SCIENTIFIC ABSTRACT KAPLAN, S.A. - KAPLAN, S.I.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R000520430013-3
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: June 13, 2000
• Sequence Number: 13
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

Introduction to Space (Cont.) SOV/1235
PART III. RELATIVISTIC GA$-DYNAMICS
Ch. T. Relativistic Gas Dynamics Of An Ideal Gas
1. Basic thermodynamic relationships
2. Continuous motion of a gas
*3. One-dimensional-inotions of a gas
Ch. TI. Relativistic Magnetogaodynami .as
Elements of relativistic magnetogaadynamics
5. One-dimensional notion of a conducting medium
6. Elements of the shock-wave theory
Ch. III. Problems Of Motion Of A Medium In The Relativistic
Camp '?
Dispersion of a gas
Sound waves
References
AVAILABLE: Library of Congress
IS/nah
Card 9/9 2-25-59
351
351
35T
363
376
3 6
3~
396
410
410
421
424
--F q
q
aw
'p

AUTHORo Kaplang S*A~ SOY/115-58-1-2/50
TITLE: on the Planning of Measuring Laboratories for Linear Measure-
ments (0 proyektirovanii izmeritellnykh laboratoriy dlya
lineynykh izaaroniy)
PERIODICALt lzmeriteltnaya tokhnika, 1958, Nr 1, Pp 5-7 (USSR)
ABSTRACTs The article contains detailed information on the basic stand-
ard layout for measurement laboratories of non-mass produo-
tion machine-building plants, worked out by the Department
of Measures and Measuring Devices of Vptistroydormash (former-
ly the Ministry of Construction and Road Machine-Building).
The information includes a building layout, a basic minimum
list of required laboratory equipment, and a distribution
plan for this equipment within the building. Equations to
be used for estimating the required quantities of instruments
and the number of workers are given. There are 2 tables and
1 diagram.
I. Laboratories--Design 2. Laborttary equipment 3. Laboratories
--Organization 4. lAboratories--Instrumentation 5. Mathematics
Card 1/1

soV169-59-4-W68 -
Translation frcini Referativnyy zhurnal, Geofizika, 1959, Nr 4, p 127 (USSR)
AUTHOR% KaDlan.-S.A.
TIME- Mwetio Gas Dynamlos_and the Problems of Cosmogony
PERIODICALt V ab.i Vopr. koamogonil. Vol 6, Moscow, AS USSR, 1958, pp 238-
264 (Engl. Rea.)
ABSTRACT: The basic principles and the general results obtained in the
magnetic gas dynamics are discussedt 1) the existence of the
4idheslon" integral; 2) the description of the "entanglement"
-and the "disentanglement" of the magnetic force lines; 3) the
increase of the density of magnetic energy in gas dynamic shook
waves; 4) the notion of the gas magnetic turbulence. Certain
coamogonic hypotheses are discussed, in wh1ch the methods and
results of magnetic gas dynamics are used to some degree:
a) the hypothesis of the connection between spiral &me and the
regular magnetic field; b) the hypothesis of the formation of
terstellar gas clouds as individual vortices - nuclei of the
Card 1/2 ~4nnterstellar magnetic turbulence; c) the hypothesis of the

KAPIAN, SA-.
'k .--
Miu-StIon of the motlez of artlfi~W earth sateUites and the
control of observations, Astron. tair. no*189:1-3 P 158.
(MIRA 11: 8)
1,Llvovelmys stantelys sablyndonly Iskumstv,-unop Sputniks Zoult,
(ArtIfIcial satellites)

,%~N, 8*A*
Approximate, calculation of ephemerides and the determination Of
orbits of artificial earth satellites. Astron.teir. mo.1920-6
NY 158. (KTU 11:10)
1,10yovelays stantelya nablyudenly Iskusetvannykh Sputnikov Zemli.
(Artificial vatellitea)

KAPLM- 2. A.
I
'Ibook Wsv" In Stoller InteriMs."
raw to be submItted for the 9th Intl. Iftown Imp Belglan Inst. of Astropbystes.,
MOSS, Belgian" " julY l"9.

AV retsenzent; SANSOKMO,
IY. David AllbertovIchl KAPLAML
L.Top redo; YXI"OTA, Ye.A., t-51175,red,
[IntervAl physical processoa in stars] FixichasIde protsessy
vantri svead. Koskva, Gom,,Isd-vo fislko-notem.lit-ry, 1959.
543 p. (Astrophyslos) (NIRA 13t3)

UPLAN, S*A.; IiDGYINMMO. A.A. Clegvymenko, 0.0.1; PODSTRIGACH, T.S.
(Pideti7bach, Togo]
42cuUtlox of gasomagnotle shook wave parameterse Ukroftso
shur. 4 uo.4:436-W? JI-4 159o (XIU 13:4)
1. LIvovskly gosudaretvaur4y uMverattet lu.lv.]Pranko.
(Shock waves)

30)
AUTHORS% Klimiohin# I.A. SOV/33-36-2-21/27
TITLE% On the Correlation Between the Observed Differences of the
Degree of Interstellar Polarization and the Angular Distance
of the Corresponding Points on the Celestial Sphere
PERIODICALs Astronomicheskiy zhurnal,1959,vol 36pNr 2,pp 370-371 (USSR)
ABSTRACTs By evaluating the data of Hiltner Z-Ref 2-7 the authors ob-
tain approximatively the relation
15
(P1 P2) 2 'Zi 5t2ac Og24 P
where (PI - P2)- 2 Is the mean quadratic difference ok the de-
grees of interstellar polarization (in per cents) in two points
of the firmament, and or. the angular distance of these points
from each other. It is reservedly conjectured that this cor-
relation can be explained by thi turbulent character of the
interstellar magnetic fields,
Card 1/2

SOT/33-36-2-21/27
On the Correlation Between the observed Differences of the Degree of Inter-
stellar Polarization and the Angular Distance of the Corresponding Points
on the Celestial Sphere
There are 2 references, I of which is Soviet, and I
American.
ASSOCIATION Lfvovskaya astronomicheskays. obaervatoriya (L'vov
Astronomical Observatory)
SUBXITUDs June 21 1958
Card 2/2

30),100)
AUTHORS t 33-36-3-3/29
Kaplan,S.A., and Klimishin,I.A. SOV/
TITM Shook Waves in Stellar Envelopes
PERIODICAL& Astronoxiobeekly zhurnal,1959,Vol 36,Nr 3,pp 410-421 (USSR)
ABSTRAM The authors considor physical properties of stellar shock 4aves,
the possibility of separation of the envelopes etc. The shock
waves are assumed to by stationary, at the other hand, the inter-
action with the radiation is considered. �1 contains the
derivation of the formula for the Hugoniot-adiabatic curves and
other general relations. Because of the complicatedness of the
obtainAd system in the following paragraphs, the authors restrict
themselves to especially interesting speoial cases. �2 is devoted
to the so-called dotonation-recombination shock waves in a gas-
radiation-mixture (these waves move due to the energy liberated
during the recombination of ions in the wave front). The waves
are described by the equations
2 #2-1) ' X'
X4(6r -3r2 [3r2'(2-A,) + 6r2(P2-#j) + 8-3p, +
+ Lq!l 2]
Card 1/3 p1_T2+1) + r2(r2+8-392) . 0

3
Shock Waves in Stellar Envelopes SOV/33-36--3-3/20,
P2 x2+1 92 (r2+1)x2 v1
Tj_ 1_+ Ti r 71710Lx
2 2(x2+1) 1
r. ~+ 4~4-3e)2 ; 6'- 5/3
3A+24(1-P)
The indices 1 and 2 denote the values before and after the
passage of the wave. A - "g/P is the ratio of the gas pressure to
the full pressure; q is the set of nascent energy, v is the gas
velocity with respect to the front of the wave, 9 is the density.
The system is solved by successive approximationg where the fact,
ttat the detonation-recombination waves are weak, facilitates the
solution. In �3 the conditions are found under which a separation
of the outer part of the envelope of a red giant taking place
with a small velocity is possible. An undisturbed separation of
an envelope mass amounting ca. 10-3 * 10-5 solar masses is
possible e.g. if the radius of the giant is 80 - 100 times
greater than the solar radius, the mass of the giant nearly
M
equals the solar mass and its absolute magnitude is -4 .5 or
Card 2/3 -5m-8. The velocity of the separating part is 50 km/seo, the

