(SANITIZED)UNCLASSIFIED CZECH PAPER ENTITLED, " CONTRIBUTION TOWARDS SOLVING THE QUESTION OF THE OCCURRENCE OF CHROMOSPHERIC FLARES BEFORE GEOMAGNETIC STORMS"(SANITIZED)

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A CONTRiLJUTIN .\-)::ARJS L,OLVING HW22-210N OF THE OCCURRENCE OF.CHRO-
1:0Si;HERIU FLARES aE2ORE GEOMAGNETIC STORMS.
by Bohumila Bedndi'.ova-Novakova
Geophysical Institute,
Czecosl. Acad, Sci., Prague
ABSTP.!;.CT
The incorectness of the hypethesf-, according to which flares
should be the source of corpuscular solar radiation, which is
responsible for the origin of ge3,magnetic storms, is proved on the
basis of determining the number of geomagnetic storms not pre-
ceded by any flares. Using the list of guaranteed large flares
from the IGY of C.S. Warwick 114 and making an analyel..s of the
solar situations occuring simultaneously with flares but on the
CM 61' in the centre of the solar disc, it was shown why some fla-
res were followed by a geomagnetic storm while after others, on the
contrary, a period of absolute geomagnetic qtiet set in.
Since it was shown t1-.1at geoffgnetic storms are preceded by changes
in the magnetic fields- in the solar chromosphere and because flares ,
also occur during such changes, the question arises, what role
do flares play here? Are they the cause of such changes or are
they their pLoduct ? It is deduced, and observations confirm this,
hat olthough flares are prouced as a sort of consee_nc_ of
nges in the photospheric :fie:L:3, they can simultaneous l,; be
resrded to a certain as the cause of substantial cnanges
in the chroLosphere which. lead to annulling of the field at
least in that component ',hich is rel.,:esented by chromospheric
structure and filaments. Their relationship to geophysical effects
of a solar corpuscular origin is,.holwver, quite int4rect and
very limited.
The fact that after the first historically recorded observation of
a flare on September 1, 1859, by Carrinton and Hodson and also after
the two consecutive flares on August 3 LI,t 5, 1872, which were observed
by Young 1 a strong geomagnetic storm always followed., led to the hy-
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2
pothesis of a connection between flares and geomagnetic storms. This
'hypothesis was also supported by the classical observations of G.E.
Hale, carried out from 1892, using the new instruments developed by
him : a spectroheliograph and later by means of a spectrohelioscope.
After the discovery of the radotelescope and after it was found by
means of it that in the period vhen a:flare occurs on the Sunlradiation
is sometimes magnified on some %:a%!e-lenths (much longer than the opti-
cal), it was hoped that this meant an indicator of an effusion of cor-
puscular radiation had been found, i.e. such radiation which is respon-
sible for the origin of geomagnetic disturbances. It was only later
that it was discovered that not even this fact can be used for exam-
ple for prognoses etc.
From the hypothesis on the connection between flares and geomagnetic
storms the opinion gradually civeloped that flares were the direct sourCe
of geoactive corpuscular radiation. However, flares in themselves are not
-
high formations land than th:::; are observed on the edge of the solar
disc, they do not exhibit any :asrked rise of matter to any great height[1.
They are often accompanied by rising prominences which, as will be seen
later, may be conceived as the consequence of changes in the local mag-
netic field which occur often vihout flares and sotimes during a flare.
It is this random simultaneity of the two effects which is the cause
of frequent mistakes so that tare are some authors who speak of fla-
res but obviously have in mind rising prominences. That the are two
quite different effects, whi:2 probably have no direct physical
inter-relationship, is borne o..rt by the fact that disappearing filaments-
rising prominences occurs-.4---4,si:7.:-.z.-a::-.--:.`4,c-xzzdx-ct&arttmz.x-i-EizzazaccidE
very often in absence of flares. It seems that the two phenomena are
likely the consequences of one and the same cause. Sometimes they
occur simultaneously and other times only one of them appears.
