SCIENTIFIC ABSTRACT VERNOV, S.N. - VERNOVSKIY, A.I.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001859520008-3
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: September 1, 2001
• Sequence Number: 8
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

L 1553-66 FSS-2/EWT(1)/FS(V)-3/FC(;/IWA(I)/EdA(h) TTIGSIGW
ACCESSION OR: AT50236io uni /6/006/000/69 5
AUTHOR: oarnnv- R- 9-- Miulnknv- A- Yin- V
A n
~hev~-Xu--I "t6snovets. E. N.
Kutnetso 11;
EV r. A.
-RubinsAteym:'T' . A E121poyXi. 1. G. tekov~
4,f ss~ _, 'S -,
TITLE: Geometric ponition and particle composition Pf the earth's radiation belts
SOURCE. Vsesoy-uzneya konferentaiya po
1965. (Space research) -, trudy konferentsit.
IMoscow, Izd-vo Nauka, 1965, 394-405 1-1
I TOPIC TAGS: cosmic radiation, earth radiation belt, cosmic ray, ~~lekt:Cqn 1. Elek-
tron 2
ABSTRACT: An exhaustive study is made of data recorded by the'Elektron-1 and -2',#
isatellites, which were launched on 30 January 1964. Orbital dw,"a are given in t
Table 1 of the Enclosure. The first orbits were positioned so that the satellites 7-
passed their apogee at about 3 o'clock a-m local tide. The outer boundary of the
radiation belt was thus crossed at about midnight and again at about 7-8-lrlm. on the
return branch of the orb1t. The subsequent otblte were shifted toward the sunaet I
Elektron-1, by 8 min, and Flektron-2, by about 4 min in the 24-hr period. Elek-.-).'l
i Card 4_

-L. 155?-66
ACCESSION HR: AT5023610
tron-1 and -2 were equipped with similar Instrumentation. In some cases, however,
there were differences ij~f ertrg y th regholdd. J A Watt sura adzi3g &I d#a dious ft electron
and proton fluxes of different energies In t~e equatorldl plane tmd for comparison
gives IMP-1 data. The following conclusions can be made from the chart: 1) A belt;
of artifically injected electrons exists at distances closest to the Earth's centerl.
The maximum of the bd1t in February 1964 was at L - 1.35. The flux of electrons
with energy above 2 Mev at the maximum was about I x 101 cm-2-aec-1-ster-1. 2) The
average directed flux of protons with an enerF of 45-70 Mev at the maximi of thel
inner belt (L = 1.45) was about 1.5 x 103 Car -see-1-ster-1. A change in the inte-
gral spectrum at proton energies above 50 Mev was observed at L = 2.2; the spectrum
of these energies is in the process of hardening, which could be explained by the
theory of albedo neutrons. 3) The spatial distribution of protcnis with an energy
of one to several Mev differs from that of the electrons. There is a definite reg-
ularity in the distr%ibution of protons according td their energien. The average
directed flux of protons with an energy above 2 Hev was about 4.5 x 105 Cd-2 see-1.1
ster-1 in the equatorial plane at L = 2.8. It appears that the mejority of Z
protons in this energy range are created by transverse drift with respect to the
magnetic field lines, 4) A belt of high-energy electrons was observed at L a 2-T%~
Its width at the equatortvas about 0.4 earth radii. The average directed flux of
electrons above 6 ~Lev was about 102 em-2,ged-l-ster-l. 5) A mimimam of distribution
card

L 1553-66
'ACCESSION NR- - 5
AT 023 0
of electrons of above 150 kev energy was observed in the regiort between L 3and
L = 4. The altitude intensity shift Is subject to large fluctuations in time and
may drop at times to negligible magnitudes. 6) The maximum of the outer belt is
positioned, on the average, at L - 4,6. Tlie maximin ratitude intensity shirt in-
dicator m a 0.5 +O-3/-0-2~v1fh1r1 a wide range of L. Thera is a sharp Intensity
jump~on the night side at L u 7 + 0.5. On the morning side, a slow monotonic drop
of intensity was observed. The average directed flux of electrons with an energy
of over 70 kev at the maximum, of the outer belt is about 5X 106 =72-sec-l-ster-i
and can change by more than an order of magmitude. The electran energy spectrum
116ba-i-e-r-ved within is' in data of othe_~ re-_1
1~searchers. The electmrr-eterV. spadtrum Ln-tbe 6'ndr'g3rPrtu2gb above 1 Hev appears t-~11
be s,:,ft-n4ng, in 7omparison with measurem,-!ntn of earlter years. Ortg. art. has:
11 figurea, [FP)'
ASSOCIATION. none
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L 1553-66
EffCUEM, 011
Table.-I.-Orbit4l.-data.-
IncIlAsti4t
J orbital-21me
Period of
F.lektron-1
Gov altitude)
- t Vlektron-2
high eLltitude)
Altitude, apogee T, 14o km 68,2oo km
Altitude, perigee W6 km 46o km
Orbital period 2 hr 48 min 22 hr 30 min
of 610 611*

rotation 40 etec 19-0 gee

L 2 886--66 F33-2/4~r( F~
_1,.~L TT
!ACCESSION NR:"AT5023607 UR/0000/65/000/000/0381/038V
AUTHOR: Vern S. N.; Hqj~nkj!-,ov, V. V e a
zl~
T.
TITLE: Recording of charged particles of energies of 0.1-10 kev v1th a spherl'ca
electrostatic analyzer
SOURCE: Yj~ ~qq:~naya konferentsiva vo fizike kosmicheakogo_pyq~f~qanstva. !fq~tco
1965. Issledovaniya kosmicheskogo pro~t~ai~stva (Space research); tr onfereatsil.
Moscow, Izd-vo Nauka, 1965, 381-387
TOPIC TAGS: satellite, satellite data storage, particle counter, electron density,
ion,'density/Elektron 2 satellite
ABSTRACT: Identical s herical electrostatic ed to record posiXtve
and nggati Cith one - -- - --- _qqqlyzers'were us \~o- Cosmos-Wrnd
particles ,, rgies of up to I kev on Cosmos-12 and
up to 10 kev on Elektron-2.y', Each analy7er was comprised of A spherical capacitor
some 60 mm In diameter, with input apertures leading to plates spaced 12-mm apart,
on which a periodic high voltage was programmed so as to allow passage through the
annular gap of only particles of a desired energy range. A Faraday cylinder at the';
-Cafd

L 2886-66
CCES-SION NR': AT5023607
~Sap output served as the collector. The input apertures and the Faraday cylinder
were furnished with biased grids to eliminate thermal particles and secou
Aary emis-
sion, respectively. A diagram of the two analyzers used
on Elektrort-2 is shown in
IFig. 1 of the Enclosure; accumulated charge was converted to binary code. The Cos-~~
mos data generally showed that electron flux at the 1-kev level did not exceed
107.1cm2/sec/kev at night and was only slightly higher by day. A maximum was noted
during the Bouthernmost portions of orbit, in a region south of New Zealand, attaining
up to 12 X 108/CM2/sec/kev. Electron fluxes recorded on Elektron-2 showed strong
~variations at sunrise and sunset (referred to the satellite); these variations
ireached values on the order of 109/cm2laec/kev. Irregular-variationd in flux readings
correlated with known geomagnatic e~rents observed during the flight. Data show that
I t II
the satellite was at all times within ihe magnetosphere. 4ositive ion flux regis
tered by Elektron-2 in the 0.1-10-kev range did not exce ed 5 X 107/CM2/sec. Orig. i
I
art. has: 5 figure6--and I table..- ISH]
]ASSOCIATION:- none
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~ACCESSION 9R: -ii5'0230'7 ENCLOSUPS:
f Collectnr f S Ch
Scaler--
wi t Ch,
Power
Tr- 44?,
SUPPI
Al:
Rearo uce command I
Com
Cort- Pwiteb 1
mand I'
unit mand
Tr
'A
Com--
rre
Colle t
switch~
Fig. 1, Spherical particle analyzer an Eleltfr'on-
Tr - High voltage transformers; Com'- commutators;':,
Al - 0.1-1 kev range; A2 - 1-40 kev range.

3281-66 FSS-21VX(I T'~IGSIC;W
ACCESSION NR: AT5023614 UR/0000/65/0001000/0425/0433
AUTHOR: Vgrnoy, S. N. t Chudakov. A. Ye. VAwjg_vj!_,__Y. ; ~uzqets2K._L._j&
gachev StolRovskiy. V. G.
o
L
ITITLE: Irregular flows of high energy electrons close to the boundar of i'h6
y
earth's.radiation belts
SOURCE: Vsesoyuznaya konferentsiva Po fizike kasmicheskoov) prostranstva. Hose^
'1965. Issledovaniya kosmicheskogo prostranstva (Space rese~~rch); Trudy konferentsii.
Moscow, Izd-vo Nauka, 1965, 425-433
TOPIC TAGS: geomagnetic field, satellite data analysis, radiation belt".;-
ABSTRACT: The authors analyze data obtained from "Elektron-l" and "Elektron-2" dur,
ing their first month of operation. The equipment used on the satellites is briefly.
described. Analysis of data pertaining to the midnight meridian indicates that thel
lintensity of th0l electrons at the boundary of the outer'belt decniases by two or
three orders of magnitude within a narrow range of radial distances. It is estab-
lished that the radiation belt on the night side of the earth terininates on quiet
days at L On th a day side, the boundary of the belt extends on the

L 3281-M
'JACCESSION NR: ATS023614
average to L 9-10. (Here L is the nominal McIlwain parameter calculated in the
dipole approximation and expressed in earth radii.) It is found that irregular
flows of electrons outside the boundary of the earth's radiation belts appear with
an increase in perturbation of tile geomagnetic field both at the surface of the
earth and at distances of %,30,000 km from the earth. A theoretical explanation is
given for this phenomenon. The experimental data support the hypothesis of a closed
system of lines of force in the earth's magnetic field up to latitudes of 750.
Orig. art - has: 9 figures, and-l table. [14)
ASSOCIATION: none

L 30L6-66
ION NR t AT5023615 UR/0000/65AXO/000/0433/0434
AUTHORSs
-'Y' I.: Alc6l4yevp A. 0. RuWinshteyn
Logachev, U. L.';' Sosnovo~4,
Ternovskay-a~, H. V.
T1TLRz Pulsations of the earth'a magnetic field, from the measuromonts taken by
the Elektron-3 natellito
SOURCEz 4'Vse-oyuznaya konferentsi-va po fizike kosmiq4op~go o.-pr- tran t .- Noaccvj
P 65 . I s"s-l-e d lov aT -dy ae s-k-
gD prostranstva (Space research); trudy
konferentsii. Moscow, Izd-vo Nauka, 1965, 433-434
TOPIG TAGSt satelliteo satellite data analysis, pulse counter, pu~lso amplifier,
pulse amplitude, earl-h maoAtic fteld ~
17'- 1 -, 1"r -~ , S~'
ABSTRACT: The Llektron,-3 satellite, launched on July 11, 1964, carried a coil with a
ferrite core. Signals from this coil were transmitted to two amplIfying circuits
one for the band of 1-10 cps, the other Cor 30-30C cps. Both circuit8 recorded
pulses with amplitudes exceeding ~- 1) 25- Y v The type and operation of
the meaory bank are briefly described. from a small amount of data processed it
can be seen that no pulsvis with the amplitudes k 25'Y were recorded, that at
Card 1/2

