THE PHYSICS OF SOLAR CORPUSCULAR STREAMS AND THEIR INFLUENCE ON THE UPPER ATMOSPHERE OF THE EARTH

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP81-01043R004500220001-3
• Release Decision: RIPPUB
• Original Classification: K
• Document Page Count: 73
• Document Creation Date: December 23, 2016
• Document Release Date: May 30, 2014
• Sequence Number: 1
• Publication Date: January 1, 1957
• Content Type: REPORT

a
1
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
THE PHYSICS OF SOLAR CORPUSCULAR STREAMS
AND THEIR INFLUENCE ON
THE UPPER ATMOSPHERE
OF THE EARTH
Fizika solnechnykh korpuskuliarnykh
potokav i ikh vozdeistvie na
verkhniuiu atmosferu Zemli
Moscow, Izdatel'stvo Akademii Nauk SSSR 1957,.
PP. 8-39, 40-50, 69-86, 2144-158, 167-181, 1=968.
Selected articles translated
by John Miller and Judith Danner
for
STAT
Geophysics Research Directorate, AF Cambridge Research
Center, Cambridge, Mass., by the American Meteorological
Society, Contract number 19(60U-1_936
T-RC-13 4
STAT
STAT
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
E. R. Mustel'
A. B. Severnyi
E. A. Ponomarev
A. P. Nikol'skii
A. I. 01'
S. I. Isaev
E. I. Mogile-:skii
TABLE OF CONTENTS
Discussion of the possible sources of
geoactive corpuscles in the solar en-
velope
(Obsuzhdenie vozmozhnykh istochnikov
geoaktivnykh korpuskul v obolochke
saints a)
Spectroscopic investigation of cor-
puscular ejections on the sun
(Spektroskopicheskoe issleduvanie
korpuskuliarnykh vybrosov na Solntse)
Solar corpuscular radiation and the
topology of the magnetic field in the
solar corona
(Korpuskuliarnoe izluchenie solntsa
i topologiia magnitnogo polia v
solnechnoi korone)
Discussions on the lectures of F. R.
Mustel', A. B. Severnyi, S. K. Vse-
khsviatskii et al., C. M. Nikol'skii
and E. A. Ponomarev
Magnetic disturbances in the region
near the Pole and the existence of
a second zone of their increased in-
tensity
(Magnitnye vozmushcheniia v okolo-
poliusnoi oblasti i sushchestvovanie
vtoroi zony ikh povyshennoi inten-
sivnosti)
The connection between solar ac-
tivity and geomagnetic disturbances
(0 sviazi mezhdu solnechnoi aktiv-
nost'iu i geomagnitnymi vozmushcheni-
iami)
1
57
73
81
94
112
Discussions on the lectures by O. A.
Durdo and A. I. 01' 121
Hydrogan radiation in the spectrum
of polar aurorae
(0 vodorodnom izluchenii v spektre
poliamykh siianii)
The equation of quaststationary
ionization equilibrium in the F2
region and solar corpuscular radiation
(Uravnenie kvasistatsionarnogo ioni-
zatsionnogo ravnovesiia v oblasti F2
i korpuskuliarnoe izluchenie solntsa)
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
126
130
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
DISCUSSION OF THE POSSIBLE SOURCES OF GEOACTIVE CORPUSCLES
IN THE SOLAR ENVELOPE
by
E. R. Mustell
1. METHODS OF STUDYING CORPUSCULAR STREAMS
Undoubtedly, the most important problem in the study of corpuscular
streams is the localization of the sources of corpuscles in the solar enve-
lope. This is a very important problem because the methods of predicting
the invasion of the earth's atmosphere (its upper layers) by solar corpuscles
somehow must derive from the known sources of ejection of solar material.
Various methods can be used to determine the source of corpuscles in the solar
envelope:
1) comparison of the different formations and phenomena in the solar en-
velope with geomagnetic and ionospheric disturbances, amplifications and
attenuations of the intensity of cosmic rays and other effects on the earth;
2) attempts at direct spectroscopic *detection of corpuscular streams en
route from the sun to the earth;
3) study of the possible mechanisms of ejection of atoms from the sun and
their further study.
In practice, one must combine these methods and add others to solve the
problem. Before proceeding to a direct discussion of the whole problem, we
will mace some remarks about the above methods.
When using the first method, the method of comparison, we must first turn
to the directly observable formations in the solar envelope. Only when there
are no details visible on the sun which could be considered the source
0I
various effects on earth (geomagnetic disturbances, etc.), should different
hypotheses be introduced on the nature of corresponding regions in the solar
Declassified in Part - Sanitized Copy Approved for Release ? 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
envelope not marked by directly observable formations. Such ',hypothetical"
regions include, in particular, Bartels' Ni-regions, which are frequently
cited in discussions of this problem.
The spectroscopic methods of detecting and studying corpuscular streams,
which will be considered in other papers at this conference, are very impor-
tant and interesting; they are usually based on the assumption that the
optical thickness of corpuscular streams along the line of sight, for certain
spectral lines, can be either comparable to unity or not much less than unityc
Thus, the corpuscular stream can form its absorption line shifted from
the normal position (due to the movement of atoms from the sun). When super-
imposed on its corresponding ordinary absorption line in the solar spectrum,
this line must cause a certain asymmetry in the ordinary line. There are
reasons for assuming that if this effect actually does exist, it should be
observed first of all in the most intense lines of the solar spectrum, in the
H and K lines of Ca+ and in the first lines of the Balmer series of hydrogen,
especially in line Ha with the wavelength A ag 6563 2.
Above, we said that the stream can form its own absorption line. How-
ever, this does not exclude the possibility that, due to very peculiar, ano-
malous conditions of the excitation of atoms in the streaqvamission effects
will predominate over absorption effects. In this case, the stream will form
an emission line rather than an absorption line, then the asymmetry effect on
the basic absorption line of the solar spectrum will be opposite in sign to
the effect which would be observed were absorption to predominate.
Unfortunately, thus far attempts to ddtect the effects of absorption from
corpuscular streams have not led to unambiguous and indisputable results. In
any case, the asymmetry effect lies at the threshold of accuracy of contempo-
rary photographic and photoelectric observations and, thus, a great deal of
work is required in this area. A. B. Severnyi, at the Crimean Astrophysical
;.
Declassified in Part - Sanitized Copy Approved for Release
?
?3-.
Observatory of the Academy of Sciences, obtained very interesting results on
the asymmetry effects due to the additional emission of atoms in corpuscular
streams, and will pres/ent them in his paper.
One should note the intrinsic fault of the above method. When this
method is used, it is extremely difficult to determine the final direction of
the streams coming from the sun, since the ionized calcium and hydrogen atoms
should be ionized rather quickly in coming from the sun, whereupon the ab-
sorption processes in the corresponding line cease. In other words, these
effects should be substantial in the immediate vicinity of the sun's surface.
Further, study of the different solar phenomena shows that there are certain
factors (no doubt of an electromagnetic nature) which can deflect the streams
in various directions from their
Sun
a
initial direction. In this connection, the
effects of asymmetry in ab-
sorption give us an idea only
of the localization of atoms
in the streams near the sun's
surface, but do not give an
accurate indication of the
direction of ejection of these
atoms. Figure 1 illustrates
this. In the first case, the
the direction of the atoms
by the letter B, in the second
to ea;th
Figure 1. An explanatory drawing of the ab-
sorption and emission effects from corpus-
cular streams.
ejected from
+
the active region AA is indicated
case by C. These atoms can create possible absorption activity only to dis-
tances delineated by line aa. Therefore, we cannot determine the final direc-
tion of the ejected atoms. The same applies to emission effects, The inten-
1r)
Generally, however, this zone should differ somewhat for the H and K lines
and the lines of the Balmer series.
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
14,
Declassified in Part - Sanitized Copy Approved for Release
sity of these effects (besides the other factors) should be determined by the
density of the matter in the stream, which decreases with distance.
We would be able to make considerable progress if a systematic study could
be made of the asymmetry effects in the far 'ultraviolet lines La, Lp At*e
of the Lyman series of hydrogen. These lines start from the ground
levels of the hydkogen atom and, due to the extremely high hydrogen content
of the solar envelope, mist be exceptionally strong; therefore, it is quite
possible that the effect of ionization in the given case may prove to be sub-
stantial at far greater distances from the sun than is the case for the H and
K lines and the lines of the Balmer series. This zone is indicated by the
line bb in figure 1.
However, even here there are difficulties. First, the lines of the Iiyman
series can be studied only by using high altitude rockets. Second, only in-
tegral solar radiation is recorded by contemporary rockets, i.e the radiation
of the entire solar disk. Further, as follows from figure 1, in studying the
direction of the streams we must investigate the effects of asymmetry in lines
at different points of the solar disk. In other words, only a study of the
displacement of the effective center of the "corpuscular" line of absorption
(or the emission line) on the disk can give an indication of the direction of
the stream. These same things must be considered when one studies the possibi-
lity of radio emission from corpuscular streams. Since the density of the
matter decreases with distance from the sun, probably even in this case we
would get information on the movement of atoms only in the immediate vicinity
of the sun.
