SCIENTIFIC ABSTRACT KUZMIN, A.A. - KUZMIN, A.D.

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• Collection: Scientific Abstracts
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• Document Creation Date: January 3, 2017
• Document Release Date: July 31, 2000
• Sequence Number: 7
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

KOZIMT11) A.A,, AMAMEDOV, A.
Waters of the red series of the KemIr-(7hIkiahIyyAr legion Tru~ty
Turk. M. VNII Paxt 0 ncAsA--42 163 (MIRA 17,--?)

_A.A.; GLAZOV, B.M.
Automatic program control of oil trap machinery. Mash. i neft, obor.
no.22:20-23 164. WRA 1811)
1. Moflkovskiy inistitut "Soy-uzvodkanalproyakt".

Lmm/ Electronics - Television receivers
Card 1/1 Pub. 89 20/28
Authors KuzImin, A.D.
Title A television receiver built with the 31U-',IB cathode-eleatron tube
Periodical Hadio 1, 43-47, Jan 1954
Abstract A 24-tube television receiver built with the 31LKIB cathode ray tube
is described. One of its main features is an automatic video stabilizer.
Detailed circuit diagrains are presented with a description of the prin-
ciple components. Methods for winding the chokes and transformers are
described. A. Kuzlminskiy, the constructor, was aviarded a diploma of
the firzt degree for the receiver at the Ilth A.11 Union Exhibition of
radio amnteurs'. Drawines; diaerams.
Institution: ....0
Submitted: .....

K-IJZ'14IN,..Arkadiy Dmitriyeyich; SHAMSHn, V.I., rodaktor; SKVORTSOV, I.N.
~. . r6da)ctor.
[Measuring the noise co6fficient of receiver and amplifier]
Izmermnie koeffitatenta shuma priemno-unilitellnykh ustroistv.
Moskva, Gns.energ.izd-ye, 1955. 63 P. (MLRA 9:1)
(RaAio-Interference)

ft-~JJ21W
0~, 3.

a-ra poreo, cLj spen s e s
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n,- tno R.-97inir-a nr -,Lun,
7 1 . t I ro-; - , a - ~E 1 . 41 1 '- ~ 1 1; . - - - , -, . I . - ~
- - --- -- --- - . % - _ .- - . -- -, - - - _- --- - - - - - . --- - -------
,-card -5/3 -- . - --- -- --- - - - - - - -- ----

Category : USSR/Radiophysics - Application of radiophysical methods 1-12
Abs Jour : Ref Zhur - Fizika, No 1, 19579NO 1975
Author KuzlmtLn A.D.
Measurement of the Intensity of Radio Waves from Cosmic
Title Noo~l
Sources
Orig Pub Tr. 5-90 soveShchaniya po vopr. kosmogonii. 1955, M., AN sssR, 1956, 106-1l2,
d$skuss, 112
A16stract A noise generator employing a 2D2S diode, the noise current of which is
due only to shot effect, was used in the meter-wave band to measure the
equivalent temperature of p radio source, referred to the antenna. The diode
was loaded by a resistance equal to the output impedance of the antenna it
rep2#ced. The intrinsic capacitance of the diode was neutralized by a par-
alle(L -inductame. The problem of measuring the equivalent temperature of the
source was reduced to determining the diode 4-q current at which the noise
generator, connected to the receiver input, produces the some signal as the
measured source. The inertia of the electrons can be neaectmfor waves long-
er than 20 cm if the 2D2S diode is used. A start was made, using the des-
cribed procedure, to measure the intensity of the radio waves from the.s='"
and from a source at Ca~siopeia at 1 and 1.5 meters.

IiA~E I BWK EXPLOITATIOR
494
SWLrnov, V. S.; Anisiforov, V. P.; Vasillchikov, M. V.; Granovskiy, S. P.;
Kazanskaya, I. I.; Km 'min, A. D.; Mekhov, N. V.; Fobedin, I. S.
Poperechnaya prokatka v mashinostroyenii (Cross Rol-ling in the Machine -building
Thdastry) Moscow, Mashgiz, 1957- 375 P. 4,500 copies printed.
Ed.! (title .~W):Tseldkov, A. I., Corresponding Yember of the USSR AcadevW of
Sciences.. and Smirnov, V. S., Doctor of Technical Sciences, Professorj Ed.
(inside book): rmmv,, P. V.; Ed. of Publishing House: Leykina, T. L.;
TLach. Ed.: Sokolova, L. V.; Managing Ed. of the Leningrad Branch of Mashgiz:
Bollshakov, S. A., Engineer.
PURPOSE:TEi6 book is intended for process engineers and machl designers e d
in the field of metalworking.
COVERAGE: The book contains a systematic discussion of the theory of cross rolling
and helical cross-rollin , and presents generalized conclusions from theoretical
and experimental research work carried out, and experience gained in machine-
building and metallurgical plants in the USSR. The cross-rolling processes.,
'which are considered by the author as having wide potentialities, are currently
used in several Soviet plants for the manufacture of bearing rolls and rollers,
Cani-lby

-Crf3ss Rolling in the Machine-building (Cont.) 494
Some* mehine-buil din plants, e.g., the Gor1kovskiy avtomobillnyy zavod (Gorlkiy
-4ut=bile Pliant), have developed mills of their awn design for cross rolling.
The book is divided into four parts. Part I was written by V. S. Smirnov. Part n
was written by S. P. Granovskiy, I. S. Pobedin, N. V. Wkhov and V. S. Smirnov.
Part III was written by V. P. Anisiforov and 1. 1. Kazanskaya, and Part IV by
A. D. Kazlmin and M. V. Vasillchikovs There are 65 referencesaJ] of which
are Soviet,
TAB1Z OF
CONM
0
3
Introducti '11\~ PART I - GENERAL THEORY OF HELICAL CROSS ROLLING
Ch. I. Deformtion aAd Stress Distribution Daring Forging, Cross Rolling and
Helical Cross Rolling of Round Bodies
1. Deformation and stress distribution in forging, cross rolling and
heUcal cross, rolling of round bodies
Cald 3/T - I--, - . .

AUTHOR:
TITLE:
PERIODICAL:
KUZJMIN,A.D.
Some Radiation
ha rakteristiki
Radiotekhnika,
Received: 2 /
PA - 2012
Characteristics of Cosmic Objects. (Nokotorys
radioizlu8enija koemi8eskih oblektov, Russian)
1957, Vol 12, Nr 1, pp 12-21 (U.S.S.R.)
1957 Reviewed: 3 / 1957
ABSTRACT: As cosmic radiation sources are utilized for a number of radio-
technical measurements, the present paper deals with the characteristics of
these radiations. One of the most fundamental among these characteristics is
intensity. For the quantitative characterization of the intensity of radiation,
radiation flux, brightness, and temperature are, as usual, used. After an ex-
planation of the latter the determination of intensity at the input of the
radio-receiving apparatus, which depends on cosmic radiation, is dealt with.
The equation for the full power emitted by the antenna is set up, and for the
purpose of comparing the intensity of the cosmic radiation at the input of the
receiving apparatus with the power of its own noise, the temperature of the
source, which is known in radioastronomy as antenna temperature and which irra-
diates the antenna, is used. Formulae are set up which make it possible to com-
pute the equivalent temperature of the source for the case in which the diagram
for the directivity of the antenna and the distribution of the characteristic
temperature of the radiating object are known. For further analysis the notion
of the effective solid angle of the antenna-directivity diagram is introduced.
Two special cases of practical importance are investigated: 1. The case of a
CARD 1 / 2

Some Radiation Characteristics of Cosmic Objects. PA - 2112
radiation reception from areas the characteristic temperature of which within
the range of the antenna-directivity diagram changes only little, and 2. the
icase in which angles are small in comparison to the width of the diagram.
The last chapter deals with the characteristics of the radiation intensity of
cosmic objects, namely, the radiation of the sun, in which case it is
necessary to distinguish between the sun "at rest" and the "fluctuating" sun,
of the galazyt and of the discrete sources. The coordinates and the intensity
of the radiation of eight of the most intense discrete sources on USSR terri-
tory are shown in form of a table. As to planets, it is only said that
radiation flux is very small because of the smallness of the angles of vision.
ASSOCIATION: Not given
PRESENTED BY:
SUBMITTED:
AVAILABLE: Library of Congress
CARD 2 / 2

2- JD
AUTHOR: Kuz'miril A,.D.
TITIE- Mo dula t 4.c. n iii -a Rad ~t c1 - ~-n t e. i,.r o c t c Roc ive r 0 dulyat s ii
PERIODIULL- Pp il-lor- T.:;, 1 rlx i-o- ~5
u-,, (USSR)
ABSTRACT: In a common aralan~;*ci:-o nt rl' P,:l recc-iver,
th.-erc -,irn t-vjo a .9iodulator
and a 11cod T!,e -2-1,fll:--~I--~ 4Q-Le latluer arc, co.,~bined
in a coramon F!- o - u L
detecGed -at the , o, lat4on
f requency. f :,,ne ii)odulotor omitUed tie
-P o v: e r. It
is then stated Lf oril-, a r i
ae a
th-e ol t-~i.~t -.-,,l'a- e IT
j
1~ I ~ I.A-
ystem th
14 Mo (,%u ki ors T.I. S 13 5 s L e m s
v"Lose pel-If'orman';Q i-.; Jifditc~l by c),j,,,er and no t by
S ensitivJLty. Tl;eie are -2 f
ASSOCIATION: Phys-*Lc~-, It',ot-itu-to P.L.. Lobede~- Ac.&--, US;3R.
F It'. Ii. i % c, t t-- I P. 14 , Le 1, t- ~,:e v o All SS;~R)
SUBMITTED: A-)ril
AVAILABIEV: Libr--iry of Ccrn~~ro3s,
uard 1/1

109-7-16/17
The Reception Diagram Control of a Radiointerferometer by Frequency
Shifts of a Local Oscillator
the transformer being of unequal lengths.
ASSOCIATION "PoNeLebedev" Institute for Physics of the Academy of Science of the
U&S9S.R*
FRESENTED BY
SUBMITTED 4.1.1957
AVAILABLE Library of Congress
Card 2/2

Ku 1151& -,
'. -,
',-
Some radiation characteristics of celestial bodies. Radiotekhnika
12 no.l-.12-21 Ja 157. (MLRA 10:3)
(Radio astronomy)

KUZIMIN, A.D.; UDALITSOV, VA.
-
J Polarization of the radiation of the Orab Nebula on a 10 an wave
4ngth. Astron. teir, no.187.-14-16 D 157. (MIRA 11W
1.7izicheekly institut im, P,X, lebedeva, AN SSSR*
(Nebulm ) (Radio astronomy)

KU7~[[J.,11 , A. D. ,
',-.-'ITH VITMVICIII, V. V., UDALTSOV, V. A. and SOLOMM.'OVICH, A. E., " Radioimage
of the Sun on the 3 cm Wavelength,"
withUDALTSOV, V. A., "Polarization of the 10 cm radioemission of the Crab
Nebula,"
papers submitted for the Symposium on Radio Astrononw, 30 JLY 58 - 6 Aug 58,
Paris, France.