L-3096-66
iAGUM1011 NR: AT5023615
the maximum sensitivity Q 1'Y) the count exceeded seven pulses ptw 2 miautesp
and that at t-he intermediate sensitivity (-> 5-*y) about 2-3 pulseo were record6d
by the low-frGquency circuit and about I by the high -frequency circuit. It is
noted that the number of magnetic. field pulses with the amplitude t 5 ~ is
generally greater in the frequency region of -1-10 cpsr than' in the region 6f 30-300
cps and that the pulse intensity tends to increase in sone geographical regions.
Normally, this increase is recorded by the low-frequency circuit but not by the
high-frequency one. [o4)
ASSWIATION i nOne A: lkllsi,"
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L -2~22-66 E~IT(d)IFSS-21EWT(I)IFS(v)-310EC(k)-21FCCIFVIA(h), TTIASTIGSIGW
ACCESSION YRs AT5023616 WCOOO/65/000/000/0434/040"
AUTHORSi Ve:mMqo2Yj--3*,,,L.; Hesterovt V. Ye-.; Pisareakot ff. F.; Savenko, I. A-i
.Tverskaya,"r. V., Shavrin, P. 1.
.TITLEi Investigation of the upper Van Allen radiation belt at low altitudes ditring
:.~the flights of the satellite ships and artificial earth satellites "Ka9mos" fron
j1960 to 1963
:SOURCE.: Vresoyuznaya konferentsiya po fizike koFimicheakogo prostranstva. Moscow,
is a 0 comicheskogo prostranstva (SDace research); trudy konferentaiie
'Moscow, Izd-vo Nauka, 1965, 434-4-8
TOPIC TAGSt sputnik, artificial earth satellite, Van Allen belt, radiometryp
,geomagnetio field
ABSTR&CTt The results of radiometrio measuremente of the Van Allen radiation bel
;from several "sputnik" and "Kosmos" satellites are discussed. - tl~-e-radioaet-ers----
iconsisted of inner and outer scintillation counters and gas disc."aarge counters.
,The internal scintillation counters recorded electron energies b,3tween 50 to 300 k-M(
I i
:Among the various recorded measuremental"'w"as the variation of radiation intensity
-iij-p-arent in the outer belt and which could
,with longitudat which was qiiff-e be
:explained clearly by the struobire of the actual geomagnetio field, Several
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L 2322-66
'ACCESSION NR: AT5023616
altitudo-versua-longi-tudp--~ip4;~ttcle-drift-trajectoxy---cur-v,.sit-wero-:obtained-to -explain-j:-~
Ithi W&imw geomagnotio anomalies observed. Next, data were obtained to determine
!the location of maxima in the outer Van Allen belt. Over a period of four yeare
I
';this varied within the limits 4 L < 6, and this variation cauld be assooiated withl
~geomagnetio dist-arbances. As a tbir7d observation, an electron eneray gap was dia-
loovered between the outer and inner radiation belts on 2 L -i 3. The special
Trofile of the outer Van Allen belt is shown to be characterized bjr the location of
a maximum, a maximum radiation Intensity I , and a half-width corresponding to
max
0-5 IM 0 Intensity measurements emd geomagnatio line-of-foroo arose seotion
estimates gave the following values for the eleotron lifetimes lit the outer belts
5
:for electron energies > 100 keir# r 5 x 10 sea, Car energies > 600 isvp T m 5 x
'U
10 sea. Orig. art, haet 13 filWas and I formula. [04)
ASSOCIATIONt ane
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j, 2321-6 6. EWT(d)/E',vT(1)/EEC(k)-?/FCC/~-",iA(b) as/GW
iAGCMION NRs AT5023618 UR/0300/05/000/000/0454/0460
iAUTHORSt j_~Enova S. No; gE!!~jn L. L,; q4~!EaWqhtMnj_A. N~; Charakhch' nt_,,,
--f T, N.
FT1TLEj Outer Van Allen belt 4ind bursts of x-rayj in the stratosphere
SOURGEA V8eq0YUznaya konferejARiya pp f;K:~~q_kRqr kpZq_prcjt;!anstva. Koscow,
LA95.- IssAe_d-ov_ani_ya kearaichaskoeo prostranstva (Space research); trudy
koaferentsii. Hoscov, I2d-vo VaWca, 1965, 454-46o
W
TOPIC TAM radiatio belt- z ray, stratosphere, magnetic storm, solar activityl
Van Allen belt In-
ABSTRACTs Observations of burstri of x-rays in the stratoaphere., which are
apparently the result of brmsstrahlung or high-energy electronit trapped in the
magnetic field of the earth, are discussed. The -work a=l results from a number of
American and Soviet groups are described. The results of obserimtions made during
1964 above Hurmansic and Miniyy are presented,, giving the integrated photon energy
spectra ani the dependence of couat rate on press-we for the fotr events described.
By comparison with the previou3 results, it was found tb&t inartased radiation In
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L 2321-66
ACCESSION NRt AT5023618
the stratosphere is correlated with recurrent magnetic atorms,, itith large
ionospheric disturbances, and, in the aurora zone, with the absorption of radio
waves in the F2 layer of the ionosphere. Toward the minima of solar activity
the frequency of x-ray bursts remained unchanged, and the photort energy spectrum
became more stable. Satellite made at the same tiate showed no
increase in galactic cosmic ray intensity.1013irace the number of high-energy
electrons in the outer Van Allen belt is insufficient to explain the intensity of
x-rays in the stratospherej it is concluded that the x-ra" must, be caused, in
part, by an additional flux of electrons produced by transient electron-accoler-
ating processes occurring ir. the magnotosphere of the earth@ Orig, arts hast 3
figures and 3 tables* (041
ASSOCIATION% nahe
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L 2io2&66 TT/aS/GW-
=ESSION NFL: AT5023619 UR/0000/65,10OP/000/0460/046hi
Vernov, So No; SavenL-o, I. A.; Talltsoyj M. V.;
iAUTHORSt
;TITLEs Some results or measurements in the outer Van Allen belt by the satellite
Kosmos-41
Vf
URCE: Vaesoyaznava konforontaiya po fiziko kosulcheskogo prostranstvao Moucowl
s
o
1965. Isolodovaniya kosmichoskogo pro3transtva (Space resoarch)j trudy konforontaiL
Moscow$- lad-vo Nauka, 1965j 460-464
TOPIC TAGS: raoiation belt, Van Allen belt, proton bombardment, electron
bombardment
ABSMGTx Some results of measurements of proton and electron intensities in the
outer Van Allen belt axe presented. The measuremont3 were made during September
arA October 1964 on tile satellite "Kosmos-41," which was I-aunched Augu.,it 22, 1964.
The form, shielding, geometric factor, and enera range ol the nino detectors
Used are given. Tile results are preseated as a series of graphB givln~,? tile
measured particle intensities, magnetic field intorlaity, and. altitude above the
earth's surface as a function of the parameter L. Tile inLensity of protons with
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L 210"
AGG&WI011 NR: AT5023619
energies 0. 4-3 Mev reached 2-105/cM2 see ster for 1,0'3.5, whareas the intensity
of protons with energies 3-8 Mai, during the same talme was always below the
detector threshold of 3/cm;2 see star. The maximum electron intensities were
measured at L-5. Orig. art, buit 4 figures i and tables, 041
ASSOCIATIONs nona
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L 1.552-66 FSS-2/EWT(I)/FS(v)-3/FCC/EYA(d)/F-4A(h) TT/Gs/(Jw
ACCESSION NR: AT5023628 UR/0000/65/000/000/0502/0506
AUTHOR* Vernov. S. I.; Vilkulov, P. V Zatsevin,, V -1,; Loxachev._Xu. I.;
Okholovkov, "; 'CMudakox. -A. Ye
14&1, 5-4- '1 q,5
TITLE: Primary cosmic radiation investigations
SOURCE: a konferentsiya po fizike koamigheskolzo p_Mqt cav,l
Vsesoyuznay rAMst,~a. Nos
1965. Issledovaniya kosmicheskogo prostranstva (Space research); trudy konferentaft.
Moscow, Izd-vo Nauka, 1965, 502-506
TOPIC TAGS: cosmic ray, cosmic radiation, primary cosmic rgy, primary cosmic
radiation, Elektron 2, k1ektron 4 'i't, 57-5~-
ABSTRACT: Experimental data obtained by Elektron-2 and -4 on primary coamic ra,diaL
tion are presented and interpreted. The data, coverIng the period 30 January to
I November 1964,. were obtained primarily by means of gas-diacharge counters with
an average frequency of 20 pulaes/sec. The apogee of the satellite,% was 68,000 km"--
keeping them outside the earth's radiation belts most of the time. The higher t
count frequency as the thickness of the screens was increase 'd, made it possible to~
conclude that the primary radiation did not contain particles within the 50 to
110 Hav range. Two types of radiation intensity variations were distinguished: i
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L 1552-66
ACCESSION NR: AT5023628
those connected with the 11-year period of solar activity, and fast variations,
with a period of the order of two weeks. The 11-year period variations grew in
intensity at the rate of about 2 percent per month during the first half of 1964.
During the second half of the year the intensity reached a ceiling and in October
indicated a tendency to decline. These data are in fair agreement with those of
the Fort Churchill and Deep River observation posts. Certain indications of a
phase shift between the periods of solar activity mid the intensity of cosmic rayal
were discerned in the sequence of monthly averages f)f the intensity of cosmic
radiation, the relative number of solar spots, and zhe solar flux of 10.7-cm radio
waves. These observations, however, are not considered conclusive. The short-
period variations of radiation with a 1.5-percent anplitude periodically acquire
a clearly cyclic character. The same observation wits made in April 1963 by the
Luna-4 interplanetary station. In general, however, the cyclicity is not very
regular and the nature of these.variations remains cbscure. There are also
indications of a 27-day period in the data for 1964. An attempt was made. to
correlate these periods with the sun's rotation. A regular coincidence was not
observed, but In some cases (rotations 11920 1793, amd 1794) there was a fair
indication of parallelism. The 6sence of a conclusive cxmnection with the* sun's
rotation suggests the possibility that the short-perLod vartatic.as havii a comwo
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L 1552-66
ACCESSION NR.- AT5023628
origin with the 11-year variationa. It is also possible that the intensification
of cosmic radiation during decline of solar activiq, Is not monotonic, but displays
ups and downs stemming from changes in the condition of its propagation ar.;dimenaions
of the region of its effective scattering within the solar system. Grig. art.
has: 4 figures. (FPI
ASSOCIATION,. none
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I

kELDYSH, M.V., akademik; SIFI)TLV, V.I.; VEjullov, S.N.
Explorero of the Universe* Krylorodo 15 no. 4t6-7 Ap 164.
(MIRA 17:5)
1. Presidnet Akademii nauk SSSR. (for,Keldych). 2. Chleny-kor-
respondenty AN SSSR (for Stforov,, Vernov).

_I-AZC-RWt- AR5020397 UR/0313/65/000/WJ/005510035
SOME Ref - zh. Issledovaniyo ko=icheskoeo prostranntys, Abs. 0. 6 2.238
ALMIOR: Vernov. 8.N.; Chudakov. A-Ye4 Gorchakov Yc-V.; Logache -ff1~44 Nesterov
Y.Xe-; SiTv-qnko,._j.,_A.; Shar
TITIF.: Ra-UaAlm-b-olte of the earth
\I I
CITM SOURM Geofiz. byul. Mezhduved. geofiz. k(xs-t pri Prezidlume AN SSSR,
no. 14, 1964, 96-109
TOPIC.TAGS: satellite, roCket, radiation effect, cosmic radiaticu
TRMIATION: A short outline Is given of the results obtained from stulics conduct
using Soviet artificial satellites and cosmic rockets of the radiation belts and of
primary cosmic radiation beyond the limits of the magnetic sp1iere.
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L 24�L4-66 (h) -M/W
ACCESSION MR: AP5020993 LtR/0203/65/005/0014/rj6;;5/o648
523.165
~AUTHOR: Vernov, S. ff.; Savenko, 1. A.; Tel'tsov,
Shavrin,__P. I."
;TITLE: Measurement of 0.4-8 Mev protons by "Kosmos-41"
~SOURCE: Geomagnetizm i aeronomiya, v. 5, no. 4, 1965, 645-648
'TOPIC TAGS: p~joton intensity,- satelliteftPP.Q1~J~l-'L
,:ABSTRACT: Two semicorductor proton detectors, each capable of coverin3. ~,l sterad
and sensitive to 400 kev-7 Meir and 3-8 Mev protans, respectively, were nounted on
."Kosmos-lsl'~'.' Readings were taken for L = 3.5-10 (C. E. McllwRin's paremeter). Re-
sults showed that maximum intensity for 0.4-3.0 Mev protons was 2-105 prot/cm2 se,
:sterad at L = 3.5 'and B = 7.6-10-2 gauss. A comparison of data collected near the
~plane of the geomagnetic equator with those taken at higher latitudes, at L re-
;vealed that the dependence of Lntensity on height can be eirpresEed aa (B/B,quat )-k9
!where k Id 1. The drop in proton intensity varied with L in the form L-n, where
,n = 30; however, this depended on gecmagnetic conditicns and on variations in the

