The suggestion is substantiated that the periphery of the heliomagnetosphere, the region in which properties depend on both solar wind and interstellar space parameters, plays a much more important role in the solar modulation of galactic cosmic rays than previously believed

Charakhchyan, T. N.

Krainev, M. B.

Stozhkov, Y. I.

English

NASA Technical Reports Server

481
SH-4.2-19
ON THE INFLUENCE 0P THE HELIOMAGNETOSPHERIC
PERIPHERY ON THE GALACTIC COSMIC RAYS
Kralnev M.B., Stozhkov Yu.I.,
P.N.Lebedev Physical Institute of the Academy
of Sciences of the USSR, Leninsky Prospect, 53,
117924, Moscow, USSR
Charakhchyan T.N.
Institute of Nuclear Physics, Moscow State
University, 119899, Moscow, USSR
ABSTRACT
The suggestion Is substantiated that the
periphery of the heliomagnetosphere - the
region which properties depend on both solar
wind and interstellar space parameters -
play much more important role in the solar
modulation of the galactic cosmic rays than
usually believed.
I. INTRODUCTION.
As a rule the electromagnetic fields in the galactic
cosmic ray modulation region are specified by the extrapola-
tion of those known at r_ 30 AU. Clearly the restriction
imposed on the possible modulation region characteristics
in this scheme also limits the range of the explicable by
means of it galactic cosmic ray phenomena. Let us call the
galactic cosmic ray modulation accomplished In conformity
with the above scheme the "Inte1_al"modulatlon.
The mentioned extrapolation is valid only in the case
when the whole modulation region is inside the supersound
and superalfvenlc solar wlnd which properties are control-
led entirely by the Sun. In thls work the suggestion is
substantiated that the galactic cosmic rays should (and pro-
bably do) undergo considerable transformation In the transi-
tion region between the supersound solar wlnd and the undis-
turbed by the Sun galactic space.
2. THE THEORETICAL REASONS.
Plrst of all note the discrepancy of the "internal" mo-
dulation scheme during the periods when the large-scale mag-
netic field distribution in the quiet (l.e.und_urbed from
the outside) solar wlnd is a dipole-like one. In this case
because of the space charge the potential of the inside of
the modulation region boundary surface considerably depends
on the heliolatitude while the exterior of the same surface
conforming to the undisturbed galactic space Is equlpoten-
481 
SH-4.2-19 
ON THE INFLUENCE OF THE HEL I OMAGNET 0 SPHERIC 
PERIPHERY ON THE GALACTIC COSMIC RAYS 
Krainev M.B., Stozhkov Yu.I., 
P.N.Lebedev Physical Institute of the Academy of Sciences of the USSR, Leninsky Prospect, 53, 117924, Moscow, USSR 
Charakhchyan T.N. 
Institute of Nuclear Physics, Moscow State University, 119899, Moscow, USSR 
ABSTRACT 
The suggestion is substantiated that the periphery of the heliomagnetosphere - the 
region which properties depend on both solar 
wind and interstellar space parameters -play much more important role in the solar 
modulation of the galactic cosmic rays than usually believed. 
1. I ODUCTION. 
As a rule the electromagnetic fields in the galactic cos ic ray odulation region are specified by the extrapola-ti n of t ose kno n at r~30 AU. Clearly the restriction i posed on t e possible odulation region characteristics i  t is s e ls  li its the range of the explicable by eans f it galactic cosmic ray phenomena. Let us call the galactic cos io ray odulation accomplished in oonformity ith the above soheme the tfinte:Pa.ltfmodulation. he entioned extrapolation is valid only in the case hen t e hole odulation region is inside the supersound  peralfvenic solar wind which properties are control-l  ntirely y the Sun. In this work the suggestion is bstantiated t at the galactic cosmic rays should (and pro-ably do) undergo considerable transformation in the transi- r i n bet een the supersound solar wind and the undis-t r ed by the Sun galactic space. 
. E RETI AL SONS. 
