SCIENTIFIC ABSTRACT SALOMATINA, YU. - SALOMONOVICH, A.YE.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001446910010-5
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: August 25, 2000
• Sequence Number: 10
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

KRAVCHICNKO,I., kandidat tekhnichaskikh nauk; SAIDMTINA,Yu., inshener
Cement for reinforced concrete products made using steam curing.
Stroi.mat. izdel. i konstr. 1 no.4:21-23 AP'55- Wak 8:10)
(cement)

SOXHATSKAYA. G.A., kandidat telchnicheakikh nauk; SALOKATIMA, Yu.F.,
kandidat tekhnicheekikh nauk. bu,;-
Experience of the "XomsomoletmN cement factory in Increasing the
durability of rotaz7 kiln linings. Mement 23 no.2:13-18 Mr-Ap '57.
MRA 10:7)
CKilns. Rotary)

PIMOV,, A.A.j LM., U.N.; SMUTSKAYA., G.A'O; SAIMMA., YU.Fo;
Testing the lining of the clinkering zone in rota27 klins by
unfired products of magnesia concrete, Sborensuchotrade MMO
no.5-.234-253 1(4* 4KIRA 15212)
1. Ukrainskiy naucbno-iseledovatellskiy institut a-
(for Pirogov, 4ve). 2. Gbsudarst7ennyy vveeoy=yy vaucbno-
iseledovatellskiy inatitut teementa (for Sokhatskaya, Salomatina).
(Kiino, Rotary) (Napesia-cement)

SHORYGINAv N.N.; IZUNRUDOVA, T.V.; ADEL't I.B.; ZAGARMISTRv O.S,;
SALOMATINLy Z.T.
Prospects for the use of hydrolytic lignin in the protroleum
industry, Gidroliz, i lesokhim. prom. 4' no. l.-5-6 161.
(MIRA 3-4:1)
(Lignin) (Petroleuin industry)

SALQ4ATOV, A.D.; PODVYAZKIN, Yu.A.
Laboratory apparatus for shaking. Soob. DVFAN SSSR no.17:49-51 163.
(MIRA 17:9)
1. Dallnevostochnyy filial im. V.L. Komarova Sibirskogo otdeleniya
AN SSSR.

S
inzb.
AutomaLic welding in a carbon dioxide atmosphere. Svar. proizv.
no.3:33-34 Mr '62. (MIRA 15:2)
1. Sibirsk zavod tyazhelogo masbinostroyeniya.
i4lectric welding) (Protective atmospheres)

BOV/136-58-6-13/21.
AUTHORS: Donchenko, P.A., Novozhilov, A.B. and Salomatov,-*N.K.
TITIZ: Mastering the Slag-fuming Installation at the Us -
gorsk Lead-zinc Combine (Osvo7eniye shlakovozgonochnoy
ustanovki na Ust'-E-amenogorskom avintsovo-tsinkovom
kombinate)
FERIODICAL. Tsvetnvye Metally, 1958,, nr 6, pp 74 - 82 (USSR)
.ABSTRLCT: The slag-fuming installation at the lead works of the Ustl-
Kamenogorsk Combine was started in January 1956, having been
built to the imperfect designs of the Giprotsvetmet.
The authors briefly describe the installation and the
improvements made in the des@ggn of individual units and
outline operating results. e installation (Figure 1)
consists of a fuming furnace fired with a coal-air mixture.
An electrically heated settler for separating matte from
slag, waste-heat boilers, sleeve filters, coal pulver-
isation section and air blowers. The furnace (Figure 2)
is a rectangular shaft (internal hearth dimensions
2.107 x 3.12 m, height 5.3 m) with a capacity of 26 tons
of adag (1.5% Pb, 12.8% Zn, 0.8% Cu). The fume amounts
to 19% of the slag weight and contains 7.5% Pb, 60% Zn
(Zn and Pb recovery 82 and 97%, respectively). The coal
Card 1/3 L

SOV136-58-6-13/21
Mastering the Slag-fuming Installation at the Ust'-Kamenogorsk
Lead-zinc Combine
used is Prokoplyevsk @calorif4e value 6 800 cal/kg,
15.8% ash), ground with a type SM-18 hasm'er mill an&
crushed with a type Sh-10 mill; the dust is passed
through a system of bunkers and injected with the aid of
feeders of the type used at the Podol'sk Tin Works., The
settler (Figure 3) is lined with chrome-magnesite and fire-
clay bricks and has three graphite electrodes fed by three
type KPOM-250 transformers giving a current of 2 500
3 000 A. The waste-heat boiler type UKTBM 15/40 was
specially designed by Giprots@etmet and reduces gas
temperature from 1 200 - 350 C. Experience showed
that the original cast-iron furnace ports were unsatis--
factory, the receiver of the filling runner was too small,
the combustion of gases was completed in the waste-heat
boiler. The Kazgiprotsvetmet-designed settler was also
found to be unsatisfactory in most respects and the dust-
catching arrangements were insufficient. To find optimal
operating conditions tests were carried out jointly by the
VNIItsvetmet Institute, the experimental shop of the
combine and personnel of the fuming depwtment (table).
Card 2/3

SOV/136-58-6-13/21
Mastering the Slag-fuming Installation at the Ust'-Kamenogorsk
Lead-zinc Combine
The dependence of the metal contents on duration of
blowing of the metal contents in the slag (Figure 4), of
metal concentrations in the fume (Figure 5) and of gas
dust contents (Figure 6) were among the factors studied.
In spite of its original failings, the 'adoption of the
installation has proved profitable; oxygen-enrichment of
the b1mt should improve efficiency further.
There are 6 figures and 1 table
ASSOCIATION: UYSTsK
Card 3/3

ONAYEV, I.A.) KUROCHKIN, A.F,- TONKONOGIY, A.V.j SAL(NATOV, NJ.@
Overall processing of Balkhash copper micentrates by the avelone
method. Vest. AN Kazakh. SSR 20 no,2242-49 F 164.
(MIRA 1821)
Lt

KERSHANSKlY., I.I.; R071-DVSKIY, A.A.; SALOMATOVf N.K.; KERSHANSKAYA, L.K.;
AFASHAGOV, Yu.M.; KIJUR, V.P.
Pilot plant tests in Frecipitation reduction smelting of antimony
concentrates in electric furraces. TSvet. met. 38 no-5:34-41 My 165.
(MIRA 18:6)

SALCRATOV, V.V.; BOYKOV, G.P.
Initial period of heating solids by radiation vith-a variable
temperature of the heat source. IzV. vys. ucheb. zav.; chern.
met. 6 no.32:177-181 163. (KM 17: 1)
1. Tomskiy politekhnicheskiy institut.

IVANOV, V.V.; c@it&)MATOV, V.V.
Use of substitutions in solving boundary value problems In
heat conduction theory. Izv. TPI 12504-57 t64.
(MIRA 18:8)

L 6.1911-65
51 ESSION NR, AR5_0i@967 UR/0044/65/000/0-07/-B-0-7:1-~i6~i-i-
517-9:536.2
SOURCE: Ref. zh. Matematika, Abs. 7B344
,AUTHOR: Salomatov, V. V.; Boykov, G. P.
ITTLE: Heating of bodies in a radiation medium with variable temperature
CITED SOURCE: Izv. Toinskogo politekhn. in-ta. v. 125, 1964, 58-66
,TOPIC TAGS: boundary value problem, heat conductivity
:TRANSLATION: A boundary value problem for a oiie-dimensional heat --equation is@ -stud-
;ied for the case when one of the boundary conditions is homogeneous of the second
kind and the other is nonlinear (defining heating of a body in a radiating medium),
Th-? given boundary value problem is linearized, and an integral Laplace transform i.9
used to solve the resulting linear problem. Solutions are exhibited (in the forit 0
infinite series) for an unbounded p.Late, a cylinder., and-a. sphere in the ame of ex-4--;-_
1ponentially changing temperat&es in thei-extern'"al medium* L-0spenskly
SUB CODE: TA MA ENCL! 00
Card 1/1

SAIPI-MI-W. V.V.; BOYKOV, G.P.
A radiant heat flux due to the heating of bodies by a source
of variable temperature. Inzh.-fiz. zhur. 8 no.3:369-374
Mr 165. (MIRA 18:5)
1. Politekhnicheskiy institut imeni Kirova, Tomsk.