L 2464-66
ACCESSION-M,_-AP5020993
I Outer-- ra-diation-belt ----Intense rotoIn---itreanm vere observed-a-t-urge-valmer. of-L___~
Orig. art. has: 3 figures and 1 table. jWC]
;ASSOCIATION: Moskovskly 90Sud-hrStV0nWf universitet (Moscow State University);
InstLtut yadernoy fiziki (Institute of Huqlea~j~h_q~
-Y C21i
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*.,- '6'137-67 E''Tr(i)11.,CC Ou
ACC N-%. A117001643 SOURCE CODZ: Ua/0203/661006/004/0658/0660
Varnov, S. N.; Savcn!~o, 1. A.; Telltsov, It. V.; Shavrin, 11. 1.
0:2 : ins, t itu. ta-of 'Nuclear Physics, ~bscow State University (Moskovskly
j;osudar-,tv(nuiyy universitet, Institut yadernoy fIzIkI)
TI'MS: Intensity of protons and electrons In Cho outer radiation belt in the
period 1961-1964
SGUIRCE: Goomagnotlzm I acronomiya, v, 6, no. 4, 1966, 658-66b
,OPIC ZIGS: radiation belt, proton, electron, solar activity
ABST1XT: 7ho authors present the results of equatorial measurements made In 1964
of the intensity of protons with energies >/ 400 koV and electtons with energles
?2 ',.:eV -,it the center of the outer radiation belt. , These results are compared with
similar data obtained in 1961. The conclusion Is drawn that there is a tendency to
a decrease of the mean absolute Intensity of the hard electrons of the outer radiation
belt in 1964 in comparison with 1961-1962. IA' the noted variations In the absolute
intensities of hard electrons and low-energy protons are considered within the frame-
work of the theory of the formition of the radiation belts it con be postulated that
the moan dennity of protons with energies of tons of 1ceV beyond the limit of stable
trapping varies little with a change of solar ac 'tivity.i/At tho sane times the
density of electrons with energies of hundreds of kaV, forming during the drift of
hard electrons at the center of the outer radiation belto risou Mradically .'only
Card 1/2 UDC: 5ES-72-

L 08737-67
ACC NR: A117001643
!n periods of rather strong goomagnetic disturbances, leading to the formation of
diffusion. waves. The Intensity of the hard electrons in the outer radiation belt
therefore is subject to long-period variations associated with the cycles of solar
activity. Tho authors thank B. A. Tverskoy for discussions of the work, and Ne-N.-_~_
Rachotkina for taking part In the processing the experimental materials. OrIg. art.
r PRS: 38v230-7
has. 2 tables LJ
SUB CODE: 03,20 / SUBM DATE: 04Feb66 ORIG REF: 007 OTH RE:Ft 007
C.,d 2/2 bc

L 42150-66 FSS-2/ENT(1)/FC;C TT/Gvj
ACC NR, AP6028350 SOURCE CODE: UR/0203/66/006/004/0661
IAUTHORI. Vernov, S. N.; Savenko, 1. A.; Telltsov M. V.; Shavrin, P. 1.
..................
ORG: Moscow State Universityk Institute of Nuclear Physics (Moskovskiy gor-adaretvemyy
universitet. Institut yadernoy fiziki)
TITLE: Observations of a diffuse wave of relativistic electrons in the outer
radiation belt
N71
SOURCE: Geomagnetizm i aeranomiya, v. 6, no. 4, 1966, 661-663
TOPIC TAGS: relativistic electron, radiation belt, - geomagnetic storm,
electron flux, r"' -SUM4MM, geomagnetic latitude
ABSTRACT: The generation of relativistic electrons in the outer radiation belt can be
attributed to the transfer of charged particles across the drift shells. The prpaga-
tion of diffuse waves of r!~Yativistic electrons, first recorded by Elpl2rer X1rV! was,
also recorded by Kosmos 41~'when it passed the outer radiation belt. At the high geo-
magnetic latitudes, the propagation of the diffuse wave may be distorted by changes in
the.pitch-angle distribution. However, in the present case, the diffuse wave exhibited
characteristics peculiar to the dynamics of a diffusion wave of hard electrons. The
intensity of relativistic electrons decreased somewhat at the beginning of geomagnetic
perturbation. It increased at distant L shells (> 5) of the magnetosphere several
days after geomagnetic perturbation. Further shift of the intensity maximum toward
Card 1/2 UDC: 523.72

L 42150- 66
[_AC_CNRz AP6028350
the region of smaller L occurred In the absence of geomagnetic disturbances. This W&81
followed by a decrease in intensity and a shjjt in the Intensity maxim= to its
initial Position. During the magnetic stormlon 1 September,1964, recorded by
Koamos 41,the intensity of electron flux with energies grea.ter than 2 Mev at L 5
was 3.5 x ld2/cm2sec. A peak of hard electrons with an intensity of 103/cm2sec was
recorded on September 3-4 at L - 6-7. This eak wag shifted to smaller L shells
until it reached a maximum intensity of 104/cm 3sec. Variations in the protonosphere
were of smaller amplitude. The diffuse wave of relativistic electrons was thus first
observe d in the outer radiation belt at high geomagnetic latitudes. This wave was not
accompanied by low-energy protons. Orig. art. has: 2 figures. (EG)
SUB CODE: 04/ SUBH DATE: l8Feb66/ ORIG REF: 006/ OTH REP: 003/ ATD PRESS:

VERNOVv-5.N.; KHRISTIANSEN, G.B., ABROSIMV, A.T.; BELYAYETA, I.F.;
DMITRIYEV, V.A.; KnIKOV, G.V... NECHIN, Yu.A.; SOLOVIYEIA, V.I.;
KHRENOV, B.A.
Recent data on the stlidy of extensive air shawers by mean3 of
an elaborate setup. Izv. All SSSR. Ser. fiz. 28 no.1"Li1886-
1893 N '64. (WaA 17., 12 1)
1. Nauelmo...ttii3ledovat(ill,-iki-y institut yadernoy fizJ.k-l Moskovskogo
gosudaretvennogo universitata.

A 1!12 ~ f: 3 j I
k dw, ,
29

S(Zr,~I- dava
SE
L;a"c

!CFUDAKOV, A. Ye.; VAKILOV, P*V.,- GORCHAKOV, Ye.V.;
vu B
IrTATOM, P.P.; Mal-31507, S.I.,-LOGACHIN, fa.l.; LY B 'DVpG.P.;
IIIXGI~YEV, A.G.; Ui,HW740V, V&P.j SUSBOVETS, EX.; TYAR;OVSKAYAg M.V.
Radiation studies by means of the artificial satelite "Kosmos-17".
Izv, AN SSSR Ser* fiz. 28 nool2t2058-207,4 D 164 (IMIRA 18 t2)

n.'U-:OV S.V.- 17lJUSTLV:S7'T, G.2.; ABROSE~'OV, A.T.; ATUSHTE71CH, V.B.;
~!~~YEVA, O.V.; LUIT71YEW, V.A.; KUTLIK07.0 G *
1'.135CHIll, YuA..; SOLOVIYEVA, V.I.; SOLOV' 7, K.I., R. A
YE - FG,' ', Yu. .;
KEROJOV, B.A.
Description of a moderrized conplp-x setup for studying exten-
Bive air showers. Izv. Mi SSSR Ser. fiz. 28 no.12:2067-2002'
D 164 (t-JU 18:2)

L 4528-66 EWT~M)/FCC/T
AICC N2, AP5024632
IJP(c)
SOUR(M OODE: Ult/0048/65/029/009/1616/1681
AUTHOR: r
Kh istiansen, G.B.; Abrosimov Atrashkevich
Belyayeva. I.F.; Vedenoye~. O.V.; Kulikov, G.V.; Fomin, Yu. A..; Nechin, Yu. A.;
Sotov'yeva,. V.I.; Khrenov. B.-A.
ORG: none
TITLE: -- Investigations of - f uc ua
with a fixed total number of charged particles and a fixed total number of muons /Re-
port, AAj-Ajnjqr;_CoAference on Cosmic Ray physics held at Apatity 24-31 August 1964/
SOUWE: AN SSSR. Izvestlya. Seriya fizicheskaya, v. 29, no. 9, 1965, 1676-1681
TOPIC TAGS: cosmic ray shower, muon, charged particle, extensive air shower, particle
distributic particle distribution
ABSTRACT: The authors have employed the modernized installation at Moscow State Uni-
versity, described elsewhere (S.N.Vernov et al., 1--i. A3 SSSH Ser. fix., 28, 2087,
1964), to investigate the simultaneous distribution of total number N of charged par-
ticles, total number M of muons, and age parameter S in extensive air showers. Show-
.-ers were selected-for which the zenith angle of the axis was less than 300. M was de-
termined rrom the number of muons recorded by the muon detector and the perpendicular
distance of the muon detector from the shower axis with the aid of tho known lateral
distribution of muons. The relative error in determining M did not exceed 35 %. The
Card 1/2

L 4528-66
ACC NRs AP5024632
error in deten-iining S was estimated to be 0.02 by processing "artificial" showers of
known age, calculated by Monte Carlo methods, The data presented were derived from
some 3GO showern with total numbers of charged particles ranging fravi 105 to 4 x 106.
Histograms are given showing the distribution of showers with respect to N with fixed
H, with respect to R with fixed N, with respect to S with fixed N, and with respect to
3 with fixed H, and scatter plots tre given for N vorsta 9 wiT.,h fixel 14 and for 14 ver-
sus 3 with fixed N. The cormlation coefficient of 8 with H for fixed X ranged be-
tween 0.62 and 0.72; the correlation coefficient of 8 with H for fixed M was 0.67.
Orig. art. has: 10 formulas, 4 figures, and 1 table.
BUD CODE: NP/ SUBM DATE: 00/ ORIG REF: 005/ OTH REP: 001

L 4.529-66 . FWT(m)/FCG/T. IJP(,,)
ACC NRs AP-5024633
SOUXE CODE: Uft/0048/65/029/003/1682/1685
AUTWOR: Vernov, S.N.; Khrenov, B.A.; Khristiansen, G.B.
ORG: Scientific Research Institute of Nucleir Physics, Moscow State Universit
im. M.V.Lomonosov (Nauchno-issiedovatel'skiy institut yadernoy fiziki Hoskovskogo
gosudarstvennogo universiteta)
0
TITLE: Structure of the central region of a 1--FA17-mor at 40 m.w.e. /Report,
Union Conference an Cosmic Ray Physics hold at Apattty 24-31 August tgG4/
SOURCE: AN SSSR. Izvestiya. Seriya fizicheskaya, v. 29, no. 9, 1965, 1662-IM
TOPIC TAGS: cosmic ray shower, extensive air shower, muen
AWWACT: The authors have employed the complex modernized Installation at Koscow
State University, described elsewhere (S.N.Vernow et al., Izv. AX SSSR. Ser. fiz., 23,
2097. 1964), to investigate the stn=ture of the central regions of muon qhowers ac-
companying extensive air showers. The muon flux at 40 m.w.c. under-ground was found
to be proportional to rn, where r is the distance frNxa the showar axis and n = 1/2 for
7 m =-- r %::=15 m and r = I for 15 m .::Z r -c.--_100 M; Lt was not possible to obtain the
lateral distribution for r ---- 7 m because of the errvirs in determining r. The ratio 01
the numbers of counters triggered in the two halves if the muon detector and the pro-
bability for triggering neighboring counters were sul)jected to statistical analysis,

L 4529-66 - -----
ACC NRe AP5024633
And after correction was made for Paisson fluctuations there remained evidence that
there exist in the center of the muon shower groups of associated Mucas with diameters
from 2 to 3 m which are capable either of contracting into narrow groups with dtamct-
era less than 30 cm or of producing secondary showeri. Orig. art. has: I formula, 3
figures, and I table.
SU13 CODE: NPI SUBM DATE: 00/- ORIG REF: 005/ OM REF: OW
(9 D
---. '2/2

ACC NR, AP5024635
SOURCE CoDi,' I 04s/65/029/009/1690/1642
AUMOR: Ve mov, S. H. TIA.; Yertmov, N.H.; Krastllnikov, D.D.; Kuz'aln, A.I.
Makslmai-,-. 'Sv.-.- 1("tetova, N.M.; Nikol'skly, S. 1. ; Sleptsov, Ve. I., Shater, Yu. 0.
ona: none
TI TIZ Plan for a large installation at Yaktitsk for study of "tggqg1Vg aLr--!ik
/Reporl, All-UnIon-Conference on Q)-,anic hysics held at Apatity 24-31 August 1964/1
SOURCE; AN SSSR. Izvestlya. Serlya fizicheskaya, v. 29, no. 9, 196.15, 1690-1692
r .'11,
TOPIC TAGS: prima cosmic ray" secondary cos-mic ray, extenFive at- shamer, spectral
energy distribution, cosmic radiation corpositlon, cosmic radiation anisotrap
I I
ABSTRACT: After a discussion of the signifIcance of extensive air i;howers for the in-1
vestigation of ultrahigh energy primary cosmic rays, the authors briefly describe an
installation to be completed in the next two or three years near sea level at lati t"de
620 N in the Yakutsk region; it is anticipated that the installation will yield Infr)r-i
mation concerning the energy spectrivi, composition, and anisotropy of pritlary cosmic
rays with energies up to IG20 eV. The inscallation, inten(teJ for investigation of
tengive air showers, will comprise 65 stations spread over an area of 23 1=2. Fach
station will be equipped with scintillation counters with a total sensitive area of
m2 or 4 m2, and at the central station - 10 n2. The total sensitive area of scintil-
Card 1 /2

