SCIENTIFIC ABSTRACT SEVERNYY, A.B. - SEVERNYY, V.V.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001548220006-3
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: August 23, 2000
• Sequence Number: 6
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

The Spectroscopy of Solar Flares With an
Echelon Grating
78oo4
SOV/33-37-1-4/31
Is
Card 2/11
Fig. 2. Diagram of the spectrographi with an echelon
grating.
Figure 2 shows the design where S is the slit; Ml, thE
collimation mirror; E, the echelon; P, a prism; and G.
a grating designed to spread the spectra of various
orders in a direction perpendicular to the plane of
dispersion; 14 , the camera mirror; C, the plate
holder; and I is a mir--,-or compound which corrects the
plane of atmospheric dispersion. This instrument

The Spectroscopy of Solar Flai,eu 1,41th an 7 8 0 C-) L'
Echelon Grating SOV/33-37-i-4/3i
Card 3/4
is practically free from Rowland's "ghosts" and from
scattered light. It is uzed for a simultaneouj
photography of the whole spectrum of short duration
flares and "whiskers", while previously such photo-
graphs could not be obtained simultaneolisly. With
exposures from 0.5 to 1.0 seconds, the spectrum is
well exposed over the range from 3,200 to 6,6oo
A. During the suimner of 1959, over 30 flares were
photographed; three of these are reproduced here.
The spectrum of a'flare near the solar limb obtained
on Au ust 30, 1959, showed 11 emission lines of He;
over ~50 emission lines are shown on a photograph
taken on August 17, 1959; theze are listed in a table
which indicates the intensities of the lines and of
the same lines in Rowland's catalogue. The authors
express their appreciation to F. M. Gerasimov who
suvulled an excellent copy of the echelon grating.
T'here is 1 table; 5 figures; and 4 references, 1
Soviet, 3 U.S. The U.S. references are: J. T.

.,-SEVERNYY. A.B.: SHABAITSKIY, V.P.
Generation of cosmic rays in flares. Astron.zhur. 37 no.4:
609-615 Jl-Ag 160. (MMA 13:8)
1. Krymskaya astrofizichaskaya observatoriya AN SSSR i Hauchno-
iBBledovatellakly institut yadernoy fiziki Moskovskogo
gosudarBtvennogo universitata.
Oolar radiation) (Cosmic rays)

SEVERNTY.. A.B.
Generation of flares with the growth of solar magnetic fieldo, Aotron,
zhur. 38 no.3t402-408 W-je 161. (MM 14:6)
I* Krymakaya astrofizicheskaya observatoriya AN SS&L
(Sun)

AUTHOR:
TITLE:
22107
S/035/61/ooo/oo3/034/048
AOO1/A1O1
-Severnyy,..A.B.
An Investigation ot' magnetic fields connected with flares on the Sun
PERIODICAL: Referativnyy zhurnal. Astronomiya I Geodeziya, no. 3, 1961, 53-54,
abstract 3A455 ("Izv. Krymsk. astrofiz. observ.", 1960, v. 22, 12-
41, Engl. summary)
TEXT-.- The task of this investigation was to check the conclusions arrived
at by the author (RZhAstr,,, 1959, no. 5, 3659) on the origination of flares in
field neutral points and on annihilation of magnetic fields by flares in their vi-
cinities. Twenty records of magnetic fields of active groups'were taken by means
of an essentially improved solar magnetograph (RZhA'str, 1959, no, 8, 61359; 8 of
them provide information only on the location of the flares and 12 enable one, in
addition, to judge on field.changes during flares. Field recording wa5 made in
line)-4886 (Fe I) and sometimes in this line and in the H line. The problem of
calibrating the field of both of these lines is considered. There is a similarity
in the general pattern.of field distribution in H Oand ;~48W, especially above
the groups of sunspots, although noticeable differences are observed in details.
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22107
s/o-i5/6i/oco/oo3/034/o48
An investigation of magnetic fields ... A001/A101
The comparison of location of the main, most intensive flare seats at instants of
their emergence with locations of neutral points, made for 61 cases, shows that in
46 cases flares practically originated in neutral points, In 8 cases differences
in the locations of the flare and the neutral point might be due to errors, and In
7 cases they are beyond the limits of error but may be connected with absence of
knowledge of the field topography and with different altitude of flare formation
from the photosphere. Flares were never observed in the regions of magnetic poles,
or on the neutral line far from the strong crossed fields, The correspondence be-
tween locations of flares and neutral points is improved, if the field is consider-
ed which is recorded in the very nucleus of HP pertaining to the chromosphere, In-
tensity of fields in the chromosphere, in the limits of the active group, is of the
same order as in the photosphere. A comparison of charts of magnetic fields made
prior and after (sometimes also during) flares shows that after flares magnetic
fields are simplified and In the vicinities of flares (neutral points) are annihilat-
ed (individual poles disappear or recess far aside, neutral points disappear), and
field gradient decreases. Field gradients in the flare regions amount usually to
0 Me 4- VeS
from/--jO,02 to 0,1 gauss/km. Bright filaments emerging during devel p n. of fla
tend to align along (or parallel) the neutral lines. An interesting case of or-4;;i-
nating a flare along a closed neutral line is also noted, which is interpreted as
Card 213

22107
S/o35/6i/000/00_3/0,34/048
An investigation oil magnetic fields... AOOl/AlOl
pinch-effect appearing during the breakthrough of a tube of one polarity into the
region of strong field of' the other polarity. Thus the present work confirms all
the main conclusions drawn earlier. There are 10 references,
Author's summary
[Abstracter's note: Complete translation]
Card 3/3

ILI J-1>
22108
-5/0.35/61/000/00)/035/o48
AQ01/A1O1.
AUTHOR: Severnyy, A.B.
TITLE, On non-stationary continuous emission of flares
PERIODICAL: Referativnyy zhurnal. Astronomiya i Geodeziya, no.-3, 1961, 5-4, ab-
stract 3A456 ("Izv. Krymsk. astrofiz. observ.", 1960, v. 22, 67-74,
Engl. summary)
TEXT: The author shows that non-stationary continuous emission of flares
and nuclei of continuous emission can be considered as a long-wave tail cf the
brehmsstrahlung of fast electrons originating near the neutral region (H=C) at
pinch-effect in flares. EAtrapolation of emission distribution energy from the
visible region of the spectrum to the region of X-rays leads to values in agree-
ment with data of rocket measurements. The number of fast electrons necessary
for the observed emission is eatimated (,;,,0.1% of the total electronic density),
and it is shown that if these electrons start from the Sun's atmosphere, their
density at the Earth's surface will be within the limits froml,_~O.j to 102cm-31
There are 7 references. Author' s sum;-mary
[Abstracter's note: Complete translationi
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4 6
/S-;9L Z)
AUTHORS:
TITLE:.
22388
S/035/61/000/005/021/04 2
AOO1/AlO1
aposhnikova, Ye.F.
Severnyy, A.B Sh
Dynamics of limb flares on the Sun and pinch-effect
PERIODICAL: Referativnyy zhurnal. Astronomiya i Geodeziya, no. 5, 1961, 54, ab-
stract 5A356 ("Izv. Krymsk. astrofiz. observ.", 1�60, v. 24, 235
257, Engl. summary)
TEXT- Of 180 H4 pictures of limb flares 25 were selected and 14 of them
were subjected to a detailed quantitative investigation. It has been discovered
that most flares over the disk edge have the appearance of a bright hill (often
with a conical top) the frort side of which rapidly extends and then contracts.
These extensions and contractions are non-uniform (their speed varies from 50 to
600 km/sec); sometimes they have the nature of pulsation C rrespon5 ing accelera-
tions of motion of the front side are very high cm/sec ). There
(5 x 10 10
is an analogy with reverse ejections, although extension of a flare proceeds con-
siderably faster (on an average 3 min). Altitudes.attained by the front side are
no more than 50,000 km, and the brightness is the same as in flares on the disk.
Extending and contracting of a protrusion proceeds practically synchronously with
Card 1/ 2

22388
S/035/61/000/005/02i/042
Dynamics of limb flares on the Sun and pInch-effect A0011AI01
the change in the area of the flare bright region. Cumulativeness of protrusions
is especially characteristic (formation of a conical top or tips), which excludes
the possibility of interpreting the flare as a plain non-cumulative explosion and
its subsequent contraction. It is also shown that the growth of the front separa-
tion from the initial flare nucleus proceeds with time faster than at nuclear ex-
plosions. Simple calculations show that liberation of thermal energy during flares
must amount to rilo3 erg/cm3 see in order to assure observed accelerations on ac-
count of expansion. If this energy arises at the expense of a magnetic field,
then it is sufficient to destroy a field ofr,-.,100 gauss (e.g. at pinch-effect) to
cover these energy losses. Cumulativeness of explosion-like protrusions in flares
and, possibly, motion along the channels can be generally explained by geometry of
crossed magnetic fields surrounding the flare which arises in the neutral point of
such a field as a result of pinch-effect. The high-temperature plasma of the flare
is in these cases in magnetic traps. The plasma tends to get out of the trap or to
expand in directions of least resistance from the surrounding field. Fields of
about 100 gauss are sufficient lest the flare should pass across the field. Cur-
rent arising in a neutral region at pinch-effect is subjected to electrodynamical
acceleration which can attain the observed values at surrounding fields of,_/100
gauss only. There are 14 references. Authors' summary
[Abstracter's note: Complete translation]
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AUTHOR:
TITLE:
22384
S/035/61/000/005/ol7/042
A001/A101
Severnyy, A.B.
Some features of plasma motion in solar magnetic fields
PERIODICAL: Referativnyy zhurnal. Astronomiya i Geodeziya, no. 5, 1961, 53, ab-
stract 5A349 ("Izv. Krymsk. astrofiZ. observ.", 1960, V. 24, 281-
292, Engl. summary)
TM: A magnetic field of about 60 gauss was recorded in the chromosphere
over the disk edge, near a sunspot, by means of a solar magnetograph (in the H~
line); simultaneously were recorded radial velocities in the chromosphere and in-
tensities of the center of the H~ line. The analysis of these records has-shown
,that gases of ~he chromosphere flow into the sunspot approximately along the force
lines. At the same time, records of radial velocities in the sunspot nuclei in-
dicate, as a rule, the flowing of gases from the nucleus. The analysis of simul-
taneous records of the field and radial velocities in the sunspot groups shows
that neutral field points are practically always (in 30 cases out of 37) loca-
ted on the neutral line of the velocity map where radial velocities are oppositely
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2Z384
3/035/61/000/005/017/0112
Some features of plasma motion ... A001/A1O1
directed. It is shown that the concept of fluxes moving towards each other to
the neutral point corresponds statistically to observational results. Some con-
siderations are presented on the field geometry in sunspots and neutral points.
There are 10 references.
Author's summary
[Abstracter's note: Complete translation]
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38809
S/035/62,1000/006/015/064/
AOOI/AIOI
,AUTHORS: B !~?val 1, A. N.
TITLE: investigation of broadening of emission of flare strong lines and
whiskers.I. I
PERIODICAL: Referativnyy zhurnal, Astronomiya i Geodeziya, no. 6, 1962, 55-56,
abstract O'A414 ("Izv. Krymsk. astrofiz. observ,", 1961, v. 26,
3-40, English summary)
T--,',.'f- Profiles of emission wings in whiskers and an-eruptive flare over
the limb are analyzed. It was found that distribution of_~mission in the wings
of %..,hiskers and in the eruptive flare over the limb cannot be explained by the
Stark effect. although in nuclei of strong hydrogen lines-the Stark effect may
play a marked role. Distribution of the form e_'~ AA also does not satisfy the.
observed distribution of emission in the wings of whiskers and eruptive flares;
fair agreement with observations, which is s6metimes obtained, may be due to
poor image quality, tremors of the image in the slit, and low resolving power.
Doppler emission distribution shows good agreement with observations in all
cases considered. The authors discuss the possibility of representing emission
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S/035/62/000/G06/015/064
Investigation of broadening ... AOOI/AIOI
of whiskers and wings of flares as emission arising in a comparatively cold jet
with a constant velocity gradient, which was formed during a contraction or
expansion of a flare. In most cases such a concept agrees with observations U
even better than Doppler effect. Mov,,iment velocities of these jets 300 krq/
sec) turn out to be of the same order as mean observed velocities of extension
and contraction of flares on the limb. In individual cases the best agreemdnt
with observations is shown by Doppler broadening due to macroscopic disorderly
movements at speeds of -1100 km/sec, The analysis of profiles of emission of an
er-aptive flare on the limb presents a rather complicated picture of comparatively
slow movement of the protrusion as a whole and more rapid extension of a region
giving rise to broad emission. Superposition of emission in such a multi-step
movement is fairly well presented by Doppler distribution. the analysis of
ernission of metallic lines warrants the conclusion that it can originate in the
chromospheric region surrounding the "nucleus" of a flare or in a region in
Which originates strongly broadened hydrogen emission. There are 20-references.
Authorts summary
FAbstracter's note: Complete translation]
Card 212

