Energy flux values calculated for solar plasma in sectorial structure of interplanetary magnetic fiel

Kovalevskiy, I. V.

English

NASA Technical Reports Server

National Aeronautics arid Space Administration 
Goddard Space F l i g h t  Center 
Contract No, NAS - 5 - 1 2  4 8 7 
ST-IMF-SP-10671 
ENERGY FLUX OF SOLAR PLASMA I N  A SECTORIAL STRUCTURE 
OF THE INTERPLANETARY MAGNETIC FIELD 
by 
I .  V. Kovalevskiy 
(USSR) 
8 FERRUAKY 1968 
A 
https://ntrs.nasa.gov/search.jsp?R=19680007551 2020-03-12T09:16:44+00:00Z
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ST-IMF -SP -10671 
Geomagnetizm i Aeronomiya 
Tom 7 ,  No.6, 978-981, 
Izdatel'stvo "NAUKA, 1967. 
by I. V. Kovalevskiy 
Computed in this paper are the three-hour values of the density of 
kinetic energy flux of the directed motion of the plasma q , and the flux 
density ofbtheml (q,) and electromagnetic ( q 3 )  energies #or the positive 
and negative sectors of the interplanetary magnetic field, observed from 
December 1963 to February 1964 with the aid of AES IMP-1. The character 
is discussed of 41. q2, q 3  distribution in sectors and their relationship 
with solar plasma velocity. It is shown that q i > q 2 = q 3  and that there is 
no particular difference between the sectors. 
fluxes through sectors' cross-sections. 
Estimates are made of energy 
* 
* * 
The detection at the distance of Earth's orbit of sectorial structure 
of the interplanetary magnetic field on AES IMP-1 (December 1963 to Febru- 
ary 1964) [l] and the subsequent corroboration of this discovery on the 
basis of data of MARINER-4 (December 1964 to February 1965) and Mariner-2 
(August through December 1962) [2] have shown that the sectorial structure 
is apparently a constant property of the interplanetary medium. 
The investigation of the sectorial structure for a quiet interplanetary 
magnetic field (in a period of low solar and geomagnetic activities) allowed 
to establish in [3] the character of the distribution in it of magnetic field 
H intensity, of the velocity V, of the concentration n of the flux nV of so- 
lar plasma, the presence of approximately linear relaTionship between the 
daily sum of Kp-index and V and H, and the absence of any link between CKp 
with n and nV. Moreover, an opposite relationship has been established bet- 
ween R and the intensity of galactic cosmic rays observed on the Earth's 
surf ace. 
* POTOK ENERGII SOLNECHNOY PLAZMY V SEKTORNOY STRUKTURE MEZIlPLANETNOGO 
MAGNITNOGO POLYA. 
* 
E c 
A fu r the r  i nves t iga t ion  of f i e l d  atid plasma c h a r a c t e r i s t i c s  for  the  
s e c t o r i a l  s t r u c t u r e  has been conducted i n  [4, 51. 
According t o  da t a  on V ,  n and I I  from [ 3 ]  and plasma tcmperxturc T i n  
the  fonn assimcd i n  141 (TB is thc  uppcr l imit ,  '1'11 is t h c  lower l i m i t ;  ana- 
logous i d  iccs  have valucs  corresponding t o  the  l a t t e r )  , thrce-hour  values  
valiic>s a r c  coiiipiited i n  the  cu r ren t  work of the  dens i ty  of k i n e t i c  energy 
f l u \  of tlic d i r e c t e d  plasma iiiotion q l  , the  f lux  dens i ty  of thermal (q ) and 
clcc-troiiiapict ic ~ q , >  c n c r g i i s  for  tKc pos i t i ve  and negat ive  seco t r s  oLserv:.d 
011 A I 5  IbIP-1. All t11c valiics r-cfc.rritig t o  the  p o s i t i v e  or  negative sec tu r s  
\ill 1 lw JctiotCd lwlo\v by symbols "pl~is" or  "minus';. 