ACC NRS; AP5024635
lation counters in the whole lastallation will be 204 mZ. Each station will be equip-
ped with photomultipliers (total cathode area 190 cm2 at each station) for rec5rding
the Cerenkov ftash accompanying a iihower. In addition, thcre wilt be muon detectors
witit a total sensitive area of 22 m2. Pulses will be transmItted from the more remote
stations to the central laboratory by radio. It is anticipated that thi's installation
will record 2 x 10 showers per year with energies exceeding 1015 OF and 2 showers per
year with energies exceeding 1020 eV. Orig. art. has: I tlguve and I table.
5U13 OODE: NPI SUBM DATE: 00/-- ORIG REP: 002/ OM REF: 008

L 4127-66 FSS-2/sE'tri (!)/FS(v)-3 'IT 10111
ACCESSION NR: AP5026220 Utt/()048/65/029/010/1794/1199
AU111OR: Vernov, S.N. Me-l-Inikov, V.V. ; Savenko, 1. A. I Savin, _P01.
TITLE- Investigation of low--onorgy charged pftrticlea with the Cosmos 12, Cc %Q
11 lp, and Electron 2 intellitea 41eport, All-Union Conference an Cagmir Ray P iys lea
hold at Apatityj24-31 August 196.9
SOURCE.- Alf 69.19R. Izvoqtiya. Soriya fizicheqkaya, v. 29, no. 10, 1965, 1794-1799
TOPIC TAGSt artificial earth satellite, spectrorKyter, chnrged pm-tiole, alectron
flux, ton flux, low onargy particle
ANSTRX"tt SfAierical eloctroqtatic charged particlo nnalyzera exrricd by the Coa-
mas 12, Cosmos 15, nnd Electron 2 satellites mro describcxf %,-ory L)rlefly atid pre-
liminary results obtained with them are piN-cented. The radii of the two concen-
tric algiorioal deflecting olectrodes wore 5.4 and (3.6 ca, and tho cliftrged particles
traversing, the nnaly7.or were collected In a Fnraday cup. no mi-11mirm [Flobal in-
tensity that could he rpeorded wa,; kpproximntoly 6 x 106 1' -1 part1elc-;;/cm2 one
K-1 this intensity is two oMers of magnitude below the threshold intensity for
the instrument carried by 9xplorer 12. The luminosity at maximica transmission was
Card 1/_?

L 4127-66
AOCESSION MR: APS026220
0. 7 cm2 sterad with 4 E/EO and the geometric factor was 0.1 EO cm2 aterad
kev. The analyzer on the Cosmos 12 was sequentially programmed to record 0.5 kev
electrons or I kf-v electrons or io--q, and that on the Cosmog 15 recorded I kc*v
electrons or ions and was provided with a ponitively charged screen to reject
thermal ions. The Electron 2 carriod two analyzers, which were prograrmed to
recomi charged particles (if seven different energries ranging from 0.1 to 10
The fluxes of I r- rharg-d partic1eq ribser-.,ed with the two Cosmos ,;atellites -_ r1a
ordinarily near or 1w.)(Yw the threshold. Fluxes exceeding 107 partlclf-s/c.2 see
k,-v ob~iRrved on the daylight side are ascribed to photoolectroru; from the srrpe..,
althotif-ti there are trylleRtIntin of thv prc-once of pArticle fluxiis. I;tpnzfy fluxes
up to 2 x 107 particl-i,;/cm wore aouth of New lealand in the re-
gion of the maximiLen southern igochasm. It ta ruggested that FLn interviity incroase
over the equatorial Pacific obierved on 27 Dc-c may be asaociated with the golar
flare of 24 Dec. The Electron 2 t:~eas tire top n ts revealed a broad region near the
Earth of increased electnon intensity. .~'. -! t.tils reri n ar'~l ~'~:
, 1:' -r-.s I !,-/ f 11 A C 1. " --11'-L - J~. t .! ' ~; ,Rlectron intensities o:! 5 x 108 partlcl-n/
cm2 gee kp,,, at 0.2 v-: and 5 x 107 partlcles/cm2 qnc k-v at 10 were observed
In this region. Intensity Increases were also aometimea obgervf-d near the &Pogee.
Orig. art. ha-gi 5 figures.
Card 2 11

L W'1-66
ACCESSION MR., AP5026220
ASSOCIATIONt none
SUBVITTEDs 00
tIOREF SOVs 004
r
Card 3/3..,--,
ENCLi 00
OHIERO 005
Sun ("WE's MP, Z~
ATV PRESS:
77 WY

--stoy
above 63
TITLE, Measurements of the Intensity of cosmic rays in the stratosphere
Antarctica
SOURCE: AN SSSR. Izvestiya. Seriya fizicheskaya, v. 29, no. 10, 1965, 1805-1806;
y, outer radiation belt, artfficial
TOPIC TAGS; cosmic ray, primary cosT!E
_ra
radioactivity, critical energy, proton
ABSTRACT: Simultaneous measurements of the intensity of cosmic rays in
hemispheres are of great importance for investigating low-energy
cosmic..radiation, temperature effect, Jisturbances in the earth's outer r,;(;iz1Lio1)
belt, and artificial radioactivity in-the stratosphere. Although 0e critical
energy in Murmansk is about 100 Hev and in Mirnyy about 10 Mev, m!asurenents are
2
carried out in atmospheric layers above both places with a pressure of J.0 ,,,/cm
which can be penetrated by protons with energies above 100 Nev. Data obtai,led
simultaneously in Murmansk and Hintyy are obtained at different seasons,.and
they arrive from different directions in the atmosphere. Sounding takeei place in
all stations at a given time. Four times a week cosmic rays are measured with a
Card 1/_2

L 3646-66
ACCESSION NR:: AP5026222
single counter and two times with a special telescope. Results of measurements
are represented graphically. The difference between flurmansir and Mirnyy varies,
depending upon the season of the year. The difference is small when the pressure
is between 20 and 200 g/cm2. The difference increases at other pressures. Orig.
art. has: 2 figures. (EG)
ASSOCIMION: Fizicheskiy institut im. P. N. Lebe,deva Akademii nauk SSSR (Institute
of Physics, Academy of Sciences.SSRO; Hauchno-isaledovatel'skiy institut yadernoy
fiziki Moskovskogo gosudarst~ennoga universiteta im. H. V. Lomonosova (Scieatific
Research Institute of Nuclear Physics, Moscow State UniMpreity); VIII Sovetskaya
antarkticheskaya ekspeditsiya (VIII Soviet Antarctic Expedition)
SUBHITTEDs 00 ENCI.: 00 SUB CODE:
AA,45
No REF SOV: 001 OTHER:' 000 ATD PRESS:

j- S,~N.; YdIRISTIAINS-ENT, G.B.; ABPOSEMOV, A.T.; AIR,1,511?:EVICF, V.B.;
VEFT~V
BMAYEVA, I.F.; KULIKOW, G.V.; SOU-41YE'VA, V.I.; FOMIN, Y-U.A.;
KIMENOV, B.A.
Ultrahigh-ener,gy prlmar7 cosmic radiation according to data on
extensive air showers. Izv. All SSSR.Ser.fiz. 29 no.10:1876-1880
0 165, (MIMA 18:10)
1. Nauchno-iBsledovatellskiy instituL yadernoy fiziki. Moskovskogo
gosudarstvennogo univerBiteta im. M.V.Lomonosova.

-"~d i I
ml

- -i : " -"
~Y. 'A.
I Illy
A. -

t, A.

P F3 d
7X.,
f

SOURCZ CODE:
08
UR/c,
AUUDIOR: Vor jl-_~03,vayova, 1. F.; Voden?y~y, q..Vo; DrIatri3roy, V. A.;
Nechln, Yu-.X-.,- 1G0-R-ian5on_,
OAG: IWI:Atuto of Nucloar Physics, floncow State University Institut yr-dernoy fiziki!
140skovivo-g'o -,g,o-s*,uccl,,a,r-s-t-v-*o-'ii~'o---g,o-,-~ia,
TITIZ. Fluctuations of the energy 5luxes of the nuoloar-activo aid olectron-photon
componants in oxtonsivo air ffhia papor was given at the 14th Annual Conference
on Nuclear SRET-roscay, Tbmsl,-f~-~uaz-y lq&_J
SOURCE: Yadornayn Mika, ve 2, no. 6, 1965, 1075-1086
TOPIC TAGS: extonsivo air shomr, electron, photon
AB~VMCT:' 11-cporimental data are given on the fluctuations of tho*onorgy f1wc-of tho-
nuclear-active and electron-photon components in extensive air showors and on
connections of these fluctuations with oach other and with fluctuations of the ago I
parainoter-s. It is shot-m that the bulk of these data disagrees with the model described
by Nwuzdlc and Sk(jqjqpeKov (Materials on the All-Union Conforenco, Apatites, 1964).. 1
T~j_ _la~g__erole'of the parameter s and other _cT~acto`F4_R1a_s &oFt&;-C-&ir;i~ct _s6iiing-up.
of experiments concerning extensive air-shcrwers aro-AwUsAwd. Orig. art. has: 10
figures and 3 tables. Leased- -on authors' Eng, abstj LJPRPJ
SUB CODE: 03 / SUBM DATEI 23Apr65 / ORIG REFz 014 /' OTH REF: 003
Card

C06~. UR/0020/661:
AUTHOR: Vernov, S.- (Corresponding member AN SSSR); Vakulov, P. V.; Gqrchakov1_Je.
Lo achev.~ Tu. 1.'J-L bimov. G. P
Nikola-yev, A. G.; Pereslegina. N. V.
ORG: i e
TITLE: Measurement of intensity of penetrating radiation on the MoonIs surface%4
[Paper presented at the Seventh COSPAR Meetinz-held in Vienna in Y%ay 19661
SOURCE: AN SSSR. DoklaTy-,v--.lr'Y,-no- 5, 19662-11z?~i-1047
TOPIC TAGS: moonp radiation intensity, lunar probe, radiation measurement/
Luna-9 lunar probe
ABSTRACT: Thelunar prq~e_"LunLa~" launched by the Soviet Union on 30 January 1966
maiie''a soft landing on the Moon on 3 February at 24 hr, 45 min, 30 see
(Moscow time); it was qquipped with an instrument containing a 6 x 10-mm
discharge counter to measure the intensity of radiation. The minimum
shi.elding of the counter mounted inside the probe near its jacket was 'U1 gm/cm2.:
The instrument was switched on immediately after "Luna-9" was put
ln~o orbit and was kept in operation until the probe,~topped functioning. The
data on the intensity detected with the gas counterk averaged over 14 time
intervals are shown in Fig. 1. The fijqst five time intervals are those for the
flight from the Earth to. the

ACt Nk--.-VPby3
0
Moon. The next (sixth) interval
coun~flec
Time of
lan ing
Measurements durIMHeasurements
the flight to the Moon on the Moon
J11 11 Zff iff U SH 10654
is that for the flight near the
Moon (beginning with at a dis-
tance of P-50, 000 kzn from the
Moon), the landing, and the
first 5 minutes on the Moon' s
surface. The subsequent eight
intervals are related to operations
on the Moon' s surface. Table 1
shows the accurate values of the
time intervals and the mean-
count rates recorded in these
intervals. The basic errors in
determining the count rate are
statistical.
Fig. 1. The mean-count rate'of "Luna-~91'
_.discharge count.er
The data in Table 1 show that the mean-count rate recorded on the
Moon' s surface was about 63% of the count rate of the same counter in
free space. In other words, if only primary cosmic rays had been detected,
the counter on the Moon's surface would have counted not quite half as
muckas during the flight in free space. The detected excessive radiation
Card