We will comment briefly here on the mechanisms of corpuscular ejection
from the sun. It is quite evident that in working out the mechanism of the
flaw of matter from the sun, we should begin our study by establishing the
forces that cause this flux. Furthermore, the regularity of this mechanism
5
er
A
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
must be checked constantly on the basis of regularities in the effects of
these streams on the earth, such as the 27-day recurrence of geomagnetic dis-
turbances, seasonal regularities in geomagnetic activity, etc.
Keeping these general remarks in mind and since the study should begin
with the various directly observable forms of solar activity, we will discuss
the various formations on the sun's surface, examining them as possible sources
of solar geoeffective corpuscles. We will start with sunspots.
2. SUNSPOTS
Sunspots were discovered much earlier than the other active formations
on the sun. They are the most conspicuous and easily observed details of the
sunls surface. This is why the comparison of geophysical manifestations of
solar activity and solar phenomena began with sunspots. Very abundant data
have already been gathered on comparisons of this kind, from which it follows,
apparently, that sunspots are not an important source of corpuscular emission
and That the "geoeffectiveness" of sunspots "discovered" by various authors is
not due to these spots but to other forms of solar activity closely related
to sunspots. Among these forms are faculae, flocculi and chromospheric flares,
about which something will be said later.
However, for the sake of clarity we will formulate the present state of
the question. Even in 1929, when making a comparison of sunspots and geomag-
netic disturbances, the Greenwich astronomers, Greys and Newton, found (see
pp. 188-190) that the number of spots in the central Dart of the solar
disk at the moment a magnetic storm begins is greater than the number of spots
on magnetically calm days, and this increase becomes conspicuous beginning
with quite intense storms and is most sharply expressed in the case of very
large storms. This conclusion was confirmed in 1948 by Newton C2.7 on the
basis of more complete data. We give his graph here (figure 2). The days,
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
sity of these effects (besides the other factors) should be determined by the
density of the matter in the stream, which decreases with distance.
We would be able to make considerable progress if a systematic study could
be made of the asymmetry effects in the far *ultraviolet lines La, Lp 00e
of the Lyman series of hydrogen. These lines start from the ground
levels of the hydilogen atom and, due to the extremely high hydrogen content
of the solar envelope, must be exceptionally strong; therefore, it is quite
possible that the effect of ionization in the given case may prove to be sub-
stantial at far greater distances from the sun than is the case for the H and
K lines and the lines of the Balmer series. This zone is indicated by the
line bb in figure 1.
However, even here there are difficulties. First, the lines of the Iiyman
series can be studied only by using high altitude rockets. Second, only in-
tegral solar radiation is recorded by contemporary rockets, i.e. the radiation
of the entire solar disk. Further, as follows from figure 1, in studying the
direction of the streams we must investigate the effects of asymmetry in lines
at different points of the solar disk. In other words, only a study of the
displacement of the effective center of the "corpuscular" line of absorption
(or the emission line) on the disk can give an indication of the direction of
the stream. These same things must be considered when one studies the possibi-
lity of radio emission from corpuscular streams. Since the density of the
matter decreases with distance from the sun, probably even in this case we
would get information on the movement of atoms only in the immediate vicinity
of the sun.
We will comment briefly here on the mechanisms of corpuscular ejection
from the sun. It is quite evident that in working out the mechanism of the
flaw of matter from the sun, we should begin our study by establishing the
forces that cause this flux. Furthermore, the regularity of this mechanism
5
I.
must be checked constantly on the basis of regularities in the effects of
these streams on the earth, such as the 27-day recurrence of geomagnetic dis-
turbances, seasonal regularities in geomagnetic activity, etc.
Keeping these general remarks in mind and since the study should begin
with the various directly observable forms of solar activity, we will discuss
the various formations on the sun's surfacej examining them as possible sources
of solar geoeffactive corpuscles. We will start with sunspots.
2. SUNSPOTS
Sunspots were discovered much earlier than the other active formations
on the sun. They are the most conspicumis and easily observed details of the
sunis surface. This is why the comparison of geophysical manifestations of
solar activity and solar phenomena began with sunspots. Very abundant data
have already been gathered on comparisons of this kind, from which it follows,
apparently, that sunspots are not an important source of corpuscular emission
and that the "geoeffectiveness" of sunspots "discovered" by various authors is
not due to these spots but to other forms of solar activity closely related
to sunspots. Among these forms are faculae, flocculi and chromospheric flares,
about which something will be said later.
However, for the sake of clarity we will formulate the present state of
the question. Even in 1929, when making a comparison of sunspots and geomag-
netic disturbances, the Greenwich astronomers, Greys and Newton, found (see
17, pp. 188-190) that the number of spots in the central part of the solar
disk at the moment a magnetic storm begins is greater than the number of spots
on magnetically calm days, and this increase becomes conspicuous beginning
with quite intense storms and is most sharply expressed in the case of very
large storms. This conclusion was confirmed in 1948 by Newton r2.7 on the
basis of more complete data. We give his graph here (figure 2). The days,
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
such places places and seem darker by contrast.
The author surmises that
faculae or calcium flocculi
(which are the same from the
point of view of the position
of the active region on the
solar disk) are one of the chief
sources of geoeffective solar
+1
corpuscles. In 1942, the au-
thor DJ discovered that the
passage of each facular field
across the visible center of the
solar disk is accompanied, after
a fixed time interval (several
days), by geomagnetic disturb..
ances of various intensities.
This finding was verified in
1942-1945 by the data of the So-
lar Service of the P. K. Shtern-
berg State Institute of Astron-
++)
omy and then by the data of
the Meudon synoptic charts for
this same period. Furtc7roreA
the comparisons were checked a-
gainst the data of MAudon syn-
optic charts for 1929-1935.
??1
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Figure 5.
Hydrogen and calcium flocculi.
;7 -This agrees, in particular, with the fact that floccular fields are usually
relatively stable formations (as opposed to spots) for many rotations of the
sun.
++)
Sluzhba Solntsa Gosudarstvennogo atronomicheskogo instituta imolai P. K.
Shternberga.
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
11
Further, in 1951-1954 a continuous check on this finding was made by the
Solar Service of the Crimean Astrophysical Observatory of the Academy of
+)
Sciences of the U.S.S.R. This is a particularly important period, because
for it we have photographs of the calcium flocculi for every day of the summer
and nearly every day of the year. The material was provided by the above
mentioned services and those of the other observatories of the, U.S.S.R.
Figure 6. The radiality of corpuscular streams from flocculi.
All these comparisons confirmed our finding. From the geometrical point
of view, this means that the corpuscles travel radially from the calcium floc-
culi, which is easy to understand from figure 6 where is the solar equator.
The shaded areas A, B, C are flocculi which are moving across the central
meridian of the sun POP due to the sun's rotation; PP is the axis of rotation
of the sun. Flocculus B is traveling across the visible center of the solar
disk. If the corpuscles actually travel radially, the streams from flocculi
A and C will bypass the earth and the stream from flocculus B will approach
the earth sometime after the flocculus crosses the central meridian, after
whi-h 4-11 c.n.r.th
yr1 1 1 'he.
nsde htiit sream. However, it should be stipulated
that radial streams from the sun cannot cause a large part of the geomagnetic
disturbances in all years of the 11-year cycle of solar activity. We know
that the mean latitude of different formations on the sun changes with the
Sluzhba Soin
tsa Krymskoi astrofizicheskoi observatorii Akademii Nauk SSSR
9114/m
Declassified in Part - Sanitized Copy Approved for Release ? 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Figure 9.
Chromospheric flare of 26 June 1952.
L. CHROMOSPHERIC FLARES
The name chromospheric flare is usually given to the very rapid (sometimes
almost sudden) increase in the brightness of individual sectors of the sun's
surface, which is observed most frequently in he lines of the Balmer series
anu in the H and K lines of ionized calcium but which also appears frequently
in some other lines of the solar spectrum. Chromospheric flares are only
rarely observed in total light and not in lines, and then for only a short
time. Usually a chromospheric flare appears as a sharp intensification of
light in some part of an existing bright flare. Chromospheric flares are also
closely related to sunspots.
Figure 9 shows photographs
of one of the flares taken at
the Crimean As Ob-
servatory L.11.77 in the light
of line H. Figure 10 shows a
photograph of a large chromo-
spheric flare taken by d'Azam-
buja at Naudon on 2i5 July 1946.