PARIYS.KIY* N.V. kand. -fii;-61mat',' uAu1c,otvO, rod;,. PROPOTNK,, Zj.-, red,;
KWHIN'. ZD,~mna.' tekhn. nauk,rea.; MOGILZVSKIY. E.I.. kand'
"frZ.--ma"I.- Haut. red.; MUSTEL'. E.R..red.; YBOOROVA. N.B., red: izd-va,
KASHINA, P.S., takha. red.
(Total solar eclipses of Yebruary 25, 1952 and Juno )0, 1954;
proceedings of Us ezpaditionj Polnye solnechnye zatmeniia. 25 favralia
9. 1 30 iiunia 1954 g.; trady ekspeditaii. Moskva, 1958. 357 p.
(MIRA 11:12)
1' Akademi7a, nauk B56R. Skepeditsiya po nablyudaniVu polnykh
solnechnAzatmeAi7., 1952 1 1954. 2. Chlen-korrospondent AN SSSR(for
mustell).
(Eclipses, Solar)

AUTAOR: Kuz'min- A - D
TITL~,O T-ite Problem of Measurement of the Intensity of Radiation
of the 3ources liavin,-- 8;-~all Angular Dimensions (X'-' voprosu
ob ivmcronii intensivnosti radioizlucheniya istochnikov s
malyi,ai u. -lov,r-. a-mi
j ...A raz-aerc
PERIODI"'AL: Radioteldmika i Ele'111-1tronika, 1958, Vol 3 , Nr 4,
') 561-562 (USSR)
ABSTR&OT: Tlie equivalent temperature of a radiating source at -15-he
rec-eiv= antenna is -iven by Eq.(1), where T((p, G) is
,3htness temperature of the source, G is t-e -ain
the bri,~
0
of the antenna and F(~p 0 is the directivity of the
antenna. lNormally, Eq.4) is simplified to Eq.(2), where
Te is the effective temperature of the source, sLe is the
si-oherical an-le of the source , and ZL is the ann-ular
C3 a
width ol the antenna. It is shovm that i-" the radiation
U ~L I -
pattern of th-- anten-na is exi.ressed by Eq.(4), and if it
fulfils the c-o-nditions -iven by Eq.(5), the teTa r -a ture T
C,
can be ex-,raosed by wilicre (po.5 and is th-e
'aO5
wiath of the radiation T)attorn. The accurate e:.-r)ressiDq
-u)arod
iven by Ea.(G) is co,~, vii6h L~a.("') -and t'le resultin
Car', 1/2

,T'ne Froblem of ",leasurement of the Intuensit.7 Of Radiation of
the Sources having Small Angular Dimensions
0 C)
errors AY6 are shoan in ~he table ,)n ~) 562. If A is to
be less than 2'yo'l the applicability of ]]o. (2`) is r~!stricted
to the range defined by Eq.1117). There is 1 table.
ASSOCIATION: Fizicheskiy institut iii,P.N.Lcbedeva Ai; Sj3R (Physics
Institute Ldi.P. N. Lebedev, Soviet AcaC.eTay of Sciences USSR)
SUBI-1.1ITTED: October 30, 1956
Finally on ';jay 22, 1957
1. Temperature--Determination 2. Radiation--Measurement 3. Antennas
--Performance 4. Antenna radiation patterns--M--asuremen'. 5. Mathematics
--Applications
Card 2/2

AUTHOR: Kuz'min, A.D. 109-3-5-15/17
TITLE: Combin -a-t-ion-&Y-Several Radiators of Different Wavelen6ths
U
in the Focus of a Parabolic Reflector (Sovmeshcheniye
neskol'kikh obluchateley raznykh dlin voln v fokuse
parabolicheskogo reflektore.)
PERIODICAL: Radibtekhnika i Elektronika, 1958, Vol III, lir 5,
t pp ?22 - 723 (USSR)
ABSTRACT: It is pointed out that a parabolic antenna can be
simultaneously employed at several wavelengths if it is fitted
,%kith a number of radiating;, dipolps (see. Fig.1). Sueb - --vstem
i-- --structed in 1955 in the Krymskaya radioastronomicheskaye.
stantsiya Pizicheskogo instituta AN SSSR (Crimean Radio-
astronomical Station of the Physics Institute of the Ac.Sc.USSR).
The parabolic reflector had a diameter of 4 m and was fitted
with two receiving systems operating at wavelengths of 10 and
20 cm (see leig.2). The radiator for the 10 cm band was in the
form of a dipole which was excited by means of a waveSuide
placed in the focus of the paraboloid. The radiator of the
20 cm waveband consisted of two half-way dipoles with reflectors;
these were situated in the focal plane at a distance of 5 cm
from the focus; the dipoles were fed in phase. The
irectional patterns of the antenna for the two wavelengths
UardJ2

109-3-5-15/17
_L
Combination of Several Radiators of Different Wavelengths in the
Focus of a Parabolic Reflector
are shown in Fig-3. It is thought that apart from radio-
astronomy, this type of antenna can also find applications
in radio-relay communication links.
There are 3 figures and 1 Soviet reference
ASSOCIATION: Fizicheskiy institut AN SSSR im. P.N. Lebedeva
(Physics Institute of the ' AS . USSR im. P.N. Lebedev)
SUBMITTED-. May 30, 1957
AVAILABLE: Library of 0ongress
Uard 2/~
1. Parabolic antennas-Operation 2. Dipoles-Applications

AU~HORS: Kuzlmin, A.D., Khvoshchev, A.N. -30V/ 108-13-7-4/14
TITLEt A Wide-Range-Noise (-Voltage) Generator for the Decimeter Range
(Shirokodiapazonnyy shumovoy generator detsimetrovogo diapazona)
PERIODICAL: Radiotekhnika, 1958, Vol. 13, Nr 7, PP- 36-42 (USSR)
ABSTRACT: A noise generator is described which serves the purpose of
measuring the noise factor in radio receiving sets of the deoi-
meter range. Without the necessity of re-tuning it covers the
frequency range of 300-3000 kilooyoles. Within this range the
noise-temperature of the generator is constant and equals
15 9000 K + 7%. The voltage standing wave ratio is lower than
1,5, dying down is less than 35 db. Low noise temperatures can
be obtained by switching on a oalibrated attenuator in series
connection with the noise generator. - The construction of the
device and its experimental investigation are described. As a
technical device this generator is not complete and its pruduc-
tion is complicated. The most important part of the experiments
was carried out in the NII MRTP by A.A.Sidor-ova and V.S.Savellyev
with the collaboration of M.T.Levchanko, L.A.Levchenko and
V.S.Borodach~v. There are 7 figures, and 6 references, 2 of which
a are Soviet.

AUTHORS'- Vitkevich, V. V., Kuzlmin D 20.118.-6-11/43
LKu min A. D.
~
~

a
Salomonovioh, A. Ye., dal.tsov, V. A.
I tsov,
C.,
TITLE: A Radio Image of the Sun on 3,2 cm Wave Length
(Radioizobrazheniye Solntsa na volne 3,2 cm)
PERIODICAL: Doklady Akademii Nauk SSSR, 1958, Vol- 118, Hr 6,
pp. 1091-1093 (USSR)
ABSTRACT: In July, 1957, the construction of a new great radiotelescope
which consists of a stationary parabolic reflector with a
diameter of 31 m was begun on the Crimean station of the
Institute of Physics imeni P. N. Lebedev of the Academy of
Sciences of the USSR (Krymskaya stantsiya Fizicheskogo
instituta im, P. N. Lebedeva, AN SSSR). The geometric axis of
the paraboloid is inclined by + 220 in the meridian plane
which facilitates the annual observation of the radio
radiation of the sun in June-July. In July, 1957, the
investigation of the two-dimensional distribution of the
intensity of the radio radiation over the sun disk was started
on the wave lengths 3,2 and 10 cm. For this work the radio-
Card 1/3 spectrometers worked out by A. Y." Sa-1646hoyich and

A Radio Image of the Sun on 3,2 am Wave Length 20-118 .6-11/43
A. D. Kuz'min were used. The occurring signal was modulated
by means of ferrites and circular wave guides. The carrying-
out of the measurements is discussed in short. These
measurements made possible the recording of the curves of the
distribution of intensity of the radio radiation over the sun
disk, i.e. on a series of subsequent strips the orientation
of which approaches the north-south direction. The totality
of these curves permits the construction of a two-dimensional
image of the distribution of the radio brightness. The small
width of the diagram on the wave 3,2 am makes possible the
detection of a very detailed image of the distribution, i.e.
a radio image of the sun. On the wave 10 a rather coarse image
of the distribution is obtained because of the great width of
the diagram. The radio isophotic lines of the sun on the wave
lengths 3,2 and 10 cm are illustrated in several figures. In
the case of passage of the sun single regions with increased
radio brightness occur in the diagram which is observed as o,
dazzling flash in the recording. With the wave length 3,2 cm
regions with increased radio brightness are observed which are
Card 2/3 distributed very irregularly over the disk. The position of

A F~adio Image of the Sun on 3,2 cm Wave Length 20-118-6-11/43
these regions is very similar to the position of the group3
of the optic spots observed on the same days. The radio
isophotes on the wave length 10 indicate the existence of
active regions the position of which is also similar to the
position of the optic spots and of the active regions with
the wave length 3,2 cm. At present the measuring results ob-
tained are exploited and compared to the optical data.
There are 1 figure and 1 reference, 'hich is Soviet
ASSOCIATION: Fizicheskiy institut im P. N. Lebedeva kkademii nauk SSSR
(Institute of Physics imeni P. H. Lebedev, AS USSR)
PRESENTED: September 25, 1957, by D. V. Skobelltayn, Member of the
loademy, USSR
SUBMITTED: September 19, 1957
Card 3/3

3(l),24(4)
,kUTHORS.- J~umi~nA.D,., and Y.A.Uda.lltsov SOV133-36-1-5131
TITLE: An Investigation of the Polarization of 10-cm Radiation of the
Crab Nebula
PERIODICAL% Astronomicheskiy zhurnal, 1959,vol 36,Nr 1, pp 33-40 (USSR)
ABSTRACT: On November 28, 1957 the extended full assembly of the committee
for radio-astronomy heard a report about the content.s of the
present paper.
The polarization of the radio emission of the Crab nebula at a
wave length of 9. 6 am was measured at the atman Radio-Astronomical
Station of the FIAJ from October to November 1957 with a 31 m
radio telescope by means of a polarizing radiometer. The
preparation of the apparata was carried out by the engineers
IT.T.Levehenko, L.I.Matveyenko, and the technicians M.V.Komarov,
and V.V.Loktionov. The sensitivity of the radiometer amounted to
0.6 - 0.90 K for a bandwidth of 10 Mc/s and a time constant of
20 sec. The antenna temperature of one component of non-polarized
emission was T = 100 0. The authors observed a linear polariza-
a
tion of radio emission of the Crab nebula with a degree of
L+0.5%. The position angle 1420 + 50, and coincides with the
Card 1/2

An Investigation of the Polarization of 10-cm SOV/33-36-1-5/31
Xadiation of the Crab Nebula
direction of the greatest extension of the Crab nebula. The
authors estimated the depolarization effects of the interstellar
medium and the medium of the Crab nebula. They thank V.V.
Vitkevich for giving the theme.
There are 8 figures, and 10 references, 7 of which are Soviet,
and 3 Dutch.
ASSOCIATION:Fizicheskiy institut imeni P.N.Lebedeva Akademii nauk SSSR
(Physical Institute imeni P.N.Lebedev of the AS USSR)
SUBMITTED: January 10, 1958
Card 2/2