.I ACC NRI AP6030010- Table 1.
?LI
interval boundaries Averaging interval Mean-count
rate Note
31 Jan 1966 18 h 38 min 40 see 10 h 12 min 0
3 see 3..229*0.010 Duringihc
. flight
I Feb 1966 04 h 51 min 10 see 10 h 54 min 20 see 3.277tO.OlO II
11 15 h 45 min 30 see
23 h 01 min 45 see 07 h 16 min 15 see 3.2670.011 It
2 Feb 1966 16 h 29 min 00 see 17 h 27 min 15 see 3.27810.007 is
3 Feb 1966 15 h 34 min 15 see 23 h 05 min 15 see 3.28610.006 Of
21 h 50 min 00 see 06 h 15 min 45 -sec .3.24510,012 Near the
Moon and
on te YxM
4 Feb 1966 00 h 06 min 54 see 02 h 16 min 54 see 2.0650.016 Ch the Iftn
06 h 35 min 04 see 06 h 28 min 10 sec 2.069W.010 of
17 h 02 min 00' sec 10 h 26 min 56 see 2.074A.008 is
19 h 52 min 30 see 02 h 50 min 30 see 2.07710.014 It
5 Feb 1966 04 h 00 min 40 see 08 h 08 min 10 see 2.05810.009
19 h 01 min 40 see 15 h 01 min 00 see 2.05510.006
20 h 37 min 30 see 01 h 35 min 50 see 2.059iO.O2O

I 22 h 42 min 20 see 02 h 04 min 50 see 2.(159'0.017
The mean-count rate during the flight is 3.27.210.004
The mean-count rate on the Moon is 2.06410.004

ACC NR: AP6030010
is 0.43 count/sec or -26% of half the cosmic-ray intensity. This-excessive
radiation may be due to the radioactivity of the Moon's surface and to the
secondary cosmic radiation produced by the primary cosmic radiation in
the matter on the Moon' s surface region closest to the station (cosmic-ray
albedo).
Until now, no experimental data have been availa*ble on the radioactivity
of the Moon's surface. The "I~una-9" measurements make it possible ~o
evaluate the radioactivity of the Moon' s surface in the landing area near the
Ocean of Storms. Assuming that the total detpcted additional radiation is due,
to the radioactive gamma radiation from the Moon' s surface, the radio-
activity of the Moon' s surface may W nu 20 times greater than that of the
Earth's surface (the count rate of "Luna-9" from the natural radioactivity
on Earth was 0.02 count/sec). However, the radioactivity on the Moon' s
surface has been evidently overestimated, because the effect of raultiplica-
tion of the primary cosmic radiation producing the cosmic-ray albedo
'particle fluxes may explain the major part or even all of the additional
radiation detected. Using the data from an earlier Soviet paper, it can be
.shown that the albedo particle flux is 201/6 of the total cosmic-ray flux or 4076
.of half the cosmic-ray flux. Additional considerations show that at least
.in.the region of the "Luna-9" landing, cosmic rays will be the m*aIn source
Card 4/8

04703-67
[-ACC R_R._AP6_cFS0010-------
.of radiation hazard and that the radioactivity on the surface of the Moon is
,close to the radioactivity on the surface of the Earth.
It was shown during the flight of the second Soviet space probe in
September 1959 that at the distances greater than 1000 km fron'l the Moon, a
surface, the intensity of the radiation trapped by a possible lunar magnetic
field does not exceed 1016 of the cosmic-ray intensity. The "Luna-9" data
make it possible to evaluate the fluxes of the trapped radiation at distances
less than 1000 km from the Moon' s surface.
The mean-count rate just before and during the first minutes after the
-landing was 3.25.� 0.012 count/sec (see Table 1). If this count -,:-ate is
corrected for the geometric shielding of the counter by the Moon during the
approach of the station to the Moon and during the period of radi'Lation de-
tection on the Moon's surface (this correction is about 176), the resulting
count rate is 3.28 count/sec. This prnctically coincides with previous
:measurements. The time required for the "Luna- 9" to cover the last 1000 km
to the Moon' s surface was "v 276 of the time measured in the given interval.
At the measuring accuracy mentioned above, an increase of 50% in the count
rate during this time interval would be noticeable.
Card

INV.:
Thus the upper limit for the possible radiation flux penetrating t,he
"Luna-91' jacket and trapped by the hypothetical magnetic field of the Moon at
the altitudes below 1000 km from the Moon' s surface is not more than half
-the primary cosmic -radiation flux. The variation which would decrease the
intensity of cosmic rays might somewhat change the evaluation of the upper
limit of the hypothetical trapped radiation near the Moon, but the main con-
clusions that the Moon has ro radiation belts and consequently no marked
magnetic field remain unchanged.
Fig. 2 shows the mean-count rates in free space and on the! Moon' s
surface. The intensity in the. transition interval has been corrected for the
geometric shielding by the Moon.
It can be seen from Fig. 2 that the . cosmic-ray intensity undergoes
slow gradual changes (solid curve) similar to those recorded during the Right
.of "Luna-4. "ryTfiis makes it possible to assume that'during the period of
Ahe station's approach to the Moon, no appreciable variation in cosmic-ray
,intensity occurred. Neither the available neutron-monitor data nor the
.stratospheric data of.A. N. Charakhchyan and T. N. Cliarakhcb.yan (unpub-
lished) revealed any considerable decrease in the cosmic-ray intensity.
Card

1. 047C3-67
ACC NR: A P 6 UfffO'
r count/sec
All 71 ILI
.3,23-
Ti~m~o~ i~n'dlng
Time of landing
Meadureaents durin suremento on.-
;0,1 thel M a a
$.to f light to tPe MI th P bloon'
.1 Jr ic 9
11 count/sec
..Fig. 2. The count raies of the.discharge counter during the "Luna-9" flight:
in free space and on the Moon's surface. The mean-count rate on the No-on's
surface has been reduced to the mean-count rate during the flight, and.tbe
.scale has been changed in proplortion to the mea'n-count rates du:ring the
.flight and on the Moon's surface.
The absolute flux of the cosmIc-ray particles detected by ".1,una-3," waa
.equal to 5.35 :F 0.5 cm-2 see-1. The great error in the determination of the
absolute 'nuxes is due to the 10116 uncertainty in the operational dimensions
of the counter. Analogous measurements from "Luna- 7 and "Luna-B"-
stations performe 'd on 4-6 October and 3-6 December 1965 have shown the
2
.particle fluxes to be 5.4 and 5.0 cm see, respectively. The cosmiic-ray
.intensity in February 1966 decreased compared to December 1965. This
Card 7/8

ACC NRt AP60-3-0-0-1-0-
is likely to be associated with the beginning of a new cycle* of sdLar acti~viiy-'-
Thus the cosmic-ray intensity maximum occurs during the period
December 1965-January 1966, and the lag in the cosmic-ray in-tensity
.maximum behind the solar maximum detected for the protons of energies
.higher than 30 Mev is about 1.5 years. This conclusion is also -confirmed
by the data of the,"Zond-3," "Venus 2," and "Venub-311 space probes.
(FSB: v. 2, no. 101
SUB CODE: 22 SUBM DATE: 1]Xay66 / ORIG REF: b03 / CFnI REF: 001
Card 8/8

ACC NR. A117007061 SOURCE COM UR/0048/66/030/010/1685/1689
AUTHORs Vernovq S. N.; Yhristlansen, G. B.; Abrosimovo A. T*; AtrashkovLchp
V. B.; Vedeneyev, o. v.; Kulikov, G. B.; Nechin, Yu. A.;
SolovlyeGirV. I.; Fomin, Yu. A.; Khrenov, B. A.
ORG: none
TITLE: Phenomenological characteristics of_broad atmospheric showers with
a fixed number oftc-mesons and electrons /Paper presented at the All-Union
Conference on Cosmic Radiation Physics, 1,f6icow) 15-20 Nov 196j/
SOURCE., AN SSSR. Izvestlya. Serlya fizichaskaya, v. 30, no. 10, 19669
1685-1689
TOPIC TAGSt mu mesonp cosmic radiation
SUB CODEs 20
ABSTRACT: in an earlier work by Vernov et al Qzvestiya Akadernil Na k SSSR,
Seriya Fizicheskayal 29, 1676, 1965), iesults obtained In a study at an Instal-
lation of MoscdW State University on broad atmospheric showers -with Zenith
angles of 0-300 were reported. These results included the distribution of showerni
with a fixed number of electrons N with respect to the number of high-energy
e
mesons 11,14 and the age parameter S, distribution of showers with a fixed N,*.k with
respect to Ne and S'f and the coefficienti of the correlation twatween S and the
fluxes of electrone,and A-mesons. In the work reported in this Instancep the
same relations were determined for broad atmospheric showers with zenith angles
Mo.
of 30-450, The fluctuations of N'"s S, and No, observed for an effective at
2
spheric depth of 1240 g/cm # were the some as those for vertical showers ests-
blished In the earlier work* To determine thi differencee due to an Inctease..W.:
Sa-rdl 2

ACC NRs AP7007081
the effective atmospheric depth of 200 0=2, calculations must be carried out
with greater statistical precision. When results of the theoretical calculation
.on characteristics of broad atmospheric showers at 1240 g/cm become available,.
'the experimental data reported will be useful for the determination of thecou"O.
IsiXion of primary cosmic radiation In the superhigh-eneray r
5 figureaq 2 formulas a:nd'I table LJFIU ISKJObJ58
OrIS, art, hass 9
Carj,

'ACC.NR, AP7007082
I
SOURCE CODEt UR/0048/66/030/010/1694/1696
AUTHORS Vernovj, S, N.; Khristiansen, G. B.; Neching Yu, A.; Stcoyanovs, D. A*;
ORGt none
TITM Groups of particles at a depth of'AQ meters entering into the
composition of broad atmosphertc showers Lraper presented at tho All-11nion
Conference on Cosmic Radiation Physicsp Moscow# 15-20 Nov 196V
SOURCE; AN SSSR. Izvestlya. Serly4 fizicheskaya, v. 309 no. 10p 1966,
1694-1696
TOPIC TAGS: muon, physics conference
SUB CODEs 20tO4
ABSTRACT& -A study of the flux of particles at a depth of 40 m underground was
made using the Moscow State University installation for the Investigation of
broad atmospheric showers. The purpose of the work described-was determination
..of the shower-Earming capacity of particles belonging to non-Poisson groups
observed in the vicinity of the axis of showers. By assuming that the particles
present in the groups observed were muons and using the experimental data ob-
tained, the authors estimated that the average energy of muons in these shower-
forming groups wag 1012 < E^ < - lo13 ev. The determination of the shower-
forming capacity is of value in estimating the full amount of energy carried
away by a muon group In a broad atmospheric shower. It was shown that the Muons
in a group have an energy of ---, 103 Bev H
< ",, < 104 Bev. This indi-
cates that a muon group cannot carry away more than 10Z of the energy of d
primary.particle, and therefore cannot be responsible for the escape of a signi.
.;prd 1/2__

NRt AP7007082
ficant amount of energy In the atmosphere. Prezience of concentrated groups of
high-energy muons (H 1012 ev) at's depth of 40m cannot be explained
.from the standpoint of theoretical concepts concerning the developme-nt of broad
atmospheric showers that have hitherto been advanced, Origs art. hast 4 figures*
CJPRSS
CWd 212.