The appearance of a quite
intense chromospheric flare on
the sun is accompanied by poor
shortwave radio communication
on earth. This is due to the
sudden increases in solar ultraviolet (and x-ray) radiation in the region of
*
-
?
Figure 10.
Large chromospheric flare of 25 July 19/46.
the flare. This "ultraviolet," purely radiational effect is accompanied by
a so-called "hook" on the magnetograms. If the chromospheric flare is intense
enough (class 3 or 3+ in a three point system, where 1 is the weakest flare)ard
isrannere than t45 the center of the solar disk, strong magnetic disturbances
TY
Declassified in Part - Sanitized Copy Approved for Release ? 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release
-.32-
radiality of streams and cannot be explained by other effects connected, for
example, with the fact that the inclination of the sun's polar axis varies
with respect to the direction earth.-sun. By polar axis here, we mean the
solar axis taken in the sense of the magnetic dipole axis.
Further, it should be noted that a part of the streams from the sun is
non-radial. The non-radial streams are those from large spot groups and
-0
chromospheric flares. Woreover, a number of storms are caused by non-radial
streams, namely streams with sudden beginning. Evidently, these are basically
T-storms (table 1). It should again be emphasized that weak storms with sudden
beginning differ sharply from weak storms with gradual beginning as follows:
a) there is a difference in the very nature of the storms 27173 and
particularly in the nature of their beginning;
b) there is a conspicuous tendency toward a 27-day recurrence of storms
with gradual beginning and an almost complete absence of this tendency with
storms of sudden beginning. These differences appear particularly clearly in
the work of Thellier and Thellier
Figure 18. 27-day recurrence of
disturbances with gradual begin-
ning (top) and the absence of
such a recurrence in disturbances
with sudden beginning (bottom).
2720.7. Figure 18 is a graph taken from
their work. We see a sharply expressed re-
currence for disturbances with gradual be-
ginning (top curve, where the intervals be-
tween the maxima are 27 days) and the com-
plete absence of this recurrence for dis-
turbances with sudden beginning (bottom
curve). The top curve was constructed for
328 storms, the bob-born for 210 storms. The
central maxima on both curves correspond
to the disturbances which were taken as the
source material for computation of the
Besides floccular streams dc-fletarl
hrr magnetic fields of spots.
-0
In
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
-33-
average data on geomagnetic activity before and after these disturbances;
c) both kinds of storms have different distribution (according to number)
in the solar activity cycle (figure 15). Weak storms with sudden beginning
are closely
nected with
d) the
connected with spots; storms with gradual beginning are not con-
spots (flocculi).
most intensive of the weak storms are those with sudden beginning.
2. The role of the radiality of corpuscular streams increases consider-
ably from maximum toward minimum solar activity.
The following facts attest
to this: I) the increase in the seasonal variations of magnetic activity to-
ward the minimum, 2) for a large number of disturbances, the lag of maximum
ITgtmaritTvity behind maximum solui.'a-e'EVity, 3) the increased recurrence
of geomeq,netic disturbances during this period (figures 12 and A and D in
figure 17) et al.
The increase in the role of radiality of the streams from maximum toward
minimum activity is caused by: a) the decrease in the number of flares and
large spot groups; b) the increase in the ratio of the number of M-disturb-
ances to T-disturbances; c) the decreased
role of the magnetic fields of spots
(as a deflecting factor) in connection with the decrease in the area of the
spot groups and the number of spots; d) the decrease in the mean latitude of
the active formations in connection with the radiality of the streams. To
avoid misunderstanding-, let us note that the recurrence of disturbances in it-
self does not indicate radiality of streams.
In 1932, Bartels L21_7rdisputed the existence of corpuscular stream
radiality. However, at present his critical remarks have lost all value. In
revealing the effect of radiality, he used sunspot data for the hemispheres
(southern and northern). Further, since the corpuscular beam is so radial,
Bartels' method is too crude. horeover, Bartels did not differentiate between
the large chromospheric flares and T-disturbances and thus did not find such a
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release ? 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
distinct lag of magnetic disturbances behind solar activity as was found in
r17J. At present there is no doubt that most corpuscular streams aru radial.
6. SOlAR FTOINENCES
Gaseous formations of differeit form situated above the chromosphere in
the solar corona are called prorninences. On an average, prorninences are 100
times denser than the corona surrounding them, but their kinetic temperature
is approximately 100 times less than that of the corona and is close to that of
the chromosphere. Prominences are very complex formations, forming a number of
clasees. First let us note that prominences of the sunspot class, associated
with sunspots, cannot be a source of corpuscles. They are formed in the
coronal area and the luminous matter is directed from there down toward the sur
Eruptive prominences are particularly interesting. Figure 19 shows a
photograph of such a prominence, taken by A. B. Severnyi at the Crimean Astro-
physical Observatory of the Academy of Sciences of the U Eruptive
. .
prominences are sometimes expelled from the sun at such velocities that they
are completely ejected from it. However, such instances are fairly rare, being
observed not more than once a year (on the average, per cycle EJ)
The quiescent prornirinces are the most stable type. In projection onto
the disk, quiescent prorninences appear as dark bands in the light of some
spectral lines. They can be seen clearly in figure a. When projected onto
the disk, prominences are usually called filaments.
As their name indicates, quiescent prominences in themselves are quite
stationary. Nevertheless, Kiepenmheuer E22J thinks that there is a definite
connection between filaments and id-disturbances. Kieoenheuer's conclusion is
based on very meager statistical data, however, and cannot be considered
4)
seriously.
Recently direct prOof has been given of the untenability of Kiepenheuer's
conclusion C3c, 36J.
-3-
Figure 19.
Eruptive prominence.
Figure 20.
Solar corona during the eclipse of 2 Febriiary 1952.
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
flocculi and
a connection
In view
Declassified in Part - Sanitized Copy Approved for Release 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
corpuscular disturbances practically excludes the possibility of
between coronal rays and geoactive streams.
of what has been stated above, the author considers the hypothesis
which identifies coronal rays with corpuscular-streams to be in sharp contra-
diction with the facts found on the basis of geophysical data and, therefore,
to be incorrect.
8. DISCUSSION OF OTHER POSSIBLE SOURCES OF CORPUSCLES
In this section we will examine other possible sources of corpuscular
emission from the sun.
1. The thermal dissipation of atoms from the sun. The solar corona has
a very high kinetic temperature, and a number of atoms and electrons, with
rather high velocities corresponding to extre:Le Laxwel_lian distribution, can
leave the sun irretrievably. This mechanism of the "ejection" of atoms from
the sun should act continuously and in all directions. However, the very fact
that the earth's magnetic field is quiescent between disturbances indicates
that this mechanism is not effective 2710_7%
2. Streams of neutrons from the sun. V. A. Petukhov 2725_77 has
the possibility that the corpuscles ejected from the sun are neutrons
subsequently break up into protons,
studied
which
electrons and neutrons. However, for the
From the
present the development of this theory has been too general in form.
physical point of view in particular, it is unclear why the sun should emit
+)
such a large number of neutrons.
c 4- wee*
cuitta
Moreover, the radiality of corpuscular
is completely jncomprehensible
prom the viewpoint of the neutron hypo-'
thesis.
3. Corpuscular streams that create T-disturbances.
We saw that some of
)
This question is also discussed in /-257.
the weak magnetic storms (the smaller part) are characterized by a sudden be-
ginning and no recurrence. The curve of variation 1? the number of T-storms
within the eleven-year
of the relative number
still difficult to say
cycle practically coincides with the curve of variation
of sunspots 2717.7. However, for the present it is
with what the streams (undoubtedly, non-radial) which
cause the investigated T-disturbances could be connected. In particular, be-
cause of the closeness of these curves, it is difficult to assume that the
T-disturbances are caused by coronal rays. The number of sunspots after a
minimum increases rapidly and the number of T-disturbances increases with equal
rapidity. According to figure 15, two years after the solar activity minimum,
the number of weak geomagnetic storms with sudden beginning increases by more
than five times. Furthermore, as we saw in the preceding section, for one-
two years after the minimum no significant variations were observed in the
number of rays in the corona or in their direction.
The close connection between T-disturbances and spots suggests that these
disturbances could be associated with chromospheric flares of class 2-3, the
more so since the magnetic storms connected with strong chromospheric flares
also have a sudden beginning. Further, let us note that of the weak geomag-
netic storms, those with sudden beginning are the strongest (relatively).
From this point of view, it should be assumed that weak chromospheric flares
(class 1) cannot generally create corpuscular streams. Newton's work
and in particular figure 2c of this work, shows that class 3 flares, possibly
even class 2 flares, can be a source of T-disturbances. Newton finds that the
spot groups within which
most geoactive. Allen's work also indicates that flares, at least class
3 flares, may cause geomagnetic disturbances.