Shock Waves in Stellar Envelopes SOV/33-36-3-3/29
velocity of the shook wave 110 km/soc. The place of the
separation lies naarly in the center of the radius. �4 treats
the influenoe of radiative cooling on the parameters of a shook
wave. It is stated that this influence is essential even at
optical depths of "30 and that it leads to a 10 - 100-fold
diminution of the temperature behind the wave. �5 is devoted to
the properties of shook waves in a degenerated gas.
There are 15 references# 12 of which are Soviet, I American#
I English, and I German.
ASSOCIATIONsL'vovskaya astronomicheakaya observatoriya (Llvov Astronomical
Observatory)
SUBMITTED: June 2, 1958
Card 3/3

24 (5)p 21 (7)
AUTHOR: Kaplan# So A. 30V/56-36-6-44/66
TITLE: On the "Larmoron" Theory of the Plasma (0 *larmoronnoy* toorii
plazzy) - -
PERIODICAL: Zhurnal eksperimenW 'noy i toorstichookoy fisiki, 1959P V0136#
Nr 6, pp 1927 - 1926 (USSR)
ABSTRACT: The wide-spread use of introducing quasipartioles into the mod-
ern quantum theory gave rise to the introduction of effective
particle@ into the plasma theory. In this case they are calls&
"larmorons"I they are effective particles with the magnetic mo-
ment p# which are in the leading center of the Larmor motion of
real partioles. p a av 2/2H (m is the particle mass and v - the
X I
velocity component which is perpendicular to H). The energy of
the larzoron is equal'to the total energy of the real particle.
Spitear, Belyayev et al, (Refs It2) already used the conception
of larmorons, withoutg however# defining it so rigorously. The
author of the present "Letter to the Editor" gives a number of
equations, which represent the components of the progressive
notion velocity of larsorons (the components U, T, W zhere w
Card 1/2 is in the R directiong and u and v are perpendicular it) as

On the "Larmoron" Theory of the Plans& BOV/56-36-6-44/66
functions of the velocity components of the real particle*,
the larzor frequency and larmoron life timeg and further also
expressions for the total energy of the larmoronag the Telo-
city distributiong the equation of motion and its solution,
The results obtained are discussed. The author thanks A. Yo.
Glaubernan for discusaing the subject. There are 2 Soviet ref-
erences*
ASSOCIATION: Livoyokiy gosudarstvonnyy universitet (L'vov State University)
SUBMITTED: January 309 1959
Card 2/2

9 KAPLAN, S. A. (LIvav)
"The Structure of a Shock Wave in Plasma."
report presented at the Firot All-Union Congress on Theoretical and Applied
Mechanics, Moscow) 27 Jan - 3 Feb 1960.

t. KAPLAN q Sa=ll Aronovich, doktor fis.-matem.nauk; CEMMIMM, V.I..
oty.red.; MMONXIKO# TN,,, red,
[Now date an cosmic spoon; results of the Interwtional
Geophyelcal Year] Navy% dounp a koemichaskon prostronstve;
ltogl NGG. Kiev, 1960. 37 p. (Obshoh*stvo po raisprostranonliu
politichiskikh I usuchalkh susall. Gor.50 no.16).
(Cosmography) (KiRA 14:2)

KAPWI. S.A.; KLI14DYM)TA. A.I.
Nquation oi thn notion of an artificial &%rth satellite In
horisontal coordinates, Blul.staeoptnable-I.-Ak.sput*Zetg* noml:
10-12 160. (Mlu 13 15 )
1. Llvovnk~Wa stantalya nab4udenly tak-unntvenvkh mputnIkm
Z~011.
(Lrtificial satellites)

J-fj0
"OV/- -3
AUTEORS., Kaplan, S. A., Kliml3hln, I. A., LLverv, V. N.
TITT,d-',: A Theory of' LIght Scattering In a ModLurn With fi Moving
Botindary
PERIODICAL: AtitronomicheuMy zhurnal, 1950, Vol -T() Nr 1, PI) 9-15
(USSR)
ABSTRACT:
Card 1/11
When the motion of a gas under cosmical c-onditions Is
considered, It Is frequently necessiry to take Into
account Its interaction with radiation. Usually, the
problem is studied by combining the equations of motion
with the equations of radiative transfer; moreover, only
the case of a steady boundary is considered, while
actually the scattering occurs either bei:ore or after
the light quantum passes through a moving boundary.
Consequently, before any modern theory of lIght scattg_:r-
Ing Is applied to hydrodynamic problems It I.; necessary
to develop a theory of scatterIng In a medium with
moving boundaries. ThUj is the problem of ths~, present
authors. The following notations are used: k, the

A Theoi,y of Light Scattering In a Medium 7"000
With a Moving Boundary OV/33-)l 2/31
S
Card 2/4
aboorption coefficient per atom; n, the number of
particles In a unit volume; x, a geometric-al coordlnati~;
'r = knx, the optical depth; t1j, the average time a
quantum Is In a state of absorption; t 2' the time spent
by the quantum before two successive scatterlrigs. Th(~n
T may also be written as T - X/ct 2 whern, c 1:3 the
velocity of light. Two case3 are considered: t 1 > t 2,1
and t2 > t11 In the first case, let u = t/t 1 be a
dimensionless time, v the velocity of the mo%ine,
boundary, and p( T U~, the probability that a quanti-m
of light absorbed at the depth 'r will leave the medium
in time t. Then if P( T) Is the probability of a
quantum leaving the medium at any time, %-.,e have:
00 on
P P (111; Z (T):~- P (T. U) Uda; DP (.r. 11) 117(bi.

A Theory of Light Scattering in a Mediwn 78002
With a Moving Boundary SOV/33-37-~-2/31
This integral equation Is rewritten as:
I e-T.1, 1- x 1 11 W) dil, +
-2(T + (T T-
CO
e v 0
2 (1 +
or
p 0 - A-.,) k,
Here Xis an.arbitrary constant. In the secondcam we
haves
JL
P + p (v'- v It - t'j)
and
(t) - I I - k (I + r)] e-Al, k - V4 (1 -44 IX- (2
(20)
Card 3/4

A Theory of Light Scattering In a MedILLM
With a Moving Boundary
ASSOCIATION:
UBMITTED:
78002
SOV/33-37-1-2/31
Equations (16) and (20) give the solutions for the two
cases. There are 5 Soviet references.
Lvov Astronomical Observatory (Llvov,3kaya astronomiches-
kaya observatorlya)
JulY 1, 1959
Card 4/4

60829
3/033/60/037/02/006/013
1,5-,3 0 E032/E914
AUTHORS: Kaplan_._.S. A,j Klimishin, I.A.
TITLE: Some Y6-tes -on-the Emission of Light under Cosmic Conditions
PERIODICAL: Astronomicheskiy zhurnal', Vol 37, Nr 2, pp 281-283 (USSR)
'%09
ABSTRACT: Ths'present authors have previously pointed out (Refs 1
and 2) that radiation, which is one of the basic properties
of shook waves in cosmic conditions I has an important effect
on the structure of a shook wave, its motion, and the possi-
bility of its observation. The present paper reports two
new resulto in the theory of interaction of shock waves
with radiation under cosmic conditions. It is well-known
that the gas behind the front of a shock wave is heated to
a high temperature and this leads to a strong emissicn. of
radiation by-the front itself. Part of this radiation is
emitted in the directiori of motion and penetrates into the
undisturbed region of the gas is absorbed, and heats the
gas, before it is reached by 1he shock wave-front. The
Cardl/5

80829
8/033/60/037/0.v/006/013
E032/3914
Some Notes on the Emission of Light under Cosmic Conditions
heating of the gas before the front of a shook wave can
be calculated us3ng the theory of light scattering in a
medium with a moving boundary which was developed in
Ref 5. In the one dimensional case, the intensity of
radiation at an optical distance z, from the wave front
is given by Eq (1), where r,-knx, v - Vkntl 9 k is
the absorption coefficient per particle, n is the number
of particles per cc, x is the distance from the wave
front', V is the velocity of the wave front, X is the
ratio of the scattering coefficient to the total absorption
coefficient (i.e. the sum of the true absorption and scatter-
ing coefficients) and t is the mean lifetime of a quantum
in the absorbed state. iq (1) is subject to the conditions
11 - X1 4.1 -0-101 which correspond to strong shock waves
under cosmic"conditions. The amount of radiant energy
absorbed per unit volume and transformed into thermal
Card2/5 energy is given by Eq (2). As the volume element in the
gas moves towards the shook wave-front, the energy 41

80829
S/033/60/037/02/006/013
E032/E914
Some Notes on the Emission of Light under Cosmic Conditions
accumulated in it is given by Eq (3). since dt/dx = --!/V.
In a steady-state wave P and 1-h rei..A.1-a uaalter,,d.
It then follows from Eq (~) Vthat the energy ,~ 4.8 given"
by Eq (4), where t = 1/kne and is the meax, I-fetime of
a quantum between iio scattering gvents. In -',-hl', first
approximation one may put F --dT in accorden-e with
sh
the Stefan-Boltzmann law where T., is the temperRture
on the front of the shook wave and is given by
Tsh ~-RI16R where R is the gas
constant. For 14 the approximate relation is
card3/5
q1