BuSTF.A, Maria, dr.; DABIJAp 'Vioricaj, dr.'I GHWRGHE, neana, dr.;
ICKESCU, E., dr.; ICHESCU, Zenobia, dr.; LUNGU, Felicia, dr.;
SAW4Et,-Naxiia, dr.; SAVIN, Valentina, dr.; STMWCU, I., dr.;
9FOICAj V*p dre; SIRBANy No.. dr.; VISAN@ Valeria#. dro
Oar'results in tfie treatment complications of dental cw@les.
Stomatologia (13acur) 12 nooll @-16 Ta-F'65.
1. (:olectirul Serviciulul de stomatologie al Spitalului uni-
ficat de adulti, Constants.

SALOMM, Ervin, ing.; FISER, Ivan, ing.
Electrical industry, of Yugoslavia. Alm metal ind 45-65 f6O.
1. Drzavni savetnik u,Saveznom zavodu za privredno planiranje
(for Salomon). 2. Savetnik u Saveznom zavodu za privredno planiranje
(for Fiser)

SALOYCN,
Calculating constants of substitute static systems with transport lag from the
results of measurements using a general form signal. p. 292.
AUrOMATIZACE. Praha., Czechoslovakia. Val. 2, no. 10, Oct. 1959.
Monthly list of East European Accessions (EEAI) LC, Vol. 9, no. 1, January 1960.
Uncl.

SAD31-.'ONOVICH, A.Ye.
CAND MSICOMPTH SCI.
Dissertation: "Dry Friction 2nd Electric2l Contact at Small Displacements."
14 March 49
Physics Inst inieni P.N. Lebedev, Acad Sci USSR.
C,10 Vechery@r -i MOqj
1:@t j.; 1.,

SALOMONOVICH, A.
"Radio" No 11, PP 23-26
Describes use of oscilloscope and eecondary-electron
multipliers by N. A. Tolstoy and P. P. Feofilov to
study extinguishing of lumiuophors. Gives examples
of how linear amplifiers,,thyratrons@ and trigger
circuits can be used in countercircuits. Graphi-
cally illustrates operating principle of coinci-
dence counter.
@177T34

SALCMONCVICHs A Ye.
USSII/Physics - Friction, Dry Jul 50
Contact, Electrical*
"Dry Friction and Electric Contact for Small Dis-
placements," A. Ye. Salomonovich, Phys Inst imeni
@ebedev, Acad Sci USSR
"Zhur Eksper i Teoret Fiz" Vol XX, No 7, pp 647-660
Discusses dynamic method for experimentlly investi-
gating-mechainical force of interaction dpL-b;--@xu:Bf
electric contact for sTmIl displacements of touching
solids. Gives new results obtained by this method.
Submitted 8 Jan 50.
168M
168T92

I lets to outIM13MOISUIP" a A '10 a U U
IN a a 9 4 d 4 a 0
:,A @ A" C -P-0 _ .
A vo-vtos is
no. PAMOFM mod of Im at Wba" 41 --00
IV =M.M:z a-&
L N. SMObDVMAVA Am A. L
A Trek. PON, VSSR. 21, 22W In -0 ,0
A Un I is Famm coaWafaw wom umd Obr
nwasorimo Ow p of, ft vill of quot .00
Cr"tasawmitta rank im
7=@ "a a 6&*Ab" WAKhromew In
00 j W the m
000 Vkhk 11deval WVWJ 40 *0 MW pol"w see
Surfom o( a *Woo. an otbW PONSWd ststram Q( do Goo
W&W beho tha. tomia( do qLwtx cryaW undw
ist4w4mi4m; ", -Ikwp two
: : . I too
woo aw ONPL TU --..obudmd
00 a vim vkwW ibnmvh iWeipim Aawl vvM a Lwnwa
*eel. for phokwwhhw ft p LMN " Wpnm
it was IVINAk so roam" a Comim appWatm in I are 0
"MI Or too ram Ot the PWM quarta CrYWA MW to
mam" It U"W mation bot"m the #vow vobw
and the mechanical d1onl4eeptent. The relmition between the norml and talW-
WOO
A#:.- 6ntisl dis"IscemOnt Of anY face Of the crYstal could also be eaftbliabod. Ulpe
We Phiphes
too*
U it -4-v .3 AS,
to it it to ov so is n og a ov a n it s; ft I a a 1 -a,
0 0

4,'!Z-]V, V. ; SIA1.0"OllOvIc" I
Wave Guides
Wave corductors. Radio no. 2, 1952.
Monthly jjj.@Lt of Russian Accessions, Litrary of Congress, I-Pril 1952. IMCLASSITIED.

A. Ye.
USSR/Electronics SelfmodLulation 'Feb..32
"Self -Modulation In Ferro Resonance," A. Ye. Ralco-,
-monovich, Inst of Phys imeni Lebedev, Acad Sci UM
"Zhur Tekh Fiz" Vol XXII, No 2, pp 245-258
Analyzes case in which circuit characteristics am
nearly linear and variations of amplitude and phase.
are slaw in ccnparison to period of external fwee..
Considers particular cases in which obuic resistswe
or capacitance of circuit depend on temp. Indebted
to Prof S. M. Rytov. Received 1 Jul 51.
2D9T59

SALOKONVICHP L.
USSR/Electronics --Wave Guides". Mar 52
'Vave Guides in Superhigh-Frequency Techniques,"
A. Salozonovich
"Radio" No 3, pp 16-20
General discussion of subject under the following
headings: excitation of wave guides and removal
of energy from them, ma+ching in wave guides, con-
nection of wave guides, and application of wave
guides - Claims that Ya. N. Fel'd developed the
theory of the slot ante and the M. S. Neyman
lst proposed cavity resonators.
229T62

SALOI f011C-IfICH, A. YE-
USSR/Electronics Nonlinear Capacitance, JU 52
Subbarmonics
"Division of Frequency in a Circuit With a Non-
linear Condenser," A. Ye. Saiomonovich, Phys Inst
imeni Lebed ev, Acad Sci USSR -
"Zhur Tekh Fiz" Vol XXII, No 7, pp'1190-1194
In the case of (livision of frequency due to a
nonlinear variable capacitance a combination of
parametric generation vith a type of ferro-re-
sonance occurs. The presence of reactive non-
linearity is necessary for the generation of half-
frequency. Received 10 Feb 52.
22iT41

UW/Iilectronies, UdiosstronM_
A. Salomonovich, Cand Phys;..
M&VA SCi
"Radio" No 8, pp 22-26
Describes antennas and receivers used in radio-
astronomy. Observations by S. S. Khaykin and
B. M. Chikachev in 1947 showed that solar radio
emission in the meter-wave band comes from the
upper layers of the solar corona. V. L. Gi=burgp
226T25
V. V. Vitkevich, and.l. S. Shklovskly are also
active in this field; the latter predicted the
"bright-line" (21-cm) emission of gaseous hydro-
gen ini interstellar matter several -years before
1-t was discovered.
226T25

USSR/Electronics.- Nonlinear Detector Dee 52
Frinvestigations of Dependence of a Nonlinear Crys-
talline Detector on Small Shifts -f the Contact
Needle," N. V. Karlov and A. Ye. Salomonovich
"Zhur Tekh Fiziki" Vol 22, No 12, pp 1981-1984
Investigate variation of detector behavior at
shifts of order of 10-4cm. Use for medsurements
dynamic method applied previously (MN, 70, 4;
1950). Results show that nonlinear properties of
detector depend on variation of gap size in simi-
lar mann r as in case of gap between metals. Re-
ceived 25 Jul 52.
24oT76

SALOMOTIVICH, A.
Chto takoe radioastrononiia fWhat is radio a,-;tronomv-
/. Y-oskva, Goskulltprosvetizdat)
1953. 80 p.
SO: Nonthly List of Russian Accessions, Vol. 7, No. 3, June 1954.