80830
.2 0
AUTHORS: Imia, A. D.-. Salomonovich,
Eli
TITLE:
,4.Radio-Emission of Venus in tlie
- %-V
PERIODICAL: Astronomicheskiy zhurnal,
(USSR)
3/033/60/03?/02/008/013
E032/E914
A. Ye.
8mm Region
1960,jol 3?, Nr 2, pp 297-300
ABSTRACT: Radio emission of Venura in the centimeter and millimeter
ranges is of great interest since it provides information
on the atmosphere and surface of the planet, a-ad also on
its period of revolution. Measurements of the intensity
of this emission by Mayer et al (Refs 1 and 3) and Alsop
et al (Ref 2) in the 3 cm and 10 cm regions have led to
a brightness temperature of the apparent disc of about
5500K, i.e. almost tivice as high as the radiometric temper-
ature measured by Pettit and Nicholson (Ref 10) in the infra-
red region of the spectrum. It is thus of particular inter-
est to carry out measurements in the millimeter range,
Measurements reported by Gibson and MeDman (Re.)' 4) gave a
value of 4100 + 3.600. Since this value is not sufficiently
Cardl/4 accurate, the present authors carried out similar measure- t4/'

80630
S/03A/60/037/02/008/013
E032/E914
Radio Emission of Venus in the 8mm Region ~v
ments on 8 mm, using the radio-telescope of the Physical
al
Institute imeni P. M, Lebedev of the Acade of
(USSRI, This EeTescope was described by Salomonovich in
Ref 6 and has a parabolic mirror 22 m in diameter, The
v~idth of the radiation pattern of the radio telescope was
1.91 x 1,91 at 3 db. The detector was a modulated radio-
meter having a sensitivity of 2-30K and a time constant of
5 see. The brightness temperature of Venus averaged over
the apparent disc is shown in Fig 2 as a function of time-,
The dotted line indicates the measuremeat reported by Gibson
and McEwan in Ref 4. The temperature appears to increase as
Venus departs from the inferior conjunction, This is an
Card 2/4 q1

D 13 -~'D
.W
~1/033/60/037/02/0081/013
E032/E914
dadio Emission of Venus in the 8 mm Region
indication of the fact that there is a temperature
difference between the illuminated and unillumirated
parts of the disc, The phase dependenoe of the bright-
ness temnerature suggests that at least part of the radiat--
ion is due to the solid surface of the planet, One of the
possible reasons for the observed difference between the
temperatures on 8 mm. and 3 cm jaay be that there is a
strong dependence of the amplitude of the variable
component,, averaged over the disc, on wavelength (as in
the case of the Moon), However, this is not very probable,
Another possible reason is that there is a stronger ab-
sorption of shorter wavelengths in the relatively cold
atmosphere of Venus. The present measurements indicate
that the bri-htness temperature of Venus averaged over
'the visible disc is 3 700K, This value wD
15 + as obtained
Card3/4

f!0830
3/033/60/037/02/008/013
.6032/E914
Radio Emission of Venus in the 8 mm Region
by averaging over 17 days after inferior conjunction,,
There are 2 figures', 10 references.. of wh:Lch 6 axe
English and 4 are Soviet.
ASSOCIATION: Fizicheskiy institut im, P.. N, Lebedeva, kkademii
nauk SSSR (Physical Institute im, P~ N, Lebedev, Academy
of Sciences USSR)
SUBMITTED: December 15, 1959,
Card 4/4

WMIN A. D - KOSCHENKO, V... SMMOWVICH., A.
"Radio emission of the Moon on 10 cm,'
paper presented at the International Astronomical Union Symposium on the Moon, Leningrad,
MRS 6-8 Sac 1960.

1~' qvq
if / 7;_0
S/033/60/037/oo6/oo4/022
E032/E514
AUTHORS: Kuzlmil~,._A. D., Levchenko, M.T., Noskova, R, I. and
Salomonovich, A. Ye.
TITLE: Observations of Discrete Sources of Radio Emission on
9.6 cm Wavelength
PERIODICAL: Astronomicheskiy zhurnal, 1960, V01,37, No.6,pp.975-978
TEXT: Preliminary results are reported of observations of
discrete sources of radio emission on 4 = 9.6 cm obtained with the
22 m radio telescope of the Physics Institute, AS, USSR. This
telescope was described by Salomonovich (Ref.1). Altogether
50 sources were recorded of which 34 were observed for the first
time In the centrimetre range. The results obtained are illustrated
in the Table on PP-976-977, which gives coordinates and various
characteristics, as well as identifications with optical objects
and radio sources observed by Haddock et al. (Ref-3) and Westerhout
(Ref.4) on 9.4 and 21 cm, respectively. The table includes a
number of interesting objects, among them two planetary nebulae
(NGC 7293 and NGc 6853) for which radio emission cannot be detected.
For these objects an upper limit for the flux density of radio
emission is estimated. These estimates are included in the table.
Card 1/2

S/033/60/037/006/004/022
B032/E514
Observations of Discrete Source-i of Radio Emission on 9.6 cm
Wavelength
Acknowledgments are expressed to the following persons who took part
in building the apparatus and in obtaining the data: G. G. Basistov,
N. F. Illin, V. N. Koshchenko, L. A. Levchenko, S. K. Palamarchuk
and V. I. Pushkarev. Acknowledgment is also expressed to
D. V. Kovalevskly who organized the programme for the radio
telescope during the observations. There are 2 tables and
7 references% 4 Soviet and 3 non-Soviet.
ASSOCIATION: Fizicheskiy institut imeni P. N. Lebedeva Akademii
nauk SSSR (Physics Institute imeni P. N. Lebedev,
Academy of Sciences USSR)
SUBMITTEDt May 14, ig6o
Card 2/2

806-9.2
S/02 60/132/01/21/064
B014 B014
AUTHORS: Vitkeviohp VoYep KuzlminjL A. R.L., Udalltsov, V*1*
Soroohenko
TITLE: Radioastronomical Observations of td'Second Soviet Cosmic Rooke
PERIODICAL: Doklady Akademii nauk SSSR, 1960, Vol. 132, Wo. 19 PP- 85-86
TEXT: The frequently used method of radiointerference was employed for observing
radio signals of the second Soviet cosmic rocket. The angular coordinates of the
container were measured by means of the scientific instruments, furthermore the
power of the signals received and its variations with time. A buzzer signal
was used because of the increased stability of the instruments, the first and
second heterodyne were stabilized by means of quartz. The distance between the
antennas of the radiointerferometerg which were directed to the eastp was
175-9 m, The angle between the perpendicular on the line connecting the
antennas and the direction to the signal source was measured by means of the
radiointerferometer. Formula (1) is given for the determination of this angle,
and formula (3), in which the Doppler effect is considered, is derived for the
azimuth of the signal source. The radiointerferometeris adjusted according to
Card 1/3
NI/

8 0,050
Radioastronomical Observations of the Second S102016011321011211064
Soviet Cosmic Rocket B014/BO14
the intensity of ooBmic radio sources. This system permitted exact determination
of the moment at which the Soviet rocket hit the Moon, as well as of the place
at which the container is located. Fig. I shows a copy of the recorded signal in
the final.stage of the rocket's flight to the Moon~ It is shown that the
recording lost'its sinusoidal oharacter (caused by interferences) as soon as the
container hit the Moon. The rocket reached the Moon on September 14, 1959,
0 h 2 min 22 sac,, The place of the container was established from formula (3)
and is shown in ?Lg. 3. The power of the signal received was determined by
oomp~Lring it ~.Lth the Intensity of the cosmic radio souroe of Oygnus-A. Fig. 3
further illustrates recordings made during the last days before the arrival of
the rocket on the Moon. Periodic intensity variations of 45 secondeq 45 minutes,
and 10 - 13 minutes were observed. In this conneotion the authors refer to the
periodic variation in the orientation of the container and to the Faraday
effect detected in the ionosphere. There are 3 figures, I table, and 8 references,
7 of which are Soviet.
ASSOCIATION: Fizicheskiy institut im. P.N,, Lebedeva Akademii nauk SSSR
physics Institute imeni P.N. Lebedev of the Academy of Sciences of
Card 2/3 V~

Cross-Rolling in the Machine-building (Cont.) Wi
mill balls, bearing rings, bushings and various periodic shapes such as crankshafts.
The ball- and gear-rolling processes developed by TsNIITWh am considered a
major Soviet achievement. Ball-rolling is said to be replacing the manufacture of
balls by pressitig, increasing productivity two to seven times, and saving 10 to 25
percent in expensive alloyed steel. Gear-,rolling is a current development project
in the USSR. Rolled-gears are reported to have been successfully produced to grade
2 accuracy, vith a class 7-10 surface finish. Methods for determining rolling
forces, stresses,moments and powerbased on modem concepts of the theory of
plasticity and strength of materials are discussed, and formulas derived. The
author states that the mechanical properties of parts press formed, or machined
from periodic rolled stock, are considerably higher than those made from convent-
iona3 plain rolled stock, not to mention a 20 to 30 percent saving in material.
The development of the theoretical principles and technological processes of cross-
rolling and helical cross rolling in the USSR is said to have been carried on
intensively since 1942. This theory was developed by V. S. Smix-nov on the basis
of experiments conducted at the Urallskiy politekhnicheskiy institut (Ural Poly-
technic Institute) and later at the Leningradskiy politekhnicheBkiy Institut
(Leningrad FoUtechnic Institute). The development of machinery and equipment
for cross #rolling and helical cross rolling was supervised by A. I. Tselikov at the
TsNIITMASh - Tsentrallnyy nauchno-issledovatellskiy institut tekhnologii i mashin-
ostroyeniya (Centi-41 Scientific Research Institute of Technology and Machinery).
C""/-9---

22310
S/107/61/000/007/001/002
4 D201/D304
1722 0 1'2 /
AUTHORS: Kuz1min._A,.Yand 8dlomonovich, A.
TITLE: Radioastronomical observations of Venus
PERIODICAL: Radio, no. 7t 1961, 6-7
TEXT- In the present article theauthors discuss briefly
radioastronomy aq a means of investigating the physical properties
of the surface ot"Venus.. The use of radioastronomy for this pur-
pose is possible because Vdnus,..b *sing a heated body, radiates ele-
ctro-magnetic waves. The power or"this radiation is determined by
the body temperatu're and the -radiation capac'ity, the latter depend-
ing on the body structure; according to Kirchhoff's law this radi-
ation capacity is proportional to its absorption'capacity. In
radioastronomy the intensity of radiation of an-ideally black body,
whi6h is characterized by the.density of radiat *Ion flux P (defined
as'the total energy emitted by the source in'the fre uency band
eg. 1 c/s and falling in I see. onto a surface of D) is detennined
Card 1/5

22310
S/107/61/000/007/001/002
IPl/D304
Radioastronomical obqervations of Venus
I 2K7'Q
by the body temp Ierat e T by the following expression!Z
where X = 1.38 x 1PS Joule/OC - the Baltzmann constant,A - the
wavelength being received,-rL- solid angle subtended by the body
under observation. The power of the signal being received is given
by. I- N here A is the effective antenna area; Having
~~A K7'QA w
2
measured the power of the signal received from Venus, it is easy
to determine its brightness temperature ( defined as the tempera.-
ture of an absolutely black body; radiating the same power, in the
same frequency band and within the same solid angle as the source).
Th6 radiation capacity of a body is proportional to its absorption,
capacity and may be different for different wa,: -~ngths. Thus.the
earth's.atmosphere is completely transparent for wavelengthsfrom
7 - 10 -m down to 2 am., but becomes. noticeably absorbing for sh6rter
wavelengths. By applying the above pri 'nelple to radiation emitted
by Venus, both its atmospheric and surface temperatures can be
Card 24