80829
8/033/60/037/02/C%06/013
E032/E914
Some Notes on the Emission of Light under Gusmic Conditione
14 - exp(-hWh), where 17 is the mean frequency of
scattered radiation. A solution of the energy, mass and
momentum conservation equations, which are given by Bq (5)
with E given by Eq (4), determines the detailed struct-
ure of the heated region. It is however, at once clear
that the width of the ~Pated region is approximately given
by Eq (6). In stellar'atmospheres this quantity is small
and is of the or-a-e-F-oT a few centimeters or meters. In
the chromosphere the corona, or the interstellar gas the
width of the heated region is considerably greater a maj
become observable. Owing to the scattering of light'in the
higher-lying layers the radiation of the snock wave will
penetrate into the outer layers before the shook wave
reaches the surface. As a result, the intensity of radiat-
ion at the point of exit of the wave will begin to increase
Card4/5 before the wave actually reaches this point. It is shown e

80829
8/033/60/037/02/006/013
E032/E914
Some Notes on the Emission of Light under Cosmic Conditions
that although in the stellar and solar atmospheres the
time during which this increase in intensity due to the
penetration effect takes place is relatively small (of the
order of a few seconds) in chromospheric flares it is
considerably greater anA may be of the order of minutes or
tens of minutes. There are 6 Soviet raferences.
ASSOCIATION; Llvovskiy gosudarstvennyy universitet (L'vov State
University)
SUBMITTED: October 11, 1959.
Card 5/5

Swhro
MISE I DOM EEPLOTPATI03
Akadmdya nwk SSSR. AstrowmichaskLy sovet
Byulleten tantaiy opticbeakogo nalblyWisniya iskaostrenaykh spatnikoy Zemll.
Ill I
no. I ( ) (Acamw of sciences of the USSR. Astronomical Council. billetin
of the Stations for Optical Observation of Artificial Earth Satellites. No. 1
(11)) lJoscow, 1960. 22 p. 500 copies printed.
Sponsoring Agencys Astronoulchaskil tow t AkAdazdi nauk SSSR.
Rasp. Ed.: Ye. Z. Gindinj Ed.s D. Yo. Shchegoley; Secretary: O.A. Severnaya.
PJLIIME-. This bulletin Is intended for scientists and engineers concerned vith
optical tracking of artificial satellites.
COMAM. This bulletin contains abaft articles an optical equlp=at, techniques,
and results of obaervaticas of artificial earth sateM a. Also covered are
the precision of satellite pb*tography and the equation# of motion of satellites.
No personalities are mentioned. There am no references.
Card 1/4

Aca&wj of Sciences (Cont.) SOV/5570
Wrkuohar V A. (Novosibirsk Artificial Satellite Observation
'Stit-r-0--n-Tt ProiZetive Cup for the Xirror of the AT-I Theodolite
Map, B.A., an& D. Ye. Shchogolev. (Xaln Astronocdcal Observatory,
Pulkovo]. On the ProcIslon of Standard Processing of Photographs of
Artificial Sarth Satellites
Upl-w B A., =4 A.I. Klimwskaya (L'Yov Artificial Satellite
-;;fee-rVLM;-n'StatIon). On the Equation of Xotion of an Artificial
Earth Satellite in Norlsontal. Coordinates
Panalotar, L.A. (XaIn Antronoodcal Observatory). Observations of
Artificial Earth Satellites in the Polish People a Reyablic
Remdts of Photographic Observations of Artificial Earth Satellites%
Dronkalla, V. Berlin-Babelaberg Observatory
b A. laspikars eftaff Kesbers
al Chaprina, A.I., and L
of the Astroncedcal Council,.AS UWQ. Odessa
Astronosdeal Observatory
Card 3/4

S/033/60/037/03/017/027
1032/E514
AUTHORS: Kaplan, S.A. and Kurt, V.G.
TITLE: On the Expansion of a Sodium Cloud in the Interstellar
Space %4-e
PERIODICAL: Astronomicheskiy zhurnal, 1960, Vol 37, Nr 3,
PP 536-542 (USSR)
ABSTRACT: Shklovskiy et al. (Refs I and 2) have described a
method for the observation of the sodlum cloud ejected
from the second Soviet cosmic rocket on September 13,
1959# The results obtained by this method were also
reported. The present paper gives a quantitative
doscrivtion of the expansion of the sodium cloud. It in
shown that the expansion con be divided into two stages,
namely, adiabatic expansion accompanied by a fall in
the temperature and a free expansion during which the
atoms preserve their thermal velocities corresponding
to the temperature reached at the and of the adiabatic
expansion, If one assumes spherical symmetry, then
the expansion of the gas in described by Eq (3), wher e
Card 1/4 in the free expansion stage the term ap/Or can be V/C

S/033/60/037/03/017/027
9032/Z514
On the Expansion of a Sodium Cloud in the Interstellar Space
omitted. In the adiabatic stage the pressure gradient
is also much smaller than the first two terms and the
solution of Zq (3) is of the form given by Eq (4),
where A in a constant and f(v) is an arbitrary function
which in determined by the boundary and initial
conditions. Certain hypothetical expressions for f(v)
have been suggested by Stanyukovich (Ref 3). Under
certain simplifying assumptions it can be shown that
the relation between the velocity of adiabatic expansion
a and the thermal velocity of the second stage c k
are related by Zq (7) in the case of spherical
symmetry and by Eq (8) in the came of cylindrical
symmetry. Assuming a Maxwell distribution of velocities
(Eq 9), it in shown that the density distribution in
given by Zq (12). Fig 1 shown the theoretical density
distribution in the free expansion stage for various
values of a which in proportional to the ratio a/c k*
Card 2/4 The dotted curve represents the density distribution /C

2/033/60/037/03/017/027
Z032/Z514
On the Expansion of a Sodium Cloud in the Interstellar Space
when the adiabatic stage in absent. Fig 2 shows the
theoretical distribution of surface brightness for
similar values of a. These theoretical calculations
are then compared with photographs obtained by
Yesipov at Stalinabad with the aid of an image converter
telescope. The observed distributiom of surface
brightness at different instants of time are shown in
Fig 3 (1 - 93 see, 2 - 103 see, 3 - 146 see, 4 - 178 see
after ejection). The experimental data are also
summarized in Table 1. According to these data
a -, 1.63 km/sec and 1, - 0.87 ka/sece The correspond-
ing theoretical value Ck = 0.90 km/sec if it in
aasumed that a - 1.63 km/sec. It also follows that
during the adiabatic stage the temperature falls by
350 to 6oo*. The observational material suggests the
presence of an adiabatic stage. It in also possible
that droplets of sodium are ejected fromoj~etevaporator,
the dimensions of these droplets being I o 10-Z cme
Card 3/4 In interstellar space these droplets will evaporate and

3/033/60/037/03/017/027
2032/9514
On the Expansion of a Sodium Cloud in the Interstellar Space
form a new gas cloud which will expand with a lower
velocity* The presence of such a secondary cloud may
lead to a loam of definition of the central part of the
main sodium cloud and to a slower fall off of the
surface brightness. It is shown that this effect does
not contributs appreciably to the outer structure of
the main sodium cloud. Acknowledgment is made to
Lo M. Lukhovitskaya for assistance in the numerical
computations.
There are 3 figures, I table and 4 references, 3 of
which are Soviet and I Dutch.
ASSOCIATION: Llvoyakaya astronomicheskaya observatoriya
Goa. astronomicheskiy in-t imeni P. K. Shternberga
(L'Yov Astronomical Observatory, State Astronomical
IrGtitufe Imeni-Pa -&,- 5hternbergi
SUBMITTED: January 16, 196o
Card 4/4 V/C-'

S/033/60/037/005/005/024
2032/2514
AUTHORS: Kaplan, 3.A. and Sivers, V,N.
TITLEi TX-e-Yenerol Problem of &ixht Scattering n a One-
Dimensional Medium with a Moving Boundary
PERIODICAL: Antronomicheakiy zhurnal, 1960, Vol-37, No.5,
pp. 824-827
TEXT: in a previous paper (Rof.1 the authors investigated
1
the problem of the scattering of ligh n a one-dimensional medium
3
i
with a moving boundary in the two spec al cases tl>> t and
t2~~ t1' where t 1 in the lifetime of alight quantum in th2
absorbed state and t2 Is the mean lifetime' of the quantum
between successive scatters. The present paper is concerned sftth
the general solution of this problem and given a solution of the
general equation for the probability that a scattered light
quantum will leave the medium with a moving boundary for any values
0, t I and t 2~ As assumed before, the medium is taken ' to be
one-dimensional and semi-infinite. The scattering is equally
probable in both direztions and the probability of scattering is
independent of the optizal depth. The derivation is not given and
Card 1/2