-7/
Category USSR/Radiophysics Application of radiophysical methods
Abs Jour Ref Zhur - Fizika, No 1, 1957,No 1978
Author Salomonovich, A.Ye. Shmaonov, T.A.
Title Conci@@thePro@bllem of the Choice of the Modulation Frequency in a
Modulation Radiometer
Orig Pub Tr. 5-90 soveshchaniya po vopr. kosmogonii. 1955. M., AN SSSR, 1956, 127-129
diskus. 130
Abstract The maximum value of the mod$lation freq@ency is determined by the width of
the anomalous noise spectrum at the output of the second detector of the re-
peiver. A spectrum analyzer for the invpstigation of this spectrum was built,
using a Aj@erodyne circuit with a quartz filter at the intermediate frequency.
The resolving power of thit analyzer is 6 clycles, the range of the investiga-
ted frequencies is from 10 to 1000 cycles. The investiqLtion was made on a
wide-band 3.2-meter superheterodyne rec&kver with a crystal mixer add a klys-
t3@ori heterodyne. The i-f amplifier had a bandwidth of 15 Me at 60 We qiA em-
ployed 6zhip and 6zh2p tubes (a total of 18). The overall gain was 100.
Measurements have shown that when the set was fed from batteries, no ancmalous
spectrum was observed above 30 cycles. When the receiver was fed from the *
power line, regardless of the satisfactory quality of the stabilized rectifiers
and the good filtering, the anomalous spectrum hex bumps at 50, 100, and 150
cycles.
7L /7L

TCAR V. N.Y.;SAWMONOVICHg A.Ye.
Application of ferrites in radioastronomy technique. Radiot-16-6 i
elektron. 1 no.1:120-121 Ja '56. (MIU T-'Il)
1. Fizicheskiy Institut iment P.N. Lebedeva Akademii nauk SSSR.
(Radio astronomy) (7arrite(Steel constituent))

URLOV, N.V.;SAWHONOVICH, A.Ye.
Automatic null-type centimeter-ways radiometer for investigation
of weak noise signals. Radiotekh.i elektron. 1 no.1:121-122 Ja '56.
(KMA (9: 11)
1. Fizicheskly institut imeni P.N.Lebedeva AkELdemii nank SSSR.
(Radiometer) (Radio astronomy)

KARLOV, N.V. -,SALOKONOVICH, A.Ye.
AutomatiC 2ero radiometer used for measurements at 3,2 ca.wavelengths.
Prib.i takh.skop.no.2:105-108 S-0 156. (NLRA 10:2)
1. Yizicheskly Institut im.P.N.Lebodeva AN SM.
(Radiometer)

16, M. V. KARWV, A. S. SALOMMMICH: Autaratu c r adFnm7ler at 2 -ff.
I- -
-.,ton
Atstract: Me Jevelopment is de!3=.4b-_,i .f an a r radIc-f
S.. a
i,AA 101F. Kili i KA I "LL-STRO14M, Vol 1, Nr b, iy5b, p 886

26-58-4-41/45
A,.;*.L`H0_!t; -Salomonovich, A.Ye., Candidate of Physico-14athematical
T -
6ciences L-lot-c-o-wT
TITLE: An Important Method of btudying the Universe (Vazhnyy metod
izucheniya vselennoy)
PZRIODICkL: Priroda, 1958, Nr 4, PP 116-119 (USSR)
ABJThACT; This is a critical review of the book "Radioastronomy" written
by I.S. Shklovskiy and published in 1955 by Gostekhizdat. The
book, written in a popular style, acquaints the average reader
with the principal methods of radio-astronomical observations,
of cosmic radio emission, radio location of the moon, etc.
The brochure "New Facts About Radicastronomy", written by the
same author, was published in 1957 and is a supplement to the
above-mentioned book. It covers recent discoveries in the
field.
V,:-VAILABLE: Library of Congress
Card 1/1
1. Radio astronomy-USSR 2. Radio astronomy-Applications

Translation from; Referativnyy Zhurnal Fizika, 1959, Nr 5,
AUTHORS: Amenitskiy, N.A.., Li Tsin-fan', Sal6monovich,
Chen Tszyun-lyan
TITLE: observations of 8-mm Wavelength Solar Radio Emission
%V Eclipse of 19 April 1958
SOV/58-59-5-11397
p 213 (USSR)
A.Ye., Khangilldin, U.V.,
During the Annular
PERIODICAL@. Solnechnyye dannyye, 1958, Nr 7, pp 69 - 71
ABSTRAM A joint expedition of the Academies of Science of the USSR and CPR
carried out observations of the total flux and circularly-polarized
component on Lake Hainan (CPR) with the aid of aflradiotelescope built
by the Physical Institute of the AS USSR. This instrument has a
t--60' radiation pattern at 0.5 power. The authors submit the
temperature-variation curve of the antenna fixed on the sun, as well
as the data resulting from the preliminary processing of this curve.
The sun's0brightness temperature on the day of the eclipse was
7,9OOt4OO K. The residual antenna temperature during the maximum
phase amounted to 1710.5% of the temperature of the uneclipsed sun
Card 1/2 (it would be 11% in the case of uniform brightness distribution on

SOV/58-59-5-11397
Observations of 8-mm Wavelength Solar Radio Emission During the Annular Eclipse of 19
April 1958
SIMIs disk at a diameter of 321). The radiation flux connected with spot group
Nr 188 (observed on longer wavelengths) did not exceed 2% of the flux of the entire
disk. With an accuracy approaching 0.2% of the total flux, no change was detected in
the circularly-polarized component during the closing and opening of the spot group
(the flux of circularly-polarized radiation did not exceed 3.5 X 10-22 W/m2c). The
authors advance hypotheses concerning the causes of the observed residual radiation
(Fiz, in-t AS USSR), A.S.

AUTHOR-. Salomonovich, A. Ye. 30-58 -5 -31/36
TITLEt A New Powerful Radiotelescope (Novyy moshchnyy radio-
teleskop).
Building Activity in the Serpukhov Station of the
Physics Institute (Stroitel'stvo na Serpukhovskoy
stantsii Fizicheskogo Instituta)
PERIODICAL: Vestnik Akademii Nauk SSSR, 1958, Nr 5,
PP. 130-131 (USSR)
ABSTRACT: This telescope has a diameter of 22 m. Its design was
worked out under the direction of experts of the insti-
tute by a number of organizations. It represents a metal-
lic rotating paraboloid with a distance of foci of 9,5 m-
By means of an electrical drive it can practically be
adjusted to any point of the hemisphere. Radio waves of
the sun, the moon, the planets, the radio nebulae and of
interstellar hydrogen can be investigated by it. At pre-
sent the radiotelescope-is mounted and it shall be taken
into o@)eration in the current year.
Card 1/1 1. Radio astronoaWa--USSR 2. Radio astrononrj--Equipment

SALOMONOVIGH. A.Ye.,
Radiowave emission of the moon in the 8 mm wavelength [with sumary
in Inglishl. Astron. shur. 35 no.1-0129-136 Ja,7 158. (HIRA 1113)
1. Fizicheskiy Institut.1m. P@N. Iebedeve. AN SSSR.
(Moon--Temperature and radiation) (Radio astronomy)

30) SOV/33-35-4-18/25
AUTHORSs Salomonovich, A.Ye., Pariyskiy, Yu.N., Khangilldin, U.V.
TITLE: Observations in the Millimeter Diapason of the Total Solar
Eclipse of June 30, 1954 (Nablyudeniye polnogo solnechnogo
zatmeniYa 30 iyunys 1954 9- v millimetrovom diapazone voln)
PERIODICALs Astronomicheskiy zhurnal,1958, Vol 35, Nr 4P pp 659-661(USSR)
ABSTRACT% The observations were carried out in the neighbourbood of
Novo-Moskovsk (Ukr.SSR) during an expedition of the Physical
Institute imeni P.N.Lebedev of the Academy-of Scienceff of the
USSR. The authors thank Ye.K.Karlova for the preparation of
tbe.apparatus and for the-assistance during-the-performance
of the observations.
The reduction of-the eclipse curve enabled the estimation of
the height o f- the effective layer of emission above the photo-
sphere (6-10 km +30%) and the distribution of radio brightness
on the solar disi. The comparison of the eclipse curve with
the curves of Troi-takiy, Zelinskays, Rakhlirr and Bobrik
Ck@f jy who observed there the solar eclipse in the centi-
meter range, shows a coincidence of some details.
Card 1/2

observations in the Millimeter Diapason of the SOV/33-35-4-18/25
Total Solar Eclip4e of June 30, 1954
There are 2 figures, and 4 referencesq 1 of which is Soviet,
and 3 are American.
ASSOCIATION:Fizicheakiy institut imeni P.N.Lebedeva AN SSSR (Physical
Institute imeni P.N.Lebedev AS USSR)
SUBMITTED% MaY 30, 1957