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Flares occur alnost universally
ly one part of a complex of events
ther or at absolutely the same time.
either a shorter or a ler inturval
ction with the different effects separately. This is even more difficult
with geomagnetic storms which eibit a longer time lag after Sudden chan-
ges occurring on the Sun. If, hc:?ver, the mechanism of the effusion of
corpuscular radiation and its pL-cpagation towards the Earth is to be found,
it must first be determined wheter such a phenomenon can be found among
the known expressions of solar ztivity which, in each period and during the
whole cycle of solar activity, would be reliable indieator of geomagnetic.,
storms. It is also necessary tfJ Ove physical reasons for each connection
found. One must also take into consideration an explanation of the fact
that sometimes no connection was; found. As is clear from the many papers
already published, it was found jn the Geophysical Institute of the Cze-
choslovak Academy of Sciences tl,t-of all the known expressions of solar
activity studied. by optical meds the best indicators of the origin of
geomagnetic storms are filamentz. and the fine chromospheric structure under
certain circumstances. As will seen below, in the period of greater
solar activity, i.e. in the pericd of flare occurence, these are erup-
tive and disappearing filaments, denoted in the Geophysical Institute by the
nne term - unstable zz filaments - which, only if they are in a suitable posi
tion, safely indicate when a geomagnetic storm with sac will occur 1-3]..
This is because such phenomena, as will be seen later, provide direct
information on changes in the mEp:netic field of the Sun. And it is then
only these changes which are actually the direct indicators of changes in the
corona and thus also of the origin of geomagnetic storms.
Doubts as to flares being the source of corpuscular radiation were
in active centres and are thus on-
which occur shortly after one ano-
From the consequences occurring after
it is impossible to deduce a conne-
raised by D.Van Sabben 4 1 R.P.abson
1
5 and O.M. BarsukovF6j . The sta-
1
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A
tistical paper by C.S. Werwick and R.T. Haneen,7 :shows the not very high.*
xima of the Ap?indices after flares in the period of greater solar activity
for flares nearer to the CM but does not give positive results for the
period before the minimum. It cen easily be supposed, and later this wili.
be quite 'clearly proved, that the circumstance can regarded as merely a
statistical phenomen,
?-?
'?
the more elements contained
two of them are found which
in a certain time interval.
also clear from the table given in [83
by tez. two series compared, the more frequently
are her simultaneous or follow one another
The etfect is
the same although one series is
much more numerous thin the oth,.1 as is the casewhen the number of
fl3res greatly exceeds, particully in periods of greater activity, the
number of geomacnetic storms. It 7:s seen from Tab. I. and even better
from ig.1 that a decrease in ti:e number of flares after the maximum
(1959-60) is followed not by deci.cese but by an increase in the number of
geomagnetic storms whether flare: of greater importance or whether alkxsia
all, including those with the stz.alest importance, are used for the comm
parison. No connection can be obEe:-ved even if one takes the number of ssc
or the greatest storms which , according to accepted world opinion, Should
be connected with flares but which, as will be sect later, indicate no pro?
nouced connection.
Table I Comnarison between nur::bea of
flares and number
of geomagnetic
ag. o
SSC
5+
storms.
Imp.
Yetr
3,3+
2
1
2
total
1?
all
1957,2ndhalf
23
203
228
5189
27
17
1958
24
327
351
9668
42
24
1959
30
259
2208
91C
269
5587
50
22
1960
19
118
1490
541
137
2168
72
32
1961
10
:58
787
294.
48
1129
35
17
.`q's
The results in the paper oyylaier;La 9 7, _\ also give rise to doubts
L
as to the direct connection between chromospheric flares and geomagnetic storms,
4
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Flares Flares
400- 10000
200
1958
Storms
771S
/ .1/41 -
5000
1961
ssc
30-
20
10
/7-
6 -8 that an unstable filament was necesbary in order that a .geomegmetic
storm might occur; the -presence of a flare was not docioive. Ifia filament
was not present a decrease occurred in the Ap-indicoo aftet nem.
In Fig. 8 d the maxima are not pronounced and aro dioplaced OD a conse-
quence of the uncorresponding and displaced pcocagoo of unstable filaments.
In the case of Fig. 8 b the decrease is caused by the CIP a the active
:J
centre which does not vary very much. It is coon from all this that florec,-)
cannot be directly connected with the occurrence of geomagnetic otortilo. The j
slight trace of connection, based on the foot that there is a lorger:number-)
of flares before the commencement of a storm than after it, nay bt=1
the consequence only of on diroctiz71 connsotion with which 170 shall deal
in the analysis of the results.
J
-
,??,?
? ? .?-?
1
C
,!
.\' )
-,)
9
3L
? ,... - ?
