SCIENTIFIC ABSTRACT SODIN, L.G. - SOFIANO, T.A.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001651920001-6
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: August 26, 2000
• Sequence Number: 1
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

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ACCESSION XR: AP5ooo6ii S/01)21/64/000/011/1464/1468
AUTHOR: Bazelyan. L.-L.; Bjr-a-LudeS. Ya. (Corresponding member AN
UkrSSR); yAy_~be_rg, V. V Krymkin, V. V.; MeA-',_A._ V.; q_odLa, Q.
TITLE: Radio emission spectral density of some discrete sources at
frequencies of 20-40 Me
SC!-,JRCE: AN UkrRSR. Dopovidi, no. 11, 1964, 1464-1468
TOPIC TAGS: radio astmnom~~-radio telescope, radio emission
ABSTRACT: Radiation"densities of eight discr-Lte sources of cosmic
radiation in the 20-40-Mc band were measured with a wide-band radio
telescope. The measurements were carried oj~~ from October 1963
through February 1964. Them r.~Lij teleAlope' consisted of two electri-
cally controlled multielement antenna- arrays (each with 128 radiators)
spaced 4TO m apart along an E-W line. The antennas formed the elements
of a T-shaped interferometer system. The width of the radiation pat-
tern of each antenna was 4.60 at 20 Me and 2.3' at 40 Me; the inter-
ference interval at these frequencies was 1.8" and 0.90, respectively.
Phase-modulited radiometers.(i-f bandwidths, -40-15 kc) were used for
Card 1/2

L191.192-65
ACCESSION NR: AP5000611
signal reception. Radiation from each source was recorded simultane-
ouely at 20, 25, 31, and 38-5 Mc.; Recorder time constant was nearly
30 sec. Cassiopeia-A was used ao,a standard source of radiation. No
discantinuitylof thy,opectrum vas.noted for sources situated within
the angles 15 0 < L < 2000, and -130 < bII N< 600. Orig, art. has3
\2 figures and 2 tables.
ASSOCIATION.: Instytut radiofizyky i elektroniky AN URSR (Institut*
of Radio P yq1cs
SUBMITTED: 2TMar64 ENCL: 00 SUB CODE: AA,W
NO REF SOV: 004 OTHERt oo6 ATD PRESS: 3161
Card 2/2

ACCESSION NR: AP4039721 S/0141/64/007/001/02IL5/0224
AUMOR: Bazelyanq Is. Le, Bruk, Yue Me, Zhuk, I. -N.,.; MenIg A. Vs-,'Sodin. I" G.;
Shar-j*kin, N. Ke
TITLE: Wide-band radiointerfermeter with electric control of antenna pattern--
SOURCE: IVUZ- Hadlof Isika, v. 7 $ no. 2, 1964 0 215-224
TOPIC TAGS: antenna radiation pattern, antenna switching, radio astronomy, radio
interferometer, radio emission
ABSTRACT: A broadband (20 - 40 Mcs) radio interferumeter with a 470 meter basep
oriented east and west, is'described. The interfervmfer is intended for the in-
vestigation of radio emission from disatNeete scumes and the' cosmic backg-ound in
the northern hemisphere by dimativity-pattern scann3ng :Ln a + 900 elevation
sector and by using the earth's rotation. The interfercmetex;-ccnsists of 220 8-
dipole plane arrays with rono e digital* control of the directivity pattern in the
meridional planes The descripFticn coym-s the princliples underlying the control'of
the bean and the sunntion of the signalsq the arrangenent of the antenna, the
control elements * the antenna directi".. pattern, the antenna effective area* ends
the antenna. pins The large base separation of the Bour-M radio
Card