AUTHORS: Vitkevich, V. V., @Kuzlmin, /A- D. 2o-118.-6-11/43
Salomonovich, A. Ye., Udal.Itsov, V. A.
TITLE: A Radio Image of the Sun on 312 cm Wave Length
(Radioizobrazheniye Solntsa na volne 3,2 cm)
PERIODICAL: Doklady Akademii Nauk SSSR, 1958, Vol- 118, Nr 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.'---S-al6WddY1ch and

A Radio Image of the Sun on 3,2 cm 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 cm 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 th@ distribution is obtained because of the great width of
the diagram. The radio isophotic lines of the sun on the wave
lengths 392 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 ascL,
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

00>-,
S/035/61/000/001/005/019
AOO1/AOO1
Translation from: Referativnyy zhurnal, Astronomiya i Geodeziya, 1961, No. 1,
p. 45, # 1A3-39
AUTHOR&, Salomonovich, A.Ye., Koshchenko, V.N., Noskova, R.I.
-----------
I
TITIE: On Intensity of Sun's Radio Emission at the 8-mm Wavelength Band
PERIODICAL- "Solnechnyye danpyye@', 1959/1960, No. 9, pp. 83-89
TEXT: The authors present the changes of brightness temperature at the 8-
mm wavelength during the period from 1957 to 1958. Observations were carried out
near Moscow with a 2-m parabolic reflector. The average brightness temperature of
the Sun during this period was equal to 8,OOOOK, the temperature of the quiet Sun
was 6 400 + 8000K. The correlation coefficient between the brightness temperature
and @@e summary area of sunspots amounts to 0.4. There are 5 references.
N. S.
Translatorls note: This in the full translation of the original Russian abstract.
Card 1/1

SALa.'0711011icl; f:11. Y C.
Th@-rmal Pzdio Radiation of the Moon and Certain Characteristics
of Its Surface Ieyer.
report pr-sented at the International Symposium on the moon, held at the
Pulkovo Observatory, Leiiingrad, USSR, 6-8 Dee 1960.

S/141/60/003104/004/019
99110 EOWEN4
AUTHORS; Salomonovich, A.Ye. and Atayev, O.M.
TITLE: Thermal Emission and Absorption of 8-mm Band
Radio Wavestin the Earth's Atmosphere
PERIODICAL: Izvestiya vysshikh uchebnykh zavedeniy,
Radiofizika, 1960, Vol, 3, No. 4, pp. 6o6 - 613
TEXT: Molecular absorption of 8-mm radio waves has been
measured by measuring the natural thermal emission by the
Earth's atmosphere. Theabsorption coefficients were obtained
using a spherically symmetrical model of a humid atmosphere,
in which absorption and scattering of radio waves by the
condensed phaseza-- neglected. For clear days, which are quite
well described by this model, the following values were obtained
for the absorption coefficients in oxygen and water vapour,
respectively*.
MOl 0.0046 neper km- o.o4 db km- 1 1per 1 gcm-3
X02 0.00046 neper km- 0.004 db km-
The natural emission of the atmosphere on X = 8 mm was
measured using a radio telescope with a parabolic reflector,
Card 1/3

85979
S/141/60/003/004/004/019
E032/E314
Thermal Emission and Absorption of 8--mm Band Radio Waves in
the Earthis Atmosphere
2 m in diameter, and a modulation radiometer. The above value
for the absorption coefficient in oxygen is in satisfactory
agreement with the value calculated by Van Vleck (Ref. 11) and
the experimental values obtained by Marner (Ref. 1) and
Aarons et al (Ref. 5). The value obtained for water vapour is
also in reasonable agreement with the theoretical calculations
of Van VIezk and laboratory measurements by Becker and Autler
(Ref. 12). There is, however, a residual discrepancy between the
various results for water vapour. This is probably due to the
fact that absorption by the condensed phase was not taken
into account. The above model should be suitably amended.
Acknowledgments are expressed to N.A. Amenitskiy,
S.K. Palamarchuk and N.D. DolotenR-ov-a--w-Tro--t-o-oR-part in the
present work and to V.S. Trotskiy for valuable discussions.
Card 2/3

8 5979
s/141/6o/003/004/004/019
E032/E314
Thermal Emission and Absorption of 8-mm 'Band Radio Waves in
the Earth's Atmosphere
There are 7 figures and 12 references: 2 Soviet and
10 English,
ASSOCIATION: Fizicheskiy institut !men! P.N. Lebedeva
AN SSSR (Physics Institute imeni
P.N. Lebedev of the AS U55H)
SUBMITTED: January 3, 1960
Card 3/3

3.1710
@LPVHORS:
TITLE:
PERIODICAL:
ABSTRACT:
Card 1/2
78028
SOV/33-37-1-28/31
Amenitskiy, N. A., Noskova, R. I., Salomonovich, A. Ye.
The Radio Image of the Moon in an 8--mm Wave Range
Astronomicheskiy zhurnal, 1960, Vol 37, Nr 1, Pp 185-
186 (USSR)
Observations of the two-dimensional distribution of
the thermal radiation of the moon in the 8-mm wave range
were made during September-November 1959 with the 22-
meter radiotelescope of the Lebedev Physical Institute
of the Academy of Sciences, USSR. Owing to the great
resolving power of this telescope, it was possible to
obtain values of the radiation temperature for separate
regions of the moon. There is considerable dependence
of the distribution of radio brightness on the phase of
the moon which appears to be asymmetrical.. Thus, at
the first quarter the western par" of the moon Is
brighter, and the reverse is true at the third quarter.
The difference between the maximum and the minimum
temperatures In the center of the disk is more than 40%.

The Radio Image of the Moon in an 78028
8-mm Wave Range SOV/33-37-1-28/31
The authors thank G. G. Basiztov, N. F. Illin,
V. N. Koshchenko, and V. I. Pushkarev, who assisted
in making observations. There are 1 figure; and 3
reCerenceo, 2 Soviet, 1 U.S. The UiS. reference
iz: J. E. Gibson, Proc. I.R.E., 1, 280-286,1958.
ASSOCIATION: Lebedev Physical Institute of the Academy of Sciences,
USSR (Fizicheskiy institut imeni P. N. Lebedeva
Akademii naUk SSSR)
SU13MITTED: December ill 1959
Card 2/2

80830
S/033/60/037/02/008/013
C-9 0 E032/E914
AUTHORS:KuzImin, A. D., Salomonovich A. Ye.
; gum, om
TITLE:,,,,Radio Emission of Venus-In:-the 8mm Region
PERIODICAL: Astronomicheskiy thu:@nal, 1960,1(Vol 37, Nr 2, pp 297-300-
(USSR)
ABSTRACT: Radio emission of Venus in the centimeter and millimeter
ranges is of great interest since it provides information
on the atmosphere and surface of the planetl and 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 twice 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 McEwan (Ref 4) gave a
value of 4100 +-1600. Since this value is not sufficiently
Cardl/4 accurate, the present authors carried out similar measure-

80330
S/033/60/037/02/008/013
B032/E914
Radio Emission of Venus in the 8mm Region
ments on 8 mm, using the radio-telescope of'the Physical
Institute imeni P. M. Lebedev of the Academv-of Sciences
(USS This telescope was described by Salomonovich in
Ref nd has a parabolic mirror 22 m in diameter. The
*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 averated over
the apparent disc is shown in Fig 2 as a function of time.
The dotted line indicates the measurement 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

.'(0830
S/033/60/037/02/008/013
E032/E914
aadic -%,ission of Venus in the 8 mm Re-ion
indication of the fact that there is a temperature
difference between the illuminated and unilluminated
parts of the disc. The phase dependence of the bright-
ness temperature suggests that at least part of the radiat-
ion is due to the solid surface of the 'planet. One of the
Dossible reasons for the observed difference between the
temperatures on 8 mm and 3 cm may 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-
zorption of shorter wavelengths in the relatively cold
atmosphere of Venus. The present measurements indicate
that the brightness temperature of Venus averaged over
CP
the visible disc is 315 +_ 700K, This value was obtained
Card3A