However, another possible interpretation of T-disturbances must be kept
in mind. In a work which will be presented at this conference, A. B. Severnyi
chromospheric flares frequently occur,
should be the
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
examines the the very interesting spectroscopic phenomena, characterized by the
appearance in some lines
from the normal position
served in active regions
of the solar spedtrum of emission which is shifted
of these lines. Basically, these phenomena are ob-
of the sun. If this emission is most intense in sun-
spot locations, it may explain the origin of T-disturbances as well. It
should also be noted that if in this case the origin of the emission is con-
nected with phenomena of an "explosive" nature, the initial velocities com-
municated to the matter during such explosions must be quite large, of the
order of 2000-2500 km/sec. Let us recall that the parabolic velocity on the
sun's surface is 617 km/sec.
All these possibilities of explaining weak disturiJanc="="751n'aidaen be-
ginning should be studied attentively. In any case, these disturbances differ
in many ways from the remaining 11-disturbances and thus can hardly be connect-
ed with flocculi.
The following fact is very important for explaining T-disturbances. From
figure lc, it is obvious that the minimum number of T-disturbances occurring
during years of maximum solar activity is considerably less distinct than the
corresponding minimum for the number of bi-disturbances. In other words, the
influence of magnetic fields on streams of corpuscles that create T-disturb-
ances is evidently far smaller (see section 5) than the influence of these
fields on the streams that form ?, disturbances.
Study of all possible mechanisms of the ejection of atoms from the sun
must be continued. In particular, a more detailed study, based on observa-
tions, must be devoted to the mechanism of calcium atom emission from the sun
due to selective light pressure (section 3). We indicated that in flocculi,
the operation of this mechanism must be connected with the fact that the light
pressure on the Ca+ atoms above the flocculi exceeds gravitation. However, E.
Milne Z726_7r noted that Ca+ atoms can be ejected from the sun because of light
pressure if, at the initial moment, these atoms have some very small velocity,
of the order of 10-20 km/sec. It is quite possible Z7.7rthat from time to
time in a number of places on the sun's surface small clots of matter are
ejected at low velocities. The total amount of matter ejected in this manner
may prove inadequate to create the observed moving details, but it may lead
to the effective emission of calcium atoms.
9. THE VELOCITIES OF ATOMS IN STREAMS
The velocities of atoms in streams have not been discussed to any great
extent in literature, but this is a very important question for the physics of
corpuscular streams, in particular for the quantitative explanation of the
different effects which appear in the upper layers of the earth's atmosphere
(magnetic and ionospheric disturbances, etc.). Let us examine different
methods of determining the velocities of corpuscles and the corresponding
quantitative data.
One of the methods most frequently used involves determination of the lag
time of geomagnetic (andother) disturbances behind the corresponding solar
phenomena. Here, a clear line must be drawn between two cases. In the case
of chromospheric flares, we observe the solar phenomenon directly and, on an
average, the disturbances on earth can be detected 24 hours after the appenr-
ance of the flare. Hence, in this case the earth meets the forward edge of
the stream (figure 23a) at the moment the disturbances begin. However, in the
case of the most frequently observed disturbances, i.e. the M-disturbances,
which tend to recur, we should-assume that corpuscles are being ejected con-
tinuously, very frequently during many rotations of the sun, from some active
region (in the author's opinion, from a flocculus). On entering the stream
every 27 days (due to the sun's rotation), the earth (i.e. the upper layers
of the earth's atmosphere) is exposed to a corresponding influence from the sum
Declassified in Part - Sanitized Copy Approved for Release ? 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
. 50
corpuscles:
1. Calculation of the concentration of corpuscles
geomagnetic disturbances. Such estimations assume the
oped mechanism which explains the magnetic disturbance
Declassified in Part - Sanitized Copy Approved for Release
from the intensity of
presence of some devel-
phenomenon. At present
we have the well developed and physically probable theory of the initial phase
of goon -,netic disturbances (for the principles involved, see Z730.27, p. 430).
This theory yields the following results in our case. Chapman Z7131_7' finds
that the concentration of protons in a stream up to its entrance into the
earth's magnetic field (for velocities of the order of 1000 km/sec), corres-
ponding to moderate and lartz; geomat, Usturbances, falls within the inter-
val 1 to 100 cm-3. Ferraro 2732./ finds that at this velocity the concentra-
tion of protons is between 25 cm"-3 for large storms and 1 cm `3 for smaller
storms.
2. Determination of the concentration of corpuscles by the intensity of
the displaced Ha line in the polar aurorae spectrum. This theory, developed
by I. S. Shklovskii 1.-33.7, gives the number of protons in the interval sun-
earth as 0.7 cm'-3. Chamberlain's calculations Z734.7, made in a somewhat
3
different manner, give a concentration of 0.2 protons/cm for moderate polar
aurorae.
Of course, these calculations involve a number of uncertainties, but they
can hardly contain any serious error. They all indicate that for moderate geo-
magnetic disturbances (and polar aurorae) the number of protons in the stream
at the earth is of the order of 1 cm3, and for strong disturbances from 25-100
.3
cm .
A number of authors dispute the accuracy of these figures because certain
phenomena which occur in comets and in the polarization of zodiacal light re-
quire considerably higher concentrations (two-four orders of magnitude higher).
However, I feel that these situations are still too indefinite to take such
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
-51-
objections seriously. In particular, there is no basis for assuming that the
+)
polarization of zodiacal light is caused by electrons alone. The polariaa-
tion of sunlight, diffused by dust particles in interplanetary space, can play
a large role. Furthermore, it is not at all clear why these electrons (if
the conclusions drawn from the polarization phenomenon are true) must be ex-
pelled from the sun, together with an equal number of protons, at "geophysical"
velocities of the order of 1000 km/sec. Rather, it should be assumed that we
are dealing here with a "quasi-stationary" medium, which, of course, has velo-
cities characteristic of an interplanetary and interstellar medium, i.e. velo-
cities of the order of several kilometers per second or, in the extreme case,
of several tens of kilometers per second. Decidedly, there are no bases here
for concluding that these electrons and protons are expelled from the sun at
velocities of the order of 1000 km/sec: The situation with regard to comets
is also uncertain.
Undoubtedly, the question of the concentration of corpuscles in streams
will be touched upon in a number of papers. Therefore we will not dwell on
it in more detail here.
QUESTIONS AND ANSWERS
The authors were given the opportunity of revising the text
of their answers for print; however, the editors felt it was
better not to change the answers to the questions, though they
were not always exhaustive.
H. N. Gnevyshev: What evidence is there that streams from eruptions
(chromospheric flares) have a large solid angle?
E. R. Nustel': There is evidence in the fact that disturbances of a
corpuscular nature are also observed when a large chromospheric flare is at a
17r?
Electrons are considered to be acomponent part of corpuscular streams.
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
-52-
distance up to 45? from the center of the disk.
D. Ia. Martynov: Can we be certain that a prominence is a movement of
matter and not the effect of illumination?
Mustel': Yes, usually we can tell this because lines in the spectra of
moving prominences are displaced correspondingly.
S. K. Vsekhsviatskii: In your paper it was noted that corpuscular emis-
sion from high-latitude flocculi is deflected by fields of sunspots. Why is
such deflection not recognized in low-latitude streams?
Mustelt: This was discussed in the introductory lecture. As one might
think, this appears in the fact that during years of minimum there are far
fewer spots in floccular fields and the area of these spots is considerably
less than in years of maximum. Thus the role of magnetic fields as deflecting
factors is considerably less in years of minimum than in years of maximum. For
a year or two before a solar activity minimum, when M-disturbances are very
frequent, no spots are observed in flocculi sometimes for months.
Vsekhsviatskii: How do you visualize the passage of corpuscular streams
through the corona?
Mustell: In order to explain the situation here, let us return to chromo-
spheric flares. It is known that chromospheric flares, usually situated in
chromospheric layers or slightly above them (sometimes lower also) are a good
source of corpuscles. These corpuscles, clearly not of coronal origin, pass
through the corona at velocities of the order of several thousants of kilo-
meters per second, during which they travel in a very broad stream, with a
total span of as much as 900. Thus, this fact indicates the possibility that
corpuscles pass through the corona.
True, it could be assumed that these
corpuscles "draw after them" the entire corona inside a solid
-le with a
span of 900. However, non-eclipse observations of the corona and data on
eclipses made over a number of years give decisive evidence against such de
formations in the corona.
Consequently, the structure of the solar corona is such that it allows
corpuscles to pass through it from below. I have examined this property of
the corona before (Akademiia Nauk 555R, Leningrad, Krymskaia astrofizicheskaia
observatoriia Izvestiia, 3: 3, 1948) in connection with the question of the
possibil.ity that calcium ions pass through the corona. In this work I indi-
catecl that the heterogenity of the corona is such that the corpuscles could
pass through the intervals between 'le individual ray systems and condensa-
tions. Recently new facts, which I have presented in another work (Astrono-
micheskii Zhurnal, 32: 177, 1955), have appeared on the presence of consider-
able heterogeneities in the corona. In these works there is a discussion of
the question of the effect of matter on foreign atoms passing through the
corona.