I f t hc  s e c t o r i a l  s t ruc  tiirc prcprcwwt s ; i n  i deal  tnagnctohydrodyn~~iii~ 
iiicdiiuii, tlw t o t a l  dens i ty  of cncrgy Clux [ h ]  is 
(1) 
1 
4n q = + pwV + - [IIlVHU, 
d i e r e  the  f i r s t  term from the  r i g h t  i s  q l  , the  second q2 and the  t h i r d  q 3 ;  
P I iiui, i<herc m_ is the  mass of the  proton; the thermal funct ion of the  un i t  
of inass is \i -= vnk'r / (Y - 1 ) ~ ;  k i s  the Holtzmann cons tan t ;  Y is  the  ad iaba te  
i n d i c a t o r ,  f u r t h c r  assumed t o  be 1.5.  
1' is rad ia l  [ 7 ]  , the  f l u s  dens i ty  rnotluli have the  following form 
Inasmuch as i n  the  f i r s t  approximation 
wlicrt. I 1  is the r a d i a l  comporicnt of  tlic f i e l d .  12 
,. Ihe compiitcd valiics of  q ~ + ,  q2+, q3+ and qi-, q2-,  93- are p lo t t ed  i n  Figure 1 
whcrc tl ic o r i g i n  of the  scc to r  i s  taken f o r  t he  zero day .  
g, e r g  - cmi . sec 
the s t a t e  of the  in t e rp l ane ta ry  mcdiiun for 2 . 5  revolut ions of the  Sun 
(I)ec.1963 t o  Februar). 1964). Note tha t  during t h i s  per iod Kp 5- . 
t i v e  sec to r  shows t h a t  a t  the  beginning of the  f i r s t  day of Ea r th ' s  p re-  
sence i n  the  s e c t o r ,  wevy low values of f l u x  d e n s i t i e s  are observed : 
iwaiys is  or' rile cha rac t e r  of fiux dens i ty  c i i s t r - i b u t i u I i  f o r  the posi-  
whicK increase rap id ly  arid reach ;I r a t h e r  sharp maximum a t  the  end of the  
second day : 
a t  the  elid of the  second and a t  t he  beginning of the  t h i r d  day. 
l o w  3 decrease of q+ 
Then f o l -  
t o  
a t  the middle of the  f o u r t h  day. 
increase  of q+ is  noted till 
A t  the  beginning of t he  f i f t h  day a small 
Af te r  t h a t  t he re  is a lowering to  the minirnum: 
a t  the  en3 o f  the  f i f t h  day. 
t he  s e c t o r  f o r  q l +  and q 2 + ,  whereas f o r  q + an add i t iona l  m a x i m u m  seems t o  
criierge with amplitude 4 . 6  erg.cm32.sec-1.  
Then a feeble  rise is  w e n  through the  end of 
Roughly speaking, t h e  d i s t i l ~ u t i o n  of q+ may be represented i n  the  form of 
;I \GILT,  of  which the f i r s t  ha l f  is contracted t o  a g r e a t e r  ex ten t  with a 
grc:itc\r amplitude by coiiipirison with the  second h a l f .  
a re '  s~ipei.iiiil~osed t o  tlwt wave. I,ct us point  out t ha t  t h a t  the  charac te r  of  
q -  Jisti-iljiit iori is aliiiost siiiii1;ir t o  t k i t  of q+.  
c v i ~ - ~ '  - ~ w s i s t s  i n  t ha t  %it tlic Iqi i i i i i i ig  of the  f i r s t  t h y  very high values of 
q ~ - ,  qz-, gs-, ;ire d w \ n , c d ,  wliicii rcicli  liiiiiost iii;ixiniuii va lues ,  d l i l c  t h e  h s i c  
i i i ; i \ i i i i i u i i  ( 7 1  (1- is witlc.1- 1)). c-oii ipiris;oii  with t h t  of q+. A t  thc  end o f  t he  s e c t o r  
t l ic '  \bc-,ihc.i. ,iddit i o i i ; i l  i i i ; i i i i i iuu i i  for is riot v i s i b l e .  