39U5
S/058/62/ooq/oo6/oi6/136
AO61/A1O1
AUTHONS: Severnyy, A. B., Shabanskly, V. P.
TITLE: The mechanism o:r'solar flares and of the gpneration of cosmic
rays in them
PERIODICAL: Referativnyy zhurnal, Fizika, no, 6, 1962, 52, abstract 6B366
("Izv, Krymsk. astrofiz. observ.", 1961, v. 25, 88 - 113, English
summary)
TEXT- The compression of a plasma around the central point of a magnetic
field can be related to the pinch effect arising under free-field ccnditions
when two power tubes (possessing, e.g., a force-free field) are approached and
their azimuthal fields are mutually canceled. The possibility of this kind of
compression in the case of a rapidly changing field of sunspots is considered.
The authors come upon the representation of strong shock waves converging at
t-he neutral point. In the vicinity of the latter (at distances of X4~-- lo7 cm),
the incident shock wave does not appear as hydromagnetic, and its front out-
5trips the motion of the magnetic wall. After reflection in the neutral plane,
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The mechanism of ...
S/058/62/000/0co"/016/136
061/Aiwi
the front of the reflected wave moves about in the compressed plasma, and the
more or less stationary high-temperature region forming behind it draws its
energy from the magnetic energy required for the plasma compression. The front
of the reflected wave, in interacting with the magnetic wall, may slow down or
stop the motion of the latter, so that compression may be replaced by expansion
or pulsations, which is also observed in the flares. Thermonuclear reactions
take place in the hot region behind the flont of the wave reflected from the
neutral point. It is shown that fragments of these reactions (chiefly protons)
with energies of the order of somp mega-electron-volts, being reflected from
the magnetic walls converging tc t~a neutral point, are accelerated to energies
of - 10 Bev.
LAbstracterts note: Complete translation]
1,
"ard ?,/2

MUSTELI, Evalld Rudollfovich; GELIFGAT, B.Ye., red.; AMBAMSUKYAN, V.A.,
red._;_~~~B ,red.; SOBCLEV, Y.V., red.; KRYUCHKOVA,
V.H., tekhn.red.
[stellar atmospheres] Zvezdnya atmosfery. Red.kollegiia:
V.A.Ambartsumian i dr. Moskva, Gos.izd-vo fiziko-matem.
lit-ry, 196o. 444 p. MiRA 14:2)
(Stars--Atmospheres)

99VEM, A. B., SHAPOSHNIKOVA, Ye. F.
"The Dynamic of Limb-Flares and Pinch-Effect."
Izv. Krym. Astrofiz. Obser, v 25 f-11144-5
VM" jj~~OQJ.
The H -film of 14 limb-flares are measured. It was found that in most of the
casesll~imb-flares appear in the form of brilliant hill wLth conical top, which
undergoes to dilatations and contractions.
The Vsations sometimes were observed, The velocities :)f dilatations are up to
and accelerations reach 10'-'-100 cm 2.
450 Stre sec
The formation of cone like top of flare is explained by the geometry of crossed
magnetic fields (cusped field geometry) surrounding a flare which appears in
neutral point of such a field as result of pinch-effect.

35076
b./7j 12 '60/023/000/01, 0/014
is -
D
2 X-5 01
Sevcrr1yy,_ .1. B.
TI T L -E' An eqt-imate o1' the ultraviolet emission of solar flares
in the resonance lines L , He I anI He II
jOURCE: nauk SSSR. Xrymskaya zistrofizicheskaya obser-
VUtJriya. IZVeStiyL, v. 23. N,Oocow, 1960, 311-321
T T Continuing earlier work the author givas calculations of the
0
-d intensities of the above three Lines. It is estima-
profiles all I
t-ed that the intensity of radiation in the th:_-ee lines at the boun-
dary of t1,.e atmosphere is as follows: (ergs/cn2 sec)
Tem-D. of flare Hle I,/~584 He II, A304 H, 41215
10,000 2.9 x 10-10 0 0.11
25,000 5.8 x 10-4 -0.1 5.5
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:)~0/023/000/010/014
S/7 ly
.,',,n estim:,.te of . . . D218 301
The -eieral conclusion is -LIhat an a~~,preciablE increase in the radi-
ation emitted by the sun in the region ~~klOO-121522 can only be ex-
Pee-L,ed in the L radiation of hydrogen and the /1304 he II line
duri),11:1.- the aj.)earance of flares of importanec. -reater or equal to
2 and occupying a considerable area. This rac.iation is variable:
C,
Ln L it :,ay continue throuSI-out t1le lifetimu of the flare (4
1 5) and it" is probable that it occurs !ai-;h a certain delay re-
lative -,lo t-l,e F, . Secondly, in theA304 line the radiation is most
a_
ol,obably eL-iitted durin.- thie "lash phase, whell., 'the emission in the
helium lineo is at its maximum (duration -10'). The increase in
'U'-,-,e emission in -he 130i-, line, which is ind-I.,ated in -'U-he table, is
very mucIi -reater than the normal level of t'iis emission from. the
solar corona. Accordin;, to G. 'E'lwert it shouLd not be more t-han.
U
10-2 e-z/c-.12 sec. The present results are saLd to be consistent
aith r,)cket experJments reported by E. Tousef. There are 4 figures,
Car~- 2/3

I S/712/60/023/000/010/014
i%.Ti eot-i'mate of ... - D218/D301
4 tables and 12 references: 5 Soviet-bloc, and 7 non-Soviet-bloc.
Th,e referenice to the En-lish-language publication reads as follows:
tz) - 0
C. 7,1.kllen, Astrophysical Quantities, 1955, Univ. of Lond6n, �28.
SUBEITTIS'D: April, 1959
Lk
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- SEMNf Y,..A. 6 -
Solar physics. IUn.tekh. 4 no-3:14-18 Mr 160.
(MIRA 13:6)
- I
1. Direktor Krymskoy ob-servatorii, chlen-korrespondent AN SSSR.
. (S=) ,
I

SEVERNYY, Andrey B.
,1,
tt&port of the Crimean Astrophysical Observatory:
(1) Spaceship satellite investigation of the helium
,-k-304 line emission on the sun, and (2) Radiation
danger of solar flares and methods of its prediction"
report to be submitted to the 13th Intl. Astronautical Congress, IAF,
Varna, Bulgaria, 23-29 Sep 1962.

3 09,
S/033/62/039/002/011/01'k
E032/E314
AUTHORS: Butslov, M.M., Kopylov, I.M., Nikonov, V.B.,
Severnyy, A.B. and Chuvayev, K.K.
TITLE: Experiments in electron-optical photography of
galaxies in hydrogen light using the 2.6 m
reflector of the Crimean Astrophysical Observatory
Pr-RIODICAL: Astronomicheskiy zhurnal, 4. 39, no. 2, 1962,-
315 - 322 + 3 plates
T&XT: Detailed studies of extragalactic nebulae require
t4e use of large telescopes. As regards detecting apparatus,
the use of ordinary photographic techniques in conjunction with
narrow-band filters necessitates long exposures and is therefore
inconvenient in practice. The authors have investigated
therefore the possibilities of image-converters as a means of
avoiding these disadvantages. An image-converter was set up
-in the direct focus of the 2.6 m reflector of the Crimean
Astrophysical Observatory. The immediate object was to investi-
gate the hydrogen emission in a number of galaxies. Four'. light
colour filters were introduced in front of the converter and
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S/033/62/039/oo2/011/014
Experiments in electron-optical ... E032/r..,.314
the screen of the latter was photographed by a motion-picture
camera. Altogether 58 galaxies were photographed in N
a
and other light. Photographs of 10 of these are reprodlLced
and their features are described (Ncc 6o4, .1-569, 4214, 44119,
4490, 4736, 5194, 5457, 6822 and 6946). Many un1mown clouds
of hydrogen- emission -wrere detected in the galaxies. In many
cases there is no correspondence between hot-star clusters and
:,3-drogen clouds. The hydrogen component shows greater conccn-
tration in the equatorial planes than the stellar component.
In some galaxies the nuclei consist of isolated condensations.
The dimensions of the nuclei in H light are in some cases
a
appreciably largerthan in other light, although in a number of
cases the reverse situation obtains. In sereral galaxie.~3,
streams or ejectibns from the nucletis, which are visible only
in H a light, were detected.
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........ SEVERNYY A.B.
Some characteristics of mkgnetic fields comected with
solar flares. Astron.zhur. 39 no.6:961-964 N-D- !62.(MIR-A 15:11)
2. Krymskaya astrofizicheskaya observatoriya MI SSSR.
(Magneti# fieldo 4Cosmic physics))
(Sul)

43545
S/033/62/039/006/008/024
E032/E414
AUTHOR: Severnzy, A.B.
TITLE; Instability or a layer of plasma with a netitrn]
magnetic field point
PERIODICAL: Astronomicheskiy zhurnal, v.391 no.6, 1962, 990-995
TEXT: It is noted that there.nre two hypotheses as regnrds the
generation of flares, namely the flares appear spontaneously as a
result of the instability of:a free fj.dId frozen into the solar
plasma, or they appear as n-result of the effect of external
fields. e.g. sunspot fields, which give rise to a contraction of
the plasma. In order to throw further 1-ight on these mechanisms,
the author considers the stability of a plane-parallel plasma layer
lying between the planes x = -xo and x = +xo in which the
field increases linearly with distance from the x = 0 plane at
which H = 0. It is assumed that the density and pressure insid6
the layer are symmetric functions of x and the space outside the
layer is evacuated. The conductivity is assumed to be infinite,
the displacement current is neglected and the line of force are
assumed to be straight and parallel during the motion. The Euler
equations for small displacements are solved and it is shown that
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S /0 3 3/62/039A)06/008/o2 4
Instability of a layer ... 1`1032/E414
instability can appear if the exterrial fie'ld decreases with
distan6e from the layer. The above three restricting AssumRtions
are then relaxed and the analysis is repeated in the case where
the field. the pressure and the densityinside the plasma layer
are of the form
H 11 x P X2
y 0 1 P P0 ir -z
x X-
0 0
while the field outside the plasina is fly = const flo.
It is shown that this type of layer is unstable. It is argued that
the stability considerations r eported by S.I.Syrovatskiy
(Astronomichesiciy zhtirnal, v.39, no.6, 1962, 987-989) are
incorrect owing to an incorrect formulation of the problem and
unacceptable assumptions. There are 2 figures.
ASSOCIATION: Krymskaya astrofizicheskaya observatoriya AN SSSR
(Crimean Astrophysical Observatory AS USSR)
SUBMITTED: July 5, 1962
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GURZAIJYAN, Grigor Ararrovich; AINBARTSTUWAN, V.A., red.; MUSTELI, E.R.,
red.; SEVERITYY, A.B., red,; SOBOLEV, V,V., red.; KULIKOV,
G. S. , re-&.-;-- bRUD I -K, tekhn. red.
[Planetary nebulae]PI-enetarnye tumannosti. Moskva., Gos.izd-vo
fiziko-matem.li-t--ry, 1962. 384 P. (MIRA 15:9)
(Nebulae) I.