Vsekhsviatskii: Where was the information obtained that 27-day recur-
rence appears only (as the author indicated) in enochs before the minimum?
hustelt: I maintained only that this recurrence is maximum in years of
minimum. The data on this is given in the introductory report.
G. M. Nikoliskii: The radiality and narrowness of streams was obtained
from observations of spots, but the spots themselves are not geoactive. How
was the role of the spots distinguished?
Mustelt: First, the radiality of streams follows not only from observa-
tions of spots. Second, it is known that the laws of latitudinal distribution
of spots and faculae on the disk (except for polar faculae) are practically
identical. Consequently, we can assume that the regularities found, reflect-
ing radiality, also pertain to faculae (flocculi). A quite different law will
apply to prominences.
E. A. Panamarev: The general magnetic field also exists in the equato-
ial regions. How do corpuscular streams pass through it?
iimilmmimmimmEmin Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
-54-
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Mustel': Naturally here it is a matter of determining those forces which
lead to the ejection of corpuscles. However these estimates yield very little,
because we do not know the intensity of the general magletic field at the
equator. We know only that it is considerably less than at the poles, where
it is of the order of one or several oersteds.
L. I. Dorman: What information on the electromagnetic fields in streams
do observations give?
Mustel': At present our information on treams is very indefinite,
Therefore it is very difficult to give an answer to this question.
LITERATURE CITED
1. Eigenson, M. S., M. N. Gnevyshev, A. I. 0111 B. M. Rubashev. Solnechnaia
aktivnostl i ee zemnye proiayleniia (Solar activity and its terrestrialmanifestations),oscow, UosteUTETiat, 1948.
2. Newton, H. Royal Astronomical Society, Monthly Notices, Geophysical Sup-
plement, 5: 321, 191.
3. Allen, C. Royal Astronomical Society, Monthly Notices, 104: 13,
4. Mustel', E. R. Akademiia Nauk SSSR Doklady, 42: 117, 1944.
1944,
5. BugosIavskaia, E. Ia. Gosudarstvennyi astronomicheskii institut im.
Shternberga, Trudy, vol. 19, 1949.
6. Gnevyshev, M. N. and A. I. 01/. Astronomicheskii Zhurnal, 22:151, 1945;
also Terrestrial Magnetism and Atmosnheric Electricity, 51:163, 1946.
7, Mustel', E. R. Akademiia Nauk SSSR, Leningrad, Krymskaia astrofizicheskaia
observatoriia, IETestiia, 3:7779473:-
8. Mustel' E. R.
9. hiustel', E. R.
observatoriia,
Akademiia Nauk SSSR,
Akademiia Nauk SSSR
Doklady, 81:363, 1951.
Leningrad, Krymskaia astrofizicheska-.7_L
a so :JocIete Royale des Sciences
zves iia, 1
de Liege, Illemoires, Serie 4, 13(3): 223, 1953.
10. Mustoll, E. R. Astronomicheskii Zhurnal, 32:177, 1955.
11. Severnyi, A. B. and E. F. Shaposhnikova, Akademiia Nauk SSSR, Leningrad,
Krymskaia astrofizicheskaia observatoriia, Izvestiia, 12:3, 1954.
12. Newton, H. Royal Astronomical Society, Monthly Notices, 103:244, 1943.
?
-55-
13. Mustel', E. R. and A. B. Severnyi. Akademiia Nauk SSSR, Leningrad, Krym-
skaia astrofizicheskaia observatorila, U:19, 1951.
14. Mustel', E. R. Akademiia Nauk SSSR Leningrad Krymskaia astrofizichedcaia
observatoriia, Tv7F67=a,--13:2-
15. Benlkova, N. P. Gidrometeorologicheskaia sluzhba, Nauchno-issledovatel'-
skie uchrezhdeniudyr-s-61-Te-s-67-issue 2; alsd-Terrestrial-ffagnetiFE
727717671-77JTFITTCTFTErty, 47:147, 1942.
16. Harang, L. The aurorae, New York, John Wiley and Sons, 1951. 166 pp.
p. 15.
17. Newton,. H. and A. Milsom. Journal of Geophysical Research, 59:203, 214,
18. Shapley, A. American Geophysical Union, Transactions, 28:715, 1947.
19. Chernosky, E. American Geophysical Union, Transactions, 32:861, 1951.
20. Thellier, M. E. and Mme. 0. Thellier, Academie des Sciences, Paris Conptes
Rendus, 227:1044, 1948.
21. Bartels, J. Terrestrial Magnetism and Atmospheric Electricity, 37:1, 1932.
22. Kiepenheuer, K. Astrophysical Journal, 10:408, 1947.
23. Pecker, J. and W. Roberts, Journal of Geophysical research, 60:33, 1955.
24. Wesley, W. Royal Society of London, Philosophical Transactions, Series A,
226:363, 1927.
25. Petukhov, V. A. Lecture in the collection Trudy trettege soveshchaniia po
voprosam kosmoconii (Transactionsof the th7F3-FORTTrence on cosmogony .
RETC131VTIzda:TeT17-177o Akademii Nauk SSSR, 1954. p. 210.
Milne, E. Royal Aetronomical Society, Monthly Notices, 86:459, 1926.
26.
27.
28.
Chapman, S. Royal Astronomical Society
Monthly Notices 89:456, 1929.
Meinel, A. Astronhysical Journal, 113:50, 1951.
29. Gartlein, G. Physical Review, 81:463, 1951.
30. Mitra, S. K. Verkhniaia atmosfera (The upper atmosphere). Moscow, Iz-
datel'stvo inostrannoi literatury, 1955.
31. Chapman, S. Annuales de Geophysique, 8(2), 1952.
32. Ferraro, V. Journal of Geophysical Research, 57:15, 1952.
33, Shk1OVSkii, I. S. Akademiia Nauk SSSR Leningrad Krymskaia astrofizi-
cheskaia observatoriia, zvestila, 1, 1
deownlemaM.
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
56 ?
34. Chamberlain, J. Astrophysical Journal, 120:360, 1954.
erffora?mmegs..graroa
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
35. Roberts, W. and D. Trotter. Journal of Atmospheric and Terrestrial Physics,
6:282, 1955.
36. Leighton, H. and D. Billings. Journal of Atmos-,Dheric and Terrestrial
Physics, 7:349, 1955.
Declassified in Part - Sanitized Copy Approved for Release
SPECTROSCOPIC INVESTIGATION OF CORPUSCULAR EJECTIONS ON THE SUN
by
A. B. Severnyi
1. INVESTIGATION OF THE PROFILES OF THE H AND K LINES OF IONIZED
CALCIUM IN FACULAE
In 1951, V. B. Nikonov and A. B. Severnyi first discovered the character-
istic asymmetry of the H and K line profiles in faculae. The electrospectro-
photometric method used in this case assured an accuracy which left no doubt
as to the reality of the asymmetry effect studied differentially, i.e. by
the difference between the residual intensities of these line profiles in the
facular spectrum and ',,I.,--t"urrt.cpuudiiig unuisturbed disk.
The apparatus for photoelectric recording of the solar spectrum in the
solar tower telescope is shown in figure 1.
Figure 1. Device for photoelectric recording of the solar spectrum.
The following important improvements were made in this new apparatus:
a) the vignetting of the spectrum, which is caused by the small size of
the speculum which "oscillates" the spectrum, was eliminated;
b) various rates of recording the spectrum were used (from 1/4 to 1/500
.asirICAMOIONISSaWKINOWINIMING021111res..,14,4
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release
cps), which allowed recording without a time lags and also various time con-
stants were used at the amplifier input and provision was made for rapid and
easy change of these time constants;
c) provision was made for a rapid and convenient exchange of one photo-
multiplier (for the visible spectrum) for the
d) VEI photomultipliers were used with
other (for the red and infrared):,
a low noise-to-signal ratio and
a small dark current, etc.
Figure 2 shows an example of a recording of the H line in a facular spec-
trum: in the center one can see a double reversal caused by a flocculus.
Figure 2. A recording of the H line of a facular spectrum.
Figure 3 shows the distribution of extra "emission" in facula No. 42 for
various days: the distances from the center of the H and K lines in a are
plotted along the x-axis, the difference between the residual intensities of
the facula and the photosphere is plotted along the y-axis (the dots correspond
to the K line, the circles to the H line). The asymmetry of the indicated
difference (in the sense "blue wing minus red wing") of extra "emission" in
I the facula (a unit on the y-axis is equal to the intensity of the continuous
+
Photomultipliers made by the All-Union Electronics Institute (Vsesoiuznyi
Elektrotekhuiehuskii Institut).