L 45257-66 ~E-"T(l)/EEC(k)-2/FCC JKT41T/P
FAcc-r4:--AP6020934 SOURCE CODE: UR/0029/66/0001006/0008/0011
I AUTHOR: Lidov, M. L. , (Doctor of Physical and Mathematical Sciences);
Lebedinskiy,__A._j., (Doctor of Physical and Mathematical Sciences, Professor
Vernov, S. N., (Corresponding Member of the Academy of Sciences SSSR)
ORG- none
TITLE: The battle for the Moo~ continues
SOURCE: Tekhnika-molodezhi, no.6, 1966, B-11
TOPICTAGS: moon, space, lunarsurface, lunarradiation, lunarlanding
/Geiger counter, Luna 9, Dina 10
ABSTRACT: The interviewer reviews briefly the history of lunar research.-
presents a table of chronology and facts and repeats questions and answers.
Dr. M. - L. Lidov stated that one of the problenis solved by Luna 9 and Luna 10
was that of landing at the most favorable time, 1. e. , lunar daybreak. Another
problem was the selection of the most 11 economical" trajectory along Which to send
the heaviest apparatus. He strebsed the importance of human initiative in the
Card -112

L 45257-66
guidance and control of space vehicles and this spoke of a third major problem
involving slowing down the space staiion. The braking process was controlled from
Earth and was etarted 2 1/2 hr before the actual landing. The flight problems
faced by Luna 9 and Luna 10 were siniilar enough but owing to a correction, Luna 10
moved to a flight trajectory along which it approached thc Moon to within a minimum
distance of 1000 km. Dr. A. 1. Lebedinskiy discussed the special features of the
lu.nar landscape as transmitted on television, explained the structure of the space
station and its operation when taking pictures, also the topography of the moon.'
The objectives of Luna 10 were research on luna.r space and lunar radiation.
Acaderiiician S. N. Vernov, a specialist in cosmic rays, stated that the Geiger
counter installed on Cii~a_ 9 recorded protons, electrons, and ma -quanta with
a strength sufficient to penetrate the hermetically sealed space,station. Lunar
radiation was found to be 10 times stronger than that of the Earth; it was found to
be harmless to astronauts clad in space suits. Orig. art. has: 5 figures and
1 table. IGCI I
SUB CODEL 14, 03.4 18, 22/ SUBM DATE: none/
2 / 2
Card

VERNOV, Yu.S.; ROMN, V.R.
Dependence of D on recrystallizatJon time in the va!3i? of the
arbitrary dependence on the probabJlity t1mo for tranriitlon
of microcomponents from one phase to another. Rudlohl.,vni!a
7 no.4:488-492 165. (1111FA 18.8)

L 24390-66
ACC NR: AP6q10988 SOURCE CODE: UR/0056/66/05o/oo/o672/0279
AUTHOR: ernovj Yu. S.,
~ORG: Institute-of Physics im. P. N. I edev. Academy of Sciences
T~b
SSSR ( izicheskiy institut Akademii nauk SSSR)
,TITLE: Connection between the asymptotic properties of the total
cross section and the ratio of the imaginary and real parts of the
~amplitude of zero-angle elastic scattering
,SOURCE: Zhurnal.eksperimentallnoy i teoreticheskoy fizi.ki, v. r-0,
~~no. 3,- 1966, 672-679
;TOPIC TAGS: scattering cross section, scattering amplitude,
,asymptotic property, elastic scattering
'ABSTRACT: The author analyzes in greater detail the connection, first.-_
-by.Y. N. Kburi and T. Kinoshita (Phys. Rev. v. 137,
established B7201.
1965), between the asymptotic values of the symmetrical amplitude of
.zero-angle elastic scattering (at 'A'arge laboratory-systesm energies).
It is sbown(tbat this connection can be made more precise and upper
Card

L 24396-66
!ACC NR: AP6010988
can be obtained for the scattering amplitude under
;certain rather natural physical assumptions. It Is demonstrated, in
particular, that the limitation on the asymptotic value of the total
toross section depends on the asymptotic value of the ratio of' the
~imaginary to the real parts of the elastic-scattering amplitude. If
,;this amplitude is not pure imaginary asymptotically, then the cross
section increases in power-law fashion If its real part is pcsitive,
,and decreases in power-law fashion if it is negative. If the
~asymptotic amplitude of elastic scattering is pure imaginary, then
the cross section can increase or decrease only slower than a certain
~power of the energy. The author thanks Ye. L. Feynberg Kor continuous
-Anterest in the work,1N. N. Meyman tor useful discussion, and D. S.
;Chernavskiy,.I. M. Drem1n and I Royzen for valuable discussions.
Urig. art. has: 45 roM=as.
'SUB CODE: 20/ SUBM DATE: OqAug65/ ORIG REF: 002/ OTH REF: 004
Card 2/p

-- FARBEROV H.I.-" KUTIIN, A.M.; USTAVSHCHIKOV, B.F.; VEEWOVA, T.P.; FROLOV, A.F,
1. 0
ConditionB for the syAthesis of 2-meth71-3-vinylpyricLine. Zhur.
priklokhim. 34 no.3:632--640 W 161. (KIU 14:5)
1, Institut monomerov dlya sinteticheskogo kauchuka i
- Yaroslavakiy tekhnologicheskiy institut.
(Pyrid-ine)

MASS I BOOK MCPWIT~tTION SOV/4350
Soweahehanlye po khlmLl, tekhnolog4l I prLmenenlyu Protavolnykh
P1 r1dina I khInol" . Riga. 1957
tokhnologlya I primenenlya prclzvcKInykh ptridina I
JzMnollna. materialy soveshchanlya (Chemistry, Technology
and Utilization of' Pyr1din,e anI Quinollne Derivatives.
Materials or the Conference) Riga. IZd-vo A.4 LAtviyskoy
23H. 1960. 299 p. Xrrat& slip Inserted. 1,000 copies
printed.
3pMearing Agencies: Akademlya naux !Atelyakoy SM. InStItUt
khIAdi; Vaesorutnoy* khInlehemkore OtshChentwo.
Rd.- S. Bashanova; '.-son. Ed..- A. Xlyallnya. Editorial
Ward: Yu. A. 9~vzkly. Candidate, or chemistry, z. v.
t=agz. Car=_;." wf C*.-.i.Lry 0i.-P. FA.). L. P. ZLIWAarey,
Doctor Of Ch*219tr7. " K. H. ralftyn'.
FMtP=- ThIs book to intended for organic chemists and
Crauleal engineers.
09VX~~s The collection contsina 33 articles on methods
Of &Ynth*Glzlng Or PrOd"Ing Pyrillsie, qalnollne, and
tbe.4r derivatives from n&t~zl OOUPteS. NO per3onallti
are osentLonod. 11.64res, tables, " referents,
the article a.
SYNTHETIC MASS OF FPr.FAMIN,:; MIDLIM3 AND
QUVOLDMS
3417k-v, A. S.. and 0. S. [Srect-ea:4 %~akjy
&. 3=2 T L MF-Ij y na (Ce nt ral
ks#a State LIr.1-voriLty *---r.1 V. 1. !or.-In); .5,,nthetic Stailet,
Card Z/ I Cl
r%rt-Z'Zv_ P. A_-! Kut*tn.
r' -a. ?!~.t cr t!'~ ~L_jstr; C.
l;__-.,,t:7jj ~f 2-M,thy-5-rth)rlpyr1d1n~
aztl 2-X-th7.'-5-vIr7lPY:'1d1r~ &-.1 Trjjr of 97
Vjr..jsr. r,__%A_Ilnstltut stnt-24 Aki-temll nauk
.vj;-Sjrc,r SSR (_njtjt,jte r,r Organ- Zynth~sts of the
,At
Of Silon--?3 L&tvtysxa,7& 334). The Transition
Pro,& --,3- Irdandtone to Pyridine Derivatives III
dl n
,c titut vysOk~GIekujy4_~ywh vo7e ne ly
I In
nrak WSR (tnstitute for H-0 Mol-tular Compounds
0 US5R)j .3ynthests and Polynerl-
xf the A'&JP-.v or -%-,Ienc.s
at.'~n Ci Ursat~ratd romp1~111 or the Pyridine and Qulno-
I.,q
P" gtqkt,- rOsuja.-:vemny7 universitet
Sta-4 uft%virlityfl. _,!ustrial synthesis or Lcpldlne
41i 127
B&I's
Kc=,. rt__j_(rvm'klT
(p,,. ;Zrj:.jI. 31n%.heals cr
,ural jratl*,t.j;.
Ba3es PrOn AJ~zt- Aclnes &~l Aietyl~ne 131
PrePtr2titn Or
1. CR13-or 3-1te Unllverj
A~,Tl Ar.11.1deA ~-_S Synth-als of
139
jV3e.,yuzn
r. _... :tl (Al'-'?n1-n
In3..- kigh "" 'Tcv
Xr_, 'tUt4 for. C"rdtal ROM .1
iteS, _ ), . th.
'n LnSt.
Vqd.rajC7quIM1Iln* pthod or SynthealzIng Quinolln1c Basis 145
Te-ov. B_ A;. 'R111o, -11~tl 3ynth~ilw or
of Qal.%Qljn~ zn~j 3ome m-Aryllepidln-i Wts
L271 Alir" 251
Koslov. N. S.. and 0. K. Ko='mi-kh I Pern3kly gos~~arqtv-nnyy
4dumill rn:t
Catalytic Synth-fies or 2-Phenyl- 5,6-t-ntoqulnollne Deri-
vatives 159
Ardash-r V I (Rostov 2"Mate Univeriltyl Catal.Ttle Con-
A.71 AnInes to Q~Inolinv. ITI
Zaluxa7e-~ L. P. Frodu~tz of the Cond"sation,Z Aniline &A
fltn AZtt3a1*h;-- n a t4eutral

82147
SOV/81-59-6-2o4O3
Translation from; Referativnyy zhurnal. Khimiya, 1959, Nr 6, pp 384-385 (USSR)
5'"5,bm
AUTHORS: Farberov', M.I,,.Ustavshchikov, B.F., Kutv'in, A.M., Vernn-ia, Tr,.P.,
Yarosh, Ye.V.
TITIE: The Methods of Technical Synthes.'s and the Applice.tion of 2-Methyl.-
5-Ethylpyridine and 2-Methyl-5-Vinylpyridine
PERIODICAL: Yaroslavsk. prom-st' (Sovnarkhoz Yaroslavsk. eXon, ai-,. r-na),
1958, Nr 3, PP 15 - 21
ABSTRACT: In the condensation of I mole of paraidehyde and 4 molee cf 40_i-,~O%
(better 50%) aqueous soluticn of NH3 in the preeence i~f a catalySt
(organic or inorganic salt) taken in -the quanti*ly of 1-2% based cr,
the weight of the paral~dehyde (20-30 Min, 2600C, pre3sure 80-100
atm) 99% pure 2-inethyl-5-ethvlDvridinel(-~.) is obtained, yield 75-80%,
b. p. i76,70C, n-O-D 1.4974, d44"~) 0 -9189: as Impurities 0~ - and t -
picoline, higher pyridines and resins are formad. The rea.,.*Icn proseeds
r-. -----------n
CHO+NH3 --->N=C(~M3'CH=,-HC(C2Ti5)=r,ii+4H20.
in the following order: 4CH3
I, diluted by water steam In the mo'.ar ratio 1:12-1:20 ts dehydr,~,genat-
ed in the presence of industrial dehydrogenation srtalysts7(K-10 and
Card 1/3 K-12) consisting of Zn, Cr, Fe and-T-1 Foxides a2tivated by K20 fcr 2
)01"

8210
sov/8i._5q_6_2o4o-,
The Methods of Technical Synthesis and the Applicati.)n of 2-M-~!.~.,YI-5-EthYlr,yr'-.4,lne
and 2-Mothyl-5-Vinylpyridine
hours at 575-6000C and a volumetric rate of 500-600 ml per 1 1 cf call-slyst in 1
hour, 97-99% pure 2-methyl-5-vinylpyridine (II) is obtained, yield 20-25% based
mm
an I having passed through, or 70-75% based on I decomposed, b. P. 75c,/15 T,
n2OD 1.5454, ate is 23-27%, tl-,e
d420 0.9579. The content of II in the catalyz I
yield of the catalyzate 89-91%. Pyridine, picoll-nes, 2,5-dimethyl-, 3_etI7_,yl_ and
3-vinylpyridine are formed as impurities. I! is very inclined to polymerizati"..
S, C6H2(OH)(NO2)3, 0~_nitroso_ /S -naphthol ELnd methol (sulfate salt of methylami-
nophenol) are usbd as stabilizers of II. In the process of II separation 8 is
used as stAbilizer and methol for storing (in co=entrations of Ip to 0.001 wetght
%). In the case of oxidizing I by 101n0i~ or Cu(NO3)2, 2,5_pyrld'_ne-carboxyli:~
acid (yield 60-70%, m. p.2360C) is obtained which is converted to nicotinic araid
by decarboxylizing with a yield ofe,-.,100% (m. p. 1630C). The dimethyl ester of
2,5-pyridinie:-dicarboxylic acid (m. p. 1630C) after reesteri fie at. ion by ethylenegly-
col is conctensed in the presence of ZnC12 into a high-polymeric resin. I with
CH20 forms 5-ethyl-2-vinyl- and 5-ethyl-2-(/3-oxyeihyl)-pyrldire wlth a high
yield. I is easily hydrogenated with a yield ofl-aIOO% by Na in butyl alcohcl,
Card 213

82147
S OV/8 I - 5 9 -06 ~ 20 ~-03
The Methods of Technical Synthesis and the Application of 2-MCttVI-5-EtIrIy.'pyrid'-ne
and 2-Methyl-5-Vinylpyridine
and also catalytically (in the
_presence of Ni-cataiysta)
piperidine, b. p. 160-1610C, n2OD 1.4530, 42c) 0.8559. = is a mrcmer for
the industry of synthetic rubber, it car, be used ',n4 the
and synthetic fibers.
Ya. D9r,3rjshevAiy
Card 3/3