45123
S/712/62/027/000/003/015'
1. 0 A001A'01
AUTHORS: Babin, A. I., Luk'yanov, S. Yu.,. Severnyy., A. B., Sidorov, G. G.0
Sinitsyn,'V. I., Steshenko, N. V.--
TITLE; An investigation of hydrogen lines broadening in a powerful pulse
discharge
ms
SOURCE: Akademiya n4uk SSSR. Kry kaya astrofizicheskaya observatoriya.
Izvestiya, ~,. 27, 1962, 52 - 70
TEXT-. Emission hydrogen spectrum of solar flares shows a great similarity.
with the spectrum of high-temperature hydrogen plasma glowing in a pulse dis-
cha~ge of high intensity. Therefore, the latter spectrum was investigated in
thepresent study by methods used in studying physi cal processes on the Sun. At
first the problem of broadening of hydrogen emission is 0onsidered. The-equip-
ment used and the methods of carrying out measurements a~e described in detail.
Discharge was studied with the aid of a spectrograph with a diffraction echelle-
grating (dispersion nil.5 R/mm). The main results of the spectrophotometric
study of broadening of hydrogen emission (H.,, - H
wings are as follows: 1) The
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S/712/62/027/000/003/015
An investigation of hydrogen lirie~... 'A001/A101
emission of hydrogen line wings"(extending to 30- 40 when observed in the
spectra of a self-constricted pinbh perpendicular in direction, turns out to be
broadened due mainly to the linear Stark-effect (at the initial pressure po
= 0.1 mm Hg); 2) at po = 0.5 mm Hg the emission extends to 50 - 80 R and is
broadened in the wing, probably-due mainly to the quadratic Stark-effect;
3) when the spectra are observed along the plasma pinch, the broadening of hydro-
gen emission in the wings of the lines is 8due to macrosoopic motions of the
plasma with velocities of the order of 10 cm/sec. The intemity variations in
the wings are well explained by the hypothesis on the jet-type plasma motion
directed along the discharge axis with velocity gradients; 4) when the spectra
are observed outside the axis of discharge, the broadening of hydrogen emission
(at po = 0.1 mm Hg) Is entirely due to the linear Stark-effect in both trans-
versal and longitudinal direction (next to the-pinch). The mechanism of hydro-
gen emission broadening in a powerful discharge is similar to broadening of emis-
sion lines of solar flares. The variation of intensity in the line wings de-
pends essentially on the direction along which the spee-;:r= of plasma emission
is observed. It is concluded that the analogy between the powerful.pulse dis-
charges in laboratory conditions and the phenomenon of chromospheric flares on
Card 2/~

S/'[12/62/027/000/003/015
An investigation of hydrogen lines... A001/A101
the Sun, is based on the close physical essence of both phenomena. There are
12 figures and 2 tables.
SUBMITTED: may 1961
-ard 3/3

45124
S/712/62/027/000/004/015
AOO1AlOl
AUTHOR: -tseverpy_v~ A. B.
TITLE: Nonstationary processes in solar magnetia fields (The generation of~.
flares, heating of faculae)
SOURCE: Akademiya nauk SSSR. Krypskaya astrofiziches,kaya obse~vatoriya.
Izvestiya. v. 27, 1962, 71 - 109
TEXT: The present article is a continuation of the author's studies of
magnetic fields related to flares, carried out in 1958. The initial concept of
generation of solar flares is complemented with an.investigation of slow pro-
cesses of heating and contraction of the solar plasma,'which are of importance
for the explanation of solar faculae. The studies of magnetic fields related to
solar flares show that the latter arise where magnetic polarity changes its-
sign. The observational data indicate that the surrounding field changes in in-
tensity, gradient and magnetic hills from the sta.~ preceding the flare to that
following it, although in the region of flares proper no appreciable changes are
observed. The changes ofthe surrounding field proceed sometimes very rapidly.
Card 1/4

S/712/62/02227/000/0041/015
Nonstationary processes in... A001/A101
The data of 1~, films and spectra of limb flares show the rapid formation of cu-
mulative jets with some gradient of velocity along the jet. The equation of in-
tensity distribution in the contour of the lines looks as follows:
I (4~ in' (1.2)
X
where Ck is some constant, and n?~m Is the full width of the wing. The picture
of spectral lines broadening during the magnetic contractionlof the plasma de-
pends essentially on the direction along which the plasma is being observed.
The author analyzes the mechanism of magnetic contraction of the solar plasma
leading to the phenomenon of flare, which he calls automodel. contraction, assum-
Ing magnetic fields to be frozen-in into the plasma. Solving the equations for
the automodel contraction, the author estimates the time of contraction to be of-
the order of 3 hours and considers it to be applicable to photospheric layers.
The next problem is consideration of rapid contraction process resulting from
the growth of the external magnetic field (flare). The solution of equations of
magnetic contraction is represented in Figure 5 which shows the origination of
pulsations. The author concludes that even comparatively slow changes in the
Card 2A

S/712/62/027/000/004/015
Nonstationary processes in... AOOI/AlO1
field of sunspots may lead to very rapid and intensive contraction and subsequent
pulsations during the times comparable with the time of flare formation. This
can lead to generation of shock waves converging to the~neutral point and produc-
ing considerable heating of plasma. Shock waves arige :.f the initial dimensions.
of the condensation are sufficiently large (> 5 x 10 cm); however, if the ini-
tial rate of the magnetic field growth.is high (- 0.1 gauss/seg), a*contraction
takes place even at small dimensions,of the condensation (- 10 cm). the last
problem considered is the slow growth*of the external maigietic field and proces-
ses related to it. The process of automodel contraction is analyzed with ohmic
losses taken into account, and it is shown that the latter are of importance in
the slow heating of faculae. The initial dimensions of condensations do. prac-
tically,coincide with the characteristic dimension .(^jIOO km) of emission nuclei
arising in the photosphere and showing characteristic spectral features (nuclei
of the faculae fine structure). The heating of condensations due to Joule losses
leads to a strong ionization of hydrogen. The existence of heated condensations
has been confirmed by both studies of the solar radio emission and studies of its
ultraviolet spectrum. There are 6 figures.
SUBMITTED: April 1961
Card 3A

3/712/62/027/000/004/015
Nonstationary processes in... A001/A101
F'igure 5. Approximate (dotted line) and exact (dots) solutions of the magnetic
contraction equation
.............
'Na
Card 4/4

S/712/62/028/000/007/020
E,032/E314
AUTHORS: Stepanov, B.Ye. and Severnyy, A.B.
TITLE: Photoelectric method ?io-r -measurili-gthe magnitude and
direction of the magnetic field on the solar surface
SOURCE: Akademiya nauk SSSR. Krymskaya astrofizicheskaya.
observatoriya. Izvestiya- v. 23. 1962. 166-193
TEXT; The aim of this work was to develop a photoelectric
Method of measuring the magnitude and direction of the magnetic
field, the direction being characterized by the angle between the
field vector and the line of sight y and the azimuth of the
transverse component of the field A search for this method
Was begun in 1958 and the developmeYrt was completed in 1959-
Since then, the method has been.used to record the fields in
active regions and a preliminary description of it was given in a
previous paper (A.B. Severnyy - Trans. IAU, 11-13, 1961 (in press)),.
The method is being used with the magnetograph.of the Krymskaya
astrofizicheskaya observatoriya. (Crimean Astrophysical Observatory)'.
+ X/4 modulation'is-employed-in measurements of the longitudinal. i
Yield and the photocurrents due to oscillations in the intensity
Card 1/3

S/712/62/028/000/007/020
Photoelectric method .... E032/E314
of "I', and "12 components at the two slits of the photometer
are subtracted. In measuring the transverse magnetic field a
0, X/2 modulation is used (ADP crystal.plus quartz X/4 plate) and
thetfo Photocurrents are added. The azimuth of the transverse
field is determined by recording the signals with the quartz X/4
0
plate in two positions separated by an angular distance of 45
In order to determine the relation between the signals and y,
the electrical oscillations for a magnetically split line are
resolved into two mutually perpendicular oscillations so that their
intensities can be added within the limits of an optically thick
absorption line, and the blending and interaction between differen-'
tly polarized a, and -Tr components can be taken into account.
Calculations used in the interpretation of the data were reported
in earlier papers (V.Ye. Stepanov - Izv.Krymskoy astrofiz. obs.,
19, 20, 1958; 18, 136, 1958). A method is described for the
calibration of the apparatus with the aid of a special magnet.
The noise level corresponds to about 100 Oe in measurements of
transverse fields, so that the method cannot be used for regions
with- very low fields (H 4t~ 100 Oe).' The noise level for the
Card 2/3

S/712/62/028/000/007/020
Photoelectric method E032/E314
longitudinal component is about 1 Oe. Charts showing magnetic-field
distributions in active regions are reproduced. The magnetic-
field charts reveal an eddy structure in some cases. The spiral
structure of Iij shows that apart from the azimuthal component
H there is a'rso a radial component H This indicates that the
Anspot field differs from a force-free field with cylindrical.
symmetry. Further studies designed to obtain more detailed
information will be concerned with the variation in the field with
height. There are 14 figures and 1 table.
SU13MITTED: December 20, 1961
;Card 3/3

SEVERNTY, A. B.
"Solar magnetic field.*
Report submitted to the Symposium on Results of the IGY-IGC (Intl.
Geopbysical Year) Los Angeles, California 12-16 Aug 1963

GOPAS-YUK, S.I.; OGIRI, M.B.; SEVERM, A.B.; SHAPOSHNIKOVA, Ye.F.
Structure of solar magnetic fields and its variations in flare
regions. Izv. Krym. astrofiz. obser. 29:15-67 163. (~ffRA 16:1o)