First f ll note the discrepancy of the "internal" mo-ulati n sche e during the periods when the large-svale mag-etio fi l  distribution in the quiet (i.e.und~urbed from  t i ) solar wind is a dipole-like one. In this case use f the space charge the potential of the inside of  odulation region boundary surface considerably depends on the heliolatitude while the exterior of the same surface f ing t  the undisturbed galaotic space is equipoten-
https://ntrs.nasa.gov/search.jsp?R=19850026543 2020-03-20T17:00:05+00:00Z
482
SH-4.2-19
tial. To settle this contradiction the transition region
should be included in the galactic cosmic ray modulation re-
gion/ 1,2/.
In /3-5/ the processes in this transition region are
considered for the explanation of some galactic cosmic ray
effects. It is important that for these explanations the
fundumental difference of the modulation parameters from
those of the Quiet solar wind is neeessary: the nonradial
flow of plasma /4,5/ and the large latitude component of
the interplanetary magnetic field /3-5/.
At the same time the qualitative character of /3-5/
should be noted as well as the obvious ins"fficiency of the
method suggested in /1,2/ to allow for the transition re-
gion influence on the galactic cosmic rays. This method us-
ing the Liuville theorem and the potential difference bet-
ween the inside points of the quiet solar wind and the in-
finity (so ca_led the "external" modulation of the galactic
cosmic rays) takes into account only the charge distributi-
on in the quiet solar wind and completely disregard the ga-
lactic space characteristics: the presence of the galactic
magnetic and electric fields, the movement of the solar sy-
stem through the interstellar matter and so on.
3. THE EXPERIMENTAL REASONS.
A. The most dramatic feature of the galactic cosmic rays
w_-_ch is evidently beyond the scope of the "internal" mo-
dulation is their behaviour in the low energy range (E_80
MeV/n) during 1971 -1978 - the "anomalous component" (AC},
/6/. The characteristics of these particles - their elemen-
tal and isotopic compositions, energy spectra - so differ
fromthe expected ones that there are many advocates of the
hypothesis /7/, according to which the source of the anoma-
lous component is the interstellar neutral gas, i.e. AC
does not have any bearing to the galactic cosmic rays. Yet
some features in cosmic ray behaviour force us to regard
the "anomalous component" as the natural part of the com-
plex galactic cosmic ray phenomenon taking place during
this period:
I) The time behaviour of the anomalous component fluxes
is very simillar to that of the protons and helium
nuclei of higher energy;
2) The very important fact, connecting anomalous compo-
nent with the protons, is the simillar (and anomalous)
behaviour of their radial gradients. With the growth
of the solar activity in 1979-1980 the gradients of
both anomalous component and protons of E:29-67 MeV
sharply drop off /8/.
82 
H-4.2-19 
ti l. o e tle t is ontradiction t  t siti n r i n 
s ould be i l ed i  t e alactic c s ic r  odulation r -
gion/1,2/. 
In / - / the processes i  t is tra siti n region are 
onsidered f r t  planation f s e alactic c s ic r  
effects. It is i portant that for these explanations the 
f dumental if ce f t  odulation ara eters f  
t se f t  uiet lar i d i  eeessary: t  onradial 
flo  of plas a / , / and t e lar e latit e co ponent of 
the interplanetary agnetic field /3-5/. 
t t  s e ti e t  ualitati e haracter f / - / 
ul  e ot d s ell s t  vi us ~ficienc  f t  
ethod suggested in /1,2/ to allo  for the transition re-
gion influence on the galactic cos ic rays. This ethod us-
ing the iuville theore  and the potential difference bet-
een the inside points of the quiet solar ind and the in-
finity (so called the "external" odulation of the galactic 
cos ic rays) takes into account only the charge istri uti-
on i  the iet s lar ind and co pletely isre ard the ga-
lactic space characteristics: the presence of the galactic 
agnetic and electric fields, the ove ent of the solar sy-
ste  through t e i t rstellar atter and so on. 
3. THE EXPERI ENTAL REASONS. 