22310
S/107/61/000/007/001/002
D201/D304
Radioastronomical observations of Venus
determined. Since the angular dimensions of Venus are very small
its radiation flux is very small, e.g. at a wavelength of 10 cm
p = 10 - 25 watt
M2/c/s
and observations are therefore extremely difficult. After mention-
ing the first observations of Venus in 1956 by American scientists,
the authors point out that fuller data were obtained by them per-
sonally using a 22 meter radiotelescope of the Pizicheskiy institut
(Institute of Physics) of the Academy of Sciences, USSR. The ob-
servations were made at a wavelength of 8 mm. The resulting in-
crease in signal strength permitted determination of Venus' tempe-
rature at various degrees of its illumination by the sun. It can
be assumed that the illuminated surface of the planet has a tempe-
rature of several hundred degrees centigrade. It follows that
future radio installations on Venus would have to be able to with-
Card 3/5

22310
S/107/61/000/007/001/002
D201/D304
Radioastronomical observations of Venus
stand working temperatures of this order. The temperature of Venus
as obtained using an 8 mm wavelength is about 1.5 times smaller than
that obtained using lower frequencies which seems to indicate that
shorter waves are partly absorbed in its colder atmosphere. It
seems that the dark side of Venus has a temperature of about OOC.
Another deduction which can be made from the above observations is
that because of absorption of 2 am. waves in the atmosphere of
Venus, this atmosphere should contain water vapor or carbon dioxide
or both. It also proves that it is unlikely that the surface of
Venu5 consists of nothing but oceans. An "all-water" surface would
eliminate the large differences in temperature observed between its
dark and illuminated parts. The above is based on the assumption
that radiation from Venus is of thermal origin. There are serious
indications that this is so, e.g. the fact that measurements using
3 and 10 cm. both gave the same brightness temperature. Nevertheless
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22310
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D201/D304
Radioastronomical observations of Venus
certain scientists r Abstractors note: Not mentioned. 7do not
exclude the possibility of the so-called non-thermal m7e-chanism of
radiation from the planets, in which case the observed temperature
would not be the true planet temperature. There is 1 figure.
Card 5/5 A

26658
S/560/61/000/007/002/010
3, 0 0 o 4 2, E032/Ell4
AUTHORS: Vitkavich, V.V.j Kuz'min, A.D., Sorochenko, R.L.,
and Udalltsov, V.A.
TITLE: Results of radio-astronomical observations obtained
with Soviet space rockets
PERIODICAL: Akademiya nauk SSSR. Iskusstvennyye sputniki Zemli,
No.7, Moscow, 1961, pp. 23-31
TEXT: An important problem in satellite and rocket
experiments is the determination of the coordinates of the space
vehicles. Since the satellites and rockets usually carry a
stabilized transmitter, the problem is reduced to the determination
of the position of the radio source and is analogous to the radio-
astronomical problem of the determination of the angular
coordinates of discrete sources. Such determinations are usually
carried out by the radio-interferometer method. The present
authors have used this method in the observation of the radio
signals from the first, second and third Soviet space rockets.
The use of radio astronomical methods has enabled them to measure
the intensity of the signals as well. The observations were
carried out on 183.6 Mc/s. The apparatus and the experimental
Card 1/8

26658
Results of radio-astronomical .... S/56o/61/000/007/002/010
E032/Eli4
method employed are described by the present authors in Ref.1
(Radiotekhnika i elektronika, 1961). The impact of the second
space rocket container on the lunar surface oi-curred on September
14, 1959, at 0 hr 02 min 22tl see (this time Is corrected for the
time of propagation of the signal). The selenographic coordinates
of the centre of the region of impact were found to be:
latitude 300, longitude -30 (crater Archimedes.). During the
observations of the first and second space rockets use was made of
antennas with horizontal polarization. It i3 clear from the
records obtained that in addition to a "quasi-sinusoidal" intensity
variation due to interference there were also faster changes.which
were apparently due to the rotation of the container. The period
of these changes was 30-50 see for the first and 4o-6o see for the
second rocket. Comparisons of the records of signals from Soviet
space rockets with those for known discrete sources of radio
emission were used to estimate the intensity of the signal
throughout the entire period of observations. The Cyg A source
was used for the comparison. Figs. 4 and 5 show the variations in
the intensity of the signals (slow component) in units of the
power reduced to an isotropic emitter at the distance of the
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26658
Results of radio-astronomical .... S/560/61/000/007/002/010
E032/Ell4
rocket. A consideration of these curves shows that in addition to
the fast changes mentioned above there were also slower variations
in the signalfiam the first space rocket (characteristic period$
8-12 min and 40-60 min). In the case of the second rocket there
was a period of 45 min, reducing to 10-13 min. These changes may
be due to the rotation of the container and the Faraday effect in
the earth's atmosphere. In the case of the third rocket antennas
with both horizontal and vertical polarization were employed.
Typical records are reproduced. Analysis of the intensity records
with two mutually perpendicular polarizations showed that there was
signal fading on October 4. 5, 6, 12 and 17, 1959, with a period
of about 3 min. In addition there was a signal variation reducing
the amplitude to about 50% which had a period of about 1.5 min.
These variations are apparently due to the rotation of the
automatic inter-planetary station. There was some evidence that
there was a further variation with a period of 20-30 min, and this
may be due to the Faraday effect. The energy flux p was
calculated from the expression
P = jAf-m
Card 3/8

26658
Results of radio-astronomical S/56o/61/000/007/002/010
E032/E114
where j is the energy flux from a discrete source with a
continuous spectrum, b6f is the bandwidth of the receiver used to
record the discrete source, and m -1.9 the ratio of the space-
rocket to discrete-source signal. The emitted power P was
calculated from: P = p47ER2
where R is the distance from the earth (isotropic source emitting
equally in both polarization componentB).
There are 7 figures and 7 referencesl 2 Soviet and 5 English.
The four most recent English languag-~ references read:
Ref.4; P. Moore, Nature, V.184, 502, 1959.
Ref-5: H.P. Wilkins, Nature, V.184, 502, 1959.
Ref.6: G. Fielder, Nature, V.185, .11, 196o.
Ref.7: G. Whitfield, Paris Symposium on Radio Astronomy, Stanford,
California, 1959, p. 299.
Card 4/8

310351621W0100210131052
~lo Y 7) AOO11A1O1
AUTHORS: n_z~~ I Salomonovich, A. Ye.
TITLE: Radio observations of Venus on wavelength 9.6 cm
PERIODICAL: Referativnyy zhurnal, Astronomiya I Geodeziya, no. 2, 1962, 43,
abstract 2A375 ("Astron, tsirkulyar", 1961, apr. 30, no. 221, 3-5)
TEXT: This is a report on radio observation of Venus on wavelength 9.6 cm
by means of a 22-m radio telescope of the Physical Institute imeni Lebedev,
AS USSR. The authors present an example of recording the transit of Venus
across the direction diagram of the radio telescope near the instant of Inner
conjunction of the planet on April 22, 1961. Brightness temperature amounted on
some days to - 1,OOOOK and was subjected to strong variations from one day to
another. The authors hold that an essential part of the Venus radio emission in
the 10-cm wavelength range is played by a non-thermal component; its source is,
possibly, Venus radiation belts, similar to Earth's belts. There are 15 refer-
ences.
M. Frolov
[Abstracter's note: Complete translation]
Card 1/1

s/141/61/004/003/003/02-0
E)-,3/E435
AUTHORS: Koshchenko. V*N,-,~ Salomonovich, A,,Y6,`1'
TITLE: Thermal radio emission from the moon in the 10 cm band'
PERIODICAL: Izvestiya vysshikh uchebnykh zavedeniy, Radiofisika
1961, Vol.4, No-3, pp.425-427
TEXT: Previous investigations in the 10 cm band have been
described by H.L.Kaydanovskiy et al (Ref.1; Transactions of the.
Fifth Conference on the Problems of Cosmogony, Iz&. AN SSSR,-H*#
1956, P.347) and K.Akabane (Ref.2: Proc, Japan. Akad., 31, 16l
(1955)). According to the first, the mean lunar brightness
temperature, averaged over the disc, is 1300K with a variation 'of
8% due to the phase changes. The corresponding values in the- -
second are 315*K and 25% variation. A single measure of 2150K in
referred to in the paper of J.H.Piddington and H.C.Minnett
(Ref.3: Austr. J. Sci. Res., 4A, 459 (1951)). In order to
clear up these discrepancies and to study the variation in thermal
radio emission with phase, measurements have been made by the-
present authors at a wavelength of 9.6 cm.' The 22 m telescope
of the Lebedev Physical Institute was uBedj this and the receiver
used have been described in earlier work. Antenna temperatures
Card- 1/ 3

S/141/61/004/003/003/020
Thermal radio emission from ... E133/E435
were obtained in the range 132 to 1540K, depending on the phase.
Successive scans were made across the lunar disc, systematically
displaced from one another. The maximum value thus derived for
the antenna temperature corresponded to central passage acrosa-the
disc. The temperature obtained was averaged over the whole disc.
Amplification and scattering coefficients had been obtained
earlier from observations of Taurus A (Ref.6: A.M.Karachun et al,
Radiotekhnika i elektronika, 6, 430 (1961)). The present
observations, made during April -May 1960, gave an average
brightness temperature of 230 1 3-5*K. The variation from this
average did not exceed 1 1.5% at any lunar phase. This result
agre,es well with the data given in Ref.7 (P.G.Mezger, H.Strasslg
Planet Space Sci., 1, 213 (1959)) for the 20 cm band (2500K :t 12%)
and also with a single measure made by G.Westerhout (Ref.8: Bull.
Astron. Inst. Netherlands, 14, 215 (1958)) of 232 �-50*K.
The absence of temperature change with phase in the decimeter
band agrees with the thermal emission of the Moon predicted by
V#S.Troitskiy (Ref.10: Astron. zh. 31, 511 (1954)).
]~.L.Kaydanovskiy, M.T.Turusbekov and S.E.Khaykin are mentioned in
Card 2/3

41/61/004/003/003/020
Thermal radio emission from 3/E435
the paper. There are I figure and 10 references: 5 Soviet-bloc
and'5 non-Soviet-bloc. The referencei to English language
publications read*as follows:
Ref.2: an quoted in textj
Ref-3: as quoted*in text;
Ref.7: P.G.Mezger, H.Stranal, Planet Spa-,~e Szi., v.1, 213 (1959).
ASSOCIATION: Fizicheskiy institut im. P.N.Lebedeva AN SSSR
(Physics-InatituteF imeni P.N.Lebed-ev AS USSR)
SUBMITTED: November 10, 1960
Card'3/3

//17/ 119-~)
AUMORS Kibiyakov, A,G,
TITLE Ract i o e- rr.', s -s in f j~-ni Vc-r-,
PERIODICAL., I zve S va vys 311 ! k1i %I, h 1
1961, Vol.it, Nv.3,
TEXT~ Obaerva,,!-ns ~~f Vewis wi~,-- tht
22 m radio 1~eleszope *f tht Fi~_' 11-
P.N.Lebede-~,- AN SSSR In-0411_
AS USSR)
~n the 4 mm band, The. ineo -hod wlt! b,-~,n
Jes:lri.bed previou_~Iy (Ref,- A~D,.K,,z . ; 11,_
AsIxon, MI., v~37, 297 11960)),
by
obser,--at-i3n w.ith -.Antsnna
4emperature wa6 dek~srm'rit-d by two,m
4 by
inz6r*.ing an absorbLng
a t h, Tho,~ &rroi- the IN, I T"U'., t wo S
.Within 7% The se-:)nd mFthud w"-
gna
---,h
Values for 4 mm wA-,n-c~ well h -a;
us6d as a :hec,k on t1he iii-6t. 'T'11,., W_'i 114~
Card 1/2