S/033/60/037/005/005/024
9032/9514
The General Problem of Light Scattering in a One-Dimensional
Medium with a Moving Boundary
only the final formula* obtained are quoted. There are 2 Soviet
references.
ASSOCIATION: Llvovskaya astronomicheakaya observatoriya
(L'voV Astronomical Observatory)
SUBMITTED: January 22, 1960
Card 2/2

KAPIAN, Sammil Aronovich; KUIJKOV) G.S... red.; PLAKSHE, L.Yu*,q
~-re ~.-
[Pbyslco of staral Fizika avezd. 'Hoakvaj, Goo. izd-vo fiziko-
matem. lit-ry,, 1961. 151 p. (141U 15:2)
(Co=ic pbYsics)

KAPLAN, S.A.
0:;-~
Effect of anisotr;:~pic conductivity in a maenetic field on the
structure of a shcA ~' in nagnetic gas dyncmics. Zhur. ekep.
i teor. fis. 38 no,ii952-233 Jan 160. (MIRA 14:9)
1. Llvovskiy sudaretvannyy univer8itet.
rmagnetio fields) (Shock waves)

UnANs SA.
OAptromon in the U.B.A.R.. forty ywa; colloot#4
U4101". leviewd by SA, . Astron.shur. 39 no.ltl7O-
171 Ja-F 162, (AstromW) (KMA 15t2)

KRAVTSOVo A.F.;_KAPLAN, SoA.
Efficient oyeten for selecting identical seismic receiving
units. Goofis. rasved. no.6s89-92 161. (MIRA 15:4)
(Seismic prompecting-Equipment w-A supplies) -

:;/702/62/OOQ/009/001/002
1046/1246
AUTHO?: Uplan, j.A.
TITLE: 'The dtornination of the optimal excitation jonditions of elastic
vibrations
SOMCI;: W:;H. Glavnoye upravIr-fiiye geologii i o~hrwW nedr. G*ofizicheakaya
razvodka, no. 9, 1q,2o 28-36
73=1: Ahe conditions of excitation are assessed from the amplitudes of the reflected
waves Cenerated in microneianotor7io-doing. This method cannot be used unless A) discon-
tinuitie3 with hi& reflection corIfficients exist within the eeismogeological cross
section, and b) the reflected bode waves are known to *require identical or similar
excitation conditions. There are 3 fieurea.
0
CWM VI

- UnO, S.A.
Theas7 of light soatterivi In a nowtsay.-state mwdi= Astron.zhur.
39 no*4&702,,-709 J1-Ag 162, (KWA 15:7)
(ught'-soatterim)

.'---W-W,-S.A"-Aoktor fis.-mat, nauk, red.; KIRKO, I.M., doktor fiz.-
mat. nauk. red.; STAMYUKOVICH., X.P... doktor fiz.--mat. nauk,
red.; SHIROXOTp M.F.,, doktor fiz.-mt. nauk, red.; FPJJM-
KAKMSK379 D.A., doktor fiz.-mat, nauk, red.; V1XGPJU4'OVICJ1,A.,
red.; UMMO., A.j. tekba. red.
(Problems of magnetobydrodynamics and pla=u dyn=ics; reports)
Voprosy magnitnoi gidrodinnmiki i diDamiki plawW; doklady. Hign,
Izd-vo Akad. nauk Iatviiskoi SSR. Vol.2. 1962. 660 p.
(MM 15:12)
1. Sovoshchaniye po teoreticheekoy i prikladnay magnitnoy gidro-
dinamiko. 2d,, ligal 1960.
(Magnotolwdrodynamica) (Plamaa (Ionized gases))

--S/124 3/000/003/007/065
34YD6308
D
2
-'Kt I TW
mi
ios;
~'n
e~
21 ___~
Us- s- Ound--Dy- Ej:s-
Aquau
-author D01- asseri- the
ves the problem-of-thefidw past a body moving with
AlfvenFs-velocity along the magnetic field.
duce The basic equations',re-
to Ozeen's Z-tranalit. 7 equation whose solution is well known.
Energy dissipation due to vIBOOSity and finite electrical conduc-
tion is determined. ~_Abstraaterls note: Complete tranalation-.2
Card 1/1

sA24/63/000/001/008/080
D234/008
AMMOR:
'hTLE: Simple waves and fomation of shock waves in stars
PERIODICAL: Referativnyy zhurnal, Hekhanika, no. 1,1963, 12,
abstract IB69 (Tairkulyar. Astron. observ.. L'vovsk.
un-ta, 1962,-no. 37-38,.3-8)
TUT: -The 'authar--investigates the problem of conversion
of ".a simple travellind wave into a shock wave inside of a star., It
is 'assumed that the wave is plane and that'the gravitational acceler-
ation is constant' The time of formation of the shock wave, as well
as'the orcssure oi this instant for isent'ropic and nonisentropie mo-
tion are calculated.
fAbstracter's note: Complete translation 7
Card VI 4L

MordVinov- .-4 1'

d.

S/058,163/000/003/02EV104
A062/A101
AUTHMs.- KOY "0.- KorOUshin, V. M.,
iov
7'
on n r#1
64atria aorAudtivity and diffusi i ittiviAto
ohe-OOMP6641h. 0] AMU
6'
3, 19;~ -'~;4betitat"' 3113-~,;71
0
..4 F
or", z-V
_~ ~" -m ~ rii no 110
2~1
T"
Aho-coeffloiehU of difftsion
eleetric-conductivity it! a relativistic-one-component plasma In the preseno of-
electric and magnetic fields. Expressions for the components of the "four-
dimensional velocity" of the particles are averaged, for the cases of parallel I
and perpendicular-electric and magnetic fields, by means of the distribution
function in the zero approximation. Transfer coefficient is obtained in the
presence of an electric field and the gradient of concentration of the particle*',':-
For a relativistic plasma, at a power exponent of the particle spect'rvm 2,
the diffusion coefficient is Inversely proportional to the intensity of the i,!9.
miasnetic field.
t YU. Mordvinoir
~Abstvoter s notat Complete translation]
ard I

Acennom mRs Ap4oo?673
3/0214/63/000/006/0053M59
AuTHoRS3 Kaplan, 3, A.1 0strow"s L. A.
TITLEs Theory of shock ways fontation in chromosphere and Ocr0n&
MOM Soln"hMV* damMe, no. 6, 3$63, 53-59
TOPIC TAGSs sacmAgtical theory# gowd wave,* sound velocity# magnotic force tubst
energy dissipation,, shock ways, coronal shock waves supersonic flow# gas flow,
coronas chromospherej, wave formation
ABSTRAM The authors have examined the conditions for converting sound waves to
shock waves in an inhomogensous atmosphere within a gravitational field. This
consideration in associated with determination of magnetic turbulence. The authors
describe the application of a method that permits investigation of conditions for
converting sound waves to shock waves in any distribution of density and toWera-
ture,, under conditions that the wave length of the sound is much lose than the
equivalent, height and that oaf-excitation Is smalle The mothod has been discussed
elsewhere by K. Yoo Gubkin (3b. NVokotoary prohlwr* matematiki, 1, mokhmikiP AN
SSSR,p Novosibirsk, 1961, stre 69) &M 09 Be F~ (Zhe prikle mkh. i tokhe fisep
Cmd 1/2

Accmuom xR, A&Mu
nos 2# 15p 1961). The authors consider velocity of the gass the effect of gravity,
and energy. flux* p~mu the relationship that shock waves form when the steepness
of the sound-wave front approaches infini j they
0 oc~s (Qnd expressions f or the distance
a sound wave must travel before ruptur t is,, befRre & shock wave is
generated). This distance it found to be on the order of 107 cm, The distance a
sour4 wave will travel bef6re half its energy is dissipated is on the order of
291W cm, It is concluded that a substantial part of the kinetic energy of the
wave is dissipated in a very short distance as corfared with the dimensions of the
chromosphere. It is possible that this circunstarxe explains the sharp rise in
temperature at the inner boundary of the oorona, Further dissipation of energy
$p_ ccurs in the corona, but this extends over a great distance,, and does not load to
y a high temperature gradient@ Orige art, bast 30 foraulast
AS=IATIONs Gorikovskly nauchno-issledavatel'sk1y raftofisicheskly institut
(Gorkiy Scientific Research Radio PkWalos Institute)
SUBKETT TED t 00 DAIS AGO 22Jan64 ZKOLS 00
SUB CMIs AS WO 1UW awe .02=1 006
Coed 2/2