.... z_
4
/ /...../
r1TY -7
Declassified in Part - Sanitized Copy Approved for Release
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
rio
1
.52
12=0,22
0,1
14 VIII 52
p - 0,14
?????
0
A'
0.1
15 VIII 52
2U,28
1"r"'-?-r__"zmt,py.5:r_ircr=7:r
?
0.1
0,1
52
(1,4g
17 VIII 52
p 0,tig
f 204
Figure 3.
H and K emission profiles in facula No. 42.
spectrum) is shown in the upper
left for each day. Every distri-
bution of extra emission was ob-
tained by averaging the results
of 3-9 separate recordings. The
mean square error of one indivi-
dual measurement (according to
the records of 1952) is 0(.5?6 ;
at present this error has been ra
duced to 0.2516. The extra
emission and its asymmetry were
obtained by differentiations
therefore, the measured effect
cannot be related to any system-
atic errors whatsoever, in parti-
cular errors of an instrumental
nature (e.g., the polarization
of light in the instrument and
its variation during the record-
ing, et al.).
more than 30 faculae were
studied (1952-1954). An examina-
tion similar to that shown in
figure 3 showed: 1) in practice, the profiles of the extra emission
line agree well with the profiles for the K lines 2) in most cases,
wing of extra emission is higher than the red wing; 3) the position
for the H
the blue
and magni-
tude of the extra emission and its asymmetry vary from facula to facula
and
also, with the passing of time, for the same facula. The position of the
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
- 6o -
Declassified in Part - Sanitized Copy Approved for Release e 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
asymmetry maximum varies from 300 to 1000 km/sec (if the distances from the
center are expressed in velocities), the magnitude of the asymmetry varies
from 1 to 5%. In this case, the position and magnitude of the asymmetry do
not correlate with the intensity of the H2, K2 emission in the center of the
line which is produced by a flocculus. Further, except for one case (facula
No. 42, given in figure 3).0 the position and magnitude of asymmetry are not
functions of the position of the facula on the disk. In the case of facula
No. 42, the position of maximum asymmetry shifted approximately according to
the law AX--cos 8 in its passage across the disk; however, the magnitude of
this emission did not reveal any relationship to the position of the facula on
the disk. Hence, if the investigated asymmetry is connected with radial
streams of particles, these streams do not go beyond the limits of the chromo-
sphere, since otherwise the intensity of the blue wing, as compared with that
of the red wing, would have increased statistically as the facula approached
the center of the disk.
Basically, the observable effect of the extra emission asymmetry is not
connected with the possible difference in the behavior of the metallic lines
in the facula and in the photosphere, which blend lines H and K, since the
disposition of the blends differs in the H region and in the K region and both
lines e;enerally give results that are in agreement. Furthermore, the examined
effect cannot be connected with the mutual blending of the H and K lines, since
(as calculations of the theoretical profiles of these lines have shown, with
consideration of their mutual blending) blending can lead to an effect of the
opposite sign revealed at distances 6X>10 R and cannot in any way explain
such diversity of the profiles of the extra emission. Figure 4 gives the
theoretical profiles of the H line for the disk (solid line) and for a facula
(dashed line); the theoretical emission profile in the facula is shown below,
and its asymmetry is shown on the left.
Declassified in Part - Sanitized Copy Approved for Release
'
- It) -II) -
0
# 4
Figure 4. Theoretical pro-
file of the H line.
magnitude of this emission and
-61--
If the extra emission of the blue wing
(asymmetry) is connected with corpuscular
streams, its measured magnitude makes it possi-
+
ble to judge the density of the stream of Ca
ions, considering that the stream does not ex-
tend above the upper chromosphere (otherwise
we would observe a relationship between the
cos 8). On an average, the equivalent width of
the excess emission , 0.1 X and is concentrated in a column of approximately
40,000 km, so that the emission per unit volume is approximately
2.106.0.1
? 101-'5 ergicm3sec. (1)
Calculations show that the process of recombinations of a Ca+ ion to the 42P
level does not explain such emission. The process of collisions of the Ca+
ions with electrons explains it more effectively; in this case, for the energy
we have
Zchv Z qvnen(Ca+); hv;
when v2:108 and q::10-15, we get, from (1) and (2):
Zchv 2 ? 10'18nen(Ca+)2:5 ? 1r5
whence, assuming nea1010 $ we get
n(Ca) ::104
If we calculate the distribution of ne on the basis of velocities, the
(2)
maL;nitude n(Ca) will be still smaller. Thus, s
corpuscular streams h
surface).
p ctrosconic data show that
ave low density, of the order of 1 cm-.3 (at the earth's
The as?-mmetry of the extra emission in the H and K lines of faculae is a
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
_62
eallb
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
very real effect, beyond possible errors. One cannot conceive of any sensible
physical mechanism for its appearance, except the ejection of corpuscles from
the faculae. If this effect is caused' by corpuscular streams, they cause
illumination only in the low layers of the solar atmosphere, otherwise we
would be able to observe them above the chromosphere as well as we do the
prominences.
Recently a very interesting spectrogram with K4 emission above the chromo-
sphere over a facula was obtained on the solar tower telescope. It reached
a brilliance of approximately 10043 of -Lim continuous spectrum, while its pro-
file was non-turbulent with a half-width of appl-eximately 0.15 ii,-ee.c-respond-
ing to a purely thermal Doppler broadening, as if this were a stream within
which the particles had only a thermal distribution of velocities.
Further evidence of the connection between this effect and corpuscular
ejections from faculae is given by the good agreement (800/o of the cases) be-
tween the precomputed moments of corpuscular disturbances (according to our
spectral data) and the actual moment of the magnetic disturbances based on
K-index data.
2. INVESTIGATION OF THE PROFILES OF THE Ha LINE IN THE SPECTRUM
OF FACULAE
A similar investigation was made for the hydrogen line Ha in the spectrum
of faculae. The preliminary results of this investigation also indicate the
presence of a clearly expressed asymmetry in the behavior of the difference -
c1L;LA?LcaG
tJaivvyukiLs
4
fn-r. 44-tcs
cmmn fnr.1,1nn 4-1-N?1+ cl-,n7IrnA
asymmetry in the H and K lines.
Figure 5 shows some typical profiles of this difference (the extra "emis-
sion" value, in an algebraic sense, in percents of the continuous spectrum is
plotted along the y-axis). In the case of the Ha line in the faculae, too, no
J/0
2
LI
- 63 -
red
blue
8 VI
A
10 Vi 53
17 VII 5.)
29 IX )3
(blue)-
-rw(red)
3% 4 v1;1 54
--LW; -01
4101 420 Aa
Figure 5. Some typical Ha profiles in faculae.
connection was discovered between the emission in the center of the line and
the nature of the asymmetry. Furthermore, no systematic variation of this
asymmetry from the center to the edge was discovered.
host interesting was the comparison of the asymmetry In the H and K lines
with the asymmetry in the Ha line _for the same faculae. Figure 7 gives the
extra (algebraically) emission in the facula for the Ha lines (dots) and the
K lines (circles). Analogous graphs were also obtained in other cases.
Are see that the distribution of extra emission of the facuale minusatwhe ,e.
photosphere is quite different for the Ha line and the ver,
H and K lines
Declassified in Part - Sanitized Copy Approved for Release ? 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
450
-614-
rv(blue).
rv(red)
900km/sec
1
W*M.5.341
10M555
I
?`???4:rw' '
?
.
/0. VIII 53a
. . -
8 . Nil .55
- 6.10.53
5. VIII . 53
- T1. Vii . 53
- le___.-1......__ .
3. i 1 I. 53 .
20. YI .53
.......or
It VI 53 ? .
?
r0 Vi 53
? 5. V/ .53
.
.
ig. Vi 5'3
450
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
if we compare the distribution of
asymmetry, i.e. the difference rv
(facula)-rv (photosphere) for the
red,. rving minus this same difference
for the blue wing instead of the
distribution of the differences
rv(facula)-r (photosphere), we will
v -
get an entirely uifferent picture:
the distribution of the Ha asymmetry
reproduces quite well the distribu-
tion of the asymmetry of the K (or
H) line and the asymmetry extremes
in the K line either agree with
those of the Ha line or they are
displaced toward higher velocities.
Several examples of the comparison
of the asymmetry in Ha (dots) and K
(circles) are given in figure 6,
where a scale of velocities (for
comparison) is given along the x-
axis instead of a scale of wave
lengths.
This comparison shows that the
asymmetry effect appears in faculae
simultaneously in the H and K lines
and in the Ha line, as it should if
streams are involved here which con-
tain hydrogen and calcium particles,
900 sec
Figure 6= Asymmetry of the K and Ha
profiles in faculae.
?
-5 Aa
17 VIII 53,101 cc
24%
29M 53, hr? 1 cc
?