--;;?-41
" (
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Recapitulation end analysis of result
It must be borne in mind that 1) a direct connection between flares
-eama3-netic storms is disputable if it is considered that is obtained in o
ly 50 % of the cases ,2:5,3; 2) if geomagnetic storms exist in periods w
:'*Iares do not occur, a direct connection must be considered deubtful
ai in no case did flares prove suitable as an indicator of geomagnetic
atoaa: in p. ,;noses 4) statistical papers dealing with the connection
:etween flares and geomagnetic storms and giving results based on the aver
aaluea of Ap-indices, exhibit low and unpronounced maxima N9]. This
t in taelf raises doubts as to the hypothesis on the direct connection
r
aa;een geoaaanetic ctorms and flares 1.11 . 5) The fact that in the. period
laafaae and after minimum no conaection between flares and geomagnetic storm
a
obaiaed L7 is a confirmaticn of the incorrectness of the flare hypothe
.. 6) Not the slightest connectIon between the importance of a flare and
the occurrence of a geomagnetic storm was obtained in any convincing mannur.
:hofe are many large geomagnetic storms preceded only by the weakest flare.
at - oak this there are also the results of the present paper whe
torial from 30 .V.1. 1957 to the Ind of 1962 was used. It was fo that.7
there
exist high percentages of the number of geomagnetic atoms before while
? a,
act a irie flare was observed even in relatively long interyals (up to
aaaee days before). The percentaaas decrease if the chosen interval is ion-
and flares are taken int) consideration, and increase with a 4ecreo
ia aae amber of flares (they alao depend on li0Xations as .gar4t dicta
from Cli and importance and on the period of the ileve*.yea cycle).
is thus alear that we have to with only a statistical effect. The li5
naabar of elements being compared, the more frequently it happens that
fall simultaneously into the chosen time interval and pis is even :wr
4aaae1y if a longer interval is chosen. When there is a large number of flare
cOCE Tab. I. Fig 1 ) it is more likely that one will occur by chance In the
of three days before a geomagtistic storm beyond the maximum than
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beyond or before the minimum, when the number of flares disproportionate-
ly falls, while the number of geomagnetic storms decreases much less. This
fact was proved for all geomagnetic storms : from Kpmax - 5+, and flub lar-
ge storms: Kpmax cr- 7+ and Kpmin 5-, and els? for alltescpIr.the percen-
tages of sudden commencements without a flare are compared with other storms
the latter are somewhat lower although they are etill large, 8) The apparent
connection between flares and geomagnetic storms can beexplained by the apple
multaneous occurrence of other effects on the CM and possIbly directly in the'
centre of of the solar disc, as has been shown earlier L.21.1, [8 1?
.The somewhaAlarger,number of flares occurrAnk before geomagnet4c
storms compared with that following after the commencement of a storm
cates a slight connection, although this is limited compered wit& the high
percentages of storm occurrance without.a flare.This is
found from the observations: that during a flare there
greatek probability of the occurrence of a geomagnetic
just what can be
is sometimes a %AP
46.
storm althagh at 10004
other times this is not true at all./t seems that not a2Waya but only sometilv
,
ties do flares have the tendency to precede the ocourrence of a geomagnetic vii4
storm. And this is just what, as a consequence of point 8), is the cause ?
of AO rise in Ap-indices after a flare. Site indirect connection can be
*
explained by the presence of other affects. These are pr ily?unitable file
,
ments ; their change from filaments of other types shows th&t not even
here is there a simple connectionrbut that a profounder significance must be
a;3cribed to this circumstance. This means a completely new Aew of the re-
lations between solar and geomagnetic activIty: flares occur moitly in4ctilzole
ve centres. In such places "re are strong magnetic fieldelwhich are ma.41.;'
fest, although with smaller intensity, also in the chromosplire'and in he
corona. The way in thich such fields are distributed-in the space above
*
act iv centres is designed b! the chromoapheric structure and the shapes
of th'e fil4ments-prominences. When changes occur in the local magnetic field
wr
a change takes place in the chromospheric and coronal strictures and this
Si
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?
can be studied with great certainty on hydrogen masses above the active
centre and its neighbourhood. Under certain conditions the filaments and chroi
mospheric structure disapear altogether. It can be deduced from this that in !
such cases changes occurred in the given layers which had the rosult that,
the field was " disappear " there. This apparently, primarily concerns one ofi
^
its components.It can occutsuddenly or gradually, temporari4 or permanently.
During such changes flares often, though not always, occur. Since the "diSep- ,
pearance" of the loCal magnetic field in the centre of the claw disc - under
certain conditions also outeide the centre but on tho CU - 0=70 moan l tic
advent of a geomagnetic storm 2i1 , ri?J ,1IR5.1 flares are also classified'
among processes which occur around the same time as the commencement of the
0
geoamgnetic storm appears on the Sun.