UM MOMMATICE
-K
Mlm# Samil Ar w. chi PlIcellwArs Oblomm Borlsovich
Interstellar medivis (Mashs"sdnan szv&)s, YAsoowg Pismtgisg 196)v 5.U pe
illus,,, biblio, Errata'alip insertsO. 3.5c* copies printed.
,t6PId TAGSs Interstellar medim, interstoollar-gas.-Anterstellar br&ftmo
7
'interstellar dust, irterstonar imagnstio fleld, interstellar gas 4mmdoxv
galaotic evolution, radio trumedesion
-TABLE OF COMM labridgedle
'Forevord - 9
Ch. Is Interstellar h7drorn - 21
:Ch, II. Physical sUte of Interstellar gas 105
Ch. III, Interstellm dust
Ch., IV, Interstellar magratio fields and radio tranudesion 277
Ch. V. rnterstellar gam drummics and evolution of the Interstellar *Wim 372
Appeadees - 480
Bibliograpby - 510
cwd-],/

AN4036%7
;MB COM ?No A Bgmuxwaus 190003 Im mw WTI 2n
~O=s 261 AOQI 06AP94k

A~:CFS,SION Nil, AT5013792 wMA
P6
f ALMIOR
~1714E- nwf! hiferohnoLirv rporti!IIII
'01"ky. f ik:1 7
Int(qTlaneLany space. curnulauvf, ttno~-K %,av-
ABSTRACT: This thre-c-part paper dcaIE; with 1) interst(flar radiition A~,hose
~roonQiiv iq -alculated using a method do-scribc-d I n n -:t or -i; t i - i - in , Z~
Pikol'nez, fvIc7.hzvozerkaya srF-rb, M Iv,,
'01111gan (Ap .1 , 137 D62-
1/2 ---

T 01 ~: --l"
k:Tt AT5013792
-essum iner-eas el"X4'aa~
-Oxxt of Be ed
Oxe m~ in 15, of S. A.--'-
_erae -
i Kaplart, Ntezhzvo&itya-pkodinaiftiko~i.-M.- Flzma4ftg 10.181; arid 3) the trawfer of
-radlau" -W symmetricarar -17-- `lhe- blim-i"oTyed- th*-
kWec ispade,l pit
Wt th6- ile
ffrom.. the cmteer) as I/A In a e~ibsequent paper, these calcuUtions will be applied tD
of Lck In ,he night glow spectrum. Orig. art. tw6 2.5 if-r-muias. 2 figurt-3.
Card 2
-P

Y
KAPLAN,,S.A.; ZAYISEV, V.V.1 KISLYAKOV, A.G.; KOPRIM, M.M.; TSZY7LIN, N.M.
Fourth All-Union Conference on Radio Astronomy. Izv. vys. ucheb.
zav.; radiofiz. 6 no.4t86l-" 163. (MM 16:12)

Spectrum of magnotohydrodynamic turbulent convection. A3tron. .
zhurs 40 no.631047-1054 N-D 1639 (KRA 16:12)
Lb Radiof'Azichaskiy institut Gortkovskogo gasudarstvennogo unl-
voroitstao

KAPLM S A -, KATYUSHINA. V. V.; EM, V. G.;
Okeasurements of scattered U. V. radi&tion (1216A and 1300A) in the upper atmosphere! (USSR)
Report subsitted for the COSPAR Fifth International Space Science SMosjux, Florews,
Italy, 8-20 May 190,

KAPLAN, S.A.
Coments on 1. M. Knpylov's and V. r. Karpman's Tapers. Vopv kosm,
10s58-60 4,4- (MIRA 17110)

Ar4o15565 3/0089/64/016/002/0149/0150
;AUTHOR: Zaytsevo V. V.; Kaplan, S. A.
TITLE: Concerning the theory of the nonstItionary multiple Compton
scattering of gamma photons
~.SOURCE: Atomnaya energiyas v& 16, no. 20 1964, 149-150
TOPIC TAGS: multiple Compton scattering,, 4mall angle, photon, gamma
photon, Compton scattering
ABSTRACT: This paper presents a simple solution of the problem of thel
nonstationary scattering of gamma photons for small angles. The
approximation*
7 T
has been used.,,, The transfer equation is given for the photon flux
for a plane unidirectional source of monochromatic gamma photons.
A more detailed analysis for a point-source in a homogeneous medium
-1/2
Cwd

KAPLAN, S.A.; KLIHISHIN, I.A.
Methods of analysis of interstellar turbulence. Astron.zhur. 41
no.2t274-281 Mr-Ap 164. (MIRA 17:4)
1. Llvovskaya astronomicheskaya observatoriya i Radlofizicheskiy
institut Gortkovsk9go gosudarstvannogo universiteta.

ACCESSION NR: AP~043953 S/0033/64/041/004/0652/0656
AUTHOR: May, E. A., Kaplan. S. A.
TITLE: Cumulative shovk waves in interstellar space
SOURCE: Astronomicheskiy zhurnal, v. 41, no. 4, 1964, 652-656
TOPIC TAGS: astrophysics, interstellar space, shock wave, cumulative shock wave,
interstellar gas, globule, star, nebula, Stromgren zone
ABSTRACT: Dense circular dust nebulae (globules) are frequently observed within H II
qmission regions. As a result of the sharp temperature difference between the globule
and the surrounding Ionized medium it to possible to expect its compression by a shock
wave developing at the discontinuity. If the configuration of the globule is close to spher-
ical the shock wave will have a cumulative character, that is, there will be focussing of
the wave toward the center. If a dark nebula in a H Il zone is greatly elongated It Is also
possible to have cylindrical cumulation. At the time of development of a type 0 star,
causing the Ionization of a surrounding nebula, a StrlJmgren zone Is formed around it. If
there are such dense fluctuations within the nebula that it cannot be penetrated by Ionizing
radiation, the H II zone will "bond around" isuch formations. The time required for
establishment of the StrUmgren zone is of the order of the time required for recombination
Card 1/3

ACCESSION NR: AP4043953
of the Ionizing gas, that is, about 104 years at typical density values. Since the dimensions
of globules are much less than the radius of a StrBmgrcn zone, the time required for
establishment of more or less Identical temperature and pressure jumps along the entire
surface of a globule is also correspondingly less. This pressure jump leads to a shock
wave moving in the direction of lesser pressures, that Is, into the center of the globule.
Ills pressure wave should be characterized by the gas pressure In the H 11 zone
(temperature T and density/2 ) and the state of the gas in the globule. If the density
distribution In go globule Is uJorm (j0, = const), the problem of movement of the shock
wave can be cons' Idered by applying the biaory of similarity. lbo following example
is considered. Temperature in the H Il region Is T = 10 OOOC, the gas temperature
behind the shock wave front to T1= 1, 000CP 1A ti 111. The temperature In the
globule in comparison with T2 is neglected. If is assumed t at P2 = 1/2 Po and Poo
10. Isothermal speed of sound in the H II zone is 7 13 km/sec. Applying I o
2
formulas cited in the text, the author obtains the following parameters of converging and
-reflected waves for a spherical case;
C,,d 2/3

ACCESSION NR: AP4043953
Density jump at front Us 2. 1G 10 Converging wave
Gas velocity behind 0.24 0.67 Ditto
V8
front
Shock wave velocity 0.45 0.75 Ditto
Density Uc 10 103 Attains center
Gas velocity Vc 1.05 2.36 Ditto
Density Ud 220 105 Reflected shock wave
Shock wave velocity Ild 1.1 2.4 Ditto
no real values of the parameters apparently lie somewhere between the values cited
above. Similar results can be obtained for a cylindrical cumulative wave. Orig. .-rt.-
has: 25 formulas.
ASSOCIATION: Gosudarstvenny*y astronomicheskiy institut imeni P. X. Shternberga
(State Astronomical Institute); Radlofizichosidy Institut Gorlkovskogo gosudarstvennogo
universiteta (Radlophysics Institute of GurIldy State University) * I
SUBMITTED: 22Jan64 ENCL: 00
SUB CODE: AA NO PLEF SOV: 004 OTHER: 002
Card 3/3

---- ------ --------
t re-vu-I t S O-F - the -titto-er- ight -4 cat te r Urt--
tin, with movfng boundaries obtained aarli~ir bv the authors (Astronc.-
-hurnel, 37, 9, 19S0; Ukrainpktv fizichv-~ ZhUrnal , V
The stationary one-dinansiotial. motion of ;-n tOOAI Faf
sv the emission flow F is consilercd, ;r , -n ~ " - ~ "i i t i ou n
fnr conaervation of mesa, onargy, and momentum, under t tie a -z l~ kimp t !on
r pri-4gitra and internal anarry vf the Ond i [4 fu r b c d -q