.5 I
t 5 40
Figure 7. K and Ha profiles in faculaev(facula)-rv(photosphere)./.
The fact that the extremes for the K line are shifted toward higher velocities
as compared with the extremes Tor the Ha line shows, possibly, that the velo-
city of the Ca4 ions in the stream of particles is greater than the velocity
of the hydrogen atoms. At the same time, the conditions for the formation of
the Ha and H and K absorption lines in the solar atmosphere are highly varied,
which leads one to view this conclusion cautiously: with the same rate of
emission of Ca+ ions and hydrogen atoms, the ab'sorption action in the sphere
of the line can exert a special masking effect on the emission and create the
appearance of a difference in velocities.
3. THE FINE STRUCTURE OF FACULAE MISS ION ("MUSTACHES")
The new solar tower telescope made it possible to detect recently some
very interesting and amazing features of flare and facula emission, viz, the
so-called fine structure of this emission and "mustaches." it was found that
with good images, the continuous arid linear emissions are concentrated in in-
dividual "centers" or "grains" no larger than a circle of scattering of Oat
(-300 km) in some instances.
The emission in the lines differs from the ordinary picture of a diffuse
Declassified in Part - Sanitized Copy A ?proved for Release ? 50-Yr 2014/05/30 ? CIA-RDP81-01043R004500220001 3
-82 -
Declassified in Part - Sanitized Copy Approved for Release
for strong disturbances.
Nevertheless, in the preceeding discussions these estimates have been
disputed without sufficient grounds, and it was asserted that those estimates
based on study of the polarization of zodiacal light and the study of ac-
celerations observed in comet tails would be more valid. I have already
pointed out that these latter methods yield very indefinite results. How-
ever, the given question will be discussed in greater detail in subsequent
lectures, and I would like only to point out the following facts.
Considering that polarization of zodiacal light is caused by electrons,
Siedentopf, Baer and Elsasser have found that near the earth the corresponding
concentration of electrons, and subsequently also protons, is close to 10
om-3 Here authors defending the coronal concepts of current assume that in
this case as well we are dealing with streams of protons and electrons from
the sun moving at a velocity of about 1000 km/sec and having the indicated
concentration np',103 cm3.
On the other hand, it is known that the isophotes of zodiacal light are
stationary and are always of a completely smooth nature. This indicates that
from +.11r4 point of view of the give5n concepts, the earth is always in the
field of relatively equally distributed (in space and time) streams with
v = 1000 km/sec and n cm3,
At
At the same time it is known that even in years of maximum solar ac-
tivity the earth's magnetic field is quiescent between individual distur-
bances. In other words, in the examined case, we should have consLdered
that corpuscular streams, with the above-indicated parameters, correspond
to a quiescent magnetic field, but this cannot be, since the energy trans-
mitted by such currents with v = 1000 km/sec and n "x10 i
3 cm s so great
-3
that these streams cannot help but create noticeable disturbances in the
earth's magnetic field.
Furthermore, let us assume for the time being that the indicated currents
actually correspond to a quiescent field. But whatever theory of magnetic
disturbances we use, the concentration of atoms corresponding to strong diF-
turbances and a quiescent field should differ by 3-4 orders of magnitude. In
other words, strong storms should correspond to concentrations of 106-107
cm-3, which is already quite absurd, and differs by 104-105 times from that
which we would get if the theory of geomagnetic disturbances were used. More-
over, streams with v = 1000 km/sec and concentrations of 106-107 cm-3 cor-
respond to energies greater than the solar constant. Approximately the same
b
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
=MY
8
3 -
argumentation is applicable to comets as well.
Let us return again to the "coronal" concepts of corpuscular streams.
It should immediately be stressed that we must differentiate between the
question of the movement of matter in coronal rays with velocities up to
several km/sec and even in a number of cases to ten km/sec, and the hypothesis
which states that in the outer parts of coronal rays, matter moves with "geo-
physical" velocities of the order of 1000 km/sec. We cannot doubt the first,
since the very fact of the existence of extended coronal rays as solar for-
mations attests to the movement of matter away from the sun, and we should
recognize the service done by Ponomarev in processing the physical mechanism
which determines the kinematics and dynamics of matter in the corona. The
concept of coronal rays as well as streams of geoactive corpuscles is another
matter. I completely disagree with these concepts. I have already enumerated
my main objections; these are objections connected with the radiality of
solar corfluscular streams. Let us make a number of additional comments.
A number of observational facts presented in one of my works (Astrono-
micheskii Zhurnal, 32: 177, 1955) attest to the fact that at the base of rays,
right up to heights of O. Ra - 1 Re from the sun's surface, radial efflux
velocities cannot exceed several km/sec. Accordingly, we should introduce
some mechanisn of the acceleration of coronal matter in the outer parts of
the rays. This acceleration mechanism is as yet completely hypothetical. In
the mechanism examined by Ponomarev, the main force which determines the
acceleration outward is the pressure gradient connected with the temperature
drop. 7e cannot tell anything from the magnetic forces themselves, since
it is known that magnetic forces usually only decelerate matter.
But in such a case it should be noted thnt the efflux of matter should
be most intense not above promincncos, where the extended coronal rays*) are
directly observed, but above faculae. It is known that actually, directly
above faculae, there are regions of increased luminescence in coronal lines,
whereupon these regions are extremely hot. Accordingly, it is actually here
that we should expect a great temperature drop, although again it is difficult
to identify broad coronal rays above faculae with geoactive streams, since
above faculae as well, coronal rays are usually not radial. On the other
hand, in the base of "helmets," which are the lamer part of extended coronal
rays, monochromatic coronal luminescence is not amplified. Moreover, in the
????????.??????????-?
*)
which are also considered as geoactive streams.
.A.E.m Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
-82 -
Declassified in Part - Sanitized Copy Approved for Release
for strong disturbances.
Nevertheless, in the preceeding discussions these estimates have been
disputed without sufficient grounds, and it was asserted that those estimates
based on study of the polarization of zodiacal light and the study of ac-
celerations observed in comet tails would be more valid. I have already
pointed out that these latter methods yield very indefinite results. How-
ever, the given question will be discussed in greater detail in subsequent
lectures, and I would like only to point out the following facts.
Considering that polarization of zodiacal light is caused by electrons,
Siedentopf, Baer and Elsasser have found that near the earth the corresponding
concentration of electrons, and subsequently also protons, is close to 10
om-3 Here authors defending the coronal concepts of current assume that in
this case as well we are dealing with streams of protons and electrons from
the sun moving at a velocity of about 1000 km/sec and having the indicated
concentration np',103 cm3.
On the other hand, it is known that the isophotes of zodiacal light are
stationary and are always of a completely smooth nature. This indicates that
from +.11r4 point of view of the give5n concepts, the earth is always in the
field of relatively equally distributed (in space and time) streams with
v = 1000 km/sec and n cm3,
At
At the same time it is known that even in years of maximum solar ac-
tivity the earth's magnetic field is quiescent between individual distur-
bances. In other words, in the examined case, we should have consLdered
that corpuscular streams, with the above-indicated parameters, correspond
to a quiescent magnetic field, but this cannot be, since the energy trans-
mitted by such currents with v = 1000 km/sec and n "x10 i
3 cm s so great
-3
that these streams cannot help but create noticeable disturbances in the
earth's magnetic field.
Furthermore, let us assume for the time being that the indicated currents
actually correspond to a quiescent field. But whatever theory of magnetic
disturbances we use, the concentration of atoms corresponding to strong diF-
turbances and a quiescent field should differ by 3-4 orders of magnitude. In
other words, strong storms should correspond to concentrations of 106-107
cm-3, which is already quite absurd, and differs by 104-105 times from that
which we would get if the theory of geomagnetic disturbances were used. More-
over, streams with v = 1000 km/sec and concentrations of 106-107 cm-3 cor-
respond to energies greater than the solar constant. Approximately the same
b
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
=MY
8
3 -
argumentation is applicable to comets as well.
Let us return again to the "coronal" concepts of corpuscular streams.
It should immediately be stressed that we must differentiate between the
question of the movement of matter in coronal rays with velocities up to
several km/sec and even in a number of cases to ten km/sec, and the hypothesis
which states that in the outer parts of coronal rays, matter moves with "geo-
physical" velocities of the order of 1000 km/sec. We cannot doubt the first,
since the very fact of the existence of extended coronal rays as solar for-
mations attests to the movement of matter away from the sun, and we should
recognize the service done by Ponomarev in processing the physical mechanism
which determines the kinematics and dynamics of matter in the corona. The
concept of coronal rays as well as streams of geoactive corpuscles is another
matter. I completely disagree with these concepts. I have already enumerated
my main objections; these are objections connected with the radiality of
solar corfluscular streams. Let us make a number of additional comments.