YLADIMIRSKIYP B.M.; SEVERIM, A.B.
--. I...
Nuclear processes in chromospheric flares. Izv. Lrym. astrofiz.
obser. 29:80-85 163. (MIRA 16:10)

NOCESSION NR: Azj,cj',lfjl5
J%V I
S/0269/6h/000/,D02/0058/0058
SOURCE: RZh. Astronomiya, Abs. 2.51-414
AUTHOR: Severny*yp A. Be
TITLE: DistribuLion of atrong flares in the magnetic fields of spot groups
CITEM SOUhCS: Izv. Kry*msk. astrofiz. obsery. v- 30.. 1963~- 161-164
TOPIC TAGS: sun, solar activity., chromospheric flare, solar magnetic field,
cosmic ray, astronomical modeling., solar filament., magnetic field neutral point
astronomy
TRANSLATION: A study was made of 15 very large (with cosmic ray effect) flares'
at, the Dhase of their maximum development relative to magnetic fields. All avai-1-
able data on magnetic fields, both.ordinary determinations of the absolute field
from the spectruia and isogauss maps obtained for eight cases using the Crimean
magnetograph, were used for this purpose. The position of most of the flares was
determired from HIX films from the Crimea. Laboratory modeling of the transverse
Card 1/2

ACCESSION NR: AM021615
field by the H, method, described earlier (see RZhAstrj, 1964j, 1*51-418)p was car-
ried out for each flare. Asymptotes (lines passing through the neutral point and
like poles) were drawn. The filaments of flares were oriented in the magnetic
field either aloni; '01-D mentioned asymptotes or along the neutral line of the
longitudinal field, or parallel to these lines. This property is expressed the
more clearly the g-reater the field gradient across the mentioned lines. The fila-
ments of 'flares deviate appreciably from the neutral lines in the region of weak
fields. The cited data indicate that the filaments of flares always pass through
the neutral point of transverse field of the model. Neutral points can appear
a". the centers of spots (even over the center itself) md also over the region of
a strong transverse field. In the case of eight large flares observed in the
Crimea there was no observable separation of one filament into two parallel fila-
Prents, as reported by certain investigators -(,4ZhAstr., 1962,, 101389). Bibliography
of 10 items. Author's abstract.
DATE ACQ: SUB CODE: AS ENGL: 00
Card 2/2

KAPLAN, Samuil Aronovich; PIKELUTER, Solomon Borisovich;
AMBARTSUMYAN, V.A., red.; MUSTEL', E.R.,' red.; SEVERNYY,
A.B.,- red.; SOBOLINX, V.V., red.; K1JLIKOV,
AKSELIROD) I.Sh-j tekhn. red.
[Interstellar medium] Mezhzvezdnaia sreda. Moskva, Fiz-
matgiz, 1963. 531 P. (MIRA 17:2)

GORBATSKIY, V.G.; MININ, I.N.; ; AMBARTSUMYAN, V.A., red.; BUSTELI,
E.R., red.; UVERNYY, A.B., red.; SOBOLEV, V.V.j red.;
KULIKOVY G.S.,--r-er.-;-HSELIROD, I.Sh., tekhn. red.
[Nonstable stars] Nestatsionarnye zvezdy. Moskva, Fizmatgiz,
1963. 355 P. (MIRA 16:4)
(Stars, Variable)

SEVERNYY9 A.B.
Sun Flares and Magnetic Fields.
Reports of the following Soviet Scientists were presented at the
XII!th International t~ongress on Astronautics in Varna.,
Bulgaria,
P: Tekhnika Molodezbij #1, 19639 pp.24-25

7 7 _~--

65 W (l)/9WG(v)/EEC-4/EBC(t) Pe-~/Pq-4
SS
L 85~22 (1upkt-
-TESD(t)/'RAM(t) GW
ACCESSION ITR: AP4046586 S100301641 21 ("7
AUTHOR: Sevemy*y, A. B. tCorresponding member AN SSSP.)
12~
T IT LE: rnvestigations of the magnetic fields on the MM

SOURCE: AN 3SSR. Vestnik, no. 9, 1964, 62-67
TOPIC TAGS.- sun, magnetic field, Zeeman-effect

ABSTRACT: The author outlines the history of discovery- and investigation of the
sun s mwpetic fields. He points out thatf despite numerous studies the subject -i~* -~'.,'----;
still one of the nost enigmatic of cosmic plWsics* Such studies were begun at the
Kry-rmskaya astrofizicheskaya observatoriya Akadenii Nauk SSSR (Crimean Astrophysical
O'h9ervatory of the Academy of Sciences SSSR) in 1954. Attention was first focused
on strong magnatia fields concentrated chiefly in sun spots, and photographs were
made of the Zeeman effect on spectra of the spots and neighboring regions. The
study of w~--ak fields was begun in 1956 by means of the Photoeleotria method. This
iqe.thod is describ,id briefly. The author states that the possibility of measuring -4
both longitudinal and transverse aomponents of the field and the position of the
field vector in space was first realized by V. Ye. Stepanov and A. B. Severny*-y in
191 ". Inhomogeneities in the field, particularly transverse fields wi Vain the major
field oil a sun spot, have been oonfirmai by several investigatiinso k strong
Card 112
NFL, ..7'77 77

1W
F4,
L 8529-65
:ACCESSION NR: AP4046586
o'
- ting to., 0 and,
Totation of the magnetic vector has*been observed with depthi. amoun 9
more at depths of 100 km. Studies of flares (of 1957) in comparison with maps
magnetic fields indicate that the position of the flares cannot be related to
over points of differently oriented fields. An interesting point is that the
strongest changes in a magnetic field are observed in flares that generate co a
rays. bbiiating dat-a on the value and direction of the magnetic field permit e
mination of the nature of the electrical currents. But the existence of cantr
currents is difficult to explain on the view of a stationaryj long--4ived
syste
This needs further study. Another problem is the difference in properties of
magnetic and normagnetic segments of the sun and,: in-particulart-differenced
chemical composition of these zones. This relation should be compar Ied..with the
known fact that magrietia-variable stars change chemical composition- with change~in
map
,Tiptic field. Orig. art. hass 2 figures.
ASSOCIATION: Kry-*mskaya astrofizicheskaya observAtoriya Akademii xi"k SSSR
(Crimean AstropIxygical Observatoaj Academy of Scieftces SSSR):
LJUBMITTEDt 00
MGM 00,--
SUB GODE: AA NO REP SOVt 000 011MC 000 "i
Card 21 12

61002-6-~ L
ACCESSION NR. AP5010424 UR/0033/65/042/002/0217/0232 Q 17 T
523.745
AUTHOR: Severnyy, A B
TITLE: The nature of golar%agnetic fields (Lbe fine 'structure of the field)
SOURCE: Astronomicheskiy zhurnal, v. 42, no.,2, 1966, 217-232 A4
TOPIC TAGS: solar magnetic field, solar surface oscillation, sunspot magnetic field,
sunspot
ABSTRACT: An Investigation Is made of the fine structure of strong solar magnetic fields
obtained at high resolving power. Detailed treatment is given to 1) the appearance of a
purely transverse field wi0ft regions of strong longitudinal 1111 unipolar fields, 2) the
appearance of field peaks 2-511 in size; 3) strong rotations of the transverse field vectors
at the surface and through the depth of solar atmosphere; 4) the concentration of field
lines from the spots into separate radially emerging bands; 5) the joining (with spots) of
H /) z region of opposite polarity; and 6) the convection with sunspots. The non-
coincidence of Evershed motions vAth the lines of force of the spot fields seem to indicate
a possible iefiltration of gases Into the intervals between the Inmches where the field is

type fields, but on the other side the twisting, fine structure . H; remini cent of forbe-
free fields. The general solar magnetic field which is characterized by the absence of
any uniform coherent polar fields is also discussed. A comprehensive descriptioa of
the general micropattern is given including the appearance of "higher modes" in one or
two octaves in characteristic lengths of elements of the general field which seem to
provide evidence of peculiar oscillations of the solar surface. Orig. art. has: 5
formulas, 13 figures, and I table.
A
ASSOCIATION: Krymskaya astrofiziches1mys observatoriya Akaden7di nauk SM (Crimeaq

L OQ730-67 EWT(l) GW
ACC NR. AP6019666
AUTHOR: Severra7t A. B. 1
ORG.- qrimean Astrophygi Observato=9 Acadegq of Sciences SSM (Krymskays, 10
astrofizicheakaya observatoriya 40
Lkademii nauk SSSR)
TITLE: Magnetic fields at various depths of the solar atmosphere
SOURCE: ABtronomicheskiy zhurnal, v. 43p no- 3, 1966, 465-479
TOPIC TAGS: magnetic field, solar atmospheret chromosphere, photosphere,
astrophyaics, hydrogen, spectroscopy
ABSTRACTz Measurements of the chromospheric magnetic fields in the H, and XCa' lines
are reviewed and are shown to be misleading. In fact, the blending of the H9 -lines, Vj
with magnetic lines may pertain to fields in the photosphe-re rather than in the
chromosphere.' The author contends that H. lines will be more suitable for measure-: i
ments of chromospherio fields. To this end, the double magaetograph of the Crimean
Astrophysical Observatory is described. This installation permits the simultaneous
recording of the magnetic field in any two lines. ~Extensive amounts of data obtained!
by this magnetograph seem to repeat all the features of tha photospheric magnetic
field at the chromospherio level. Cases of anomalous appearimce of fields of F_
Card 112

L 00730--67
ACC NR: AP6019666
opposite sign in the chromosphere are discuseed,-and the appearance of small loop-
tubes of lines of force in the photosphere is noted. The direction of the field in
the photosphere is found to be opposite to the chromospherie fieldep leading to
possible contact between fields of opposite directions. Aiso noted is the presence
of isolated fields of z-ae sign only at the intermediate letrel of A - 6102.7 between
9L = 5250 and k -lineb. This factq-plus the appearance of zigsage in the Tr-
component of some spots, is considered to be evidence of the very fine structure of
solar magnetic fields. The author expresses his thanks to N. S. Nikalin, G. A.
S. 1. Gopasy , and T. T. Tsap for their part.in constructing and running the
magnetograph. Orig. art. has:-13 figures and 1 table.
SUB CODE: 20, 03/ SUBM DATEt 28jan66/ ORIG REP: 013/ OM REP: 004:
Card 2/2,~~

-- A.B.
I --
Experimental investigation of the effects of rotation of the Folar-
ization 11ane and of the nonmagnetic polarization on the sun. Izv.
Krym. astrofiz. obser. 31:126-158 164.
Obiervations of tvansversal and longitudinal magnetic fielas coninecte~i
with solar flares. Ibid.:159-199 164. 17.9).