20830
3/033/60/037/02/008/0131
E032/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 which 6 are
English and 14- are Soviet.
ASSOCIATION: Fizicheskiy institut ir.. P. N. Lebedeva, Akademii
nauk SSSR (Physical Institute im. P. N. Lebedev, Academy
of Sciences USSR)
SUM-1ITTED. December 15, 1959@
Card 4/4

87%
, 1
S/033/60/037 oo6/003/022
//2.7) E032/E514
AUTHOR., Salomonovich. A. Ye.
TITLE: Localization of Bursts of Radio Emission on 8 mm Wave-
length
PERIODICAL: Astronomicheskiy zhurnal, 1960, Vol.37, No.6, pp.969-974
TEXT: The 22 m radio telescope of the Physics Institute imeni
P. N. Lebedev, which has a parabolic reflector (Ref.4), was used
to detect and localize two bursts of radio emission on X = 8 mm.
The first burst was recorded on June 12, 1959 at 9 hours 17 min
U.T. and was located inside a calcium plage and connected with the
group of spots No.316 (Ref.5; T = +17, X = 330). It was observed
right up to 11 hours 10 min. The second burst was observed on
June 16, 1959 at 6 hours 54 min in the same region. Fig.1 shows
the records obtained in the two cases. Fig.2 gives radio charts of
the Sun for these two dates, showing a two-dimensional brightness
distribution on X = 8 mm in the region of the bursts. It is
concluded that the extended active region in the neighbourhood of
the No-316 group of spots was the source of bursts of radio emission
in the relatively wide frequency range for a number of days (at
least f or- June 9-16). It is natural to suppose that bursts
Card 1/2

87245
S/033/60/037/00b/003/022
E032/E514
Localization of Bursts of Radio Emission on 8 min Wavelength
recorded during these days on other wavelengths in the centimetre
and decimetre ranges (in particular or, 536, 808, 300 and 19 000 Mc/s),
which coincided with chromospheric flares localized in the neigh-
bourhood of the No.316 group, were also due to the above active
region, although they could not be localized owing to insufficient
resolution of the radio telescopes employed. It is estimated that
the flux densities of the above two bursts were p (9hO2m) =
21 x 10-22 W/jn2 cps and p (027m) = 830 X 10- 22 W/M2 cps,respectively
The corre ponding brIghtness temperatures are estimated to have been
5.41 x 10 r, *K and 9 x 105 oK. The former figure refers to
9 hours 02 min on June 12 and the latter to -the maximum of the
burst on June 16. There are 3 figures, 1 table and 8 referencest
4 Soviet and 4 non-Soviet.
ASSOCIATION: Fizicheskiy institut imeni P. N. Lebedeva Akademii
nauk SSSR (Physics Institute imeni P. N. Lebedev,
Academy of Sciences USSR)
SUBMITTED: April 30, 1960
Card 2/2

(@' 9 -'// @ S/033/60/037/006/004/022
J.'1720 E032/E514
AUTHORS: Kuz'min, A. D., Levchenko, M.T., Noskova, R. 1. and
SSJ.91nq2,n4q@X;k,ch,_,A. Ye.
TITLE; Observations of Discrete Sources of Radio Emission on
9.6 cm Wavelength
PERIODICALt Astronomicheskiy zhurnal, 1960, Vol.37, No.6,pp.975-978
TEXT: Preliminary results are reported of observations of
discrete sources of radio emission on X = 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

80178
S/026J60/000/05/003/068
D034/DO07
AUTHOR:
TITLE:
PERIODICAL!
ABSTRACT:
Card 1/4
Salomonovich, A.Te.
\%Lunar Radio Emission
Priroda, 1960,A# 5, pp 11-18 (USSR)
This is a popular account information on the-Ymoon obtained
from new radiological astronomical i-nvestigatil-o-na. Two
other papers on this subject were published in "Priroda".-
S.E. Khaykin, 1956, # 8, and V.V. Sharonov, 1960, # 1.
After a general introduction on thermal electromagnetic radia-
tion the author tells how radio emission from the moon is ob-
served. After explaining the principle of a radiotelescope
he states that by now it is possible to receive and separate
radio waves from areas having dimensions 10 to 15 times less
than the angle span of the moon. The major interest in this
research is in radio waves in centimeter and millimeter
bands. Thus radio emission capacity of the moon or its
"brightness temperature" as well as its "radiotemperature"
(the behavior of the brightness temperature along the moon's
45,

Lunar Radio Emission
80178
S/026/60/000/05/003/068
D034/DO07
radio wave range) can be studied with quite astonishing accu-
racy. The next section of the article deals with the radio-
temperature of the moon in relationship to the moon's phases@
Three laws, discovered up to this time in this field, are
shortly explained, namely: (1) If the length of electromag-
netic waves increases the oscillations of the radiotempera-
ture of the moon, related to its phases, diminish; (2) The
radiotemperature of the moon, measured on a 16 to 12 mm band,
always appears with a certain delay in respect to the respec-
tive tem5.erature change on the given part of th -e moon's sur-
face; (3 No change in radiotemperature of the moon has ever
been observed during the moon's eclipses. The following So-
viet astronomers are mentioned in this section of the article
-as having worked in thisfield: K.L. KadanovskjZ, !A.T. Turus-
bekov, S.E. Khaykin, M.R. ZelinsOa-ya, V.S. Troitskiy, L.I.
Fedoseye , N.A. Amenitski , R.I. NoskoVa -and the author him-
Card 2/4 self. The next section of the article deals with "radiopic-

80178
S/026/60/000/05/003/068
D034/DD07
Lunar Radio Emission
tures of the moon" as obtained with the radiotelessue of the
Fizicheskiy institut im. P.N. Lebedeva ik-adimii n -U'k SSSR (In-
stitute of Physics imeni P.N. Lebedev at the AS USSR), Pic-
tured on p 15. The reflector of the paraboLic antenn of this
radiotelescope measures 22 m in diameter. The radiopi uze
of the moon was obtained by using 8-mm radio waves. Two sche-
matic radiopictures of the moon are given on p 16. In order
to clear up the laws governing the radioemission of the moon
the author describes in the next section which thermal pro-
cesses are assumed to be going on under the surface of the
Vio-waves emitted by the moon, the
moon. The longer the ra
deeper under the surface,@ubstance which emitted them is as-
sumed to be. The scientists, working in this field (the
merits of V.S. Troitskiy are especially stressed), have
stated that the surface of the moon must be formed of a very
porous or even dusty substance over 10 cm thick. This model
of the surface of the moon, called a "one-layer" model, is
Uard 3/4 favored by the author as well, as opposed to the "two-layer" L4

80178
S1026160100010510031068
D034/DO07
I
Lunar Radio Emission
theory. There is 1 photograph, 1 graph, I set of graphs I
and 4 schematic figures. VV
Card 4/4 :@I

17.2
AUTHORS: Kuzlmin, A. and Shlomono
tITLE: Radioastronomical observations
PERIODICAL: Radio, no. 7, 1961, 6-7
22310
S/107/61/000/007/001/002
D201/D304
of Venus
TEXT11-. in the present article the authors discuss briefly
radioastronomy a@p a means of investigating the.physical properties
of the surface of"Venus.. The use of radioastronomy for this pur-
pose is possible because V4nus, being a heated bbdy, radiates ele-
ctro-magnetic waves. The power o3!-this..radiation is determined by
the body temperature and the-radiation capadi@y, _the latter depend-
ing on the body structure; according to Kirchhoff's law this radi-
ation capacity is proportional t 'o its absorption*capacityi. In
radioastronomy the intensity of radiation of an-ideally black body,
whi6h is characterized by the.density of radiation'�lux P (defined
as'the total energy emitted by the source in'the fre uency band
eg. 1 cls and f4lling in 1 sec. onto a surface of 1P) is detemined
Card 1/5