ACCESSIM NR: AP4039721
emission from the cosmic background. The two interferamter antennas are differ-
ent and can be used separately. Me eastern one can be used as a transit instru-
ment. By using the western antenna with bean scanning, it is possible to make twol
or three records of a source passing through the azimuthal pattern, with intervals;
of 10 - 20 minutes. The resolution of the interference diapyam is 1.6 - 0.80 in~_
direct ascension and 40 - 20 in declinations at frequencies 20 - 40 Mcs. It is
11'eccmmended that the antennas be used separately for-the radio emission:of the
cosmic backgound, in which case the resolution is It - 20 in ascension and 34
170 in declination fbr the eastern antenna, and 34 - 170 in ascension aM 4 20
in declination for the western antenna (both at 20 - 40 Mr-s). Some precautions-,
Orl art has
necessar-I in the operation of the interfercmeter am, ra*ioned. g. V.'
9 figures and 2 tableac
ASSOCIMON: Institut radiofiziki i e1Wctr%1W AN tkrMR (Institute of R,9,dic~_
pllYsics and Electroniess M Um-SSR)
SUBMI=: Mgr63
ENCL:: 02
suB com M, EC MR RLT SOV: 001 DIM: -003
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..........
ACCESSION NR: AP4042515 6/0109/64/009/007/1179/1161
AUTHOR: Sodin, L. G.
TITLEI.: Statistics of the phased antenna array
SOURCE, Radiotekhnika i elektronikat v, 9, no. 7, 1964, 1179-1187
TIOPIC, -TAGS: antennat antenna array, phased antenna array, electrically
goteerable antenna
A96TRACT: Formulae for the average array field coefficient and power
coefficient (describing the radiation pattern) and the average directive gain of &:
pkasediarray (electrically steerable antenna),- with correlated fluctuations of the
arnplitudea and phases of radiator currents, are developed. Simplified for
biwee&onithe assumption ofa small correlation radius as compared to-the anteftrli._'L._~
sirse-are intended for engineering estimates. It is shown that with snmdl radii,
664eff6ct of erroro upon the radiation pattern depends but little on the- carrelatiol
j"
C.
[~c

6058-65 ES C-1j/E1VG (v)1 M,(.L)/FBD GW!~WS"4
ACCESSION BR: AP5013821
AUTHOR: .1 (ling member AN UkrSSR);
BaMy~t tj__L Tot,; krA (Correzpon
kip :0~-60dln, L. G.)
V. V.; Men A-1:1. -
V
TITLE.- Ue frequency'spectra of sonic discrete:soun~.es in the -decameter radio- band,
souRCE: All UkrRSR. Dopovidi, no. 5, 1965o 580-583
TOPIC TAGS: radio astr( OT radio telescope).cosmic radio sourcei galactic radi-
ation
ABSTRACT: The results are presented of measurements of the radiation flux of six
discrete sources in the 20-40 Mcs band. The Measurements were obtained at.the
radioastrononileal observatory of Institut radiofisiki I elektroniki (Inetitute of.
Radio Physics and Electronics) AN UkrSSH using~a T-like band telescope operating
as a meridional inatrument. The telescope was described in detail earlier (Izv.
VTJZo-v Radiofizika v. 7, 215, 1964). The measu:rements were compared with the flux.
of Casniopea-A which was chosen as the standard. lbe spectra are found to be
linear in the whole frequency range and can thus bc; classified as being of the
i spectral type S. It is established that the sources bounded by,the galactic co--
ordinates 210 < ITI < 89G., -130 :~ bII /_&dio emission sourest radio emission mean-
lurement, radl loacope r
,ABSTRACT: The spectra of 14 discrete sources (in the 20,-40-mc range) veie in-
,Ycatigated at the Radio Aatronomy Observatory of the Ins ,tute of Radio Physics
and Electronics, Academy of Sciences UkrSSR, from October 1963 through July 1964.
All.observationo were made between 2200 and 0800 hours local time. The radio telt
scope employed an iInterferometer, and .its antenna system consisted of tvo videband"!-'
multielement electrically phased arrays, each rtasuring 176 x 17 m and spaced
470 m apart on 'an east-vast line. Each array consisted of 178 horizontal dipoles.
Pattern width was 40 for 20 Me and 20 for 40 Me. Lobe vidth of the interference
1;a1rd -114---

,L 59TI5-65
ACCESSION NR: AP5015584
pattern was 1.60 for 20 1,1c and 0.8' for 40 Me. Benz decl!nation along the meridian
wan regulated by remote-control delay lines. The telescope radiometers were phase
modulated by phase rWting the signal of one of the antennas through 180* at a
frequency of 60 cps. The signals of each antenno. were am~)lified by hf preamplifiers'.
The pasaband of the preemplifinra and of the phnse st'.fter was about 20 Me. The :
adjustable pausbando of the four radiometers made it possible to record each source'
at four frequencies simultancously (20, 25, 30-31. and 36.5 Me). The recordings : -1.
were calibrated with a standard-aignal generator fed through a calibrated attenuator
and a Bplitter to the preamplifier inputs. All the sources were measuredMby,com-
paring them with the standard flux of source 3c 461 (Cas-A)s which at 20
h50 x 10-7.4 V/M2 cps. Flux densities (6-1024 Y/Mc) and tb- wean probabl
(A%) for fourteen of the soUrcen are listed in Table 1 of Enclosure. On the
basic of these and previous measurements of Can-Ag Bignus-As iirgo-A, and Taurus-A,
the apectra of 18 diacrete sources can be divided Into two Jaeses: spectra vith
~ constant spectral index from 20 to 1400-3200 Me (13 sou-,,ces) and spectra with
~ spectral-indnx which is a function of the frequency (5 rources). Orig. art. has i
3 figures and 2 tables.
ASSOCIATIONt InatItut radiofIz1ki I elektronW .^'j nauk WWR (InatItute
of Radio Physics and Electronicq. Acadew of Scienceo,~5~)-
1.6,d- -v4