r
I
C
ACC NR:
EWT(l) GW
AUIMOR: Severnyy, A. B.
TITLE: Studies of the rotation of a magnetic field withid,6~th in the
,Solar tmosphere
SOURCE, Ref. zh. Astronomiya, Abs, 8,51-.442
SOURCE: Izv. Krwsk, astrofiz, obser ,.*v. 33, 1965,*3-33
TOPIC TAGS: astronomic data, solar atmosphere, solar magnetic field,
rotating magnetic field
ABSTRACT: A deduction previously made by the author (RZhAstr, 1964,
10.51-367) on the rotation of a polarization plane with depth in the
Solar atmosphere is subjected to verification. For this purpose
records of the transverse mag
,netie field were taken on the magneto-
,graph in three lines of different powers: "5302P 5250, and 4808;
for checking the possible rotation of a polarization plane, a record
was.later taken again in the original line (usually the x5250).
Studies of the records and maps of lateral oscillations of the a
vector showed a strong rotation effect in the transition from one line
to another, which was analogous to the effect described earlier. In
the majority of cases the effect of the rotation of the vector
uDc -. 523.,76

'AH601339'7 S.OURCE-CODE t~/&69/65/obq/01-1/0046/6471!
AUTHORS: Bruns, A. -V.-.; Nikulin, N. S.; Sg~~j. A. B.
TITLE: New method for simultaneous recording of the transverse magnetic field
parameters
SOMRCE: Ref. zh. Astronomiya, Abs. -11-51-412
Rai-e SOURCE: Izv. Kr,
astrofiz. ob V., v. 33, 1965, 80-85
TAG3: 'so ar magnetic, field, transverse otic field, etic fi-ld
magn mam r-
;j3S'-`1-kr-T - A Taetiiod is describod which allows the simultaneous recordin- ;)-P both
--,,npoue~As of thf,. transverfie fiela tind the direct recordin-~ of the trrLn3verse vibra-
ojoa r-~ZimJLII x on P- st'rip ch,-~rt by reprocessing the signals. This is arcom-plished
,Lcin- in frouL of the eriLrance slit of the upectroar-aph a plane pola-iz ti'017,
the lollo-11--Lng :r.3-ru-ter- A compoitnd plate o
Z1.4,1ILL er marto :Ln f two quarter--tave. plates
-;-1050
- , na~-v, ,roo-j ,,, 45o i,,j placed in front of an ordinar-j ei-,cular pularizati.or,
Ll-nalyzer consi!j(dng of art amrjouiuz phosphate cryst-P.1 and a polarGid. I'he -,:,'Late mount
L3 the armat-ure (,.C a polarized rolay- to which is qnprlied a 20-hz voltage from an
audio ooo-L.1-latur, Thu.,-, tht, at-tt-'It- between the extraordina-T-j axJE3 oC thq qunxter-wave
.L
1.11- p.-in-1pal axiij of the crystal alternately ta1ces the values 00 or
Is. To calcula.Le the vibrati ii
cacd ntc; 522.61

SEVEIMY) A.B.
-
S',-u.-dy -)r solar mgnc+i~ f-leads. V,-s4-. :,N SSSR 34 no.0162--~? S 164.
(KIRA 17:10)
J. asLrofiz-lcbesl:aya observatc-r-1-ya AN SSSR; Chlen-lkorres-
ponde.m. All SSSR.

L-06357-67 On (1) GW'
ACC NR, U1601339_6___ ___SOURCf
65/00T/61-1/0047/00471
AUTHOR:. , Severnyy, A. B.
TITLE: Investigation of the magnetic field and electric currents of unipolar ourspots!
SOURCE: Ref. zh. Astronomiya, Abs. 11-51-416 . 'q 9'
16
REF SOURCE: Izv. Krymsk. astrofiz. observ., V. 33, 1965, 34-79
\Y
TOPIC TAGS: solar magnetic field, sunspot, transverse magnetic field, longitudinal
magnetic field, magnetic field measurement
ABSTRACT: The transverse and longitudinal magnetic fields for a number of unipolar
groups, recorded on the Crimean solar magnetojraphj?~xe analyzed. A method of
calibrating the transverse field by comparing the magnetograph readings with photo-
graphic measurements is suggested. It is noted that the vortex structure of the
transverse field recorded in group No- 53 from 8 through 16 July 1962 is a rare
phenomenon; fluctuations of curvature of the vortex spirals reflecting the bydro-
dynamic torsional oscillations move quickly. Thetfield of unipolar spots is con-
centrated primarily in ropes proceeding from the spot outwards. The appearance cf
strong Iransverse fields inside spots is again noted. The values of the total field
vector H and its inclination to the vertical Y are calculated for two groups.
Analysis of the variation of -1 and I'HI with distance from the spot center shows a
I slower change of these quantities than found at Mount Wilson observatory and than
,Lcord 1/2 UDC: 523-7461

L 39743-66 EWT (1) GW/GD-2
AM IV: U6005464 SOURCE CODE: UR/0053/66/088/001/0003/0050
AUTHOR: Sever 992, A* Bo
ORG: Crimean Astrophysics Observatory, AN SSSR (Krymskaya astrofizicheskaya
observatoriya AN SSSR)
TITM: ~Iagnotic fiolds of the sun and stars
~ ,- SA,
SOURCE: Uspekhi. fizichesk:Lkh nauk, V. 88, no.' 1, 1966, 3-50
TOPIC TAGS: solar magnetic field, sunspot, transverse magnetic field, spectral
line, Doppler effect, stellar astronovV, solar activity, magnetic field, magnetic
field intensity, solar photosphere, solar atmosphere
ABSTRACT - ~After G. E. Hale discovered Zeeman fission in Fraunhofer
linc~'-O`f sunspot spectra, the problem arose of the existence of magnetic 1
;fields on the sun and stars. Although much research has been devoted to 1
4 1
this- problem,..the nature of solar and stellar magnetic fields has not. been,
thoroughly investigated. Many hypotheses have been developed, but
.none of them can explain these phenomena in detail. The stellar mag-
netic field must be stable. because of high temperatures and good plasma
Card 1/7 UDC: 52 13-638

AC AP600YP641,
conductivity. Observations prove a variable stellar field with a sudden'
change in stellar plasma. Stellar magnetic fields of the intensity of i
34 kgs have been found.
The field intensity can be measured by the magnetic fission of
''spectral lines of the wavelength x using the formula
-MI9I)t
(M297.
C
where H is the positive or negative field intensity, m represents the
magnetic quanta numbers of the upper and lower levels which may
change their sign, and g is the Lande's factor for each level. When
the field direction is inclined to the sight line under an angle Y, the
triplet components al 02 7r can be determined using the formulas
a,=- -Cos 2, x--isinty,
4
02
4 +COS
Card 2/7
a;
4

L 39743-66
Acc im: Ap6oo5464
Figure I shows the change of the components of the triplet under the',
action of the magnetic field.
Fig. 1. Relative intensi-
ties of components a,, r,
and uz, depending upon the
angle y.
Solar magr'ietograms of-the Institute of Terrestrial &agnetism, Iono-
sphere, and Propagation of Radio Waves at Moscow contain records of
Ahe hydrogen line H from selected solar regions which make it pos7
a
sible to investigate the magnetic field.of this re-aion in detail.
Card 3/7

L 32743-66
ACC IIR: AP6005464
According to Hale's and Babcock's investigations, the solar
magnetic field has variable changing polarities and, sometimes, loses
its intensity for longer or shorter periods. Measurements at Cambridge
i land the Crimean Astrophysical Observatory showed that no magnetic
ield could be found at the solar South Pole during the period 1961-196.4
t the same time a negative magnetic field was recorded at the North
,A
Pole. Changes of the polar field were recorded in 1927 and 1937. There
is some time coincidence between the change of polarity of the solar mag-
netic field and the maximum *of solar activity. The minimum activity
oincides with the maximum phase of -positive or negative fields.
The fine structure of the solar magnetic field was investigated
by A. B. Severnyy. Statistical data show that observations with an
instrument of low resolution found a weak magnetic field, and an increase.
of the instrument resolution revealed an increase in the total field. Uni-
polar regions on the sun became multipolar when the instrument resolu-
tion was increased. Histograms. of 'statistical data show the intensity andi
polarity at the North and South Poles of the sun during the first half of
1964. South polarity was predominant at the North Pole of the sun, and
no polarity was evident -at the-So,uth . Pole.-,.
Card 4/7

L 39743-V)
kcc niR: Ap6ooy~&
A strict dividing line between a sunspot and the photosphere and
between the umbra and penumbra indicates that the cooling layer is thin.
This layer is located in regions where a convection is developed in the
solar atmosphere. The magnetic field in sunspots impedes the heating
in the convection region. In 1958, during the maximum of solar activi'f_'_.1_,_
a spot couple with different polarities had the following magnetic fields:
the forward spot in the Northern Hemisphere and the following spot inthe
Southern Hemisphere had positive (northern) polarity. Both spots usually
have opposite polarities. The polarity of a spot is determined byZeeman
fission of spectral lines. High resolution ability of the spectroscope shows a
filament structure of the spot umbra. The heterogeneous magnetic struc-
ture of the spot may be checked by measuring the transverse magnetic
field, the vector of which makes rapid turns in transition from point to
point. The nature of the magnetic field in sunspots is a coexistence of
inconsistencies, as the absence of electric currents or the presence of
a system of electric currents. - -_ - - I
Solar active regions (M-regions) appear in bipolar (BM), multi-
polar (M), and unipolar (UM) forms. Bipolar regions are associated
with calcium flocculi and an increased coronal emission.- With weak.in-
Card 5/7

L 39743-66
Acc m: Ap6ooy~64
no changes in spectra. Orig. art, has: 27 figures, 8 formulas, and 1 table.
LAM PRESS: 42o4-_F7
.SUB CODEi 03, 20 SUBM DATE: none. ORIG REF: 040 'OTH REF: 124
Card 7/7

84671
S/020/60/134/006/014/0-Al I
1941w BOI 6/B067
AUTHORS3 Andrianov, K. A.9 Corresponding Member AS USSR and
Severn
------------------------
TITLE3 TelomsrizationlReaction of Organo-cXcloslloxanes
PERIODICAL~- Doklady Akademii nauk SSSR, 1960, Vol. 134, no. 6,
pp. 1347-1349
TEXT3 The use of telamerizat-ion reaction. in organosilicon compounds is
rendered difficult due to the lack of elmental-organic monomers with
double bonds between element and oxygen, and capable of polymerization.
Ths authorsq hovever, effected the telomerization of octamethy! cyclo-,
tetrasiloxane as cyclic oompound and dimethyl dichlorosilane as a
substance effecting the rupture of the molecular chain. Experiments
showed that, in additiong the former compound is polymerized by the
latter. The authors found that the reaction of the ring cleavage without
catalysts proceeds rapidly at 200-2500C. At a ratio between the first
and the second substance of 2 3 1 it was completed at 2500C within
3 hours. 01~Jgomers were obtained corresponding to the compounds of the
Card 1/3

84671
Telomerization Reaction of Organo- S10201601134100610141031
cyclosiloxanes B016/bO67
followed by the rapture of the ring and the formation of a linear ccvb)-
dichloro dimethyl siloxane. Thase presumable reaction mechanisms are
explained by schemes. The authors continug the study of this reaction by
the example of similar cycles , and they investigated further reagents
effecting the rupture of the molecular chain. There are 3 tables and
11 referenoe83 4 Soviet, 4 US, 1 Britishq and I Japanese.
ASSOCIATION3 Institut elementoorganicheskikh soyedineniy Akademii nauk
SSSR (Instit-ate of Elemental-organic Compounds of the
Academy of Sciences. USSR)
SUBMITTEDi July 9, 1960
Card 3/3