Additional va r i a t ions  
l'he most si ihstantia1 d i f f c r -  
4 
liouglily speaking, the d i s t r i b u t i o n  of q+ may he rcprcsented in t o m  of 
a W;IVC\, of which the  f i r s t  ha1 f is  mom cont rac ted  and i t s  a m p l i t d c  is g r e a t e r  
Wc sh;il l  po in t  out  t h a t  the  cha rac t c r  of q- d i s t r i l w t i o n  is a l -  
most siini lar  t o  tha t  01' (1'. 'I'hc most su1)stant ia l  dirt-crcncc cons i s t s  i i i  t h a t  
: i t  tlic I~egiriiiing 01' tlic r i r s t  day there  a r e  ollscrvcd very  high vallics ql', q2- ,  43-1 
rcach i ng 3 liiiost iriasiri iuii i  \':I l u e s ,  whi l e  tlic has ic inaxinnun of' q -  i s  i~roatlcr (widcr ) 
I)). coiiiparisoii ~i tIi thc i i1 , i s i i i i tu i i  of q+.  
tlic s c ~ t ~ r '  is not ~ i s i l ) l ~ % .  
coinparison with t h e  second half-\ .~nvc~. Additional v a r i a t i o n s  arc supcrimposed 
oii this W;IVC. 
I:or ( 1 -  3 weaker i i i a ~ i i i i i i r i i  ;it the cwcl 01- 
'The mcm values of 1 - 1 1 ~ ~  dcnsi t i e s  q and 1 imits  of  q v x i a t  ion (numbers in  
parcnthcscs) are prcscntcd i n  T a b l e  1 for the  per iod uridcr considerat ion,  f o r  
Imth thc pos i t  i w  mid negat ive sec to r s .  Moreover, fo r  the  sake of comparison 
coiiipiled i n  the  t a b l e  a r e  a l s o  the  corresponding values of cnergy fluxes f o r  
thc c l ; i t a  of bLhKINEII-2 ( p a r t i a l l y  brought out  i n  [8 ] .  
I t  
I I  
1 1  
- 1  c rg  sec 
C' 1'6 
. .  . 
Conscqucnt l y ,  t he  s t a t c  o!' the> i i i tcrplaiictary iriedium a t  a lie1 ioccn t r i ca l  
dis t t ,u icc  01' 0.8 - 1 a.11. chirinr: olwcrvat ion..; on ~tV<INl:K-Z d i  f fcred from the sta- 
tc o!' the  iiicdiluii diiri iiq i i i ~ : ~ s ~ i r ~ e i i i ~ ~ i i t ~  o i l  11\11'=1 , \ ~ h c i i  the  v a r i a t i o n  limit.; - ~ w r c  
1' 
; i d  lilz 2.5' 10"" h <ilid T',x 5 
2?0  - 340 hili SLY-- as Y % 5 1  5 hili s;c\c-i :ii i t l  I I  5 0 - 1 4 .  5 cm- as 11 % ' 1  c-111- ;, 
IO'"  h 13, 3 1 .  
l t  iiiav Iw sctw t'i*oin tlic tal)ic that the  energy dens i ty  of the d i r cc t cd  
iiiot im ~-oiis idcrahly cscccds (by 1 -- 2 ordcrs)  t he  f l u x  dens i t  ies of  thermal and 
clc'cti'oiii~igiictic energy, whiic ( ~ 2  Z ria. 'l'lie l a s t  deduct ion xgcces well with the  
wstil t obt,iiiiecl i n  [HI . Notc iiicidciitiy t h a t  t he  con t r ibu t  ioii of var-iatioiis 
~ i t h  p c i * i d  . 3 hours i s  not taken in to  iiccowit i n  q 3  , which leads t o  its cer- 
ta 111 uiiderrating [SI. I t  is  a l s o  olnrious t h a t  a s i g n i f i c a n t  d i f fe rence  between 
tlic I ' l ~ t k  Jc-iis i t i cs  fo r  tlw positive ;ind negat ive s e c t o r s  is absent ,  and t h a t  
41 < i t " ,  Q2 < qz', QsGqP, wherc qi" 
~ . ~ ~ i s t i i  c d  011 hbU<lRLl?-2.  
coii icidc with those olitaiiicd i n  [10] . 