L 50365-65
Acck;331011 UR: AP501558),
BUD CODZIA~IC
GUEMITMEM. 13Sep64 ENCLt 01
No Ru soV: o16 OTHER: 015 ATD.PRM8' 4046
Card 3/4

ACC NR% AP6OZ3856 SOURCE'CODE."-Uja:lolo8-l66-/021/007/0016/OOZS
AUTHOR: Bruk, Yu. M. (Active member); Sodin, L. G. (Active member)
ORG: Scientific and Technical Society of Radio Engineering and El e ct ro communication!
(Nauchno-tckhnicheskoye obshchestvo radiotekhniki i elektrosv-yazi)
TITLE: Calculating principal parameters of phased antenna arrays having discr6te
tier-type asynchronous control of beam parameters
SOURCE: Radiotekhnika, v. 21, no. 7, 1966, 16-25
:TOPIC TAGS: antenna array, phased array antenna
iABSTRACT: A method is describ ed of essential simplification of the time-delay
i system of beam-position control by using discrete
0 Y, x, x, x,-.9hasing delay lines arranged in a binary scheme. Both the
I I j r j 'r I i tier: I I1 -3 1 11': III ..
1

rA_&7~4k_..W_J~6b 2 3 8 5 6
lare investigated, and the pattern distortion, main-lobe displacement, and directive-
Igain reduction caused by these errors are determined. The distribution of phase
lerrors over the antenna aperture is represented as a trigonometric polynomial.
I I
IFormulas are derived for selecting the discreteness and determining the number of
!switching elements from known permissible directive-gain reduction or spurious
;side-lobe radiation. The greater the number N a 2 of delay positions, the greater
ithe simplification of the phased antenna array that can be achieved. Orig. art. has:
3 figures, 30 formulas, and 1 table.
CODE: 09 / SUBM DATE: 27.Tul64 / ORIG REF: 003 / OTH REF: 002

ACC NR: AP6036368 SOURCE CODE: UR/0109/.66/011/011/1953/1959
AUTHOR: Sodin, L. G.
ORG: none
TITLE: Statistical analysis of nonequidistant linear antenna arrays
SOURCE: Radiotekhnika i elektronika, v. 11, no. 11, 19 66, 1953-1959
TOPIC TAGS: antenna array, antenna theory
Y. T. Lo's statistical analysis of nonequidistant arrays (IEEE
AP-12, 1964, Z57) is not entirely correct insofar as side lobes are
concerned. M. 1. Skolnik's et al. analysis (IEEE,.,Trans. , AP-12, 1964, 408)
Jgnores field fluctuations. The present article fills these gaps. The antenna is
assumed to consist of a sufficient number of radiators no that an independent
failure of one of them still permits regarding the laws of distribution of various
Card. I /Z

~ACC NR: AP6036368
sums as normal. The directional pattern is required to satisfy only two
conditions: major-lobe width and n-dnor-lobes radiation level. Accordingly,
formulas for statistical parameters of the directional pattern, for field distribu-
tion density, and for the probability of exceeding a specified level of radiation
'from minor lobes are derived. -These formulas permit designing, with any degrei
Of surety, a linear antenna array (with a decreased number of radiators) on the
basis of a specified side -lobe -radiation level. However, the exact deployment of
N radiators in N possible points remains vague; the method of dynamic
programing seems promising for solving this optimization problem. Origa art.
'has: 1 figure, 35 formulas, and 1 table.
SUB CODE:. 09 SUBM DATE: 07Jun65 ORIG REIN 003 OTH REJF: U11
Card Z/2

SERY, Vladimir; MATEJOVSKA, Dobromila; JEZEK, Zdenek;-NP4-1-~
'An epidemic of gastroenteritis caused by portable water. Cesk. epidem.
mikrob. imun. 10 no.4:226-239 &W.
l. Ustav epidemiologie a mikrobiologie v Praze.
(GASTROENTEIRITIS epidemiol.) (WATER SUPPLY microbiol)

FEDOVA,D. DRASNAR, M.; SVEJDA, J.; PIPKCVA, Z.;-ISODJA, J.; SYRUCEK, 1,
Epidemic of influenza in Czechoslovakia in February-April 1964.
J. hyg. epidem. (Praha) 9 no.l-~95-110 165
1. Institute of Epidemiology and Microbiology, Prague.