22310
S/107/61/000/007/001/002
A201/D304
Radioastronomical obpervations of Venus
2-TO.
by the body temperat re T by the following expression=@
where k = 1.38 x 10`@3 Joule/00 - the Baltzmann constant,'A - the
wavelength being receivedj.@r@- solid angle subtended by the body
under observation. The power of the signal being received is given
by. KrQA where A is the effective antenna area: Having-
LM=
2
measured the power of the signal received from Venus, it is easy
to determine its brightness temperature ( defined as the tempera-
tu-re 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 proporti6nal to its absorption-
capacity and may be different for different .'.,.?ngths. Thug.the
earth's.atmosphere is completely transparent for wavelengtbsfrom
7 - 10-m down to 2 am., but becomes-noticeably absorbing for sh&ter
wavelengths. By applying the above princIple to radiation emitted
by Venust both its atmospheric and surface temperatures can be
Card 2A

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
m21cls
and observations are therefore extremely difficult. After mention-
ing the first observations of Venus in 1956 by American scientistsq
the authors point out that fuller data were obtained by them per-
sonally using a 22 meter radiotelescope of the Fizicheskiy insti.tut
(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 wavielength is about 1.5 times smallei-tban
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 cm. 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
Venus 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,
Card 4/5

22310
S/107/61/1000/007/001/002
D201/D304
Radioastronomical observations of Venus
certain scientists f- Abstractors note: Not mentioned. 7do not
exclude the possibility of the so-called non-thermal i-echanism of
radiation from the planets, in which case the observed temperature
would not be the true planet temperature. There is 1 figure.

SALOMONOVICH A.Ye.
Observations of the zioon:s heat radiation in the radio-wave range
and-some characteriAtics of the maonls@ surface layer. i3tron.tsir.
rio.218.-4-6 F 161.@ (MM 14:7)
1. Fizicheskiy institut im. P.N.Lebedeva AN SSSR.
(MDOn)

illu-11:W711 A.D.; SALC;-.'*0M)VICll'J. A.Ye.
Radio ortis3lion of Vems on the q.6 an. -.-mvelength. Astron,toir.
no.221:3.!-5 AT) 161. WIFLI 14:n)
institut ireni P,!',, Lebodova Al! SSSR.
(Venus(Planet))
(Radio astronorw)

-- ------ - --
s/141/61/00111'001/002/022
E032/r3i4
3, 1 W 0124 J/-1 3e 11 A $1' 13 1
AUTHORS: :Kaydanovskiy, N.L.. and Salomonovich, A.Ye.
TITLE: On the Determination of-the Characteristics of the
Lunar Surface Using Observations@Obt'ained with
High-resolution Radio Telescopes
PERIODICAL: Izvestiya vysshikh uchebnykh zavedehiy,
Radiofizika,-1961, Vol, 4, No. 1, pps 40 43
TEXT: According to the 'theory of': thermal radio wnission
of the Moon, as'developed by Troitskiy (Ref, 1), the brightnes's
radio temperature of the Moon for a uniform spherical model
is given by,
+ c0s)(11wt - 117
n-1
wbere
Card 1/9

25942
s/14i/61/004/001/002/022
On. th eD et erminat ion of E032/E314.,
0 - R) T. +
2
T, R) a. D (2
I + 2;.cosa@ + 277, os-a
In these expressions V and tie ake the selbnographic
longitude and latitude, respectively', R(y,.y) is the
reflection coefficient, T is the night t,emperature of -the
H
surface, D = T Tg .,, where Tn is -the temperature of the
surface dt the point directly facing the Sun, is the
temperature distribution function for the Moon illuminated
by the Sun,
I +-IN-/ 2
a q(z)cos(nz)dz w is the angular frequen
CY
n
Card.2/9

25942
s/141/61/004/001/002/022
On the Determination of E032/E314
of the Moony .
n is the phase shift of the n-th
= are tg
4
n
1
n
harmonic, 6 /x is the ratio of the depth of
n n
penetration of an electromagnetic -wave 1/n to the depth of
penetration of the n-th harmonic of the temperature wave
l/P and a is the angle of incidence of a ray from
n
within the lunar crust onto the surface. Since up to recently
the radio emission of the Moon has been recorded with low-
resolution radio telescopes, the quantity that was measured
was not T
,rathera certain temperature
(y, q, t) but
,
e
representing the average over the lunar disc. The latter
depends on the polar diagram of the radio telescope
(Troltskiy - Ref. 1). In order to determine the physical
characteristics of "he lunar surface it is necessary to obtain
TH and T F1 from radiometric measurements.
Card 3/9

on the Determination of o.e.
2@,942
s/i 1/61/oo4/001/002/022
E032/E3i4
Moreover, it is also necessary to assume some specific form
for the functions R and q . The form of these functions
was chosen as in Ref. 1, using optical data wherever possible.
Since radio telescopes measure the projection ot' the distri-
bution T e(y, -0, t) onto a plane, it is expedient to trans-
form the selenographic coordinates 9, Y to the rectangular
coordinates x, y on this plane. These axes are respectively
parallel to the Equator and the Central Meridian of the
lunar disc. The relation between x, y and y,*@ is given
by the usual formulae
x = r sin y cos y = r sin f (3)
where v is the radius of the Moon. For points on the
Equator
x = r sin y, y = 0 (4)
while for points on the Central Meridian
Card 4/9

25942
s/141/61/004/001/002/022
On the Determination of ... E032/E314
x = 0, y = r sin 41 (5)
To begin with, consider the constant component
T (x, Y) 41 R(x, Y)R% + (ao/2)D71(y)
e, 0
where
j (y) arc sin
r
In the above plane, the radio isophotes T e,o = const.
take the form of approximately oval curves with a common
centre at the centre of the disc and ft y-axis as the axis
of symmetry. This follows from the assumption that the
lunar surface is homogeneous. The variable component T e
is superimposed on the T e,o distribution and, In general,
Card 5/9

25942
s/141/61/004/001/002/022
On the Determination of .... E032/E314
distorts the symmetry of the isophotes, displacing the
point with the maximum brightness towards the point
immediately below the Sun, i.e. it displaces the 11centre of
gravity" of the emission. When the higher harmonics of T
can be neglected,and when it can be assumed that cos acv 1
an approximate distribution of the radio isophotes of the
constant component can be obtained directly, using the
Te(x, y) distribution obtained with maximum displacements
of the "centre of gravity" of the emission, i.e. for
Wt - @ =S& =1-/2 or Yrr/2 . The isophotes of the
constant components T can in turn be used to obtain the
e,o
curve I(y) and then to compute the dielectric constant. As
will be shown below, the observations must be carried out with
the linearly polarised exciter of the radio telescope
arranged at an angle of +-11-/4 to the lunar equator (the
x-axis). The distributio-n along the Equator in the case of
the constant component is then given by
Card 6/9

25942
S/141/ft/oWoOl/002/022
On the Determination of E032/E314
X 'the
Moreover in accordance with Eq.@ (1) the distribution a
constant component,along the Central Meridian is given by
0,. y, 1T/2),. 01 17*,. D Yj (Y
T
I.
JI R(6, 0)1 j T. + (a.12) DI (7)
T'. (0. 0. 42)
Assuming that the emissive'-power as
en by Eq. (6) is independent of local changes and that it.
SIV
is the same along Ox and Oy' , it is possible to choose
i_(Y) (-with T and D known from radiometric measurements) so
that the . righUhand side of Eq. (TY should be equal, as near as
possible, to the' lefthand side which is obtained from measure-
:ments. Having determin d the forlm of the function if(y)
e
and c6nsequently knowing a the value of I - R and of
0
the-dielectric constant 71 can be calculated from Eq. (2)@.
Card 8/9

25942
S/141/61/004/001/002/022
On the Determination of .... E032/F,314
The measured amplitudes of the harmonics of the variable
component of the brightness temperature can then be used to
determine the depths of penetration of the electromagnetic
and the n-th thermal waves-and to calculate the effective
elect-rical conductivity and the loss angle a -
There are 5 references: -4 Soviet and I non-Soviet.
ASSOCIATION: Fizicheskiy institut im. P.N. Lebedeva AN SSSR
(Physics Institute im. P.N. Lebedev of the
AS USSR)
SUBMITTED: September 3, 1960

