l  s t r i i c tu rc  of  thc> in te rp lane tary  f i e l d  de tec ted  on MS IMP-1 
[ 1 J appai-ent 117 rty)r-"wnts the  qu ie t  solar wind. According t o  measurements of 
plasin;i :iiicl of the magnetic Cicld of  such a s t r u c t u r e  [1] ca l cu la t ions  were 
perfot-mc~cl o f  dens i t i c s  01- these d i  f fcrcnt forms of energy and t h e i r  re l . i t ion-  
ship lvitli the gcomagnetic f i e l d  was invest igated 1 2 ,  31. Ik s idcs ,  the dens i -  
t ic\s of cnc-rgy flu\rcs 01' the  directccl ((11) and thernia1 flows (q2)  , arid a l s o  
c.lcct roitiagiict ic c~iic\rg\' (q , )  Iiavc i~ceii coiiiputcd in (41 . I n  t he  present  papcr 
\\e iiivestigatc> the char;ictcr of  thc 1-clat ionship bctwccn t h e  valucs  of the  K - 
iiidci, o r  clt' :I[), :ii-er:igcd for  t h e  corrcsponding time in t e rva l s  by a l l  pos i t i ve  
m c l  ncgati\.c s e c t o r s  (sce [ Z J ) ,  ;inJ q l ,  q, , ,  q , .  
;I scr ics  of geophysical e f f e c t  : geomagnetic and ionospheric d i s turbances ,  
a i i r o r x  and so f o r t h .  
a t  the cxpcxsc of energy of  plasma fluxes. 
110 uniqut~ opinion ;IS regards the t r a n s f e r  mechanism of s o l a r  energy f l u x  in s ide  
the  iiiagnctnsphere [ 5 - 71 . 
P 
'l'lic i n t e rac t  ion of solar  p l a s m  with the  Ea r th ' s  magnetic f i e l d  leads t o  
I t  is  c l e a r  that  t h i s  complex of phenomena is  crea ted  
However, t he re  has been t o  da t e  
For this reason i t  is important t o  know the  magnitude 
(*) S1'Y-A~ ' (;liObfl(;NI'I'NOY AKl'JVNOS'TI S I'LO'I'NOST'YU POTOKA ENlR(;T I SPOK0YNCK;O 
- - -~I_ -- 
S01,NI :(:I No(;o VI i ' l 'RZ.  
2 
of the energy f lux t h a t  may lie acquired by the  magnetosphere from the  s o l a r  
wind. 
inate o f  the  mean and l i m i t  values  of energy fluxes inciclent upon t h e  c ros s -  
sect ion of  the  magnetosphere S (according t o  [SI S = S - 10'0 cm'I f o r  orie 
sccond (CIS) and f o r  t 24 hours ((1st) ( i n  the  ttssunption t h a t  t 24 hours 
correspond.; t o  tlw ; ivcr;i~c dura t ion  of a storm) . 
G3S, (1151. qaBst, i j d t ,  ij.-Ct a r e  givcn i n  ?'able 1 ( the  l i m i t  v a ~ u e s  being in  pa- 
rcnthcscs)  fo r  the p s  I t ivc and ncgtitivc s e c t o r s .  'I'he indices  and poin t  
t o  the f a c t  t h a t  q,, was compiited by thc upper and l o w r  leve l  of' tcinperature 
( sec  i n  this r c s p e t t  1 .21) .  I t  may bc secn from the  t a b l e  t h a t  t h e  d i f r c r e n -  
ces  i n  the  f l t i x c s  €or the  p o s i t i v e  :md negat ive  s imply  do not e x i s t .  Moreover, 
(7,s '"W q3S. Note t h a t  t he rc  i s  criough energy f l u e s  oE each hind scpara te -  
l y  f-or the  c rea t ion  of  the  e n t i r e  complex of events  even i n  time OS a magnetic 
stonii i n  the  per iod of wliicli the  r a t e  of energy in j ec t ion  in s ide  the  magneto- 
sphere must c o n s t i t u t c  % l 0 l 8  - 10l9 erg/scc [SI],  although the  above da ta  Erom 
TMP-1 are inherent t o  q u i e t  s o l a r  wind. 
medium, observed i n  1962 on MARINLR-2, higher  energy d e n s i t i e s  arc charac te r -  
i s t i c  (see [8] and the  t a b l e .  12et u s  paiise on values of q s t .  I t  is known t h a t  
f o r  the  c r e ~ t , i o n  of a magnetic storm during t h c  main phase 2. 100 ( energy of 
al,olit .3 * 10- 
gJt, g&q& scl):irately a r e  suf  F ic ien t ly  for  inducing such ;i storm. 