00 83164
'0-~21Z S/056/60/039/002/001/044
/. // o 0 BoM/N56
AUTHORS: Li Ga Ye~f Osetinskiyt Go M , Sodnc-m, N., Govorov, A.M.,
~T-zov, 1. V. , Salatakiy, V.
TITLE: Investigation of the He3 + H3 Reaction
PERIODICAL- Zhurnal eksperimentallnoy i teoreticheskoy fiziki, 1960,
Vol. 39, No. 2 (8), pp. 225-229
TEXT: The He3 + H3 reaction develops according to the following modes:
He 3 + H3 --i~ L i 6He 4 + H2 + 14. 3 1 Me v ( I )
--.oHe4 + H1 + n + 12.08 Mev (2)
--~-He5 + H1 + Q.
(3)
He4 + n + Q
The authors determined the total cross section of this reaction by
integral neutron counting, using a thin gas target. The ratio between the
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833.6h
Investigation of the He,) + H.J Reaction S/056/'60/039/002/001/044
B006/BO56
results obtained by Mook (Ref. 2) are.plotted. One of the charged-
particle spectra recorded for determining *the branch ratios is shown in
Fig. 2. The spectrum has two peaks corresponding to the alpha particles
and the deuterons of branch (1). Between these peaks is the continuous
spectrum of the protons from (2). The proton peak corresponding to the
ground state of He5 is, as regards energy, near the deuteron peak of (1),
and could not be separated spectrometrically. Analogous spectra were
recorded at triton energies (150 - 950 ke'v), which were equal in each
case. The average fractions of the three branches in the rpaction were
determined to be (4112)% (1); (5512)% (2); (410% (3); the total reaction
cross sections in the range 150 - 970 kev amounted to 3.2 - 63-0 mb.
From the experimentally determined proton energies of (3), the He5 decay
energy was determined from the relation
L(HO) = 0.4 E H3 - 1.2 EHI + 12.08 Mev, where EHI = (9.6 � 0.1) Mev.
& = (0.8 t 0.1) Mev was obtained. This value agrees quite satisfactorily
with those obtained by other authors. The authors finally thank
Professor V. P. Dzhelepov, Professor I. M. Frank, and L. P. Lapidus
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83164
Investigation of the He3 + H3 Reaction S/056/60/039/002/001/044
Boo6/BO56
for their interest and discussions, and they also express their
gratitude to the members of the generator team I. A. Chepurchenko,
N. N. Schetchikov, and M. V. Savenkova. There are 2 figures and 8
references: 3 Soviet and 5 US.
ASSOCIATION: Ob",yedinennyy institut yadernykh issledovaniy (Joint
Institute of Nuclear Research)
SUBMITTED: January 27, 1960
Card 4/4

ACCESSION NR: AR4015666
S/0081/63/000/021/0478/0478
SOURCE:- RZh. Khimiya, Abs. 21S36
AUTHOR: Sodnomov, a. M.
TITLE: Effect of the duration of stationary contact on the magnitude of.the
static friction force for polymers
CITED SGURCE: Uch. zap. Buryatsk. gos. ped. in-t, vy*p. 22, 1961, 17-23
TjING Ti~G,'; ~olyniar, polymer friction, static friction, static friction force,
s!--~:-ionary polymer contact, stationary contact period
A31STRACT: A study of static friction for a numer of polymer materials (laminated
polastics, pol,',.:thylene) -nd glass in contact with organic glass showed that the
st-at;c friction orce ir.,-reases with an increase in the duration of contact. This,
incrcase c-tenua tcs with time. Diagrams are given for the dependence of static
friction force On time. The author suggests thai thi mutual intrusion of surfaces
in contact with each other is accompanied by plastic amalgamation of the material
in the conzac: a;-eb. I. U.
'On'TE ACQ: 09Dec,-S3 SUB CODE: MA ENCL: 00

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