ACCESSION NRI AP4043954
itial v-eLoclty of the emission front, n w oo/v where o, is eoentiit,?
of Elie flowing gas and a is the density of the noncitsturbed gts, ~ is
~~-P !mentro7ic exponent, 2 to an Ideal ;as constant, and uirth-- nolac-
vlar Weight, On Lhe basis of light scattaiing Lheory, diffei-ential
ttkionurw- b*h1n4--the--# hock- WAIVOL-f ran 0--9ft'4
"e &ertved. To detarmt-atr~
knowng T. and T-, expressions dertved eArlier fo- T anI F 'or
eq behind and ahead of th- q, ~r~ wnv~- r
lc-ur e-,uations in clerive-d fr~m
P lt~t;lnre r o mrp
I er 0 Rt 'R oh i
of shock wbves in OtelLar enveiopvs. 11 9110vu Int"
r 0 a I n t f. a ts e tA t s dRace immedi it. ' v ihead of aid hahlud i~:-,
wave front are of the tome order, Or I a r t. h 11 o rv-u I a s
3
2~
I ; VIA F4,1171

FED /E,a (I ),,EViP V-E-E-C-4,
ae- I i-4
- 41 F
Ref. 0i. Aqtronomlya. Otdol'nvv A
i A WHOM Kaplan, 5, A.
n=: R e I a t--rvToTrc- 0 c't ve
v L in tntergatdctlc gev
,CLIO SUMCK: Aqtreiv--t.9trktt
TOPIC
TAGS-.1-a9trcp-KlyTS-cff -shockijave, relativfstic qhock -wrave, I r lac t I c
gas, fntergalactfc 9pace, synchretre(i radiatioi, ra-lt~~ vmjs-,,nr
ot rhe fertiation of rEl
VA L It iv I q! ;h
inrpr~:,!lactfc pacp h-ia been deT
ion,; t t -i t
T I r,;1 rllne t P r QR
~yi-nEmuon radtatior cir
A 3C273. 1. F.
SUB CODE: AA
DIM: 00
Card

o',"Iteletic tuAL~ of cirruit breakcnl;

KUr
TITLE: Investig-s-Ati-o-n- in the upper e=apher-c-.
100TOCE, Kosmicheskiye issledovaniy&,-V- 3, Ar, 2, 1965, 237-243
.7 i~77
-adi o-
n counter
m- -t:ha mrer
-~zd have UF ra4lation windowz tar ::.e

L 41818-065
1ACCESSION 14R. AP5009640
a- afre cfrcilft, tra"Ista---fzel d-c
pu stc~r-,- - ~4
hag figuxes.
'20 -3-235
NO P=F S) VIVF 1. 002 &TD PRZSS.

ACCESSION -NR:
rool/002,/0251/0256
resonance rr-diati--.n theo". upper
C~11 7cocorena, L sub Alpha radlPtIon,
Din c r c hydrog-cr, distribution
1~6 r Fm no III t uUt that thte vq Z. ~T f-~r,
pro1#14cim in h c theory or scaccermg WLr-n a.L1crwRv9f7 j:c3T.-
of gi.iphic formu!7.e. nn v
-MA Ifinim tn-ttits- case Is gCe~-t tO t-1E SEeir G1ffErLL-UtL1W1-.
cal ta f ac, !--~dpr -PP! rh(? ejj_qtrtb-j-

L
ACCESSII~N NR: APS009643
-rc-0, stricter con.%fderatiori Cif the gcuvatrly Of 'hc' 1
P rj r, t,
p i A T I T
art has: f 2 li rF, ;i n-,4 o rmu a F
ENCL: X. tA
OTIMR.. GG6

6,;
IT NP.
IP50019
04
S. A. Kurt V. G
TI-MYE: t t%
Interpretation of' 4eLjovjjtj6nj 0 It e 6T(i 13(
_U triplet in the upper
-3 j no It 2, 1765 256- -7
61
P T 'L~ T A(;.S :airelov intensity, light di6persion, Ibedo, integrril rAdiation.
Doppler contour. Lorentz contour
BZT, RAU!, - the, chenge of airglo%flintenalty with height#
-11-je -JJ7~ale atmo4phere Is- -divided -Int +v- layers. Thc lover lever. extenis up to-
o 0
c... Tn this lwrer the diffuerffteff
In the lover layer the fL1t,A,i- ttir T-,,
b I e
p. nj!
fror e r int c;,ur 3A
I t i b'
1/2

Acci:SSION NR: AP500964h
t- ehe cmputation "multa in giver, In tht! rirlgina r~. I Vt. r e t. h
I ty occurs at 180 km. Orig. art. hap fLn'!
,MO~IATION: none
summiwm 23jul64 ENCL: 00 SUB CODE: - e~
NO PIET GOV, 004 (YllMR.- 004 A-7D PRms. 3237

Crd 2/2

~ ~ 4~.' ~ ~E V'S9
KAPLAN S A.
Continuous malt method for the production of syntbetle nitron
fibers. Biul. tekh.-ekon. inform. Goo. nauch.-isol. inst. nauch.
i tekh. inform. 18 no.3:20-21 Hr 165. (MIRA 180)

KAHAN'~ S. It. ; 1'.S.
Theciry of convection In a polytropic atmoslIPere with a uniform
rragretic field. Astron. zhur. 42 no.l:'Ii,-?7 Ta-F 65.
(1-11RA 18:2)
1. Radlofiztchenkiy inatit,"t krlkovskago gosudaratvennogo uni-
veraiteta I Urallskiy gosudarstvennvy universitet.

~N, ;,. ". ; MIRT, V.6.
Theory of the rescnanie v(,qtt,.-rlng of I.C -rrd',a,,jct) the gto-
corona. Kn8m.losl. 3 no,;i:251-2":c, Mr- 365.
In Wrprt!tAti on of' obpwvat. I otm of t,):,. I -- [1-let I()] ( L -~ 301; ,,~~,; In
jl,~.., ~
" fi ~
thF3 itijc-r atnnniht-re. Ibid. I . . ", I -

KMAN, 3.A*j LUPANOV# G.A*
Relativistic instability of po3ytropic spheres. Astron,zhur, 4.2
no*28299-304 Xr-Ap 165. (MIRA 1814)
1. Gortkovskir nauchno-iealedovatellskI7 radiofizichesk'LY institut,

64T i URI
Pod3trigach, T. 3.
plazi
-5 shock wavggj i.1 P.17-t-~n: 17 0- 70'
innminhaskly zjiurnai, v. 4.2, nc-.
The author3 inva!3ttgated t1to sysl~lm j1- i1 ho -,c-
of tha shock wave front in the L7wn caries, and ullian thic 15 lArKa tlxl lota in
=A- I-
n n rin a tvu.3 2,~ ai %et-4 a um
1 1-0 Lh ~n t 5 i~

L 6-1-646-65
AX C E'S 3 11 Ql "I IN'R: A.P5015581
"Ina" I an o tho ,!ai
01- lGnIs
Ofr d. XCj ti :2. no
Ti -n
to
'ri-t
006
OT FfER 000
'
'4$! 1
ZS ME

L 3430-60' EWT(l)/FCC/9WA(h) G~/R~
ACCESSION NRs AT5023572 UR/00O0/65/0O0/C00/MWMU
V. G.
AUTHORS: KaEMn, S, A-j Burt
(Vol'
TITIE: Scattering of radiation in the SMr atmosa!re of the earth (7besi
sy
SOURCE2 Vaeso7uznan konfsrents~ya-po fizike-kosmicheskogo prostrAmptva. MsooWA-i
19650 Issledazanfya kosmicheskogo prostranstva (Space research.); trudy
lennf;rentaii.
Muscow, Isd-vo Nsuka, 1965, 13.1-112
TOPIC TAGSt solar radiation scattering, solar rad3Ation absorption, upper ataos-
phere, atmosphere model, optic thickness
ABSTRACT.- The scAttering of 0 1 1300 R) radiation in the upper atmosphere
of the earth is considered, using the double layer model or tho atmosphere a
great optical thickness. Scattorirg or the incident solar radiation is assumed
to take place in the upper layer without absorption. Absorption by molecular
oxygon occurs in the lower layer where it is assumed that the albodo por unit
scattorine e7ent of A increases linearly with increaning optical thickness The
solution of the shift equation vpplied to this modol of the atmosphore indi;ates
that tho intensity bogina to decreaea Bharply at an altitude of about 180 km,
which agrees well with observations'4-Tho original article was published in the
Cord 112,