A number of observational facts presented in one of my works (Astrono-
micheskii Zhurnal, 32: 177, 1955) attest to the fact that at the base of rays,
right up to heights of O. Ra - 1 Re from the sun's surface, radial efflux
velocities cannot exceed several km/sec. Accordingly, we should introduce
some mechanisn of the acceleration of coronal matter in the outer parts of
the rays. This acceleration mechanism is as yet completely hypothetical. In
the mechanism examined by Ponomarev, the main force which determines the
acceleration outward is the pressure gradient connected with the temperature
drop. 7e cannot tell anything from the magnetic forces themselves, since
it is known that magnetic forces usually only decelerate matter.
But in such a case it should be noted thnt the efflux of matter should
be most intense not above promincncos, where the extended coronal rays*) are
directly observed, but above faculae. It is known that actually, directly
above faculae, there are regions of increased luminescence in coronal lines,
whereupon these regions are extremely hot. Accordingly, it is actually here
that we should expect a great temperature drop, although again it is difficult
to identify broad coronal rays above faculae with geoactive streams, since
above faculae as well, coronal rays are usually not radial. On the other
hand, in the base of "helmets," which are the lamer part of extended coronal
rays, monochromatic coronal luminescence is not amplified. Moreover, in the
????????.??????????-?
*)
which are also considered as geoactive streams.
.A.E.m Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
-86-
and from data (observational) on the distribution N(r) in the ray. The
velocity v will increase-.2P, where n is the gradient of a decrease of N(r).
Computations give8 cm/sec in outer parts of the corona.
However, the established, as it were, absence of macroscopic velocities
in the non-eclipse observations of the inner corona do not exclude the ex-
istence of considerable microscopic velocities in rays where the rays are
visibly stationary. Here we should note that non-eclipse observations made
in emission lines do not give us a picture of movements in rays, since we
know that there is a lack of correspondence between regions of increased
luminescence in coronal lines and "white" rays. At the same time, Waldmeier's
recent observations indicate the existence of mass macroscopic movements in
the inner corona, which follows from the lifetime of monochromatic rays, 0-'15
minutes, which he established.
S. B. PIKELINER. In examining a ray as a stream we should consider the
place of formation of rapid particles. If they come from the chromosphere,
the ray is a two-phase system; a great part of it is in egailibrium and the
stream passes through it. If, however, rapid particles form in the corona,
from the continuity equation we gets motion of all matter of the ray upward,
with gradual acceleration. Data on the asymmetry of lines attest, rather,
to particles from the chromosphere. Ponomarev's theory is interesting and
worthy of attention.
Not all streams of the corona can be geoactive. I believe that the
estimate of the density of the stream is somewhat too high; it hardly ex-
ceeds 102 cm-3 for moderate disturbances. The slight divergence of the
stream is also doubtful. In this case, there would be little probability
of the current's striking the earth.
V. A. MAT. The question of the mechanism of the ejection of geoactive
particles has been of great interest at our meetings. The main thing now is
to establish the location of the centers of geoactive corpuscular radiation
on the sun's surface and to associate them with the actually observed phe-
nomena. On the sun's surface, such regions can only be chromos2heric layers
and facular fields (which, as A4 B. Severnyi has succeeding in establishing,
are accumulations of small chromospheric flares). In this case we can es-
timate the velocity of ejections of corpuscles, and establish the fact that
they c:L.f.ceed the critical velocity.
The question of the connection between flares and the phenomena in the
outer corona should be examined separately since there are, as yet, no obser-
Declassified in Part - Sanitized Copy Approved for Release
vational data for it.
.L46 BUGOSLAVSKAIA. The ccronal forms are determined by formations
on the sun's surface; the question of their stability is connected with this.
Coronal forms are disrupted, aid the corresnonding formations on the sun's
surface disappear, but not immediately; it is interesting what the present
theory gives in this case.
In the lectures we have spoken of the rays above prominences. Above
faculae, there appear direct rays running in a broad but slightly divergent
stream. The forms and interactions of coronal streams attest to the presence
of electromagnetic forces.
The velocities of movement of matter along a ray can be determined only
indirectly from photographs. In two cases, such velocities were estimated
to be no less than 100 km/sec.
N. IA. BUGOSLAVSKAIA. 1. The orominence observed during the solar
eclipse of 19 June 1936 attests to the transfer of matter of the prominence
into the corona; like the prominence, it stopped glowing. In its place
there remained coronal clouds of the same shape but considerably expanded.
'flart of the matter falls back 81d part evidently scatters.
2. The difficulties in explaining irregularities in the behavior of
disturbances, as indicated by Tustell from the point of view of the action of
corpuscular streams, disappear, if we consider the possibility that the
earth enters the corpuscular stream.
50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
Declassified in Part - Sanitized Copy Approved for Release @ 50-Yr 2014/05/30: CIA-RDP81-01043R004500220001-3
-88 -
MORNING CONFERENCE
23 November
CONTINUATION OF THE DISCUSSIONS ON THE LECTURES BY
E. R. MUSTEM, A. B. SEVERNYI, S. K. VSEKHSVIATSKII
ET AL, G. M. NIKOL'SKII, AND E. A. PONOMAREV
S. K.,VSEKHSVIATSKII. 1. Yesterday we heard convincing evidence that,
according to Mustell? the mechanism of light pressure cannot explain the
formation of streams. But even if such a mechanism were active, and recti-
linear streams were to form (Which actually cannot occur), would they pass
through the corona? Here Mustell and certain others defend the position
that geoactive streams have nothing in common with the corona. But what
does this mean? If they acknowledge that coronal matter is plasma, either
the streams are formed by coronal el?.ctrons and protons, or they do not
exist at all. There cannot be any other geoactive streams besides corpuscular
streams. This would be the same as acknowledging the fact that streams do
not exist. However, complete denial of streams means that all geophysical
data have to be disregarded.
Thus1 the concept that streams are not connected with coronal structures
which Mustel' suggested long ago, is logically unsubstantiated, and contra-
dicts physical concepts.
2. Here Mustel' used alleged proof of the radiality and narrowness of
geoactive streams, which therefore cannot be, as it were, coronal rays.
However, it is actually-the coronal rays that are characterized by narrowness
and directedness. Furthermore, the conclusions of M. N. Gnevyshev and A. I.
01' were obtained from statistics of the spottiness of the central regions
of the disk as compared with the average geomagnetic features. Knowing about
these deviating fields of spots, we should recognize that the relationships
of Gnevyshev and 011 are actually proof of the non-radiality of streams which
is in complete agreement with the structure of the corona. The Gnevyshev-011
relationship attests only to the fact that the disturbed region, character-
ized in particular by spots, --yiel.141 more coronal particles and consequently
greater density in geoactive streams. The conclusions about the narrowness
of streams are of the exact same statistical nature. They can in no way be
an objection against the representation of coronal rays.
3. Everything that Mustell has said about the alleged non-correspondence
between coronal rays and geoactive streams is a misunderstanding. Our com-
putations actually indicate the stability of coronal rays, their rotation with
- 89 -
the sun and accordingly, the obligatory nature of the 27-day recurrence. The
pulsations of rays which liustell tried to attribute to our statements are
simply untrue. Actually, we show that coronal radiation and structure are
an important path toward understanding geomagnetic phenomena.
1:ustell is mistaken when he asserts thdt the recurrence of storms is
observed only in pre-minimum epochs. Bartels' carpets prove that in the
maximum epoch, sequences do exist, but they are less stable. This is under-
standable from the viewpoint of the concept of coronal streams, but conk-
pletely unexplainable from the positions of Hustells concepts.
E. I. MOGILEVSKII. 1. The interesting results of the photoelectric
observations of emission in lines Hal H and K in flocculi, given in the lecturc
by A. B. Severnyi, should be, as we know, diligently analyzed from the point
of view of the computation of the experimental errors which arise during sucl?
highly accurate measurements. Ps has already been pointed out at the last
plenum of the Solar Research Commission*) in the photoelectric installation
of the Crimean Noservatory the instrument polarization of light, occurring
during reflection of light from the mirrors and the diffraction grating, is
'analyzed1 by the diagonpl scanning mirror and by the concave photocathode
of the photomultiplier. We can.shoC that after the disgonal scanning mirror,
whose reflection coefficient is T TW, the light intensity is determined
by the expression
I=T 0T cos2y(Pcos2y+sj112y) +sin2y(cos2y+sin2y)-s1n22y. VT /2(17E1
cos2y(cos2y+Psin2y)+Tsin2y(Pcos 2y+sM2y)+sin22y. '/T/2(1-P)
where y is the angle of incidence of light onto the diagonal mirror and p is
the instrument light polarization. With a change from y to y + dy in the
angle of incidence onto the scanning mirror, the computed magnitude dl with
Possible values of the parameters ) and T (the latter are taken from measure-
ments using the photoelectric