Radio tatission front VenuA
obsex-va,tions probably ii"-s iri the
tempsrature over the whole of tho
,.onne!7,,ion, the half-idth of thi-- -m,
found to be 11,6. The amomit -.f
investigated by oLser-vi.ng the Stir. Jt,,;
t empera tur e of V~6nus ~ a -.era ged
found to be 390'K # 120'K, r
bloc and I non--So,,,i;~# -blo_ rh"-~
publio:atIon r6ada Na
Ref.32 A.W.Straj'.!on
j,
LI s
and
hen
E,i4-1-sn language
ASSOCIATIONS. Fiz1:-.heskt;y
(Physic's
P,r! Gcjz K A T h
Ins: tute foi-
SUBMITTED: M;%V 9,
C-ird 2/2

21659
3, / 7/ 0 0 ol//, // 2.9, fl 2,7) S/109/61/006/003/014/018
,/,/goo E032/E514
AUTHORSa Karachin, A.M.,.Kuzl in&-&Q. and Salomonovich, A.Ye.
TITLEt A Study of Some of the Electrical Antenna Parameters
of the 22 m Radio Telescope of the Physics Institute
AS USSR
PERIODICALa Radiotekhnika i elektronika, 1961, Vol.6, No.3,
pp-430-436
TEXT: The present authors report the results of preliminary
studies of the polar diagram, directivity and a number of other
parameters of the parabolic antenna of the 22 m radiotelescope of
the Phys�cs Inst�tute of the AS USSR imeni P. N. Lebedev. The
experiments were carried out on 9.6 and 0.8 cm. Fig.1 shows a
typical polar diagram obtained from a record of transits across
the Cassiopea A source. The average of 27 measurements of the
width of this pattern at 3 db was found to be 19'.0 + 0'.15. The
theoretical width at 3 db under optimum conditions sKould be
18'.3 and 191.6 in the H and E planes. The side lobes do not
exceed 20 db. The above figure is corrected for the finite
angular dimensions of the 'source, as described by P~ G. Mezger(Ref5)
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A Study of Some of the Electrical ... S/109/61/006/003/014/018
E032/E514
The Taurus A source was used to determine the effective area of the
antenna, and assuming that P = 7.9 x 10- 24 W M_2cps -1 and the
measured antenna temperature T a = 52-30 + 0.50, the effective area
was found to be A = 190 m2 + 15%. The antenna surface utilisation
factor was found to be 0.59. Fig.2 shows a typical polar diagram
in the H plane; the width at 3 db with the feeder in the optimum
position was found to be V.7 + 01.1. The width in the E plane
at 3 db was found to be 21.1 + 0'.1. The expected widths were
V.6 and 11.7~ respectively. The first side lobe w2s found to be
at 12~2 db. The effective area on 0.8 cm was 150 m + 20% and the
antenna surface utilisation coefficient was 0,45. IT is
concluded that the accuracy with which the surface of the reflector
has been manufactured ensured a polar diagram approaching the
theoretical form. The following persons took part in the
measurements N. A. Amenitskiy, G. G. Basistov, V. N. Koshchenko,
M. T. Levchenko, N. F. Il'in, S. K. Palamarchuk and V. I. Pushkarev.
D. V. Kovalevskiy and K. 1. Stepnov are thanked for arranging for
this work. There are 3 figures and 12 references: 7 Soviet and
5 non-Soviet,
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A Study of Some of the Llectrical ... S/109/61/oc)6/003/014/ol8
E032/E514
ASSOCIATION: Fizicheskiy institut im. P. N. Lebedeva AN SSSR
(Physics Institute imeni P. N. Labedev AS USSR)
SUBMITTED: I-lay 19, 1960
F 1 1
Card 3/3
Fig. 2

ew.a X0
AUTHORS: Vitkevich, V.V.,
Borochenkop R.L.0-Ord-THI-rYsov,
TITLE: Radioastronomical
rockets
SX 285
10~1~161/006/009/001/018
D201/D302
Kuzlmin, A.D., Matveye%ko, L.I.9
V.A.
observations of Soviet- cosmic
PERIODICAL: Radiotekhnika i elektronikay v* 6t no. 9, 1961,
1420 - 1431
TEXT: This is a description of a specially designed radio inter-
ferometer with phase modulationp as used in tracking the first
three Soviet space rockets. The principle of a two channel phase
divergent reception was used to detect changes in the signal ampli-
tude, due to relative changes of the position of transmitter with
respect to the lobe of interference diagram. In receiving a signal
with continuous spectrum the fluctuation sensitivity in units of
temperature (T a) of the antenna is given by the well known equa-
tion
Card 1/7

2851-8
lOY61/006/009/001/018
Radioastronomioal observations ... D201 D302
ST a,,To _T (7)
a Ve V=-r
where ct, - a dimensionless factor depending on the properties of
the receiverp T 0 - standard ambient temperature; F e = (Ta + T id/
/To - ~he equivalent input temperature determined by noise of the
receiver; Tin ~ (F - 1); P. noise factor of the receiver; T -
r V a
antenna temperature; T - time constant of the output cct; Af -
passband between input and detector. The bloc diagram of the recei-
ver is shown; the operating frequency was 183 .6 Mc/s, that of the
transmitter in the rocket capsule. The interferometer had two pa-
rabolic antennae 8 x !a and 11 x 28 m, spaced in the E-W direction
by approximately 176 m. Total length of both antennae was 8 m. The
antennae were reilluminated from their focal points by specially
designed radiating systems, assuring best possible illumination for
two linear polarizations perpendicular with respect to each other.
Yu-P. Ilyasov participated in their design. A schematic of the LAy
Card 2/7

~8518
S/109/61/006/009/001/018
Radioastronomical observations D201/D302
illuminating system is also shown, the three resonant dipoles were
connected by equal lengths of a PK-20 (RK-20) cable to a common
feeder. The directional patterns and utilization factors of the an-
tenna areas were determined from solar radiation. For both antennae,
the area utilization factor was about 0.5. Phase modulation at a
frequency 72 c/a was adiLeved by changing the phase by 1800 by mean:3
of periodical variation of the electric length of the wall connect-
ing the local oscillator with one of the mixerag so thaL the re-
ceived signal was ampiitude modulated al thie frequency. The phase
modulator was designed around a standard hybria switch. The switch-
ing elements were light house diodes type 6 A39 (6D-)D) driven by
the sinusoidal modulating voltage. The attenuation introduced did
not exceed 2 db. The change in ihe diode slopes by way of changing
the bias and the insertion of The modulat3r into the local oscilla-
tor circuit permitted the parasitic amplitude modulation of earlier
systems to be reduced considerably. The modulator used perm-A'Ated
the radio meter with phase modulation to be changed into that with
AMt this was achieved oy suppressing the modulating voltage at one
of the diodes. The signals were preamplified ai UHP by ampiifiers 14
Card 3/7

2P518 9/001/018
S1109/611 006/'()0
Radioastronomical observations D20./D302
placed directly at -the antennae. The noise factor of UNF preampii-
fiers was 5. The amplilfied signals from each antenna were changed
afteAr buffer stages to -the jet IF of 6.95 Mc//s and fed into two
channels with a 900 phase shift between them. A double frequency
conversion was ueed. The 1901. 554 mc/s frequency of the first 1c-
cal oscillator was pr~auced by a thermostatically controlled cry-
stal oscillator workin,~ at 9,07A mc/s with subsequent inultipilLcia--
tion by 21. Ps relarlve -Mi3tability was -.C,-6 and hence the pass-
band of a mono chroinati c aignal was chosen to be 2Kc/s. To secure
,ption with the s:_gna, Crequency shifting due to the Dopple:r
rece
eff6ctp step tuning w.*"hi% '~ K,c/s was provided formed by 5 reac-
nant ci:rcuits detunei in --! Kc/s steps. On -.cp of the first L.O.
could be continuously -tu.:A-d with-in 3.2 Kc/s. For calibration pur-
poses, when a urider-pass:and is required, he second amplifier pass
band could be switchea f_-.irt 2 -to 10 Kc/s without affecting -.unilig
and gain. The signal, dei-cted by a synchrono.ts detector, was tuken
from an RC outp*xt fi.-Lter ii'rh 't,ime constant E _- 26 see. This va-
lue permits achieving -thc requ%red fluctuation sensitiv'lty and in
practive does not. affect -he iiiterference arn-,:.Lituae. All power 6up-
Card 4/7

S/169/'61/006/009/001/018
Radioastronomical observations ... D201/D302
3
plies were stabilized with a stabilization factor of about 10 . The
signals were recorded on electronic automatic recorders type 3n[7-9
(EPP-4?9) monitored by one minute time markers. The experimental da-
ta of'the receiver sensitivity are tabulated. The experimental sen--
sitivity was about half that calculated from Eq. (7). The maximum
sensitivity of the interferometer, corresponding to The minimum
detected power levels, are also tabulated. In making final adjust-
ments (M.V. Gorelova particiRated in the final adjustment method
evaluation) constant and timevarying parameters had to be conside-
red. The constant parameters are y - angle between the horizontal
plane and the projection of the base onto a vertical east-west pla-
ne, e - angle between the east-west direction and projection of
the base onto a horizontal plane and D - e of the interferome-
ter distance between the antennae"'are dArmined by fixea antenna
geometry: Tn/;Lon the ot*r hand :.s determined by electrical
lengths of the cables and phase characteristics of input stages
and can vary with time. A geodesical survey gave the follow-Ing re-
sults: D = 175.896 m; Y = 20441; 0 7.41 so that the expression
Card 5/7

2A511
S/I0q/6"I/0O6/OO9//0O.';'./O18
Radioastronomical observations ... D20I./D302
for the azimuth of the source is given by
A- - 1790461 + arc sin[2-' OOU 006 ~ (r, - YO -
Sin Z (10)
- 0.047669 ctg zjq
where n is the number of the lobe and z - the zenitb angle of
the 8oufte. The paramet-r -r was determined from
r tA source
V kil)
T
where T - the period'-'. Pf the interference lob,-., t r - The calculated
and tA source - the real instant at which the source parses through
the maximum of the interferen~~e diagram. Owing to !he fInite value
of the output cct time constant, the instani t at which
'A source
the source crosses the maximum of the diagram does not '~brrespond
with t repreeenting the maximum deflection of ihe seconding instru-
Card 6/7