. he ost atic t r    l cti  ic s 
nIch is evidently beyond the scope of the tlinternal" o-
lati   ir aviour   l  r  e  ~ 80 
eV/n) during 1971 -1978 - the "ano alous co ponent" ( }, 
/ /. he c aracteristics of t ese articles - t ir ele en-
tal and isotopic co positions, energy spectra - so differ 
from the expected ones that there are any advocates of the 
hypothesis /7/, according to which the source of the ano a-
lous co ponent is the interstellar neutral gas, i.e. AC 
does not have any bearing to the galactic cos ic rays. et 
s e f t r s i  c s ic r  aviour f r  s t  r r  
the "ano alous co ponent U as the at ral art of the co -
plex galactic cos ic ray pheno enon taking place during 
this period: 
1) The time behaviour of the ano alous co ponent fluxes 
is very si illar t  t at of t e protons and heliu  
clei f i er e er ; 
2) The very i portant fact, connecting ano alous co po-
nent ith the protons, is the si illar (and ano alous) 
avi ur  t i  i l ients. it  th  r t  
f th  l r ti it  i  -  th  r i ts f 
both ano alous co ponent and protons of =29-67 e  
sharply drop ff / /. 
483
SH-4.2-19
In Fig. 1 the behaviour of
the anomalous component
,,, _,, _ r, r,,,' _ I (Hg spectral index: dJ/dE _ADDITIONALCOMPONENTINSTRATOSPHERE,
_0- _ MURMANSK I E o, /8,9/,_) is correla-
--R>0.SGV ted with that of so called
_j_mrm n ,., "the additional component
____ in stratosphere", (_),
105 which, as shown in /10/, is
due to the primary H and
_.oo He nuclei in the energy
range 100-500 MeV/n.
The likeness of the
0_ behaviour of the anomalous
component and of protons05
H,SPECTR^L,N0eX(_ ~E r) is rather difficult to un-
fair_.: i derstand from the viewpo-0 _ ,_.-" --_6-55_ int of the current hypothe-
/ ._J":."'.:_,_,._O-20_-Q see on their origin /6/,In /2/ we suggested the
0.5 _'ik,_!+ scheme of AC formation
by
a the acceleration of low
4.0 i.I-I++ energy galactic cosmic rays
I in the process of their+ "ex ernal" modulation. The
, , , J J _ z , _ _ , _ J , , same process results in the
_970 75 _980,.,VE_R& considerable increase of
FIGURE 1 higher energy particles.
B. The unusual from the viewpoint of the "internal" modu-
la--_ionthe galactic cosmic ray phenomena take place during
the periods of the inversion of the general magnetic field
of the Sun (GMFS).
In /11-13/ we subdivided the galactic cosmic ray beha-
viour during GMFS inversion into two phenomena:
I- Due to the supposed attenuation of the interplanetary
magnetic field strength the decrease of the galactic cos-
mic r;y modulation so much the greater (and the more pro-
longed) the greater the particle energy is. This explana-
tion of the "energetic hysteresis" is entirely in the sco-
9e of the "internal" modulation scheme.
II- The phenomenon depending on the type of GMFS inversi-
on (characteriz@d by the sign of the dM /dr, where M_ is _the projection of the general magnetic field of the _un ma
gnetic dipole moment on the Sun rotation axis) delaying
with respect to the first phenomenon by I-2 years. We re-
late this delay to the location of the process responsible
for the second phenomenon on the periphery of the hello--mag-
net osphere.
Fig.2 shows the galactic cosmic ray behaviour accor-
ding to the stratospheric data (M_rmansk, R^--O°5GV) during
the periods of GMFS inversions in 1969-71 (_dMz/dt>O,a)
483 
ADDI I NAL COM NENT IN ST TOSPHER  
f fO::J M MANSK ' 
-;:;- - R> O,5GV 
vnort"l 
lOS ct 
wo 
095 
0.5 '}( He SPECTRAL INDEX l ~~ '" E -r) 
B r/lN4.· .:... -/6-55 M~B o 
:' :: .... ::~ ·fO-20~ 
I e. \ I II 
,0.5 +! \ ~HJ 
r 
' I r 
, "J' ~/ + 
T L"l + \ /1 + 
75 
FI URE 1 
19 0 Y£flRS 
SH-4.2-19 
In Fig.  the behaviour of 
the anomalous component 
( e spectral index: dJ/dE~ 
E-6, /8,9/,8) is correla-
ted with that of so ca led 
"the a ditional component 
in stratosphere", (a), 
which, as shown in /10/, is 
due to the pri ary H d 
He nuclei in the energy 
range 1 0-5 0 MeV/n. 
The lik n ss of the 
behaviour of the anomalous 
component and of protons 
is rather difficult to un-
derstand from the viewpo-
int of the current hy the-