50, 3) SOV/153-58-5-16/28
AUTHORS: Farborov, M. I., UstaV3hchikov, B. F., Kutlin, A. If.,
Vernova, T. P., Yarosh, Ye. V.,
TITLE: Technical Synthesis of 2-Methyl-5-Ethyl Pyridine and
2-11ethyl-5-Viul-Pyridine, and Their Fields of Application
(Tekhnicheski.ve sintezy 2-met-ii-5-etil-piridina i 2--metil-5-
vi nilpiridina i oblasti ikh primeneniya)
PERIODICAL: Izvest'Lya vysshikh uchebnykh zavedeniy. Khimiya i khimicheskaya
Lekhunclogiya, 1958, Nr 5, pp 92-99 (USSR)
ABSTRACT- The wu--hors te;ok the synthesis of 2-methyl-5--ethyl pyridine
(MEP) from acetaidehyde and ammonia with a further dehydro-
genation to 2-methyl-5-vinyl pyridine (MVP) as a basis for
the working out of technical synthesis of these twb'substances.
The pape-rs recently published in patents (Refs 11-13) tend to
show an intenije elaboration of these reactions. There are,
however, no publications on the first, and especially on the
3e'oond stage of this pr*ocess. The authors first clarified the
most important riles governing the reaction between acetaldehyde
and ammonia for the purpose of an induatrial utilization.
1) S y n t.h a a i a o f 2 - m e t h y 1 - 5 - e t h y 1
Card 1/4 p r 1 d '; n o. Acetaldehyde 1.3 used as paraldjhyde. Thi.,3

'OV-153-58-5-16/28
Technical Synthesis of 2-Yetkiyl-~--Ethy-, Py-ridire and 2-Y
and Their Fields of Application
offers much higher yields. Stoichiome"ric ratins (1.33 Mol
paraldehyde per I mol ammonia) could, however, not Secure a
sufficiently high MZP yield. The optiaftm ratio amounts to at
least 4 mol ammonia per 1 mol paraldehydeo The presence of 1%rtv
quantities of water has a favorable effect. The opinions on tho
formation mechanism of MEP in literature contradict each other
(Ref 14). Up to 30 different salts, among ther. ZnCl 2' Pecl 21
S11C1 31 COC12' NiCi 21 CH3 COONa, NH4C19 CH3COONE41 NH4F , NV-Hl~'
KF, KHF 2 and others served as catalysts. A catalyst was selected
which corresponds to the technical process. Its concentration UsUal 11'
amourtutO-1-2% of the paraldehyde. The reaction takes also place
without catalyst, however, with much smaller yields.
2) D e h y d r o g e ri a t i o n o f 2- m e t h y 1 - 5
e y 1 p y - i d i n a. S y n t h a s i a o f 2 - m e t h y 1
-5 v i n y 1 p y r i d i n e. The best industrial dehydrogenat-
ing catalysts served for dehydrogenation: K-10 and K-12, which
consist of zinc oxide, chromium oxides, iron and aluminum
Card 2/4 OXide3, act-ivated -xilth potassium oxide. The paxtial pressure

SOV/'153-58-5-16/26
Technical Synthesis of 2-Me thY-',--5- Ethyl Pyridine and 2-*-fhy:.-5-Vi-ry1 Pyridine,
and Their F-Ioldr of Application
best decreased by dilution with steam. Figure 2 shows typical
dehydrogenation curves of MEP (catalyst K-12 at 5750)- Under
optimum conditions the MVP yi.elda per passed MEP amounted to
20-25%, and pel, decomposed NIEP to 7C-75%- 3) 1 s o I a t i o n
and s t a b 1 1, i z a t i o n of MVP, ioe. the separation of
MEP from MVP is a diffi-~ult process as their boiling points
are clos;~ to each k;ther (176.7 and 1670). Furthermore MVP in
easily pclymerized. Fer *,his reason a high vacuum is required.
Sulf-ur, picric accid, a-nitrosc-P-naphthol and sulfurous methyl
amino phenul. (Figs 3,4) were thp best stabilizers of some dozens
.'.nvestigated. 4) E q u i p m e n 46 .-and a p p a r a t u s f o r
t h e MVP a y n.t h e s i s-Fig-are 5 shows a corresponding
scherne. 5) The scheyie (p 98) shows s o m e m o r e s y n -
t h -~~ ., e s p r o e e e d i n g f r o m MEP (Refs 15,16).
6) Finally, r u b b a x a n d 1 a t e x t y p e a o n M
basis are discussed. Some of them show better adhesion to cord
from viscose and nylon, high elasticity, frost resistance, and
resistance t-o wear and tear. Some branches of industry announce
at present a high demand for those rubber types. '
Card 3/4 There are 5 figures and 18 references, 6 of which are Soviet.

~;07/1 5 1 6/2~
Technical Synthesis of 2-Methyl-5-Ethyl Pyridine an".
and Their Fields of Application
ASSOCIATION: Yaroslavskiy tekhnoloricheakiy institutiopytnyy zewod Ministerst,-
va khimicheokoy promyshlennostt (Yaroulavil Technological
Institute and Test Plant of the Ministry of Chemical IndustryN
SUBMITTED: December 28, 1957
Card 4/4

S/079j6O/O30/O4/O9/M0
Booi/Boi6
AUTHORSt Farberov, M. I., KStlin, A. M., KishinskiX, Go-I.,
Vernova, T. P.
TITLEs Diene Synthesis on the Basis of Olefins and Aldehydes.
II. Synthesis of DivinylAon the Basis of ?~SopZ~Ieneand
Formaldehyde - k
PERIODICALs Zhurnal obshchey khimii, 1960, Vol* 30, No- 4, PP- 1099-1106
TEXTt Some patents in publications indicate the possibility of obtaining
divinyl from 4-methyl dioxane (Ref- 5) but without an experinental basis.
The authors of the present paper thoroughly investigated the contact con-
version of methyl dioxane (I) (obtained from propylene and formaldehyde) in
the gaseous phase by means of various catalysts (mainly metallic phosphates)
in which connection divinyl Is formed in hiGh yield. It was further shown
that under certain conditions divinyl and allyl carbinol (IV), approximate!y
in the same quantity (Ref. 6), may be obtained at the same time. On the
basis of previous papers (Refs. 1-4) (Scheme 1) the synthesis of divinyl
Card 113

Diene Synthesis on the Basis of Olefins and S/079160,/030/04/:09/060
Aldehydes. II. Synthesis of Divinyl on the Bool/BO16
Basis of Propylene and Formaldehyde
was carried out by allowing propylene to react with formaldehyde by
of a catalyst. As a result of the investigation of the contact coLversioil
of the principal reaction product, methyl dioxane (Scheme), an 82p divif.,.,-
yield was obtained (calculated for the methyl dioxane having pass,,A re.-
action). By a suitably conducted hydroeenation of the allyl carbi,iol, (T7),
butanol-I was obtained quantitatively. At the same time, divinyl an., a_L_*"j' V,
carbinol could be synthesized in about the same quantities. The authors J_-- --
vestigated the contact conversion of the by-product of the above-mer;~Iioned
reaction# 4-hydroxy-tetrahydropyran 111~, by means of the RSD catalyst,
in which connection compound (' , divinyl (15-20%), and the un-
saturated alcohol (IV) resulted. The divinyl yield could be increased up
about 70% at a higher temperature (5500), A reaction mechari;~u wir.3 6aCt;estel
for the formation of the products which are formed on contact conversion of
methyl dioxane and 4-hydroxy-tetrahydropyrano 3 dingrams and 3 tables il-
lustrate the investigation results. There are 3 figures, 3 tableo, and
13 references, 11 of which are Soviet.
Card 2/3

Diene Synthesis on the Basis of Olefins and S/079/60/030/04/09/080
Aldehydes. II. Synthesis of Divinyl on the BOOI/BO16
Basis of Propylene and Formaldehyde
ASSOCIATIONs Nauchno-isaledovatellskiy institut monomerov dlya SK
(Scientific Research Institute of Monomers of Synthetic
Rubber). Yaroslavskiy tekhnologicheskiy institut
~Yaroslavll Institute of Technology)
SUBMITTEDs April 7, 1958
Card 3/3

-5 -3400
SOV(9-30--'. -28/6'-
AUTHORS: Farberf,'z, T., K%;.4,-,-, M.,
Vernov,
TITLE: Synthesis of' Dlu~neL; From Olefins arid Aldehydes. I.
Syntheolo all.' I.-,-,opvenc~ From DtobuLylcrie and Formaldehyde
FERIODICALt Zhurnal obohchuy 1rhinill, 1960, Vol 30, Nr -1, pp
875-8811 (US` R)
ABSTRACT; Among many catalysts tested, the best reoulti: weve,
obtained wIth KSD catalyst (a inixture of calclum
phosphateo of a defInIte composItIon). Thr: cul-~ily-t
needs regew-,ratior, after 2-A hourj of work, arid thi-~
can be best done With a -,team-alv whLch
removes depoolted "coke" fvom It. The act.1v.1ty (A'
the catalys"-. decreases sharply when the
cai,ried out without steam. The de-pendenc,~- o,'-
rate of dime thyldioxane conver2lon on coriil~-(:(,
and tern-perature 16 ohown in Fig"-. 2 arid
Card 1/6

Synthusl~3 of' Dlenv-0~ Fut-,m nd Ald'--hydi-L; 7`2711
SO V/( 5 -3 0 - 3-1-) 8/6
G
fy
Fig. 2. Conversion of dimethyldioxane (I) Into
unsaturated hydrocarbons (C 5if8 and iso-Cl, 118) At
different tempei~ature3 and with steam dilution,
1-.14 (rri-olar';,~I) 3000; (2) 3250; (3) 3500; (4)
3750; (5) /10
Card 2/6
I~C'AIIVC CI)Njf~rT FC)

)h "I 11,~ :III,!
V/'['-i - 3 0 - 3 - 2
Fig. 3. Yield of isoprene based on rea2ted dimethyl-
dioxane (I) at different temperatures wLth steam
dilution 1:111 (111oles :0~1) 3000; (2) 32::)0; (3)
3500; (4) 375"; (5) )tO
Card 3/6
V 0.4 11 1.6 2,0.
rEI-Allyr- (_a;jrAf.T I-IMF (Src)

I T
I o --oi-I)Iones 1, -ro- 01 ~111 at id, A Idt-l"QVde., 7 8 27 4
SOV/(9-30-3-28/69
Dilution of' dlrnr~thyldiozzirie with ;3team 31giilflcantly
increases the reaction rate. An appropriate reelection
of the reaction conditions could yield 75-78% isoprene,
based on reacted diniethyldioxane, or 80-85% isoprene,
based on decomposed dimethy1dioxane. Among the
reaction products of Isobutylene with formaldehyde,
In additlon to the main product, dimethyldioxane (I),
diol (7-10% based on unreacted formaldehyde), and
cyclic alcohol (III , 7-8%) are present. They can
also be converted into isoprene over the KSD catalyst.
The mechanism of reaction is shown in Scheme 2.
Card 4/6

Sy! u L' Die t Lt--
1:11, i. (A 1j)
f I y PC 054 1
'A I
(1)
-
cI 1, cIf,
I - I I
c1l'-f :11-c1 1 :114) r,11,-4 0If --- (Al, ~:f: -CII Al
(VI
cli,
11C, CIII I I j; CIII C11,1-01 -CIf -CII.,- 'If J
I I I I (IX)
11 1C cIf. I,,, Q 1-1
"I( )~ " *\0 /
(VI 1) (Vill)
C113 CII.,011 DlcrcTe 0 CH3
I (OAC1.0oaq I
1 r --C11- 1 :11, .1 N :1120 j I 1 0
( V)
SCHEME Z
Card V6