25518
3/109/61/006/009/001/018
Radioastronomical observations D20!/D302
ment. L T thus was introduced, as given oy
'12 (:E)216 (12)
tA - tAsource 3 T
in adjusting the arrangement.~, The above 09strument and method of
observations were applied to tracking the first, second and third
Soviet- space rockets, launched January 2, Septei;ber 12, and Octo-
ber 4, 1~59, respectively; measuring their angular coordinates and
measurements of the intensity of the received signal were also
carried out. There are 8 figures tables and 11 references: 5 Sov-
iet-bloo and 6 non-Soviet-bloca T e references to the 4 most recent
English-language publications read as follows; G. Fielder. Natmre,
1960~ 1851 4705, 11; H.P. Wilkinsq Nature, 1959, 1849 4685, 502;
P. Moore, Nature, 1959, 184, 4085, 502; J.G. Dairies, A.G.B. Loyell,
Nature, 1959, 194, 4685, 501.
ASSOCIATION: Fizicheskiy instiiut im. P.N. Lebedeva AN SSSR (Tnsti-
tute of Physics im. P.N. Lebedev, AS USSR)
SUBMITTED: October 4, 1960 OK
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89323
S/033/61/038/ool/oo6/olq
E032/E314
AUTHORS; Karachun, A.M., Kuzlmin, A.D. and Salomonovichq A.Ye.
TITLE: observations of Some screte Ra o Sources on 3.2 cm
PERIODICALs Astronomicheskiy zhurnal, 1961, vol. 38, No. 11
pp. 83 - 86
TEXT: The 22 metre radio telescope of the Physics Institute
imeni P.N. Lebedev of the AS USSR (Salomonovich - Ref. 8) was
used in June, 1960, to investigate a number of discrete radio
sources on 3.2 cm. The sensitivity of the radiometer at a time
constant of 4 sec was 1.5 0K. The parameters of the aerial were
determined from measurements on Tau A. Fig. 2 gives the radio
emission spectra of the following sources; Orion; Omega;
Cyg A; Cas A based on the published results and the results
ob*uained by the present authors. The present results are
indicated by the double circles. The following table gives
results of measurements and calculations of the flux p and
angular dimensions G) of the observed sources:
Card 1/5

89323
S/033/61/038/ool/oo6/019
E032/E314
Observations of Some Discrete Radio Sources on 3.2 cm
Source a 19
0 61950 TiK P.12 24 0 G
5 W/M cps
Tau A 05h3lm.5 220 00, 40 [61 L3A]
Orion 05h32m.8 -5 a 251 24.5 3.6+.o.8 5'pl+O*.5
Oinega 18hl7m.65 -16 '151 33.5 570.8 5.87o~5
G-yg A 19h57m.75 4o* 35f 1.1.5 1.770.4 -
Cas A 23h2lm.2 580 321 34 571 41
The figures in square brackets are assumed. A consideration
of the above spectra of Orion and omega confirms the thermal
mechanism of their origin. The spectrum of Cyg A cannot be
A
described by a power law of the form p = Af with n = const,,
The numbers on the giaphs, Fig.2,refer to the reference list at
the end of this paper. The angular dimensions for Cas A are in
Card 2/5

89323
S/033/61/038/001/006/019
E032/E314
Observations of Some
good agreement with
Minkovski (Ref. 27).
N.A. Amenitskiy, N.F.
assistance.
There are 2 figures-,
and 20 non-Soviet.
Discrete Radio Sources on 3.2 cm
the data of Jennison (Ref. 25) and
Acknowledgments are expresseci to
Illin and Y.N...Koshchenko for their
I table and 27 references: 7 Soviet
ASSOCIATION: Fizicheskiy i-t im. P.N. Lebedeva Akademii nauk
SSSR (Physics Institute im. P.N. Lebedev of
the Academy of Sciences of the USSR)
SUBMITTED: August 25, 1960
Card 3/5

L , E9, -12 3
S/033/61/038/001/006/019
E032/E314
Observations of Some Discrete Radio Sources on 3.2 cm
Fig. 2a: Fig. 2b:
0 /a
-A 11 015
101
/ON
ft

.0pUVH

MOM IN
- -
0
~ J.,
%,Dig

Omen
1
1 1 A[
'0
to
Of IGH
lUCM
6
IN, /am
Card 4/5

893?3
S/033/61/038/ool/006/oig
E032/E314
Ubservations of Some Discre-te-Radio Sources on 3.2 cm
2c: Fig. 2d:
0, lee
101
;0fl
tat
Card 5/5
d 7S
IPZ3
4
19 2zz

x
IM 16M

pe 1

173o
3
o
S/033/61/038/002/009/011
E032/E4i4

AUTHORS: Kuzlmin, A.D., Salomonovich, A.Ye. and Udalltsov, V.A.
TITLE: On the Radio Emission of the Planetary Nebulae
NGC 6853 and,NGC 7293
PERIODICAL: Astronomicheskiy zhurnal, 1961, Vol.38, No.2,
pp-373-375,
'
TEXT: '.
The present authors have made an attempt to detect the
j.radio emission of NGC 6853 and NGC 7293 on 9.6 cm. -The,NGc 6853
nebula was examined at the end of 1958 with the 31 m radio-
telescope of the Krymskaya stantsiya (Crimean Station) of FIAN.
The above radiotelescope has been descr~.bed by V.V.Vitkevich and
V.A.Udalltsov
(Ref.2) and the radiometer has been described by

A.D.Kuzlmin and V.A.Udalltsov The radiometer had a
(Ref-3).
sensitivity of 00.5
at a time constant of 20 sec. It is
dug to the'
estimated that the flux density of radio emission
2
1
2
W m-
cps-
NQC 6853 nebula on 9.6 cm, must be less than 4 x 10-
.
The NGC 7293 nebula was examined with the 22 m radiotelescope of
FIAN at.. the beginrAiiig of 1960.. This radiotelescope has been
described~by A.Ye.Salomonovich (Ref.4). It is estimated that the
Ca r dA A

2.083
S/033/61/038/002/009/011
On the Radio Emission E032/E414
flux density for.the above two nebulae on 9.6 cm turns out to be at
i least by an order of magnitude lower than that reported by
A-F.D.Drake and H.T.Ewen (Ref.1) on 3.75 cm. Since the accuracy
of the present results is said to be higher by an order of
'
]
magnitude than the results reported by Drake and Ewen, it is
suggested that the latter are incorrect. Using the upper limits
for the flux density, the present authors estimated the emission
measure ME the electron density n and the mass M of the.
above two planetary nebulae. These three quantities are
estimated from the following formulae
NE = 38 - I Vpq)-~;
a P. 1(pi

-
4.8. 10-1 its
T
'
ie

where y is the angular diameter of the source in fractions of &
degree and R is the distance in parsecs. These formulae are

a
C
rd.2/4

S/033/61/038/002/009/011
On the Radio Emission E032/E414
taken from G.Westerhout's paper (Ref-5). The estimates are
summarized in the table. The angular dimensions of the nebulae
which are quoted in the table are taken from B.A.Borontsov-
Vel-lyaminov's paper (Ref.6). The aistances are taken from the
latter paper and from the paper by I.S.Shklovskiy (Ref-7). There
are I figure, 1 table and 7 references: 5 Soviet and 2 non-Soviet.
ASSOCIATION: Fizicheskiy in-t im. P.N.Lebedeva
Akademii nauk SSSR
(Physical Institute imeni P.N.Lebedev,
Academy of-Sciences-USSR)
'SUBMITTED. June 7,
1960

INN
30822
S/033/61/038/005/010/015
31030 9133/19435
AUTHOR: Kuzlmin, A.D,
TITLE: The discrete source of radio emission
a . 8h53m7; 6 . i0i6t
PERIODICAL: Astronomicheakiy zhurnal, v.38, no-5, 1961, 905-911
TEXT: The 22 metre radio telescope of the FIAN has been used'to
study this source at 9.6 cm. It has been found to have the same
dimensions in R.A. and'Dec - 181 + 3' or 201 + 3' - depending on
the method of computation. The flux dens itg for a Gaussian
brightness distribution is (140 + 20) x 10-2 V M-2. cps-3 . The table
compares this with values obtained'by other authors. The values
obtained by G.Westerhout (Ref-3: Bull. Astr. Inst. Net!--rl., V.14
no.488, 215, 1958), B-T-Mills, O.B.Slee, X.R.Hill, (Ret.9: Austrai.
J. Phys., v-11, 360, 1958) and-G.R,Vhitfield (Ref.11: Monthly
Notices Roy. Astron. SOC., vf1201 6, 581, 196o) have been
corrected by the author. This data can be represented by an
equation of the form p . Akn with n w-0.4 + 0.1. A source with
similar structural characteristics is IC 443 Zhich is believed to
be the remnant of a type II supernova. Fig.2 compares the spectra
Card 1/0 ~

30822
S/033/61/038/005/010/015
The discrete source of radio ... E133/E435
of the two sources. IC 443 has a spectral index n a 0.5 � 0.1.
Assuming that this non-thermal radiation is due to relativistic
electrons, it is possible to calculate the total electron energy of
the radio source: as Burbidge has done for IC 443 (Ref.19:
G.R.Burbidge, Paris Symposium on Radioastronomy, 1959). It is
first necessary to know the distance to the object. Using
I.S.Shklovskiyls method of distance determination for type II
supernovae (Ref.20: Astron. zh., V-37, 369, 196o), a distance of
3500 PCs is obtained. This gives a radius of 9 PCs for the
nebula. The radius of IC 443 is 12 pea by the same method. The
upper and lower frequency limits for the nebula (correspondinf to
the maximum and minimum electron energies) are taken to be 10
and 1010 c/s as in Ref.19. The source then radiatea
2 x 1o34 erg/sec as compared with 4 x 103 for IC 443. The author
next tries to estimate the magnetic energy of the nebula (assumed
spherical). Assuming that the magnetic energy is equal to the
kinttic energy of the particles, he derives a value for the field of
10- gauss. The total energy of the nebula is then 1o50 erg,
compared with 4 x 10-5 gauss and 1.2 x 1050 erg for IC 443.
Card 201k

08 2
S/033 61/038/005/010/015
The d> rote source-of radio ... E133/9435
of the two sources. IC 443 has a spectral index n a 0.5 ;t 0.1.
Assuming that this non-thermal radiation in due to relativistic
electrons, it is possible to calculate the total electron energy of
the radio source: as Burbidge has done for IC 443 (Ref.19:
G.R.Burbidge, Paris Symposium on Radioastronomy, 1959). It is
first necessary to know the distance to the object. Using
I.S.Shklovskiy's method of distance determination for type II
supernovae (Ref.20: Astron. ah., V-37, 369, 1960), a distance of
3500 Pcs in obtained. This gives a radius of 9 pce for the
nebula. The radius of IC 443 is 12 pcs by the same method. The
upper and lower frequency limita for the nebula (correspondinf to
the maximum and minimum electron energies) are taken to be 10
and 10-10 c/s as in Ref.19. The source then radiates
2 x lo34 erg/sec as compared with 4 x 1o33 for IC 443. Thw author
next tries to estimate the magnetic energy of the nebula (assumed
spherical). Assuming that the magnetic energy is equal to the
kin%tic energy of the particles, he derives a value for the field of
10- gauss. The total energy of the nebula is then io5O erg,
compared with 4 x 10-5 gauss and 1.2 x 100 erg for IC 443.
Card 2/p q

30822
S/033/61/038/005/010/015
The discrete source of radio ... E133/E435
This seems to confirm that the object is a type II supernova
remnant. It might be expected that polarized radiation could be
observed from such an object. It has been shown, however, that
symmetrical objects do not produce polarized radiation (Ref.22:
A.A.Korchak, S.I.Syrovatskiy, Astron. zh., v-38, 885, 1961).
It would be interesting to search for an optical identification,
but the probability of finding one is small. The results
previously obtained by Yu.N.Pariyskiy (Ref.2: Izv. G1. astron.
observ. v. Pulkove, V.21, no.5, 45, 1960) are wrong as they are
based on the assumption of thermal radiation. The author thanks
I.S.Sliklovskiy for valuable discussions. A.A.Korchak and
S.I.Syrovatskiy are mentioned in the article for their
contributions in this field. There are*3 figures, I table and
22 references: 5 Soviet-bloc and 17 non-Soviet-bloc. The four
mosi recent references to English language publications read as
follows: Ref.4: D.E.Harris, J.A.Roberts, Publs. Astron. Soc.
Pacif., v-72, no.427, 1960; Ref.5: R.W.Wilson, J.G.Bolton,
Publs. Astron. Soc. Pacif., V-72, no.428, 196o; Ref.11: as quoted
in text); Ref.19: as quoted in text.
Card 3/0 Lf