The question remains, what is important from the point of view of
theoretical opinion as well as for practical use: are flares the cause of
changes in local magnetic fields or their consequence ? TO8 will certainly
be the subject of discussion for a long time to come, until the very nature '
of flares is known. A flare as the cause of a disturbance of magnetic field
in the chromosphere is also considered by M.A. Eliison [S] . Perhaps this:
question could be answered by the conception of a combination of magnetir,
and electric conditions in the eater solar layers.
1
It is also necessary to xplain some facts which, if incorrectly
interpreted, might lead to controYersies. This is primarily the question
of changes and the possible annullfLng of chromospheric fields. These occur ',-
sometimes during a flare and at other times simply without it. Flares occur
in the majority of cases above active centres with a complex structure of
magnetic fields. It can be expected that a very effective interference will
be required to annul chromospheric fields which in this case have conside-
rable intensity. And it is during s flare koften rega4esa of the importance)"
that the disappearence of chromospheric structure and filaments can be obser-
ved in dif*.ent places. On the other hand, if the fields com are verg 'weak.
,,...m?.?????Ir??? -??? -.??????10111+,1.
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such as those distributed above facular Brew) without sunspots a quite erne
change is enough to bring about such an effect. In such cases quite insi-
gnificant flares are usually present in the active regionotor its auniount-
dings or flares do not occur there at all.
It is certain, of course, that sometimes, after .pertain time
after a 416e, the chromospheri: structure is restored to what it was be
and the filaments also appear 03 though they had not disappeared at all.
441
This happens if it id\a region above strong photospheric fields. As soop a
after a flare in the outer layeTs above the active centre is renewed th
normal state, i.e. the state they had before, than the hydrogen masses;
pertly still unionized and partly already recombined, begin to rewind%
around the lines Of force of the still,existing magnetic field reaching
here from the photosphere. Tis could explain the cpronal origin of pro-
minences considered by K.O. Kiepenheuer [251
Another objection to considering flares as the cause of changes i
netic fields might be the fact .at the changes in local magnetic fields
actually occur before the flares. But , according to our own subjective
impressions obtained duripg observations, the changes before flares are
of a different kind to Uwe() observed immediately after them. Befoie.a
flare there is an 'increase in intensity and extent of the\field which
becomes more and more complicated. Then surges and mall filaments are
produced. These a
henomena of short duration. It depends on the aspect
from which we explain the process leading to the annulling of the field.
In any case, boweyer, we must admittat we have here the conditions for t
superposition of fields and their temporary compensation, wIlich is manifes
differently in different places. These are changes appearing rather as
. isolated cases. While large and 'extensive changes occur only during the ,1216
mk
re and after it. If an active centre is observed1just after a flare, it can
be said that a considerable and very striking simplification of the chro-
mospheric structure has taken place and sometimes it completely disappe
over large areas. Anyone who deals with the observation and study Jr fine
p.
11.
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chromospheric structure and filaments can find this difference himself an
there are certainly many who have already observed it.
However , there should be no misunderstanding. The question of
whether a flare is the cause or consequence of changes in magnetic fields
in the chromosphere cannot for the time being be decided even by the argu,
ments given here. It should also be borne in mind that, whatever the ca-
se, one cannot in any case speak of a direct and universal connection betT!:
ween flares and geomagnetic storms. This might be permissible perhaps
only in very limited cases when annulling of the fields occurred in the
active centre just in the centre of the solar disc or under certain con-
ditions on thAFM and when flares also occurred just in this centre. But
even then the connection would be indirect. The actual and nearest indi-
cators of this fact are always unstable filaments. This can be explained
by means of the known relation between filaments and coronal formations
extending above them. As has already been shown [3] a geomagnetic storm
occurs when some coronal formation is directed towatd the Earth. Tne dens.1
of the
ty of the coronal plasma, in other words the densifiluscular streams
is apparently directly related to the magnitude of the geomagnetic storm
and vice versa. A filament and the chromosphere obviously contribute IV
their masses so that after their ionization, which occurs in certaill
layers of the corona - apparem:y layers at heights to, which the rising
minences reach - the coronal plz.sma becomes denser. As was tobe 404eCteae
perhaps, there definitely exis.; no simple relation between the size of
,
a filament and the magnitude of a geomagnetic storm. This is natural since
f
the main question here is to whet percentage the atoms were ionized. It
is not impossible, however, that the necessary parameters could be de rmin
A
ned by a detailed study, e.g. by determining the amount of ma es which
4
returned to the chromospere etc.