ses on their origin /6/. 
In /2/ we su gested the 
scheme of AC formation by 
the a celeration of l  
energy galactic cosmic rays 
in the process of their 
"external" modulation. The 
sa e proce s results in the 
considerable increase of 
higher energy particles. 
B. The unusual fr  the viewpoint of the "internal" modu-
lation the galactic cosmic ray phenomena take place during 
the periods of the inversion of the general magnetic field 
of the Sun ( MFS). 
In /11-13/ we subdivided the galactic cosmic ray beha-
viour during GMFS inversion into t o phenomena: 
I - Due to the su posed a tenuation of the interplanetar,y 
magnetic field strength the decrease of the galactic cos-
mic rJY modulation so much the greater (and the more pro-
longed) the greater the particle energy is. This explana-
tion of the "energetic hysteresis" is entirely in the sco-
pe of the "internal" modulation scheme. 
I - The phenomenon depending on the type of GMFS inversi-
on (characterized by the sign of the dM /dt, where M is 
the projection of the general magnetic field of the Sun ma-
gnetic dipole moment on the Sun rotation axis) delaying 
with respect to the first phenomenon by 1-2 years. We re-
late this delay to the location of the proce s responsible 
for the second phenomenon on the periphery of the he io~ ­
netosphere. 
Fig.2 shows the galactic cosmic ray behaviour a cor-
ding to the stratospheric data (~urmansk, Rc=0.5G ) during the periods of GMFS inversions in 1969-71 ( dMz/dt.> 0, a) 
484
SH-4.2-19
and 1980 (dMz/dt<O,b) mar-
_-4--STPATOSPHERE, R>O,5GV _. J ked by the t_ick section on
. _:_oF×P(Aq08_2) /_ _ t-axes. The periods of I andIT phenomena are shown as
a _r__tl well. A dashed lines indica-
3o te the galactic cosmic ray
intensity according to the
expression
'kf\ / f'"V' 'VlJ j=J6exP (_A. r_0.8 ' _-1.2),
25 _A _ I t-_ I' _ where _ and _ are the nt_-
_d \J bet of sunspot groups andtheir mea heliolatitude,re-
t------I ,I, ll-------I t spectively. This expression
u ! K I I I M I l/ is thought of as describing
_-)_ _970 Y[ARS due to the Sun alone (i.e.
"internal") and normal (i.e.
3o /o in the absence of the "ener-
getic hysteresis") galacticI\ ?i_ / cosmic ray modulation. It is
seen from Fig.2 that in the
25 r" initial stage of the inver-sion anomaly (the first phe-
nomenon) intensity quickly
increases for both types of
the inversion, this increase
persisting during the second
20 phenomenon in (dM_/dt > O)-in-
version, but changing into
_980 YEARS decrease in (dMz/dt _ O)-in-
FIGURE 2. version.
4. THE CONCLUSION. To understand the galactic cosmic ray
behaviour it is necessary to develope much more real model
of the heliomagnetosphere than used now.
REFERENC ES
I. Krainev M.B.(1981), Proc.17 ICRC, Paris, 3, 357
2. Krainev M.B.(1981), Proc.17 ICRC, Parls, S, 361
3. Ahluwalia H.S.,(1979),Proc.16 ICRC, Kyoto_ 12, 216
4. Krivoshapkin P.A. et al, (1981),Proc.17 ICRC,-_aris,_4,33
5. Kravtsov N.G. et aI,(T984), Izv.Akad.nauk SSSR, ser._iz.,
43, 2129
6. S_Impson J.A., (1983),in"6ompos.and Origin of Cosmic Rays"
7. Fisk L.A. et al,(1974),Astrophys.Journ.,190, L35
8. McKibben R.--_ al, (1983) .Proc. 18 ICRC,Bangalore, 3,63
9. Garcia-Munoz _ al, (1981),Proc.17 ICRC,Paris,3_.270
_). Svirzhevskaya A._'._ al_ (1985) ,Proc.this conf.,_H 4.4-18
11. Krainev M.B. et al,(_T9B_),Proc. 18 ICRC,Bangalore,_3,23
12. Krainev M.B. _, (1983),Proc.18 ICRC,Bangalore,_3,95
13. Krainev M.B. e_, (1984),Izv.Akad.nauk, ser.fiz. ,___3,2100
(in russ.)
30 
25 
"j" 
tI) 
"4 
I 
E 
84 
- STPATOSPHERE, R >0,5 GV 
-..... - J = Jo EXP (-A ~O,8 ~-j,2) 
a. 
(1 
I \ , 
I \ I 
.... -J V r 
Til 
\ ) 
'v 
I--1---11---
-4. -  
and 1980 (dM / t < 0, b) ar-
ked by the tfiick section on 
t-axes. The periods of I and 
II pheno ena are sho n as 
well. A dashed lines indica-
  l cti  ic  
i t sit  r i g t  t  
ressi n 
J=J6exP (-A.qO.8. 'f- 1• 2), 
U LL __ ~ ____ ~ __ -L __ ~ __ L ~ 
where q and )0 are the num-
ber of sunspot groups and 
t ir ea  li latit de,re-
spectively. This expression 
is thought of as escri i g 
      