30822
S/033/ 1/038/005/010/015
The discrete source of radio ... E133/E435
ASSOCIATION: Fizicheskiy institut im. P.N.Lebedeva
Akademii naulc SSSR (Physics Institute imeni
P.N.Lebodev, AS USSR)
SUP~!ITT,~Z,D December 3, 1960
Wort qw,

lode

P
[AT
f

1141

32437
17/ //~ Z)
S/033/61/038/oo6/oo6/007
E133/E435
AUTHORS- _KHK,_~ ` Udalltsov, V.A.
TITLE: The polarization of radio emission from the Crab
Nebula in the 10 cm waveband
PERIODICAL: Astronomicheskiy zhurnal, v.38, no.6, 1961, 1114-1115
TEXT: The authors have communicated observations of the polarization of
Crab Nebula in 9.6 cm range previously (Ref.l: Astron. zh., v,36,
1959, 33; Astron. tsirkulyar, P-0.187, 1957, 14) but corrections
were not made in the earlier work for possible parasitic
polarization in the apparatus. The observations were therefore
repeated in May 1960 with a steerable 22 m radio telescope
(Ref.2: A.Ye.Salomonovich, Radiotekhnika i elektronika, v.4, 1959,
2092). The data obtained were analysed by the method of least
squares. The degree of polarization was found by comparison with
a control signal which was 100% polarized, It was found that the
degree of polarization in the Crab Nebula was 3.7 � 0.5% and the
position angle was 132 + 5*. A comparison with two unpolarized
sources (Cas A and Cyg 1) indicated that -the instrumental
polarization did not exceed 0-5%. The data obtained with a
stationary radiotelescope (Ref.1) may therefore be considered
Card 1/2

32437
S/033/61/038/oo6/oo6/007
The polarization of radio ... E133/E435
correct. The work reported there has been re-reduced to give a
value of 3~2 + 0.4% for the polarization and 137 1 5* for the
position angle, The average of these two results is therefore
3.5 + 0.4% and 135 + 3", Observations were also made at a
waveYength of 10~7 cm in June-July 1960, using a stationary radio-
telescope of 31 m diameter (Ref-3: V.V.Vitkevich, V.A,Udalltsov,
Radiotekhnika i elektronika, v.2, 1952, 1548). It was found that
the polarization was lower by 10% and tile position angle decreased
to 130 + 31~ This agrees well with previous investigations.
However, the changes in the position angle, noted in these
investigations (Ref.4~ C.H.Mayer, T.P.McCullough, R.M.Sloanaker,
Report to the XIII General Assembly URSI, London, September 5-15,
1960) for wavelengths near 11 cm, appear to be improbable,
There are 4 references'-' 3 Soviet-bloc and 1 non-Soviet-bloc. The.
referense to an English language publication is quoted in the text.
ASSOCIATION, Fizicheskiy j_n-t im. P.N.Lebodeva, Al-adeniii nauk SSSR
(Physics Institute im, P.N.Lebedev; AS USSR)
SUBMITTED~. February 10. 1961
Card 2/2

324-i8
J 033/61/038/oo6/007/007
/0 4,// // I Z / / / 2 ~,7) 5/
E133/E435
AUTHORS% KuzImin, A-.D., Salomonovich, A.Ye.
TITLE.- Radio observations of Venus in 1961
PERIODICALt Astronomicheskiy zhurnal, V,,38, no.6, 1961, 1115-1117
TEXT,. Observations of Venus were made with the 22 ni radio-
telescope at wavelengths of 4 mm (Ref.2: A.G.Kizlyakov,
A.D.Kuzlmin, A.Ye.Salomonovich, Izv. vuzov, Radiofizika, v.4, no-3,
1961, 573), 8 mm and 9o6 cm (Ref.8.- A.H.Barrett, Astrophys. J.,
v.133, no.l. 1961, 281) from the middle of March to the beginning
of June 1961, Observations were also made at 3.3 cm from the end
of May to the middle of July. At 4 and 8 mm, and at 3.3 cm,
the brightness temperature increased continuously with the area of
disc illuminated. The minimum temperatures found were 390 + 120*K
at 4 mm and 374 + 75"K at 8 mmo These occurred before infeTior
conjunction. AZ 9.6 cm,, the brightness temperature changed
irregularly from day to day by large amounts. The brightness
temperature averaged over the disc was also greatez~ than at the
shorter wavelengths being about 680*K. In agreement with
American measurements (Ref.4: C.H.Mayer, T.P.McCullough,
Card* 1/3

~2 43 8
Si633/61/038/oo6/007/007
Radio observations of Venus E133/E4-15
R.M.Sloanaker, Astrophys. J., v.127, 1, 1958, 1; Ref.53 C.H.Mayer
et al, Report to the XIII General Assembly URSI. London, 1960i
Ref`.6~ L,E.Alsop, J.A.Giordmaine, C.H.Mayer, C.H.Townes, Astron
J.9 -.63, 1958~ 301)t, the brightness temperature of the night side
of Venus, at the longer wavelength, was about 600'K. At the
shorter wavelengths it m-as about 400'K. It seems unlikely that
the temperature of the 5urface on the da~Xight side of Venus can
be at a higher temperature than about 750'K. The fact that the
emission at all the shorter wavelengths shows similar
characteristic.s indicates that the gas pressure at the surface o-
Venus cannot exceed 5 BAM (assuming that the atmosphere is
'lomposed of C02). The methods which have been suggested by the
present authors (Ref.9; Astron. zh,, v.37, no.2, 1960,, 29?) can be
used to show that the direction of rotation of Venus is direct and
the period of rotation, though longer than that of the Earth, is
less than the orbital period, The irregular Lomponent of
variation at 9.6 cm must be due to the Ionosphere of Venus, The
maximum brightness temperature measured at this wavelength was 8,
about 1000'K. This tequires a high -~Iecl.,Yofi density (----5 x 10 _ri-3),
Card 2.13

3/033/61/038/oo6/007/007
Radio observations of Venus E133/E435
With a magnetic field 1/30 that of the Earth (Ref,7.- D.E.Jones,
Planetary and Space Sci-, v.5, no,2, i9ft, i66) this could be
obtained from solar --orpuscular streams, More improbably. it
could be produced from meteor streams, but these would have to be
3 to 4 orders of magnitude greater than on the Earth. The
observations at the 4 mm. wavelengths were carried out by the
Aspirant of NIRFI, A,.G.Kislyakov with the apparatus developed at
NIRFI. There are 10 references?, 4 Soviet and 6 non--Soviet-bloc~
The four most recent references to English language publications
Ref. 4,5,7 and 8 are quoted in the text.
ASSOCIATIONg Fizicheskly in-t im. P.N.Lebedeva, Akademii naulc SSSR
(Physics Institute lm. P,N.Leb-~dev, AS USSR)
SUBMITTEDg September 15, 1961
Card 3/3

27875
3/020/61/140/001/011/024
7:~ B104 B109
AUTHORS: Kuzlmin, A. D., and Salomonovich, A. Ye.
TITLE: The 8-mm radio-emission from the Taurus-A region
PERIODICAL: Akademiya nauk SSSR. Doklady, v. 140, no. 1, 1961, 81-83
TEXTt In March and April, 1961, the authors systematically investigated
the'discrete source of 6-mm. radio-emi8sion from the Taurus-A region with
the 22-m radiotelescope (directional diagram approximately 2mm, sensi-
tivitY 1.50 K) of the Fizicheskiy institut im. P. N. Lebedeva AN SSSR
(Physics Institute imeni P. N. Lebedev AS USSR). This radio-emission was
observed for the first time on August 21, 1959- Measurements were carried
out with a fixed antenna, the direction of which was adjusted according to
the radio-emission of Venus. The records of 21 measurements were averaged.
Two sources of radiO-eMiSBion were found, the first of which is well
known. Its right ascension is 0~' 1950 =5h31m358 + 05s. The mean antenna
temperature of this source is 4-50K + 10, its apparent diameter is
Card 1/3

27875
S/020/61/140/001/011/024
The 8-mm radio-emission from..* B104/B109
estimated at 4-5 � 11. The radiation density is estimated to be
500-10-1 6wom- 2, cps-1+ 2-5 ~. Luminance temperature is 60K + 10 %o In
all measurements, a sicond radiation source was-found. The right ascension
of this new source is C~ 1950 ~ 5h32m10' + 6's Its apparent diameter is
2'3011, and its antenna temperature is 2.8 OK + 10 %. The luminance
temperature of the new source is estimated to be 7 OK + 25 % and its radi-
ation density at 130.10 -26 WOM -2 cops -1 + 25 %. As there are no data
available on any centimeter, decimeter, or meter radio-emission from this
region, the authors assume this 8-mm radio-emission to be of thermal origin.
6
The intensity of the new source discovered is ME - 2.7-10 . The absence
of visible optical nebulae is taken as an indication that the visible
intensity does not exceed 400. Therefore, the total absorption from the
earth to the source is higher than 8 m7- Using data of P. P. Parenago,
(Astr. zhurn., 22, no. 1-3, 200 (1945)), the distance between the earth
Card 2/3

27875
3/020/61/140/001/011/024
The 8-mm radio-emission fromo.9 B104/B109
and the source of radio-tmiasion exceeds 3.8 kiloparsec. The linear
dimension 2S of the source is estimated at 2S >3 parsecs and the electron
density Ne at Ne 4103 cm-3 and M/MO>400- Hence this radiation source is
similar to the nebulae NGC 1976 and NGC 6618. *There are 2 figures and 5
references: 3 Soviet and 2 non-Soviet. The references to English-language
publications read as followss W; Baade et al., Astrophys. J., 119, 206
1954 ; G. R. Whitfield, Month. Not. Roy. Astron. Soc., jjj, no. 6, 680
57~-
M
ASSOCIATIONt Fizicheskiy institut im. P. N. Lebedeva Akademii nauk SSSR
(Physics Institute imeni P. N. Lebedev of the Academy of
Sciences USSR)
PRESENTED: May 8, 1961, by D. V. Skobelltsyn, Academician
SUBMITTEDs April 24, 1961
Card 3/3

~ KUZMIN I A. D.) SALMMOVICH, A. Ye.
"The Results of the Venus Radio Astronomical Observations Carried out at
the F N Lebedoy PhyBical Institute"
Soviet Papers -presented at Plenary Meetings of committee on Space Research
(COSPAR) and Third International Space Sumposium, Washington, D. C.,
23 Apr - 9 May 62