1)atrr on q from work [ 4 ]  a r e  u t i l i z e d  i n  the  prssent  worh f o r  t he  e s t i -  
I'he mean values rlJ, r j ~ J ,  &I$, 
For a more pcrturbed in t e rp l ane ta ry  
c=rg is rccpircd 171 .  We see from Table 1 t h a t  each of energies  
liAl3Lli 1 
, I S  , 
q, s 
- --I -- 
nu'- 1 I 
~ 1 MARINER-2 I pos i t i ve  1 negat ive ! 
s c c t o r  s e c t o r  
I 
I 
5,o. 10'8 
(0.0.5.: 20.0) ' I O ' S  
25.0.  102' 
3 
Fig. l c  
Ilowever, 
a b 1 2 .  A tendency t o  l i n k  of 5, w i t h  q211 is  seen,  though i n  t E is case f o r  
tce negati  ve scx to r  the d i spe r s ion  is greater. 
.set, 
o r  Yip > 7 .  
I'or tlic pos i t i ve  s e c t o r .  
t i v c  sector.  
t i , j -  > 2.5 * erg.cm-'.sec-' Kp > 2, o r  a 7.  A near ly  l i n e a r  dcpmdence 
K , ) c q J + )  i s  : i ppuen t ly  explained ~))r the f a c t  Phat plasma ve loc i ty  v and the  in -  
t tms i ty  of the  magnetic f i e l d  I f ,  d i r e c t l y  l i i i kcc l  with ITp are p a r t  of 
note t ha t  fo r  q1+ > 0.22 erg.ctn-2.sec-1 we observe R + 5- o r  
, 
e r g  cm-' 
> 1 2 ,  tmt q z n  > 40.10-3 erg.cm-2.sec-1, K~ -3 z9 
- 
Moreover, qzn+  > 5 . 4 .  
> 3 is inherent ,  o r  
A good rclat ionshif?  is  revealed between Kp and q 3 ,  p a r t i c u l a r l y  
A g r e a t  dispers ion of po in t s  is observcd i n  the  ncgci- 
erg.cm-2-sec-1  Kp 2 3- o r  ap > 1 2 ,  and f o r  - For 4,' > 4.5 
- 
-- 
q 3  - V I I J I I ~  - I I R ~  / 4 
(tlrl Iw itig ;I radial cntiipoiicwt of II) [ 1 I , 
The ;iiithor is indel)ted t o  Yu. I ) .  Kal inin fo r  d i scuss ing  the  work and ma- 
king remarks. 
- 
(*) i r iscr t  omission I t  and f o r  q l -  > 0.2  erg.cm-2.sec-1 Kp ? 2, o r  % >- 7 
I Z b l I M  
**** T 11 E E N D 
Received on 28 Apri l  1967 
[ lJ  . .I. bl. \VII,C:OS, N .  1 ' .  NESS. $J.  (kopliys. Res. 70, 5793, 1965. 
[:I. 
[SI. I .  1'. KOVA1,EVSKIY. l h id .  - 7 ,  No.5, 784, 1967. 
141. I .  c ' .  KOVALkVSKIY. [bid.  7 ,  No.(>, 978, 1967. 
I S ] .  Ill. 1,. ULININ, 1;. I .  bUG1LrYSKIY. Sb.Issl.Kosmicl~.Prostranstva, p.368, 
1 0 1 .  I .  A.  ZIULIN. Geotnagnetizni i Aeronomiya, 2, No.2, 197, 196b. 
171. S. 1. AKASOFU. Space Sci .  Revs, 4, 2 1 ,  1966. 
18J .  h.  (;. lVANOV, I .  V .  KOVLLVSKIY. Geom. i Aeronomiya, I _ ,  5, 880, 1967. 
[!'I. W. 1. AXFORD. The Solar Wind (Ed. Mackin 6 Neigebauer) Perg.Pr. 231, 1966. 
[lO]. J .  M. WIICOX, K. 11. SClIATTEN, N .  F. NESS. ,J.Geophys. Res. -_ 7 2 ,  19 ,  1967. 
1 .  V .  hO1~AId~VSk:IY. Geoniagnetizni i Aeronomiyz 1, No.5, 878, 1967. 
Izd.vo "NAlJKA", 19b5. 
I~1Sl1I1131l'I'TC~N: s,mic' 671, d d  GSFC 3 acld. copies  t o  codc 012 a t  t h e  expense - ~ - _ _ _  of coclc ( 2 1 4 .  Add 1 cc code 641 (S tern)  


Relationship between the geomagnetic activity and the energy density of quiet solar wind flux

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