E_@VE435
AUTHORS: Koshchenko, V.N., Kuzlmin, A.D., Salowanovlrh*, A_@T
TITLE: Thermal radio emission from the moon in the 10 cm band-
PERIODICAL: Izvestiya vysshikh uchebnykh zavedenty,.Radiofisikat
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.l: Transactions of.the-.
Fifth Conference on the Problems of Cosmogony, Izd7. AN SSSR,-N.I,
1956, P.347) and K.Akabane (Ref.2: Proc. Japan. Akad., 31, 161
(1955)). According to the first, the mean lunar brightness
temperature, averaged over the disc, Is 1309K with a variation.of
due to the pliase changes. The corresponding values in the
second are 3150K and 25% variation. A single measure of 215*K 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 -1m.' The 22 m telescope'
of the Lebedev Physical Institute was usedi this and'the-'roceiver
used have been described in earlier work. Antenna temperatures
Card l/ 3

s/14i/61/004/003/003/020
Thermal radio emission from 000 E133/9435
were obtained in the range 132 to 154*K, depending on the phased-
Successive scans were made across the lunardisc, systematically
displaced from one another. The maximum value thus derived for
the antenna temperature corresponded to central passage across-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,
Radlotekhnika 1 elektrontka, 6, 430 (1961)). The present
observations, made during AprII-May 1960, gave an average
brightness temperature of 230 + 3.5*K. The variatIon from this
average did not exceed � 1.5% at any lunar phase. This result
agre,es well with the data given in Ref.7 (P.G.Mezger, H.Strawal.
Planet Space Sci., 1, 213 (1959)) for the 20 cm band (250*K 1 12%)
and also with a single measure made by G.Westerhout (Ref.8: Bull.
Astron. Inst. Netherlands, 14, 215 (1958)) of 232 :t 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.Troltskiy (Ref.10: Astron. zh. 31, 511 (1954)).
N.L.Kaydanovskiy, M.T.Turusbekov and S.E.Khaykin are mentioned in
Card 2/3

7.'A i/61/004/003/003/020
Thermal radio emission from E 3/3,1435
the paper. There are 1 figure and 10 referencem: 5 Soviet-bloc
and-5 non-Soviet-bloc. The referencey to English language
publications read as follows:
Ref.2: as quoted in text;
Ref-3: an quoted in text;
Ref.7: P.G.Mezger, H.Strasal, Planet Sp&@_e S-ci., v.1, 213 (1959).
ASSOCIATION: Fiz,-,@heskiy institut im. PN.Lebedeva AN SSSR
(Physics Institute imeni P.N.Lebe&ev AS USSR)
SUBMITTED: November 10, 1960
Card'3/3

//17
2 0 (/1 A6
7
-
/
1

AU'THORS. Kislyakov, A@Cx, Kuz A,Ye,
--------------
TITLE, Radlo --mission from --------
t mtrt band-
PERIODICALi Izvesliya Tysshikh Radicfizika,
1961, Vol.4.. No.3.
TEXT., Observa-@ions of Venus -trt: zm, -h 1964, usLng the
22 in radio telescope of th.-i Fizl,::h--i@-
---; t imen.' ..
P.N.Lebedev AN SSSR (Phys.i,:;s P.N.Lebed*v AS USSR)
in the 4 min band, The method wh, -!i:p*--3yt-d h-2e btein
debz@ribed pre-viously (Ref @ 2@ A,D@KA@ A,Y@,
Astron, ?.b., v.37@ 297 (1960)), G,, planat w&,s by
vpti@al abservation with a!-aw trai The antenna
temperature was determined by two Thb t"irss -oras by
inserting an ab8orbing wedge. at in the signal
path@ - 'The error a-n. the reaulting f-x ih,,@ 'Itinp-trAture was
vithin +- 7%. The second msthod wa --.,rrparibcn --f tha signal
with th;-7 atmoapheri(- I-adlation, (Thl@ absorption
-alues for 4 min wave5 ara -well know-ii. fnk-i sz-,'.ond meth,@d waa
used as a -heck on.the first. rh f@ v-, -1a reduc-i-n@" th4
Card 1/2

#_..,/oO4/003/0_
9/020
Radio emissi on from Venus
observations probably liss in the the a-zarage
temperature over the whole of the In this
connezrion, the halfwidth of the m, 7:-T@ t-rah in-trestizated and
found to be 11@6. The amount of :i-% the antenna was
investigated by ob3erving the Sun The brightness
temperature of Venus, averaged d-,se_ was then
found to be 390'K i 120-K, Ther il Soviet-
bloc and 1 n on-Soviet-bla-.. The an English language
publication reads i@s follows@@.
Ref@3. A.W.S traiton, C.W@Tolb@-rt, P-., -,@48@ 898 uq6o).
ASSOCIATIONS .- Fizicheakiy in5tit'l.- AN SSSR
(Physi-,..s Institute @:-`,Lebede- AS USSR)
izi@heakiy inst-itut
pri Gor @k-_,-18kom un-- (S'_ientit1-i,. Researth
Institute for Rad@@i:.O-_ Uni-zers-Y)
SUBMITTED; May 9, 1961
Card 2/2

30674
s/14i/61/004/004/001/024
-S, 2ro V 0"@ B032/E514
130 IWO
AUTHORS: Salomonovich. A.Ye. and Koghchenko, V.N.
TITLE: Observations of lunar theritial radio emission at
2 cm wavelength
PERIODICAL: Izvestiya vysshikh uchebnykh zavedeniy, Radiofizika,
1961, Vol.4, No.4, pp-591-595
TEXT: This paper was fIrst read at a meeting of the Planet
Commission of the Astros6viet (Astronomical Council) in October,
1960. The authors repori observations of the lunar radio
emission at 2 cm wavelenith which were carried out in November-
December, 1959 using the'22 m radio telescope of the Physics
Institute of the Academy of Sciences. This telescope was
described by the first of the present authors (Ref.2: Radio-
tekhnika i elektronika, 4t 2092, 1959). The radiation was
detected with a ferrite radiometer of the "usual type". The high
frequency part of the detector was placed together with the i.f.
amplifier near the focus of the 22 m paraboloid. The open end
of a circular wave-guide was used as the feeder. The electric
vector of the linearly polarized wave incident on the system was
Card 1

30674
Observations of lunar ... s/14i/61/004/004/001/024
E032/E514
at an angle of 45* to the plane of the horizon. The beam width
at 3 db in the E and H planes was just greater than 41. The
antenna temperature was measured as described by the first of the
present authors (Ref-3: Astron.zhurn., 35, 129, 1958). The
systematic error in the determination of the brightness tempera-
tures was about +15%. Fig.1 shows typical distributions obtained
for six differen-t optical lunar phases. It is found that there
is a systematic displacement over the lunar disc of the maximum
brightness temperature and this follows the sub-solar point. An
attempt was made to estimate the functional form of the variation
in the surface temperature, using the method described by
N. L. Kaydanovskiy and A. Ye. Salomonovich (Ref-5: Izv. vyssh.
uch. zav. Rad' f'z'k 4, 4o, ig6i). The variation appears to
follow a cosi Y law: where if is the selenographic latitude.
Assuming that the surface temperatures at the centre of the disc
at lunar noon and midnight are 407 and 1250K, respectively, it is
found that the ratio of the depth of penetration of radio and
thermal waves is 6 = 4.4 = 2.2k. The result 6/k = 2.2 differs
somewhat from that obtained at 1.63 cm wavelength by N.R.Zelinskaya,
V. S. Troitskiy, and L. I. Fedoseyev (Ref.6% Astron.zh.31,643,1959).
Card 2//-.,,/

30674
Observations of lunar s/i4l/61/oo4i'004/001/024
E032/E514
Using the value 6 = 4.4 it can be shown (V. S. Troitskiy, Ref.11
Astron. zh. 31, 511, 1954) that the phase delay of the variabl*
component of the temperature relative to the optical Ohaso in
about 39", which is in agreement with observations. Fig-3 shown
the brightness temperature at the centre of the lunar disc
T K as a function of the phase LP, deg. It to clear that
the phase variation may be approximated.by the expression
T" 190 - 20 coo 4oo). Acknowledgments are,
opt opt
expressed to N. A. Amenitskiy who developed'the radiometar,.and
took part in'the measurements and to R. 1. Noskova- who assisted
in the analysis of the,.@records, There are 3 figures and
6 references: 5 Soviet and 1 non-Soviet. The'Englidh-'language,
reference reads as followst Ref.4a R. N. Bracewell, Austr.J.Phys.,
9, 1-4, 1956).
ASSOCIATION: Fizicheskiy institut imeni P. N. LebedevaAN SSSR
(Physics Institute imeni P. N. Lebedev-AS USSR)
SUBMITTED: November 10, 1960
Card 3/),7