S., Astronomical Council, Academy of
-
"
Sciences LISSR J
Optics and ge=etrY in
9607-
the matter of Saturn's rings"
PRONDFI)EV, Vladimir K., Crimean Astrophysical
"
- "on the
Laboratory imeni G. -A, Sheyn fl
~627
presence of oxygen in the at=osptere of Venus"
-SALM)NOVICH A Ye Physics Institute imerxi
i;~ ~
;~
P. N.
emy of Sciences USSR, and
dev,
Arkadiy D., Fadio Astranozy Laboratory,
P. 11. Lebedev, Academy
of Sciences USSR - "Observations of the
radioemission of Venus and Jupiter on the
wave of 8 =. "
BALMONOVICH, A. Ye., M11-MI, Arkadiy D., and
KISLXWV,._A. G. "Radicemission of Venus on
of V
SALOMONOVICH, A. Ye., KUWMN, ArkadLy D.,

VA __ P., and SHAIMOVSXI'f-1,3~* -
"
Ob vatloas of the rcf.Uoamission of Venus
and Jupiter on the vave of 3-3 cm."
SALOMNOVICH, A. Ye., P-d BIMIK21, A. D. -
"Padioemission of Venus on the wave of 9.6 cm.
SAL~MVNOVICH, A. Ye., and K=11MR, A. D. -
"Results of the observations of radioc=iasion
of Venus in ig6i"
SHARONOV, Vaevolod V., Director, Astronomicel
Dservatcm74Leangrad State University LT961
positionj- Probsb3e state of the 3urf=e and
atmosphere of the planet Yzrs according to
photometric and colori=etric. data"
MTSKET_, Sersey K., Read of the Chair of
Astroncmy, Kiev Stit-e University LT961 Po3itio-n7-
"Nature of Saturn's rings and signs of the
existMcP of a ring around Jupiter"
YEM13SYZY V. I., and MLL P., Director,
Ji~t-ronomical Crbzervatory, KEar),ov state
UniYersity LT96o Position7- "optical P-cpzrties
of the atmosphere and surface of Mars according
to photactetric and spectrophotwetric observations
carried cut at the h-harkov University Obiervatory"
rt to b& sulmitted for'tho llth Intl. AntM-pkrsjcq ST..-oai=, _%IZi&n
- Of AStrophyaicsp Co Into -Sclosa in, Belgi=, 9.n jttl 196,o.

43835
L7/ooo/003/007
;/504/6Z/O:
Io46/I246
KuzIminV A.D.
AIRIIOR I
eg of radioemiasion on
Results of observatiOns Of some discrete sourc
TITLL
the 9.6 cm, wave
Aiiche3kiY institut. Trudy, v. 17. ?Io3cow, 1962~
SWIM: Akademiya nauk S35R*
liadioastronomiyat 84-114
Tma: This paper is a catalog of 50 out of 56 discrete radiosources measured on the
e Vanuary_~,kprjl.1960) at the Okskaya nauchnaYs
9.6 cm wave with the 22 m radiotele3cOP, ef.l: A.D.Kuzimin, V,.T.Levchenkot
.Htants.iya FIAH (the Oka Research Station PhIAS) (R a' . 1960, 37, No. 6, 975). Each
R.I.Nonkovaq A.Yr.5alolionovich. AztronomichealtiV zhurn lo a coordinates
source is identified accordillf; to optical and radio classification and it
r . declination, (;alautic). Also given: angular nizet antenn
'are given (ri'lit ascension rightness temperature, spectral index. For 10 of
temperature, radiation flux density, b siona, and the electron density is given@ and
those objects, the masug the linear dizien
r~.. the probable exciting star is listed for-each of the emission nebulae; the distance to
ithese 10'nebulae is calculated from radiation data. Spectra are given of 2 .1 thermal and
11 Cara- 1/2
14. L
VUrC
L Zadlotel es. OotJrcea..
I oPec.
C
X d Inj
r f'LL 0 eacllrL
02.4i,;we P -respect, naltlea Pat 19511
n- Proc. Irely. ,, are ') 'and Of Of
the 9.6
Aotro e less th iG
a IZ, Oe rosI,
sec. 4.10-26" IZ93 cin ..d,
of p,, , 46 11 4 _e 4t V, w'1tt,r4-?J 0 radjot oeral
Ific .96o 1 eo salon of
53) and Cyc2.-I 0l '
WI Ih 4t. COPe
and B., 196C)) s-
7Z' 429) Th emen t w~ 67 (p '0-~6 v4tt how
ere th J?et, *D.Drak
8 t, - 70 (., e ftd
cures go.-Dolt
and 4 t4b, On,
,2

33421
9, 1756 (1b,511,10,6,11 17)
AUTHORS Kuz'min A D
S/033/62/039/001/002/013
E032/Ell4
TITLE: The spectra of discrete sources of radio emission
observed with the 22 metre radio telescope of the
FIAN
PERIODICALS Astronomicheskiy zhurnal, v.39, no.1, 1962, 22-28
TEXTS It is pointed out that published information on the
radio emission of discrete sources in the centimetre range in
rather limited and frequently contradictory. in view of this
the present author et alin have used the 22-metre radio
telescope of HAN to determine the radio emission of a number of
discrete sources on 9.6 and 3.2 cm. These results were obtained
in January-June 1960 and were reported in previous papers
(Ref.l: A.D. Kuzlmin, M.T. Levchenkog R.I. Noskova,
A.Ye. Salomonovich, Astron.zh., v.37, 975, ig6o. Ref.2t
A.M. Karachun, A.D. Kuz'min, A.Ye. Salomonovich, Astron.zh.,
v138, 83, 1961). Fifty discrete sources were observed on
9.6 cm; on 3.2 cm the number was 5. In the present paper the
Card

33421
The spectra of discrete sources ... S/033/62/039/001/002/013
E032/E114
author compares the above Soviet work with the results obtained
by other workers for different wavelengths, Western published
work is critically reviewed and in some cases the published flux
densities are suitably corrected. Thus, for example, all the
results of G. Westerhout (Ref.14i Bull. Astron. Netherl., V'14'
no.488, 1958) are multiplied by 0.86 in order to exclude the
systematic error pointed out by P.G. Mezger (Ref-139 Z.4strophys.,
v.46, 234, 1958). The results of this analysis are then used to
plot the spectra of two thermal and all the non-thermal sources
which have been observed so far. The table gives a comparison of
the values obtained for the spectral index n of the non-thermal
sources with the values reported by D~ E. Harris and
J~ A. Roberts (Ref.15; Publs. Astron. Soc. Pacif., v.72,
no.427, 237, 1960) and GR. Whitfield (Ref.40g Monthly Notices
Roy. Astron. Soc., v.117, 68o, 1957).
There are 3 figures, I table and 40 references% 5 Soviet-bloc and
35 non-Sovie-t-bloo. The four most recent English language
references read as followss
Ref.10i R.M. Sloanaker, J.H. Nichols, Astron.j., v.65, 1278, 109,
Card 2/4 196o.

33421
The spectra of discrete sources S/033/62/039/001/002/013
E032/E114
Ref.16: R.W. Wilson, J.G. Bolton, Publs. Astron. Soc. Pacif.,
v-72, no.428, 196o.
Ref.25'. P. Leslie, Observatory, v.80, 23, 196o.
Ref.333 G.R. Whitfield, Monthly Notices Roy. Astron, Soc.,
v. 120, 581, ig6o.
ASSOCIATIONs Fizicheskiy institut im. P.N. Lebedeva AN SSSR
(Physics Institute imeni P.N. Lebedev, AS USSR)
SUBMITTED: February 10, 1961
Card 3/X

KARDASHEV, N.S.; KUZIMIN, A.D.; SYROVATSKIYI S.I.
Nature of the emission of radio galaxy Cygnus-A. Astron.zhur.
39 no.2s2l6-221 Mr-Ap 162. (MIRA 15:3)
1. Gosudarstvennyy astronomichaskiy institut im. P.K.Shternberga
i Fizicheskiy institut im. P.N.Lebedeva AN SSSR.
(Galaxies) (Radio astronomy)

KUZ'YJNq A.D.; NOSKOVA, R.I.
Identification of exciting stars and the determination of
the parameters of emission nebulae from radio-astronomy data.
Astron.zhur. 39 no.2-241-246 Mr-Ap 162. (MA 15:3)
1. Fizicheskiy institut im. P.N.Lebedeva AN SSSR.
(Stars) (Nebulae) (Radio astronomy)

3PA.72
S/033/62/039/003/001/010
r? E032/r-.114,
AUTM;RS: Kislyakov, A.G.,,1(uz1min, A.D., and Salomonovich, A.Ye.
TlTLE: The radio emission of Venus at 4 min wavelength
P~;RIODICAL: Astronomicheskiy zhurnal, v-39, no-3, 1962, 410-417
T~-,'XT: The intrinsic radio emissio n of Venus is expected to
yield important information on the temperature of the planet, on
~he nature of its surface, on the composition of its atmosphere
and on sotiie of its rotational properties. All previous measure-
ments are said to have been carried out at wavelengths greater
than 0.8~1~!cm. In 1-iarch - 14;ay, 1961, the 22-n-etre radio telescope
of the F.izicheskly institut imeni P.N. Lebedeva AN SSSR (Physics
Institute ii,,ieni 11'.N. Lebedev, AS USSR) was used to observe the
radio emission of Venus at 4 mm. An account of the method of
reduction of the observations is given and it is estimated that
the RNIS error in the measured intensity was 1 30%. The results
obtained are shown in Figs. 11 and 5. (Fig.4t Antenna temperature
as a function of time; the arrow indicates inferior conjunction.
Fig-5: Brightness temperature of Venus 'as a function of,time).
Card 1/y

KIJZ'MN, A.D.; SALOMNOVICH, A.Ye.
Observations of radio emissions of Venus and Jupiter on 8 m.
wavelength. Astron.zhur. 39 no.4:660-668 JI-Ag 162. (KRA 15:7)
1. Fiziche8kiy institut imeni P.N.Lebedeva, AN MR.
(Venus (Flanet)) (Jupiter (Planet)) (Radio astronomy)

BIBINOVA) V.P.; IF
.2XjN,-A,D.- SALCMONOVICH, A.Ye.; SHAVLOVSKIY, I.V.
4
Observations of the radio emission of Venus and Jupiter at
the 3,3 cm.wavelength. Astron.zhur. 39 no.6:1083-1088
N-D 162. (MMA 15:3 1)
1. Fizicheskiy institut im. P..N..Lebedeva AN SSSIR.
(Radio astronomy) (Venus (Planet))
(Jupiter (Planet))

KUMM, A.D.
Radioastronomical research of Venus (USSR)
Report submitted for the I+th Internati6nal Space Symposium (COSPAR)
4a~saw, 2-12 June 63

KUZIMIN, A.D.; SALOMONOVICH, A.Ye.
Radio*emission of discrete sources in orion and Omega in the
microwave band. Astron.Tsir. no. 260:1-4 S 163. (MIRA 17:5)
1. Fizicheskiy institut imeni Labedeva AN SSSH.

VETUKHNOVSKAYA, Yu.N.;_KUZIM.,,_A..D.; KUTUZA, B.G.; LOSOVSKIY, B.Ya.;
SALOMDNOVICH, A.Ye.
Measuring the radio emission spectrum of the night side of Venus
in the microwave band. Izv. vys. ucheb. zav.; radiofiz. 6 no*5:
1054-1056 163. (HM 16:12)
1. Fizicheskiy institut imeni Lebedeva AN SSSR.

KUZIMIN, A.D.
-, - - --I
,P-' -,'17~~-, Z. -- -
An ionospherio model of Venun. Izv.vyo.uoheb,zav.; radiofiz, 6
no.6:1090-1097 163. (MIRA 17:4)
1. Fizicheskiy institut imeni Leb6deva AN SSSR.