On the basis of the above considerations and tbole series of working,
hypotheses and using the results. of observations , a new method of fore--
,JI ,
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casting geomagnetic activity, disturbances and quiet, was elaborated
Its successful try-out in practice proves the correctness both ff the 1
'
method itself and of the corresponding hypotheses. In order to e aje v
to forecast every geomagnetic storm with maximum accuracy, a correct and
continuous obdivations of the Sun is required. Only in this way is it
possible to record allisudden and of short duration phenomena whach pre-
cede the occurrence of geomagnetic storms. And only in this wa4 will it
6]?
be possible to forecast each period of absolute geomagnetic quiet which fo-
and alao 6bave whic
lows after the CV of an active centre in ch netic field was
not annulled.
Table III. The connection between flargs and agile spier 00 Avoaxpical
2-21hencnUAJULIUlttLAIELI122?E.O.211i.-91LakAdULUMILL
a) Immediate results :
, r
1) disappearing filaments exist also
rising prominences without flares
no dependent
directly on
importance
of flare
' 4.
limited
indirect
connection
2) ,SFE
?
exist only
with flare
dependent
directly on
importance of
flare
posdible
direct
connection
3) Dellinger effect
, exist only
with flare
dependent
directly on
impottance of
flare
.poslible
direct
connection
b) Later results:
4) geomagnetic storms
4.4141?41.111.1.44.4.44..41=414o.
exist also
without flares
(high percen-
tage well abo-
ve 50%)
not all flares
are followed
by geomagnetic
storms (50%)
not directly limited
dependent on it indirect
importance connection"
of flare
_
5) polar aurorae are accompanying phenomenon of geomagnetic storms and the
same holds for them as for storms.
? ? . ?
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To 'hum ap, it must be explained what form tilt, connection batmeek
flares and some solar and geophisical effects, has judgilk by' what
we have had the opportunity to observe. The analysis it gilen in Taballoil
according to which the SFJ and Dellinger effect begin immegiately after 0
a flare, depend on the magnitude of its importance and are thus di- tt
rectly related to it. Meanwhile, however , the disappearing filamentr,
-rising prominences, despite the fact that they oocur near to the flare
0
in time - and often absolutely simultaneously [p] areptlike the
4
effects occuring after it in a longer time interval, i..$ geomagnetic '4'
storms and polar aurorae, indirectly related to the flare. In order
to supplement Tab.Ill the connection between flares and radio out-
bursts will have to be verified in a radical manner. According to the
work of J. Halenka ipa] 1-one could deduce a certain dependence on
the presence of a fialemnt.
?
-'1??????"""---* '."4"111114 It qa?
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References.
[1] J.W. Warwick: Hights of Solar Flares, Ap.J. 121, 1955, 576.?.384.
[2] C.S. Warwick : Flare HightQand AssoCiation with sne S,Ap.J.'121, 1955,
385-390.
12] B. Bednaicovii-Novakovil: Connection between Geomagnetic Storms in IGY and
IGC and Occurence of some Kinds of Filaments, Studia geoph.et geod. 51
1961, 138-163.
C4TID.Van Sabben: Solar Flare-Effects and Magnetic Stoma. J.Atm. Torr. Phys.
3, 1952, 270
D:\ R. A:Watson: Magnetic Activity following a Solar Flaro. J.Atm. Terre
Phys. 11, 19571 59-61.
[610.11. Barsukov reomarnnTan OVIXIKTHBHOCTb xpomoccpcmax BCPIEMOR no
maTepilazam 1957r.8u1letin.of the Academy of Sci.,U.S.S.R.e Geophysical
Series, 1959, No. 11, 1690-169).
..7] U.S. Waraick and R.T. Hansen: Geomagnetic Activity following Large Flares.
J.Atm. Tem Phys. 14, 1959, 287...295.
,
[z:$] B. Bednatova-Novekovd: Analysis of Solar Situations During Flares and
Geomagnetic Activity Afterwards, Travaux de l'Inst. geoph. de 1/Acad.
Tchocosl. des Sci, No.191, GeofysikAlni Sbornik 1963, NCSAV, Praha, 39940r
[91J9
. Halenka: The connection between chromospheric Flares and Geomagnetic
Activity in the IGY, Studia geoph. et,geod. 4, 1960, 361-377.
[10] J. Halenka : Geomagnetic Activity after Large 8hromospheric Flares, Studia
, geoph. et geod. 5, 1961, 237-255.
[11 J. Halenka : 'On the Character of the Connection between Geomagnetic Acti-
vity and Chromospheric Flares. Studia geoph. et geod. 8, 1964 (in prcos)
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18
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ar?
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?
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