,ire the  d e n s i t i e s  of the  respec t ive  f luxes  
Notc t l i : t t  the vctlucs of q,  obtained i n  the  present  work 
Tlic above est i rnatcs  of energy f luxcs  may c o n s t i t u t e  a c e r t a i n  i n t c r e s t  
i n  ionmeit  ion with ques t ions  bear ing on tlic gciieration and emergence of plasma 
l'ltiscs from the  su r face  of  the  Sun, on their poss ib le  acce le ra t ion  i n  i n t e r -  
p 1:uictar-y space, mid :lis0 on the  cpicst ioii of rccur rcn t  magnctic dis turbances.  
Inasmuch ;is thc I)oiiridarics of- the coiisiclcrcd scctor ic i l  s t r t i c turcs  rcprcscnt  
t hc  rcgioori of  po1;irity shift of  tlic i.1tc~rpla1iet:iry Inagiict ic- f i e l d ,  tlic plasma 
: iccc~lc~tx t  ion  mc~cli;iiiisiii ; i t  t he  expc~iisc 01' field mnil i i  I : i t  i o i i  i n  t l i c $  i l c u t r d  
l:i)-c~i.  ~ 1 c ~ s c r v c ~ s  a t t e n t  ion [ 11 I . I I ~ w ~ ~ c ~ i ~ ,  the  q t i : i l  i t:it i v c  c>\:iiriiii:itioii of  the 
l i i ~ ~ i  1 : I ~ l t  ~1at; i  o i l  (1 i r i  tlic c - t i r r c i i t  work ,  ;iiicl ; i Iso 01' d : i t : i  o i i  c'iwrgy dcrisity of  
thcl c l i r c ~ c t c d  ; i d  t l ic \ r i i i : i1  iiiotiuiis ; i i id  0 1 -  t l i c  iii;iSiictic f i c ' l t l  in  [ 4 J  , f a i l e d  t o  
!.ic It1 c-(iiivincing c l c d t i i t  ioi i . ;  iii f;ivor o!' : ic-t  io11 or t-liiit inechmism. 
I ' l ic~ ;ititlior is gr;i tc\ful  t o  Yu. I ) .  K : i l i n i r i  f o r  h i s  constant  support  i n  t he  
\iorh. 
I Z h I I R : \ N  Man1 ; s c r i p t  received on 
28 Apri l  1967 
lU , l ~ I N ~ N C l  S -
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71, 2831 , l ! N ~ h .  
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[ S I .  I .  1’. K O V A L l 3 3 i I Y .  Ib id .  11.784, 1967. 
I b J  . I,. 1). LANl).AU, 1:. M. LlI~SIIl‘l’S. lilektrodinamika sploshnykh s rcd .  
1 - 1 .  I: .  I s ‘ .  LYOX. Thc Solar  Wind (Ed. Mackin 4 Neugebauer) .Perg.I’r.295, 1‘306. 
[SI. K. (i. IVtZNOV, I. V. KCIVALLVSKIY. Geom. i Aeronomiya, 7 ,  5,  880, 1967. 
[! ) I .  . J .  Geophys. Res/ 7 1 ,  4469, 1966. 
[ l o ] .  , J .  bl. WILCOS, K .  I I .  SCIIRTTEN, N .  F .  NESS. Ihid.  7 2 ,  19, 1967. 
111 J .  
lilcctrodynamics of Continua) Fizmatgiz, lflS!I. 
bl. NIXJGIJHAUER, C .  W. SNYDEK. 
1 1 .  E .  PETSUEK. - AAS - NASA Symposium on the Physics of Solar  F la res .  
NASA SP-50 (Ed. Wilmot r\;.lll:SS) 
1964. 


Energy Flux of Solar Plasma in a Sectorial Structure of the Interplanetary Magnetic Field

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