30675
s/,-41/61/004/004/002@,024
E032/E514
Ire 61 (/ 4 10
AUTHORS: Koshchenko, V.N., Losovskiy, B.Ya. and Salomonovich A.Ye.
TITLE: The lunar radio emission at 3.2 cm wavelength
PERIODICAL: Izvestiya vysshikh uchebnykh zavedeniy, Radiofizika,
1961, voi.4, No.4, PP-596-5909
TEXT-. The authors have measured the brightness temperature
of the thermal radio emission of the moon at 3.2 cm wavelength
using the 22 m radio telescope of the Physics Institute of the
Academy of Sciences. Systematic changes in the two-dimensional
radio brightness distribution were established. The beam width
at 3 db was 61.3 + 01.2 (Ref-3t V. M. Karachun, A. D. Kuz'min,
A. Ye. Salomonovl'jh, Astron. zhurn. (in pruss)). The sensitivity
threshold of the detector was 3-40 at a time constant of I sec.
Fig.1 shows some typical distributions obtained for different
optical phases. These distributions were then used to determine
the brightness temperature of the centre of the lunar disc TLk an
a function of the lunar phase. The result is shown in Fig.2
(93 - August, 0 - September, / - October,,A - November, 1960).
The average value of the brightness temperature was found to be
Card

30675
The ldnar radio emission at ... s/i4i/61/oo4/oo4/OW/024
E032/E514
2230K and the experimental points can be represented by the
formula* T ljia= 223 - 17 Cos (* - 45) deg. Assuming that the
latitude val tion of the surface temperature (A. Ye. SalomonovO@
and Vi N. Koshchenko, pp.591-595 this issue) is of the form cos 4&
the theory given by V. S. Troitskiy (Ref-7: Astron. zhurn., 31,
511, 1954) may be used to estimate the ratio of the depth of
penetration of radio and thermal waves 6 into the lunar soil.
The 3.2 cm observations yielded 6 = 6.1 so that 6/k 1.9. This is
approximdtely the same as the value obtained for X 2 cm (Ref.6:
this issue PP-591-595). The measured value of the phase delay
(450 + 50) is in good agreement with the,calculated value (410)
obtai;led on the assumption of a uniform radiating layer. There are
2 figures and 7 referencesz 6 Soviet and 1 non-Soviet. The English-
language reference reads as follows: Ref.54* R. N. Bracewell,
Austr. J. Phys., 9, 1-4, 1956).
ASSOCIATION: Fizicheskiy institut imeni P. N. Lebedeva AN SSSR
(Physics Institute imeni P. N. Lebedev AS USSR)
SUBMITTED: January 23, 1961
Card 2/P__

21658
s/109/61/oWoo/013/018
8, / 716 (1 C,'//.) 6@ E032/E314
AUTHORS; Kalachev, P.D. and Salomonovich, A.Ye. L
TITLEs The Radiotelescope of the Physics Institute of
the AS USSR, Incorporating a 22-m Parabolic
Reflector
PERIODICALs Radiotekhnika i elektronika, 1961, Volo 69 No* 3*
pp. 422 - 429
TEXT., The radiotelescope is in the form of a parabolic
reflector having an aperture of 22 m and & focal length of
9.525 m (angular aperture 2'T = 120 deg). The design of the
radlotelescope was carried out at the Physics Institute of
the AS USSR and it was brought into use in the summer of 1959.
Various radio-astronomical observations have already been
carried out, including the 0.8 cm radio emission of Venus.
The reflector can be rotated between -5 and +95 deg relative
to the horizon. Azimuthal rotations of +,80 deg are also
possible. The radiotelescope incorporatZs,a 110 mm refractor,
used as an optical telescope-guide. The following facilities
are available: a) automatic tracking of a given point on the
Card 1/2

21658
s/ioq/61/oo6/oO3/0l3/Oi8
The Radiotelescope .... E032/E314
celestial sphere to within + 30 deg; b) semi-automatic
tracking in accordance with the programme fed in by the
operator over given time intervals; c) alignment in a given
direction from the control cabin; d) alignment in a given
direction and motion with a given velocity controlled by the
operator in the visual-alignment cabin. Angles can be
measured to within 7.5tt Photographs of the telescope are
reproduced and a brief @escription is given of some it its
mechanical parts. Further details are given in the next
abstract. There are 6 figures and 1 Soviet reference.
ASSOCIATION; Fizicheskiy institut im. P.N. Lebedeva AN SSSR
(Physics Institute im. P.N. Lebedev of the
AS USSR)
SUBMITTED. May 10, 196o
Card 2/2

21659
3, / 7/ 0 N 4111 /12-9/ 1/ 17) S'/109/61/006/003/014/018
Z032/E514
AUTHORSt Karachiin. A.M., Kuzlmin, A.D. and Salpmonovich, A.Ye
TITLEa A Study of Some of the Electrical Antenna Parameters
of the 22 m Radio Telescope of the Physics Institute
AS USSR
PERIODICALS Radiotekhnika i elektronika, 1961, Vol.6. No.3,
PP-430-436
TEXTt 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 Physics Institute 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 should be
181.3 and 191.6 in the' H and 9 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(Ref.5)
Card 1/3

21659
A Study of Some of the Electrical ... S/109/61/006/003/014/oi8
IC032/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 + 0'.1. The width in the E plane
at 3 db was found to be 21.1 + 01.1. The expected widths were
V.6 and 19.7,, 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. 17 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. I. Stepnov are thanked for arranging for
this work. There are 3 figures and 12 referencest 7 Soviet and
5 non-Soviet.
Card 2/3

a
7S

89323
S/033/61/038/ool/oo6/o.19
1127) E032/E3i4
AUTHORS. Karachun, A.M., Kuzlmin, A.D. and Salomonovich, A.Ye.
11@
TITLE: Observations of Some Discrete Radio Sources on 3.2 cm
PERIODICAL: Astronomicheskly zhurnal, 1961, Vol. 38, No. it.
pp. 83 - 86
TEXT; The 22 metre radio telescope of the Fhysics 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 OK. 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
obtained 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 () of the observed sources;
Card 1/5

89323
8/033/6l/O38/ooi/oo6/ol9
E032/E314
Observations of Some Discrete Radio Sources on 3.2 cm
Source OL 1950b1950 TIK P 12 249 9
;@M cps
Tau A 05h3lm.5 22 0 00, 40 (61 f4l
19 [ 1+0.
Orion 05h32m.8 -5*251 24.5 3.6+o.8 5? "@5
Omega 18hl7m.65 -16*15' 33.5 570.8 5@.8701.5
Cyg A 19h57M.75 40*35' 11.5 1.770.4 -
Cas A 23h2lm.2 58'321 34 571 42
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
described by a power law of the form p = Af n, with n = const.
The numbers on the gjaphs, Fig.2,refer to the reference list at
the end of this paper. The angular dimensions for Cas A are in
Card 2/1":

89323
S/033/61/038/061/006/019
9032/EN4
Observations of Some Discrete'Radio Sources on 3.2 em
190od agreement with the data of Jennison (Ref. 25) and
Minkovski (Ref. 27). Acknowledgments are expressed to
N.A. Amenifskiy, N.F. Il'in and V.N..,Koshchenko for their
assistance.
'There are 2 figures, I table and 27 references: 7 Soviet
and 20 non-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, 196o
Card 3/5

L
C503.23
S/053/61/038/ool/006/019
E032/E314
Observations of Some Discrete Radio Sources on 3.2 cm
Fig. 2a: Fig. 2bi

pglo ll.@.',q

11
0 Q/S

2

V#
Cl
0PUV4 Omen
J%
IN
7@
em IM IO
U

Card 4/5
711119M

S/03839/3VI/038/001/oo6/olq
E032/E314
(,;bservations of Some Discrete-Radio Sources on 3.2 cm
F ig. 2 c Fig. 2d:
ILI
A(
/CM
Card 5/5
n-w
fleftab 17

tj

lucif
foil
tox

-- ----- I ---- ---- -

MY IN I&M