26402
-'33/062161.10001008/0061010
31, 17.,IB206
AUTHORS: Andrianov, K. A., Severnyy, V. V., and Zavin, B. G.
TITLE: Telomerization reaction of dimethy-1 -..,yelos-111anes.,
Communication 1. Production of MLear a.w-d1ch'joro-
dimethyl siloxanes
PERIODICAL: Akademiya nauk SSSR. Izvestllya., khimicheskil'sh
nauk, no. 8, 1961, 1496..146i
TEXT: The authors investigated the t,-?Xttrre thy! -cyclo -
trisiloxane and octamethyl-cyc1otetrasilnxqne iwi~,h
silane, as well as the effect of the ratio cf
siloxane to dimethyl-dichlorosilane on the ~f 'ht., reaction
products, The following were used for the syri 11 ho -,.-3 ta 11 nr,
hexamethyl-cyclotrisiloxane, melting point 2 - b
132-1360C; oc tame thyl -cyclote tra-3 iloxar,,;, boilint-7,
dimethyl-dichlorosilane with a chlorine
was found to proceed according tci
n[(CH 3)2 SiOlm + (CH 3)2 Sici2 1 m 91* j
Card 116

~/062/6 110001008100-6-101 -0,
Telomeri~zation reaction of'dimethyl... 117/B206
methyl siloxanes showed that conformable to law boiling points, specific
gravitids and refractive indices change with the number of silicon atoms
in the molecule. No anomalies are observed in this connection. The
telomerization of octamethyl-cyclotetrasi.~oxane with dimethyl-dichloro-,
silane was investigated.at different molar ratios of the components:
10", 2:1 and 3:1.
Experiments showed (Pig. 3) that telomerization doole
not yield pure products for any of the ratios investigated. Telomer
mixtures with maximum yield of the product corresponding to the ratio
concerned, develop continually. When in -creasing -the ratio of the
reacting components, the yield of low telomers is reduced and the
amount of high-boiling products is,greatly.inereased. There are*
3 figures, 5 tables, and 2 references: I Soviet and 1 non-Soviet.
The reference to the English-language publication reads as follows:
W. Patnode, D. Wilcock, J.-Amer. Chem. Soo. 68, 2291 (1946).
ASSOCIATION: Institut elementoorganiobeakikh.soyedineniy Akademii
nauk SSSR (Institute of Elemental-brganic Compounds,
AS USSR)
Card 3/6

2'i,49o
B106;V!611000100910051014
Tj
Telomerization of dimethyl B117~BlOl
where m denotes the number of silicon atoms in the initial ring, n - 1, 2,4
etc. In this study, the monofunctional trimethyl-chloro silane and not a
difunctional compound was used as chain-terminating substance for the
telomerization of dimethyl cyclosiloxanev. Equimolar amounts of octamethyl
cyclotetrasiloxane and trimathyl-ohloro silane telo:nerize in .,an autoclave
at 2500C within 5 hr according to the scheme CH
1 3
n CH + (CH ) Sin --> (CH ) Si OSi__ C1
3)2S'014 3 3 3 3 1
CH 3-4a
Pure telomers with n - 2, 3, and 4 were obtained from the reaction mixture
by fractional distillation. The physical'constants of the telomers are
listed in Table 1.. The physical properties exhibit no anomalies. Tests
carried out with various molar ratios of octamethyl cyclotetrasiloxane to
trimethyl-chloro silane showed that at ratios of 1 : 1, 2 : 1, and 3 : I
mixtures of telomers only, and no pure compounds were formed. In all of
these mixtures the telomer formed in maximum quantity did not correspond
to the stoichiometric ratio of the reactants. The telomer having a chain
by 4 dimethyl-siloxane units longer than would correspond to the
Card 2/4

27490
S/o6 61/000/009/005/014
Telomerization of dimethyl Bi 17YBI 01
stoichiometric ratio of the initial mixture was observed,to form in
maximum yield. An increase of the octamethyl cyclotetrasiloxane : Tri-
methyl-chloro silane ratio lowers the yield of the lowest telomers, and
highly increases the yield of high-boilin' products. Within the range of
molar ratios studied, lower trimethyl-chloro silane contents in the
initial mixture did not decrease the conversion of octamethyl cyclotetra-
siloxane. There are 2 figures, 6 tables, and 4 references: 2 Soviet and
2 non-Soviet. The reference to the English-language publication reads as
follows: D. Wilcock, J. Amer. Chem. Soc. 68, 692 (1940-
ASSOCIATION: Institut elementoorganicheskikh soye6ineniy Akademii nauk
SSSR (Institute of Elemental Organic Compounds of the
Academy of Sciences USSR)
SUBMITTED: November 28, 1960
Table 1. Physical properties of a-chloro~L)-trimethyl-siloxy-dimethyl
siloxanes.
Legend: (1) formula, (2) physical properties, (3) b.p., OC, (p, mm Hg),
Card 3/4

OK 17
27492
s/o62/61/000/009/007/014
B117/B101
AUTHORS: Andrianov, K. A., and Severnyy, V. V.,
TITLE: Reactions of bis(trimethyl-6iloxy)-dichloro ailane with
alcohols, phenols and alcoholates
PERIODICAL: Akademiya nauk SSSR. Izvestiya. Otdeleniye khimicheskikh
nauk, no. 9, 1961, 1624-16~9
TEXT: The reactions of bis(trimethyl-ailoxy)-dichloro silane with
monovalent alcohols, its alcoholates, di4alent alcohols, mono- and
divalent phenols were studied. Bia(trimethyl-ailoxy)-dichloro silane
(b.p. 1730C, d20 1.0017, 20 1-3983), was',prepared by heating hexamethyl
4 9
disiloxane with silicon tetrachloride at 2500C in an autoclave. Monovalent
alcohols used were methyl-, ethyl-, n-propyl-, isopropyl-, n-butyl-,and
isobutyl alcohol, Etherification of bis-(trimethyl-ailoxy)-dichloro silane
with a 105/11 excess of the corresponding anhydrous alcohol, without a
hydrogen chloride acceptor, is highly exothermic and accompanied by
evolution of hydrogen chloride. It was not possible, however, to isolate
bis(trimethyl-ailoxy)-dialkoxy silane derivatives from the reaction
Card 1/4

S, 27h92
o6 61/000/009/007/014
ReactionD of b1l)(trimothyl- B11 7YB1 01
bis(trimethyl-siloxy)-dichloro silane with sodium alkoxides. Tile physicsA
constants of these alkoxy silane derivatives are listed in Table 1. The
reaction of biE;(trimethyl-siloxy)-dichloro silane with divalent alcohols
was studied using glycol and 1,4-butanediol. With glycol, an infusible,
insoluble precipitate and products boiling below 1100C consisting mainly
of hexamethyl disiloxane were formed. In the reaciion with 1,4-butanedic)l
the latter is dehydratized practically quantitatively to tetrahydrofuran.
The hydrolyzation is obviously modified by the tetrahydrofuran present, !to
that compounds which can be distilled off between '1500 and 26oOc under
vacuum and a small quantity of a liquid residue are formed. The properties
of these compounds are being studied at present. Hydroquinone and
1 4-dihydroxy-diphenyl propane were used to study the reaction of bis(tr:.-
methyl-siloxy)-dichloro silane with divalent phenols. With hydroquinone,
both in the presence of anisol as solvent and without a solvent, an
elastic polymer (C 12 H22 Si3 04)n is formed which swells strongly in organic
solvents: on prolonged standing in air it becomes sticky and deliquesecs.
On boiling in dilute alcohol it hydrol,,~zes readily with formation of
hydroquinone. The reaction with I 41-dihydroxy-dipqenyl propane yields a
darkbrown, tough polymer (C 21 H32 Si304)n which remains unchanged on stan6ing
Card 3/4

27492
S/c62
,/61/000/009/007/014
Reactions of bis(trimethyl- B117/B101
in air and is easily soluble in toluene. There are 2 tables.and 3 refer-
ences: 2 Soviet and 1 non-Soviet. The reference to the English-languago
publication reads as follows: R. 0. Sauer, J. Amer. Chem. Soc. 66, 1707
(1944).
ASSOCIATION: Institut elementoorganicheskikh soyed_fneniy Akademii nauk
SSSR (Institute of Elemental Organic Compounds of the
Academy of Sciences USSR)
SUBMITTED: February 2, 1961
Legend to Table 1 .
d4
1) Formula, 1101 11
N b.P., oc , 0 Fo T - KgM. 1C
~3~ calculated, j(CH,),SiOj,Si(OCH,-n), 232-7~ '34 1 4003 0:8847 96 96,6,
225-227 1,3968 08757 96 94 90,81;
4 found. [(CH3)3Si0j2S1(OC4Hq-i)2 I : I
jCH3)3Si0j.S1(OCH?-n), 214-126
'j(CH3)3SiO1,S1(OC3H7.1-)2 202-203
1(CH3hSiOhS1(OC21is)2 191-1'93
1(CH3)3Si0j..S1(OCH'): 174-175-
[(CH3)3S10jjSi(0C,jH5)2 157--~159 (3
Card 4/4
1,33943
1,2875
1,Z870
1;;1855
1,4750
0,8903
018752-
0,892t,
0,9155
1,03W
87,68
69,16
106,59
87,2!,
87,3t!;
78,10,
68,841
106,8!

28271 S1/0621611000101010061018
B117/BlOl
AUTHORSs Andrianov, K. A., and Severnyy, V. V.
TITLEs Telomerization of dimethyl cyclosiloxanes. Communication 3.
Telomerization by methyl vinyl diQhloro silane and met',&Yl
phenyl dichloro silane
PERIODICAL: Akademiya nauk SSSR. Izvestiya. Otdeleniye khimicheskikh
nauk, no. 10, 1961, 1788 - 1791
TEXTz Telomerization of octamethyl cyclotetrasiloxane by methyl "inyl
dichloro silane and methyl phenyl dichloro silane is described. The aim
of this paper was to investigate the effect of various substituen~.s on
the course of reaction. In the experiments, octamethyl cyclotetrasiloxane
with boiling point 1740 - 1760c, methyl vinyl dichloro silane wi-,*h boiling
point 930C (Cl 50.6%), and methyl phenyl dichloro silane with bolling
point 2000 - 2020C (C1 37-Wo') were used. From the reaction of e:.Iui-
molecular quantities of octamethyl cyclotetrasiloxane and methyi vinyl
dichloro silane, a mixture of telomer homclogs was formed. Frora this
mixture, a-chloro methyl vinyl siloxy- W-chloro dimethyl siloxanes with
Card 1/4 A