al")  r al  
     er-
eti  steresis") l cti  
s i  r  odulation. t i  
 fro  i .  t t i  t  
initial stage of the inver-
i  al  (th  i t e-
no enon) i te sit  ic l  
s s  t    
 rsi ,   
ersisti g ri  t e second 
pheno enon i  ( z/dt  )-i -
ersi , but changing i t  
decrease in (dM / d t <: 0) -in-
version. 
t:') " 
30 
~ 
1\ , 
I \ I 
I \ I 
) \; 
 r.l' 
I 
20 
i980 YEARS 
G  . 
4. THE CONCLUSION. To understand the galactic cos ic ray 
haviour   cessary t  el e uc  or  l odel 
of t e helio agnetosphere t a  used no . 
 
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. rai ev .B.(1981), r c.  I , ari , ),  
3. hluwalia .S.,(1979),Proc.16 I , Kyoto~ 12, 216 
4. rivoshapkin P. . et al,(1981),Proc.17 ICRC7Paris,4,33 
5. Kravtsov N.G. et al,(1984),Izv.Akad.nauk SSSR,ser.1iz., 
43, 2129 
'SImpson J. .,(1983),in"6o pos.and rigin of os ic ays" 
is  . . t l,(1 ), strophys.Journ.,190,  
cKibben .B.et l,(19 ).Pr .1  I C,Bangalore,), ) 
arcia- unoz M. et al,(19 ), r c. 7 ICRC,Paris,3~270 
ir vskaya .K. et ~  f.,S  .4-18 
rainev .B. et al,(19SJ),Proc.18 I C,Bangalore,3,2) 
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. 
. 
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10. 
11. 
12. 
13. 
 s.  --


On the influence of the heliomagnetospheric periphery on the galactic cosmic rays

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