Synthe~sls of DlencL; From, -~-,i--Ld Aldehyde~3. '[82-(4
S OV/7
n ri
The
of the reaction art,:.,: Isoprene M, bp 'D
2-methylbuten-2-ol-4 (IV), bp 139-140'; 'u; w1a I e rc
aldeltyde (V!),,. H-1p ll'f .5-118':; t'-~QMPOLlrid (V-11), bl)
11" 11-- 1.41190;* k~oinpouiid (VIH~, 1, lu"t-l~l
20 D
11D I . 11.1 f)O; coinpound (IX), bp 120-1210
1 -5870- Il. K. Shi~,uiyalclna part"Ic1pated In t, hl:~ wni-lc.
Tnei-e urf-- It 3 and 10
8 Sovlel.-, 2U.S. The U.S. ref`ereiice-.,i ~~tve:
T. L., Steadman, J. Am. Chem. Soc., 71, 8V-3 W)4'1~);
U.S. Patent. M864o.
ASSOCIATION; Scientifle Research Institute of' Monome-ro for Syrithietic
Rubber, and YaroSlavl Technological (,',lauclino-
Issledovatell,,3kly instilu-ut inonotnerov dlya SK
Yaroslavskly teldrinolo'g,icheskiy instltut)
SUBMITTED; March 7, 1958
Card 6/6

S/080/61/034/003/011/017
A057/A129
AUTHORS: Farberov, M. I.; Kut'in, A. M., Ustavshchikov, 1). F., Vernova,
T. P., Frolov, A. F.
TITLE- Investigation of the conditions for the synthesis of 2-metlwi-
-5-vinylpyricline
PERIODICAL: Zhurnal prikladnoy khimii, V. 34, no- 3, 1961, 632 - 64o
TEXT: Dehydrogenatirn of 21mathyl-5-ethylpyrldine (KFJ-) was inve.-;-igatey-~
yl-g-vinylpyridine (KVP). Conditions were
in order to increase the yield o-P 2-meth
presented ensuring a 25 % yiel,3 of MVP in relation to the amount passed of MEP
and 70 - 73 % yield in relation tt decomposed MEP. Steam effects partial hyrt-o-
lysis of pyridine bases and iE thae not a completely inert diluent in dehydrogen-
ation of MEP. Inhibitors for polymerization were Investigated for ,,the stcrage-
of MVP and separation from dt--jdrogenation products. Improvement of th"s dehydro-
genation process is important for the manufacture of polymer materials. MVP is
especially significant in the prcduction of special types of synthesized litex
and synthetic rubber according t3 R. Frank et al. (Ref. 1: Ind. Eng. Ch-im., 40,
879 (1948)), J. E. Pritchard and M. H. Opheim (Ref. 2: Ind. aig. Chem, 46, 2242,
Card 119

s/o8o/61/034/cm/on/017
Investigation of the cond-itionn for ..... A057/Al2S)
1954, 47, 863, 195~), H. E. Rallsback and C. C. Biard (Ref - 3: Ind. &,g. Chem.,
48, io43, 1956),dnd V. L. Tsaylingol'd et a!. (Ref. 4: Kauchuk i rezina, 9, 1958,
3, 14959, 9, 1959). or ion exchmge resins in the manufacture of synthe'.ic flue-s.
The raw material - MEP - is syuthesized by Chlobdbabin's reaction betw~!en paraal-
debyde and ammonia in liquid phase according to M. I. Faberov et al. (Ref. 5:
Izv. Vuzov, Khim. i khim. tekhn., 5, 92, 1958) with a 70 - 73 % yield. 7he pre-
sent experiments were carried out (in as:6istance of M. Yu. Tikhvinskaya and M. A.
Loginova) by a method and with a laboratory assembly described in a prior paper
(Ref. 11: ZhOKh, 30, 875, 1960). Vapor pressure and liquid - vapor equilibria in
the system MEP - MVP was determined on an apparatus similar to Othmer's (R_~_F. 12:
Ind. Rig. Chem., 45, 614, 19-53) especially adapted for vacuum tests. Two 3ata.-
lysts, were used: no. 1 based on ZnO andno. 2 on Fe203, containing 86 - 88 % of
the basic component, some ch7omium oxide and small amounts of other components,
which are not specified. Since considerable carbon deposition occurs during the
dehydrogenation process, the ,.atalyst had to be regenerated after 2 - 8 hours
by passing an air-steam mixture at a maximum temperature of 6500 - 7000C. Re-
sults of dehydrogenation experiments with steam as diluent in varying conditions
are given in Table 1, It can be sean that the yield of MVP related to d9compo-
sition of MEP decreaseswith the contact time. This is apparently effected by
Card 2/'~

S/080/6-1/03VO03/011A)I7
Investigation of the conditionn for ..... A057/A129
side reactions and inazta4sing'carbon deposition.. The latter dej)end4 on the type
of catalyst widths degree of dilution by steam. Steam cannot be considered as
inert diluent, since with incraasing dilution by steam the yield of cat&lyzate
and of MVP (based-on decomposed MEP). decreases, in spite of the fact that the
yield of MVP based on the amount of passed MEP increases (Figure 1). Al:~o with
increasing dilution by steam formation of gaseous products (CO2, H2, NF13 etc)
and the content of pyridines ( 0.- and 6T -picoline,,2,5-lutidine, 3-vinylp;(rl~
dine) in the catalyzate increases. This can be explained by the! reaction of py-
ridine bases with steam, rai-alting -in a partial dealkylation of MEP and fc!7nia-Aor,
of pyridimes, or totaLl rupture of the pyridine ring with ammonia. evolution. A
similar reaction was observed by A. A. Baladin et al. (Ref. 8: DAN SS3R, 11:~, 79,
di-f L er-n
1956) on cL-picoline. These sids reactions of - by4rolysis occur witb 1. -- t
rates on various catalysts,-t-hus influencing the selection of the latt-r. Ra-
sults on dehydrogenation of MVP with othqr diluent's. are given in Table 3. Thi
observed affect of benzene c%ri be 4xplained by the. fact that no side r~asti3nri
of hydrolysis occur. Although nitrogen doi~s not show these side reaitltons, no
desorption of pyridine bas4s from the catalyst is effected by nitrogAn (con""rary
S4
to benzene) resulting in therm.5-1 decompo tion of these substances. Practiona-
tion of the catalyzate at 20 torr demonstrated that the fraction boiling at 63
Card 3/9

S/080/61/034/00.3/0-I'l./017
Invest~gation of the conditicnE for A057/A129
-,690c.(20 torr) [Abstracter's nc.-.,-: Error_in original paper - 2.00 torr instead
of 20.1 has an increased refraction Index,an 'd contains considerable amounts of an
unsaturated compound, appELY-snUY 3-vinylpyridine. Thus the following reaction
and side products were obtainid. in debydrogRnation of MEP: (I) CL-picoline, (II)
3-ethylpyridinep (III), 2,5-1utidine, (IV) 3-vinylpyridine, (V) 2-methyl-5---~thyl-
pyridine, (VI) 2.~-metbyl-5-viaylpyridine.. The present authors consider (1), (Ii)
and .(III,) as main cracking products of MEP (in presence of hydrogen), ythile (IV)
is a eracking product of MVP. Different stabilizers for 14VP were investigated
(Figure 3) and It was observed that 0.1 % of sulfur Is the optiorm stabIlizer In
fractionation of WV?. For the storage of MVP an.admixture of 0,001 %, methol .1Z
most efficient in e~abilfzing MVP for several weeks, or 0.01 % methol for S-~-Iqral
months!p Liquid-vapor equilibrium in the system MEP - MVP is shown ih Figure 5.
Corresponding,,expariments dawnArated that apecial conditions rmist bs =&intained
if a 98 - 99 % concentration of MVP should be attained in fractionation. Thus in
the system the maximum temperature should be 950C (for highly concentrat-,d WIP
only 8500, and highly effsotive inhibitors should be used. There arc 6- fig,-,res,
4 tables and 12 references: 8 Scviet-bloc and 4 non-Soviet-bloc.
card 4/9

S/080/61/034/603/01-1/617
Investigation of the conditions for ..... A057/AJ29 '
ASSOCIATIONS: - Institut monomerov dlya SK (Institute of Monomers for Synthetic
Rubber) and Yaro3lavskiy tekhnologicheskiy institut (Yaroslavl'
Technological Institute)
SUBMITTM ~June 6, ig6o.
Table 1! Dehydrogenation of M on the catalysts no. 1 and no. 2 using steam as
diluent. Legend: (1) no. of the catalyst, (2) temperature(OC), (3) nominal con-
tact time, see., (4) volume velceity of the MEP supply (in ml/m.1 catalyst per h),
(5) molar ratio H20/ MEP, (6) yield of the catalyzate (weight M, (7) yield of
MVP based on the MEP passed (mole %), (8) yield of MVP based on the MEP decompos-
ed (mole %), (9) carbon deposit on the catalyst (mole %)based on the MFP passed).
Card 5/9

FARBEROV, M.I.; USTAVSHCHIKOV, B.F.; MRIIN, A.M.; VERNOVA, T.P.;
YAROSH, Ye.V.
Synthesis and use of 2-methyl-5-ethylpyridine and 2-methyl-5-vinyl-
pyridine. Izv.vya.ucheb.zav.; khim. i Idiim.tekh, 1 no-5:92-99 158.
(MIRA 12:2)
1. Ynroslavskly tokhnologicheakiy inatitut i Opytnyy znvod Miniat-
eretva khimicheskoy promyshlennosti.
(Pyridine)

AUTHORS: Farberov, M. I., Kutlin, A. M., sov/1156 -58-1-36/46
Vernova T P Shemyakina, N. K.
TITLE: Industrial Synthesis of Allylcarbinol and Standard Butyl
Alcohol on the Basis of Propylene and Formaldehyde (Tekhniches-
kiy sintez allilkarbinola i normallnogo butilovogo spirta
na oanove propilena i formalldegida)
PERIODICAL: Nauchnyye doklady vysshey shkoly, Khimiya i khimicheskaya
tekhnologiya, 1958, Nr 1, pp. 148 - 152 (USSR)
ABSTRACT: In their laboratory the authors have for years studied
syntheses based on olefine and formaldehyde (Refs 1,2). Allyl
dioxanes-1,3 are converted into dienes. Catalysts and conditions
were developed by means of which 80 - goo of the theoretically
possible diene yield could be obtained (Ref 2). By passing
it over a catalyst in the presence of water vapor, 4-methyl
dioxane-1,3 can be easily converted into divinyl. As further
investigations have shown, the ally1carbinol yield can be
substantially increased by carrying out the contact process
under less severe conditions (lower tomperiLtures, shorter
contact time; Fig 1). Figure 2 shows the influence of temper-
Card 1/3 ature upon the allylcarbinol yield, given dn molar per cent

Industrial Synthesis of Allylcarbinol and Standard sov,1,:o6-r6_1-76146
ButYl Alcohol on the Basis of Propylene and Formaldehyde o
related to methyl dioxane. Table 1 shows the results of a
typical balance experiment; under such conditions as were
chosen here, the weight ratio of the allylcarbinol and divinyl
yields, related to the decomposed methyl dioxane, may be even
a little greater than unity. The author' idea about the
mechanism of this reaction is as follows: The catalyst ( a
calcium phosphate mixture) possesses hydrolyzing and at the
same time dehydration properties (Ref 9). With the same cata-
lyst, and under the same conditions, trimethyl carbinol is
dehydrated to isobutylene with a quantitative yield. The 1.
reaction stage is therefore the hydrolysis of methyl dioxane
M in the presence of water vapor to butandiol-1,3 (II), with
separation of formaldehyde. Butandiol is further dehydrated,
being converted to allylcarbinol (III) and divinyl (IV).
Propylene is formed in small quantities due to a cracking
reaction. Allylcarbinol may itself be of interest as a starting
mat#rial for syntheses. From an industrial viewpoint, however,
its use in hydration in standard butyl alcohol is of greater
importance. There are 3 figures, 2 tablest and 13 references,
Card 2/3 8 of which are Soviet.

Industrial Synthesis of Allylcarbinol and Standard sov/156-58-1-36/46
Butyl Alcohol on the Basis of Propylene and Fornaldehyde
I
ASSOCIATION: Kafedra tekhnologii osnovnogo organicheakogo nint,~za i SK
Yaroslavskogo tekhnologicheskogo instituta (Chair of
Technology of Basic Organic Synthesis and SK of the Yaroslavl'
Institute of Technology)
SUBUITTED: October 3, 1957
Card 3/3

VExU40VSKIY, Aleksandr Ivonovich; KOGAII, Ye.T-., red.
['Wh(se llpli:noll are they? On the nature and t:iet'hod'!; of
econ-mic planning in Western Europe] Ch'i c-to p1riny"?
0 sushchnosti i metodakh ekonomichaskog-o progrwmirova-
niia v Zapadnoi Evrope. Moskva, Izd-vo '17nanie," 11)64.
39 P. (Povoe v zhizni, nauke, tekhnike. III Seriia:
Ekonomika, no.12) (MIRA 17:7)