28271 SJ'062/61/000/010/006/013
Telomerization of dimethyl... B117/B101
n - 1, 2, and 3 were isolated and identified on the basis of boiling tem-
perature, refractive indices, specific gravities, molecular refractions,
results of elementary analysis, and bromine numbers. The properties of
the compounds obtained are listed in Table 1. The mean conve.;.,sion of
vinyl methyl dichloro silane was 32.8%, and that of octamethyl cyclotl-,tra-
siloxane 54.0%. The yield of telomers was 45,154 by weight of the ini-:ial
mixture. Contents of the individual telomer homologs with n - 1, 2, ;-..nd
3 were 18-5, 30.8, and 14.6%, respectively. Higher telomers with a
polymerization degree n-1-.3 were formed in the amount of 36.1~;. Thus, it
was established that telomerization is the only reaction at the moment. by
which compuunds of the a-chloro methyl vinyl siloxy-L-r-chloro dimethyl
siloxane series with given atomic number may be obtained. The reaction
of octamethyl cyclotetrasiloxane with methyl phenyl dichloro silane
showed low conversion under standard conditions (3 hr, 25000- k1so -,he
experiments with 2 M methyl phenyl dichloro silane and I It octamethyl
cy clot et ras iloxane resulted in a total conversion of only 18.40/6' at 3COOC
in 5 hr. The conversion of methyl phenyl dichloro silane was 9.1%, aad
that of octamethyl cyclotetrasiloxane 19.0%. From the reaction products,
telomer homologs with n - I and 2 were isolated. 49-Vlo of the telomers
Card 2/4

Z~ S/062/61/000/oio/OO6/018
Telomerization of dimethyl ... B117/B101
had a boiling point higher than 3500C (3 mm). The properties'of the
resultant a-chloro phenyl-(,).-chloro nongmethyl pentasiloxane and a-chloro
phenyl-o-dhloro heptadecamethyl nonasiloxane are listed in Table 2. Tbus,
it was proved that telomer homologs of the a-chloro methyl phenyl siloxj-
b3-chlaro dimethyl siloxane series are formed by the reaction of octa-
methyl cyolotetrasiloxane with methyl phenyl dichloro silane. There arl]
4 tables and 3 Soviet references.
ASSOCIATION: Institut elementoorganicheskikh soyedineniy Akademii nauk
SSSR (Institute of Elemental Organia Compounds of the Acad--~av
of Sciences USSR)
S UB MITT ED sMarch 23, 1961
Legend to Tables 1 and 2: (1) Formulai (2) boiling point, OC (p mmHg);
(3) calculated; (4) found.
4
Card

S/079/62/032/005/004/009
D204/D307
AUTHORS: Andrianov, K.A., and Severnyy, V.V.
TITLE: Hydrolysis of trimethylsiloxychlorosilanes and conden-
sation of their hydroxy derivatives
PERIODICAL: Zhurnal obahchey khimii, v. 32, no. 5, 1962, 1633-1636
TEXT: The hydrolysis reactions were studied to determine the reac-
t,
tivity of the above com ounds with electrophilic and nucleophilic
reagents. [(CH 3) 3S'OJ2 M was hydrolyzed in acid and basic media,
with and without solvents. In the absence of solvent# aqueous h-trdro-
lysis at 1000 resulted in the removal o:t the trimethylsiloxy groupt
yielding (CH j SiOSi(CH (II) and a polymer (CH SiO.Sio
3 3 3 3 3 3 1.5
(Sio 2)n (III). Solvents decreased the tendency of the trime.thylsilo-
xy group to split off; thus in ether and THP aq. hydrolysis gave an
insolubie polymer and crystalline [(CH 3)3 Sio 12S' (OH )2 (IV). No poly-
mers were obtained from the hydrolysis of I in the pre'sence of HCl
acceptors (pyridine, NH 3 NaHCO3 under similar conditions, the
Card 1/2

-19
S/079/62/032/005/004/0(.
Hydrolysis of trimethylsiloxy- D204/D307
only product being IV, in -"-'50 % yields. On heating at 200'C for-
30 min. IV condensed to HO ([(CH 3)3 SiO12S'0~2H and HO [[(OH3)3sio]2~
SW H. Trimethylsiloxy group was also split off [(CH*) Siol Sicl
'3 3 3 3
in an acid medium, without a solvent. In aq. NaHCO the latter com-,
3
pound gave [(CH 3)3 Sio]3SiOH, in 60 % yield. There ard 2 tables.
SUBMITTED: April 22, 1961
Card 2/2

ANDRIANOV, K.A.; SEVERM, V.V.
Hydrolysis of trimethylsiloxychlorosilanes and condensation of
their hydroxyl derivatives. Zhur.ob.khim. 32 no-5:1633-1636
,vq 162. (MM 15:5)
(Silicon organic compounds) (Hydrolysis)

S/062/62/000/007/007/013
B117/B180
AUTHORS: Andrianov, K. A., and
TITLE; Splitting methyl-phenyl cyclosiloxanes with dimethyl
dichlorosilane
PERIODICALt Akademiya nauk SSSR. Izvestiya. Otdeleniye khimicheskikh
nauk, no- 79' 1962, 1237 - 1242
TEXT: The reaction of trimethyl-triphenyl cyclotrisiloxane with dimethyl
dichlorosilane was studied at ratios I j 2 and 1 1 1. The telomers
CH CH CH CH
1 1-3 1 3- ' 1 3
Cl - Si (05i) - 01 (1) and oligomers C1 - Si (OSi) Cl (II),
I 3n n
CH CH ud bil
3 3 3 3
with n -2 - 10 were obtained. Despite the change in component ratio, the
products are not dominating individual substances, but always mixtures of
homologs. Reduction of the dimeAyl dichlorosiland content reduced the
yield of lowest homologs considerably and increased that of highest
homologs (distillation residue). In the reaction of tetramethyl-tetra-
Card 1/2

S/062/62/000/007/007/013
Splitting methyl-phenyl ... B117/B180
phenyl cyclotetrasiloxane with dimethyl dichlorosilane in the ratio
2.5 : 1, only highest oligomers (> silo) were obtained, with a 35.3%
yield. Products with three and four silicon atoms were hydrolyzed,' to
confirm the structure of oligomers of formula (II). The authors are the
first to have obtained 1,3-diphenyl-tetramethyl cyclotrisiloxane (yields
181/lo, b.p. 138 - 1400C (3 mm Hg); d20 1.0679;N20 1-5017; MR 95-52) a six
4. D
membered cycle with methyl-phenyl siloxane and methyl siloxane links, from
1,5-dichloro-1,3-diphenyl-tetramethyl trisiloxane. The hydrolysis of
1,7-dichloro-1,3,5-triphenyl-pentamethyl-tetrasiloxane yielded 72% of the.
,,.rell known 1,3,5-triphenyl-pentamethyl cyclote'trasiloxane with a boiling
point of 198 - 2010C at 4 mm. Hg. There are 1 figure and 5 tables.
ASSOCIATION; Institut eleinentoorganicheskikh soyedinerdy Akademii nauk
SSSR (Institute of Elemental Organic Compounds of the Academy*
of Sciences USSR)
SUBMITTED: December 27, 1961
Card 2/2

41336
8/020/62/146/oo3/ol2/019
B101/B144
AUTHORS: Andrianov, K. A., Corresponding Member AS.USSR, Severnyyj
V. V.
TITLE: Telomerization of organocyclosiloxanes with dimethyl
dichlor,osilane
PERIODICAL: Akademiya nauk SSSR. Doklady-, v. 146, no- 3, 196Z, 6ol-603
TEXT: The telomerization first observed on dimethyl cyclosiloxanes with
organochlorosilanes (DA119 134, no. 6, 1437 (1960)) proved applicable to
other organocyclosiloxanee also. The reaction was studied between
(ROR"SiO),, where RI (1) or RI (II) and
R" '. C2H5 CH3' R" ';' C6H5
(CH 3)2S'C'2 (III). Six-membered cyclic clompounds were chosen becau4e the..
eight-membered proved to be less active. The reaction proceeded according,-
.to (R'R"SiO) 3 + (CH 3)2sicl2 Cl(CH 3)2S'-(OS'R IV) 3n C1 forming telomer
homologp with n - 1, 2, 3 The reaction of I with III took place in
glass ampoules with 5 hrs heating at 2509c- Conversion of I was 65%, of
JII 53-4%. The yield of telomers with n - 1 was 64-8%, with n - 2,
Card 113

. S/020/62/146/003/012/019
Telomerization of organocyclosiloxanes ... B101/B144
17.6uj'a, the residue containing 18.6~. telomers with n> 2. For the telomer
with n = 1, the b.p. is 150 0C/5 mm Eg, d20 1.0102, n20 1-4303; for a i- 2
4 D
0 20 20
the b.p. is 175-178 C/0-01 mm Hg, d 4 0.9988, n D 1.4364. The reaction
of,II with III under the same conditions as for I with III yielded
32.9% telomer with n - 1, 4.9-/o n - 2, residue 63.2%. Conversion of II
was 88.6;4o, of III 36.5~*. Telomer with n - 1 had b.p. 198OC/4 mm Hg,
d20 1.1276, n 20 1-5116, and with n = 2 b.p. 201-203 0C/0.01 mm Hg'
4 D
d20 1-1310, n 20 1.5304- Reaction of II with III in a ste*el autoclave led
4 D
to cleavage of the siloxane bonds and formation of oligomers
Cl(CH 3)2S'-FOS'( CH3)(C6H Oln C1 owing to catalytic action of the resulting
FeCl In the reaction of trimethyl trivinyl cyclotrisiloxane with III
3'
in glass ampoules at 250-20ec no telomers could be identified, owing to
intense polymerization. The hexaorganotricyclotrisiloxanes are in the
following order of telomerizing capacity:
Card 2/3
0

S/020/62/146/003/012/019
Telomerization of organocyclosiloxanes ... B101/B144
if si6-~ > [(C H H (C H )Si > [(CH There is
(C 3)2 j 3 2 5)2S'013 IC 3 6 5 033 2-CH) C113S.'01 3
L
1 table.
ASSOCIATION: Institut elementoorganicheskikh -soyedineniy Akademii nauk
SSSR (Institute of Elemental Organic Compounds of the
Academy of Scienceg USSR)
SUBMITTED: June 4, 1962
"Card 3/3

LMIM -1~1~1-wiWOWI-IMN&I-a
3/06 62/000/012/002/007
B 1 17Y131 01
AUTHORSt Andrianov, K. A., and Severnyy, V. V.
TITLEi Catalytic cleavage of dimethyl CyClOBiloxanes in the presence
of dimethyl-dichloro silane
PERIODICALi Akademiya nauk SSSR. Izvestiya. Otdeleniye khimic.heskikh
nauk, no. 12, 1962, 2133-2138
TEXT: The effect of catalytic amounts of iron chloride on the reaction of
dime thylcyclosi loxanes with dimethyl-dichloro silane was studied. Experiments
with 1~i by weight of iron chloride, and without- any, were conducted under
equal conditions: sealed glass ampuls, kept at.2500C for 5 hrst rectific4-
tion of the mixture first at atmospheric pressure, then at 4 mm Hg.
Results; Without iron chloride, only a,to-dichloro-dimethyl siloxanes
containing 4, 7, and 10 silicon atoms formed. When using iron chloride,
telomerization takes place with the Si-O-Si bonds being ruptured and all
homologs of the formula
Card 1/4-

S/062/62/000/012/002/007
Catalytic cleavage of dimethyl ... B117/B101
CH
C'3 1
1 3
Cisi - (Osi)nCl
CH3 ~H3
being.formed with 2 to 7 silicon atoms. The following mechanism of cleavage
was suggested: The reaction begins by a coordination of the iron atom with
an oxygen atom in the siloxane chain either of the telomer or dimethyl
cyclosiloxane. An active complex forms which then decomposes. The
assumption thpt this reacfion takes place in equilibrium was confirmed by
experiments with octamethyl cyclotetrasiloxane and dimethyl-dichloro silane
at different component ratios (Fig. 2; Table 1) and also by the fact that
the composition of the reaction products is determined by the quantitative
ratio of the Si-0- and Si-Cl- bonds in the system, not by the type of
compound used. The reaction examined was suggested as an easy method of
synthesizing low-molecular and high-molecular 1,63-dichloro-methyl siloxanese
There are 2 figures and 4 tables.
Card 2/4