L 04244-67, -EWTW_ GW
ACC NRt
AR6004672 SOURCE CODE: UR/0269/65/000/010/0042/0042
_2F
AUTHORSt KapIgn, So A.; Petrukhinj No So
TITIZi Interpretation of the 11supersonic" propagation of disturbances in the solar
photosphere
SOURCE: Ref, A, Astronomlys, Abs., 10,51,311
REP SOURCEt SolnechWo danrWyel, no. lot 1964(1965)p 63-a
TOPIC TAGSs solar photosphoret'solar disturbancet solar magnetic field
ABSTRACT: A theoretical interpretation is given of the phenomenon observed by Go
Yaaasll~w on a solar magnetograph of GAO 20 July 1961. A sharp descent of gas
with a velocity up to 2 )(Watic was observed in the region of a magnetic hill. with
an intensity up to 100 o9 located far from sunspots. This descent occurred follow,'
iTig some decrease of the magnetic hill intensity and lasted about 14. min, after
whAch the gas began to ascend at half the velocity. The descent of gas began in the
central part of the magnetic hill, then the front of the region be an to propagate
aiang the surface of the sun to the east with a velocity of 50 k7sec and to the
w~st-up to 280 km/seo. The authors assume that the phenomenon began with the down-
ward drift of a m W etic force tube originally located at a fixed depth zo, because
of,which a zone of variable disturbance originated in this region. Sonic dilatation
Card- 1/2
UDCs 523.74
L 04244-67
'ACC INC AR6004672
0
waves began to propagate to all sides from this zone. The subsequent emergence to
the surface of the waves emitted at various angles to the normal led to the observed
"supersonic" propagation of the gas descent zone along the surface of the sm. A
calculation of the propagation time of sonic dilatation waves to the surface Of the
sun is carried out; the distance along the surface from the point above the source
to the point of ray emergence is also calculated as a function of the angle cpo
between the ray direction and the surface normal, It is assumed for the calculation
that the solar atmosphere is polytropic and that the temperature gradient JB constant
with depth, It is shown that for cpa, not too close to zero, the velocity of notion
of the emergence point of sonic waves to the surface is clone to the velocity of
sonic waves at th depth of the source. For a propagation velocity of the gas de-
scent zone front :f 50 ka/sect the source depth so = 20 000 kme The greater mWi-
tude of the disturbance propagation velocity to the west is explained on the basis
of the assumption that the sonic wave source is not concentrated in a m13 volume at
the depth zop-but extends at this depth in the latitudinal direction at a amll angle
to the horizontal. Thereby it in assumed that the magnetic force tube before descent
was almest horizontal for the most part and in-the region of the original =gnetio
hi-11 abruptlv emerged at the surface. The sonic ways range time from the source to
the surface along the shortest distance is close to the observed period of disturb-
ance development (3-4 mi~~ which confirm the proposed interpretation. B. Ioshpa
granslation of abstracy
SUB COEE: 03
La~rrd 2/2 I-dd_
In the magnetic field. 'Die author thanks-Go A. semnovaya and No S. Petrukhin
far help with the nunierical emputations, and Vo Vo Zhetesnyakov, who allowed
the author to readh)s work before It was pub I hViRS001692iD has: I figure
based on 4110ther's 90g0 Me I
and 19 formless L t J.
Card I I I I

~A A
SOme probIGMS affectIng the PhYflicO Of Interate1jar and 1ntej-
planetary matter. Trudy Astrofiz. Inst. AN Kazakh. SSR 5:296-
301 165. 041RA 18: 6)

KAPLAN, S.As; PIKELINER, S-14.
- W-
The Interstellar and intergalactic media. Izv. Vt SSSP.Ser.fizo
29 no.10:1830-1837 0 165. (MIRA 18.10)

NEODCVIZIY, I.N., inzh.; ALITER, V.F., inzh.1 GUTNIK, V.N., inzh.; KAPLAN, S.B.,
inzh.; LESHCHINSKIY, I.Z.p inzh.
Adjustment and the mastering of a high-speed, uniflow draving machine.
Stall 23 no.12M28-1130 D 163. (MIRA 17t2)
1. Nauchno-inaledovatellskiy institut meti2noy pronWshlennosti i Magnito-
gorskiy wtiano-metallurgicheekly zavod.

000
00
00
004
to
00.3"
000 4
004
to
- ------------
JAL-
to
:00
00
.00
1 mill I F,
NO
V.A. Xmigam, ad ML L VA=xwA 4J.
V* s 0
CAM 16 M-741)e4bft m I
hello d calbob In Ali)
*ML W-~h ;611 61~-Pl
-'F
QOW am 00na,
Q
to
SO VWA.M Md( )A
~ggg
-1-r,
goo
too
$00
409
goo
goo
Soo
goo
grow INOW&MV
moo
see
a 0 9 1 Nso I A 4 7 9 T
0 0 0 0 0 0 0 0 0 4
ISO o 00000000000000

o0
00
00
00
00
00

008

00 4

13

f.
411141-SLA WALLUNSICA& 1611"alli
r-
0::::40:00000010000:00
V U a a 11 v J, a 4, 'u a a
0
-00
.00
-00
doom me "jam.
ac '90
e
dft d
A. Killsw
p V. N.
d CA
j
M. 1333-4
w Il
-00
m- Oak madw arm. pre*.
P. d abil. ad (1) #*YNOC ~ see
A' ia 7W - IM " elbrillft
lU bY
or 14.7 mols. -00
wAb ykiw
li
lot i
* Go*
s
"w to Iml
ft "=MW fit "I sm l4s :
96 a anorest of 40.1% J'v
= -
16
U
.
%,.
ft
migivow iwl &ww.
:1
m
s
e
a
ON&W. aw mo~- I a P'- e
im"MiMAWN wkb pnwkw c"" -1rid.
A age
.A. F .Coo
Mae

Ores
too
C&ASSIPWON Lee
-TT 8- IP-1-1--ir-1
q vIt
I 1 9 ew 0 0 a I fir
00;0000100 a 99996006

03
Ali; 61 11.41 14,
00
:0
00
oof
00 it
00 8
00 a
00 1
oo.t
0o j
00.3,
0.3
A I a I L A 04161,W611CAIL 1,1111941
tL
-u
go'd., ' -.v -8-
0f a it a a X
0 0 0 0 0 0 0 0 0 0 a 0 0
.
T.-.0009000660606
0

I f .
A of T A81 A (19' 0 a ago
-1j
go
-00
-00
W 60 awsbawas al ethylene. pretyle'so o
to IsIsst Gomm at bawalwas of little f
V
n sumempbore
w
h ::
0
.
.
s
o
a
to ad PM-W"
It.
Kimv. sit. Keplam and A Rimlark,huk.
444 91 HIM) - - Ths' -Ju-
It
q
0
) S
.
.
.
,
Cbm. (
al Cjf.. McClIX11i, and MrX-Cll, in %Yk"f-
1 -00
.
14. 61 A 2in-, &---. I-a I W 210
lirairline. b. ro i0o'. and hv*%7 vwvh%bA.
N) Vv) mm, 1r-WIrs Sol &1
00
the &%I:' -A-10 SM
and the IrW11% 113941- 800
d,.,"if*d vot Soo
Chas. JUIUk'
400
noe,
we 0
000

zoo
see
see
see

U&MIFICAMN too
a 0 IA I I a Ow a a I if Is i -is"i -3 1 i
a a of a At 11 -
0 0 0 0 0 0 Ofe! 0 0 a 0 0 0 0 0 0 o 0 0 o 0
.000000*000~ooooooooooooooooooo!AA

fly a
Uj
000
004
00.
of
J
Ike al
f-_i__-_T_r
17
IS AV to 0 0 to a d a
0 0 0 0 04 0 0 0 0 0 0 0
0 0 go 0 A - 909909
mr,71W.W.O. falf 11111fol ell 4041ge
olviom
EWEN
V. A.
AM
zoo
doe
'fee
:*a
1,00
40
boo
a.* dot
_w_T I Od j ~j_
a a it 19
0 q 0 o o 0 0 0 0 0
0009000 0 0 q to go* 0 a 0 # * 0 goes so

Is Q It At to As Ad As
l A Cq
on
IN
r '11
tPL u 41 a or*

a .-
L .
a
c
A
u 4 0 A
"i'les 0 a r .1~

_
UAW,

00 I
d s mbftm ON so" Said misdams u.
rob whaft ad
mw
l
-00
Go 9
" m
1 n ve
oo" "pan
p
Kim", JL. 1--KMAV
m-
cu
a
G
U
J
M
00 a a
5
JW
i
i .
.
.
. w=rV
.
".
m. (
. W ribmem at
). d. C. A. A &MI.-Tb%
9
W
I
I
%d
at M
d
m mor atta.
s
m
mmut " native
*
in nFbw (mitit. al 3 kmmn) and in CoHX16. at
j;13
* I
H
i
C
HC16
C
l
-00
n bgmew. tubweir.
m
PbCL and at 2)
.
.
*
, 1
Wsigadgwaipm with th-v 44mbrr w4mlivis. J.L.