S/062/62/000/012/002/007
Catalytic cleavage of dimethyl ... B117/B1O1
ASSOCIATION2 Institut elementoorganicheskikh soyedineniy kkademii nauk
SSSR (Institute of Elemental Organic Compounds of the Academy
of Sciences USSR)
SUBMITTED: March.31, 1962
Fig. 2j Yield of Cl[(.C'3)2"O1n-" (CH 3)2C''oligomers depending on the
ratio dimethyl-dichlorp silane : octamethyl cyclotetrasiloxane = curve (1)
2': 1; curve (2) 1 : 1~ where the y-axis gives the yield in and the
x axis gives the numbei of silicon atoms.
Table 1: Dependence of the molecular weigh t and oligomer yield on the
molar ratio octamethyl cyclotetrasiloxane : dimethyl-dichloro silane.
Legend: (1) ratio; (2) calculated; (3) determined; (4) according to
viscoaityi (5) yield,
Card 3/4

S/062/62/000/012/002/007
Catalytic cleavage of dimethyl ... B117/B101
Table 1 Fig. 2*
Hagaeno
COGTHOme- m
Ilue
I Sin
I Af SI, Buxo;j. %
I
. I I no GI n0 BF13KOCTU
10.:1 40 2960 35-38 2750 2900 75~85
20,:j1 80 5920 71-76 5250-5630 5300 70-80
25,:,l 100 7400 89-93 6560-6870 64200
1 70-80
501%1 200 14800 150-170 11200-12600 13850 65-70
100j:A 400 29600 220-250 16700-18500 18709 55-65
Card 4/4
;
chi

S10621631000100110111025
B101/B166
AUTHORSs Andrianov, K. A., and Aevernyy, V. V. q1
TITLEz Telomerization of dimethyl cyclosiloxanes~ dommunication
Reactions with,silicon tetrachloride
PERIODICAL; Akademiya nauk SSSRI, Izvestiya. Otdeleniye khimicheskikh naukj.'
no. 1, 1963, 62 - 86
TEXT: The reaction of dimethyl cyclosiloxanes with Sicl was studied'to de-
4
termine its applicability for the synthe6is pf* tetrafunctional telomers,
and to obtain missing data. The reaction of'equimolecular amounts of hexa-
methy! cyclotrisiloxane with SiCl in a glass ampoule at 250 0C confirmed*the
4
occur Irence of telomerization according to n 1( CH5)2 sio]3 + Si-Cl4---,> C 133i
The reaction product contained 71-5% of the compound with
-[OS.i(CH3)2]3nC" . 7~
n = 1 and 13.5% with n = 2. A much more complicated mixture'formed in a
steel autoclave-under the same conditions from oe'tam'ethyl cyclotetrasiloxane.
and SiCl' by the catalytic action of FeCl traces. Compounds of the struc-
4 3
Card 1/3

J
j
�/062/63/000/001/011/025
Telomerization of dimethyl B101/B186
tures ClSi(CH ) _103i(Cli3 si-fosi cif WnCl (2), and
3 2 21n6' (1); C13 :.3
Cl3Si-[OSi(CH 3)2]n_OSiCl 3 W 11 were formed. At the, molar ratio SiCl4 .octa-
methyl cyclotetrasiloxane 4:1, the yield of substances with high chlorine
content, such as Cl Si-FOSi(CH ) Osicl OSiCI ; increased. At the
L -3n- 2-
3 r 3 2 3 0
ratio 1:2, the yield of substances boiling above.250 C/4 mm Hg rose to 38.%
I M' Chem. Abstrs
Contrary to S. Maeda, E. Noj' oto (Jap. patent 3660 (1957), 52,
5880 (1958)), no formation of dimethyl dichlorosilane was found. The cat-
lytic action of FeCl is explained by binding,of the Fe atom to an 0 atom
3
of the siloxane chain. -The resulting active.,complex Fe--O-Si:~ dec "'poses
under the action of a compound containing Sk-!Cl bonds; Fecl ~-.et fj!ee
'Ch 3
again, and an Si-O-Si bond is formed: 'Cj/Fq-Q-Si, The data for the newly
\C1 2Q 20
synthesized compounds are given in the order b:p. (mm fig), d4 , and nD
oligomers of formula (2), n - 3: 65(4), 1.1475, 1.4079; n - 4: 91 (4),
1.1043, 1.4081; n - 5: 112 (4)$ i.o968, 1.4092; n''$- 61 132 (4), 1.087.0,
Card 2/3

S1005216 3/000/001/011/02 5
Tolomerization of d."imethyl ... Biol/B186
1.410B; oligomers of formula (3), n - 3s 86 (5), 1.2207, 1.4112; n - 7-
1890), 1.1256, 1.4118; n - 8t 2050), 1.1165, 1.4123; n - 16t 2150-01),
1.4135; n - 17, 226-230(o.01), - , 1.4137. There are 4 tables.,
A330CIATION: Institui elementoorganicheskikh soyedineniy Akad:emii nauk
SSSR (In'stitute of El:emental*Organic C'Ompounds of the Academy'.
of Sciences USSR)
SUBMITTED: April 16, 19062
Card 3/3

S'/06 2/6 1/000./002/011/020
B 144" "B' 13 6
AUTPORS: Lndrianov, K. A., "~cv-Prnyy, V, V., and lzmaylov, B. A.
TITLE.- Telomerizqtion of r3imuthyl cycloailoxanes. Communication 5.
Reactions with trifunotional compound~i
rEHIODICAL: Akademiya nquk SS C R ,Izvestiya. Otkleleniye khimicheskikh
nauk, no. 2~7 1965, 2e2 - 290
TEXT; Reacting hexamethyl. cyclotrisiloxt~ne (1) with organotr1ohloro silanes
at 2500C led to tile formsition of telomera of the formula
) I Cl in which tile degi.~ce of tclomerization depended on
"'(C1)2_1OS'*"_3 2j
3ri
the oreanic radicul R, The ztetIvity of qSiCl 3 devroa2ed in the order
R - C113t C It CII r,,H, C. 6H 5' 7,llhpn R was CH3or C Hci 1 s2 excess of I
2 5 f 2' 2
effected a reduction of th" yield in the. telomer with n - 1, a slight in-
crease of the telomeri wit), n = 2 and n ~ 3, ard q sharp increase of the
higher telomera. This effect wa* absent, -wher, the reaction with PUH 3 Sial3
was brouE:ht abotit in two stages with socparf;tiozi of 1,1,'7,-trichloro-heptfI-
methyl tetraoi-loxane. I~hi3 ip. attribuLed to the dependc-nQe of the HSM 3
Card 1/3

Telornerization of dimethyl B I 44/B 186
activity on the number of CI atoma bound to one Si atom. The boiling point3l.
20 20, -nm I -
C1 40 11 1) molecuier weigMs and c . positioni Rre given for the lt new tri
functional Lelomer3 obtaivied. Ili the presence of F,~,'12' not only tTi-
functional form but, also the di-Ptinttiora-I tplomers C15i,(CH 3)2-[O:-:'(CH3)2]n cl~
For P = CH C? v ", "H wixture3 of tri- and difunctional tuelorrv~rs witb equal
3 1: 51
n formed. Wif-h R - C9114 or C H.-I the rrelalirn n,?,n was foiznd to depend on
the type of the 4-1 Ili t ial d, I.Me, thyl [(Cfi ~ SiOlm. The physical
V2
it 110=10aUCS WI!,11 11 7,8,16,20 and C
Propertkcs oF the new 06 5 'Z I ~ 41~9
homologuee with n - 4,5,7 aro givc;n. Ir, thin of FeCl 2 the percentage
of dimethy3 t2yn1nr3i.Io7-ane convers-Ion decrvzised in the ~5ane order aa in-
dicated that n-bove fc)r the I.- thrt roa-~.Aion with r.Lnyl and
Phellyl COMPOunds, T proved 11JOIre ty-t-i-riketh.,,ri
There are 8 toblen.
AES'60CIAIL'101,1. lii!Otitut ~--,oyerjiaeniy -Ikademii aauk SSSR
f
~In-".-'Xtlite r!f t-'%r,,~rinic '.cmpoun~-, or the Academy of
n r (1 2 17, -a

c! A19
/--G'
Telomeriz,ition r L
.;f' dimethyl ... JB 1 114/13 1 G (I
S UBMITT ED i May '16, 1962
I
q ",
Card 3/3

ANDRIANOV., K.A.;._SEVERNYY, V.V.
Telomerization reaction of organocyclosiloyares with
dimethyldichlorosilane. Dokl. AN SSSR 146 &t3 3 162.
1 .
tMI71 :10)
1. Institut elemomtoorganichookikh soyedirieniy AN SSSR. 2. Chlen-
korrespondent AN SSSR (for Andrianov).
(Siloxanes) (Silane) (Polymerization)

ANDRIANOV, K. A,,; SEVERNff,-V. V.
Catalytic cleavage of dimetbyleyolosiloxanes in the presence
of dimetbyldichlorosilane. Izv. AN SSSR Otd. khim. nauk
no.12:213-1-2138 D 162. ' (MIM 16: 1)
1. Institut elementoorganicheskikb soyedixenly AN SSSR.
(Siloxanes) (Silane) (Catalysis)

ANDRIANOV, K.A.;.~EVE~MJjtj IZMAYLOV, B.A.
Telomerization of dimethyleyclosiloxanes. Report No-33
Reactions with trifunctional compounds. Izv.AN SSSR.Otd.
khim.nauk no.2:282-290 F-163. (MIRA 16s4)
1. Institut elementoorganicheskikh soyedineniy AN SSSR.
(Siloxanes) (Polymerization)

ANDRrUNCIV, I.A., EVAMI V.T.
Telamarizatian of siUcam-argmio cyales.
Peport subadttefi for the 12th Ccofermos on hi4lb solsoular velabt oaq*undo
devoted. to amamrs, VWm, 3-7 4rU 69

ANDRIANOV, K. A.; SEVERNYY, V. V.
Telomerization reaction of dimetbylcyclosiloxanes. Report
No. 42 Reactions involving silicon tetrachloride. Izv. AN
SSSR. Otd- khim.,nauk no.1:82-86 163-
(MIRA 16:1)
1. Institut elementoorganicheskikh soyedineniy AN SSSR.
(Siloxanes) (Polywrization)
Silicon chlorides)

SEVERNYY, Vadim Vladimirovich, kand. khim. nauk; IICVITSKI'l.
Eduard Grigorlyevich, inzh.; STAHOSELISKAYA, N.Ya.,
nauchn. red.
(Synthesis of organosilicon oligomers and polymers and
their stabilization; survey of foreign patents] Sintez
kremniiorganicheskikh oligomerov I polimerov i ikh sta-
bilizatsiia; obzor inostraraUkh patentov. Moskva)
TsNIIPI, 1964. 34 P. (MIRA 18:5)