-so
so j -go
so
idle
0
so
W

0 000
;
9
so
k low

As. SL A .1l.ml-filtalk tillealwo CLASSIVICAllcm
lee

u a AV W) 11
0
0 IN it It aid $SRI a
0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 6
01 : 0 0 0 0,0 0 0 0 0 0 0 0 0 0 0 0 0 0 4 0 9 0 9 0 0 0 0 0 0
0 0 0 0 0 G 0 0 0 0 * 0 0 0 0 0 0 0 0 9

_lit #at

oof
gee
a
go
l

god
god
'
ow
god
M
W-
Oil. $
Goo I
at homw Ow blasi
Jim I at homw
J. J. a.

go
ta -0 ml; A i
90900199960664109*416:664

-- - -----

-00
21
Are
9"w "NSAIP
ew. "V $41
1 N 0 9 A 4 1

-t
L-1 A. 6 0 rw

00 bousial
of M.
"
W
P
Md
41=0.6
4 A
- .00
7. UCK 44, Mr-) The Pr,,~ dr-Cfibc(l Pvc
-00
f the
00
perao" *rA the cum Is. 0( the rapris, of she h. P~ o
% whN laic shnwn to 1w mwmal as"ropor
-00
00 Aow 2 j;TIslm
of .00
00 S~ 1. Koko
00 a lkd.14.%-V.-AnwtWprr-
'
4
f
d
I (
"r
r
a.
) W&O "-"
, -1, '". 067
4r;;mvsImrVI it
00
.Y. 44d valmar INV -"It I'l rshvkrw mm. in IIA I at
ffwv~
W' AM 1.41%
of It'
o
-hWri-Hhdiav
f
l
.
%
,
I" t
, III spA V. strA
h
an ""4rr pffemum Is" fit 41 "1.
coo
v
se:
0
~

lv 400

ill
i i as*

Poo

..COs
it -Ar
U AV 43
; so
0
0
000
0 0 0 0 0 a 0 of 09 00
0 000

1UPWP 1. 1.
TT.3D7 (yqLnibr:Lvm in 802ution, m, The solubility and vapour pressure of
solutions of etbylme oxide in water and in diablorethane) 0 ravnovesii v
rastvorakh. 111. Rastvorimost' I uprugostl pam rastvoroy Mal etilena v
vods i v dUchlorstans.
Al . 7 21s 545-549# 1937.

'
I IL
j 0It a 11, ajP m )p v a it a it v a a a of
L
4 M
a 11
1 It a a a
A -
-
.
011
1
0
L., -.
11
0
-
J1 10
I

go " IV. SMA" Psw at mums-

0
d
b
-so
I son 4
lepw
= m
%
00111114, am
O= d 11
~
.
101
0. M(WAMkWWN- J, 600. Ow". i1'.%

9
1 Fr"brh 261211119171 -, v(. CPA. J1.
4NU&S.-A iw wait of Me b. V. st *to. Ve we r
61WIF'Or.44M id bkwy Milli.. alwid the CSPITO. 4 thr
of
two aw IV. or. III the cle"tate from the laps
Of oil
00', MICK"CL, U41c"UrC11011 mec"cle-
ho, cloch-cCh. cit'c"CL alms CUM'.
60 j L. Mad"y
004
00 3
00 w ii:
so
00
J1
too" tl"OSAV.
1 .11.
vatsvi -se dwo dad
$an**4, -0 1
60 a
ife 0 00 :0 0 goo o :7; 61 0 0
00 N 00 0 0 0 0 go 0 000000 so o.f:: *000 ,0 ::::*:O::o
-00
-00
so*
as*
see
see
'Pee
see
400
lee
We
Noe
goo.

;0 0 0 0 0 0 0 0 6 0 0 0 0 0 a 0 0 0 0 0 0 Ow 0 0 0 0 0 0 0 411 ee -00--" 0 0 0 0
0000000e00#000000 0 0000000*0000:00000*
0
1?,. 4, IS it m a If a a v a 0 of 41 a 0 a 0
4p
0 0 Od
Not 1 0 of (6 -6 A t 0 0 0`4, 4 1 1 to " I I a , , ~' , CD a 0
00
fit all
00
0 w
00,
009- 04~
90

00'., ASXSPDJ 'y 'V

of MSAOSAI as J.'JI)l jot bjwm".w A Atoll 00
0 or? pun *a I *-IV I I 'Of * V ..) I woo. "aw Amomlow pmql-
00
- ' V '-"go& 1"JI-11 A41 10 1" 'A"SNA4111 qmwAql $SIM 441
00 Pw-#4 pus, sit$vl 441 P# ILOW "Nis" a 01 Lien 4" -0#3 00

i -4 rJelf soml, I-op'- "ow Aq 'Poir - ool -

I
00
VI am Otto
mr.t I or jt&~Sjj No I pm A's U" P- a
go- w
") 1314 p I APO mu ledpa AtS 0 sw )Nv 4 so 440
n as
et- s" 10'4 .1 JR6
is onto J41 pa -"4"m 046 p"'Wom-a
= 00
00. Pi-ml- ar)) $*am we AP044404 low"QuIP &11114WIMISIA 441
'
,
,
'
'
1
0
l".4
.oh*.,
JA
Ukw)AAw 411
" !f"ft
a
V 0
00- )L coir lot Vw rqwv -r
.
e4eviloomm"J" -0 -V OAMIMMIM.11
1
'amm"
to 110110111,10 smft 'A
-
041 00

IV
" It w a of "
a f a a 04 n
t 1 t I a
IN I
i
q of v a

got
004 "J
004
0.1
0 J
:
000
sod
T 'W-F- .1. ~17 - 1 ~11. ~741TMIIMA Im 0. ~U'F I.,
.Ott 4640 A" -0*-*# of-#
ltab= oW ?rfl!=it "Aid. 0.379.
Oct. 11, 1947. Tftb. joYramOmw is fliwiv"l to wAtef
I I. lbes 241ted out by (4 an W-Wli 11 It, t
am
Nacl'
-00
. 4
'see
[see
--**
..' Goo
7'ree
C-00
.So*
9 -400
0060900000000000000-"
alisil am ~wv all
All a 9 0 ft 0 x 9 1 it a 9 A a 11 1 q
oo*9000000000000*
00

KAPIANI S. I.
Kavlan. S. I. and Robinovichs F, E.9 A diagram of fusibility of the system
pyrauddon-water and the solubility of antipyrine in certain solvents. P. 1162.
The solubility of antipyrine in dichloroethansp ethyl alcohol and water is
studied in a temp. interval.140 to ?20. The diagram of fusibility of the system
pyramidon-vater is studied. This system forwis a eutectic mixture cortainingp 1.0170
pyramidon irith melting temp. - 0.10. In this system the region of separation is
established in a concentration interval from 211o to 637o of pyramidon at 72-5 -
730-
The Orshoniiddso An-Union Scientific
Research Inste of Chemical Pharmacy.
March 180 1948.
SOz Journal of Applied Chadstry (USM) 219 No. ll (1948)o

/t. dA
mf I-fl !-~ %'J.
0- - 0 6t % / 7e ~ A % v a 9 -
j I
AV 6. dvop
~-G eadtow I - *V*6 a 0/44vas

so 0at 0 0 0 0*1* 0

W
L I w
A f) c 0 v 4 a a L a a a ! I No 04 CI a,
t
oil .0 m ktilts 96

oft

vow"

ox Aq p pMOW &WPPW
Aq Adwp p-PW-we -1
ROO
Amu ~wijxiad vp in ANP4jA 94
U P"
tft4M
'AMAJIM

son, 0, )
"
Alill IP "p4mm -) pw*up Pw*- "POV 0
jj~v

o1
f walaw
A vul -N '(1051 *,% *(A*PNM I"-WJALAU
*
w :11. 0

too
o Slott) POW110 pom rumm
-
tq _
t ul"Im "m
I
W4 PM 1
il of
so.

set. of

r
00

--J
--
LAPIAM, S. I
o'f streptomycin from solutions by Using cation-ozebeaging
-1.0~ compounds@ Pladeprome 12 no*2**24-31 F 158, (Mu 11:3)
le Yde~oMoyy Muchno-iseledays tell ekty tastitut antibiottkove,
(OlkwNTOIN) (low KCHAWM)