"SCIENTIFIC ABSTRACT LOGACHEV, YU. I. - LOGACHEVA, L. N."

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R000930410008-6
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Sequence Number: 8
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

Investigation of Terrestrial Cor-puscular SOV/20-1 25-2- 6L
Radiation and of Cosmic Rays During the Flight of a Cosmic Rocket
high intensity is dealt with. In the center of the outer zone,
where particle density is the greatest, the effective energy of
electrons is minimal. In coi.ilusion, cosmic radiation is dealt
with. Beginning with a distanae of 66000 k7n, the intensity of
all components remains constant. The strict com3tants of all
components at distances of from 66000 to 150000 Ian indicates
the existence of & radiation upon which the terrestrial magnetic
field exercises no influence. Therefore, either the terrestrial
magnetic field vanishes at a distance of 10 earth-radii, or
there are no particles with momenta of
1-5-108 to 4.10 7 ev/o in interplanetary space.The enera-fljx
of the photom is very low and contributes partly nothing to
ionization. There are 2 figures and 4 Soviet references.
SUBMITTED: February 25, 1959
Card 3/3

LOGACHEV, Yu. I., Cand Phys-Math Sci -- (diss) "Research into radia-
tions in flights of artificial satellites and cosmic rockets." Mos-
cow, 1960. 13 pp; (Academy of Sciences USSRv Physics Inst im F. L.
Lebedev); 150 copies; price not given; (KL, 27-60, 148)

I's
v Az
will I p
1,4
FL r.
lei
2It;
f
E.
'YO -n

1).V. -W t
VERNOV.1 SAL; CHUDAKOV, A.Ye.; VAKUMV) T1JvoU-.Y--)v A.f".
LAssociate Member, Academy of Sciences, USSR.
"Radiation Measurementr During the Flight of the Second Soviet
Space Rocket."
report presented at the First Intl Space Science Symposium, Nice, France, Jan lc,.,~O.
National Academy of Sciences of the USSR, Mosccw.

-a'. 9000 679U3
3. .200c)
29 (00 2940 6/020/60/130/03/009/065
AUTHORS: lernov, S.- It., Corresponding BO14/BO14
Member of We AS USSR, Chudakovp A. Ye.v
Vakulov, V., Logache!j, L., Nikolayev, A. G.
P. _ ILWS,
TITLE: Radiation Measurement During the Plight of the Second Cosmic
_ _B,ocket Xy
PERIODICAL: Doklady Akademii nauk SSSR, 1960, Vol 130t Nr 3, PP 517 - 520
(USSR)
ABSTRACT; The equipment of the interplanetary rocket launched on
September 12, 1959 was designed for measuring the guter radi&=-
tion-belt of the Earth, for recording cosmic radiation on its
flight--f-ro-m-F-tHe Ea th to the loon and a potential radiation
belt of the Xoonr4he individual parts of the apparatu~j which
consisted of six gas-discharge and four scintillationNounters,
are described in detail. Furthermorej this paper conts 0-
sults of the first evaluation of data obtained for the range of
from 9,000 to 120,000 ka away from the center of the Earth and
in the neighborhood of the Moon, Figure I illustrates the tra-
jeotories of the first and second interplanetary rockets re
Card 1/3 ferred to the terrestrial magnetic field. Ionization measur;_

67908
Radiation Reasurement During the Flight of the 8/020/60/130/03/009/065
Second Cosmic Rocket . B014/BO14
sents are also graphically represented in figure 1. It is
noted that the shift of the ionization maximum between the
two measurements was not caused by the slight difference of
the trajectories of the two rockets. The radiation belt is
most probably deformed by streams of aolar corpuscles. This
assumption neeme to be confirmed by a comparison with the re-
sults of measuremente performed by the 1merican rocket
Pioneer III. The energy-flux density of electrons of more than
5 Nev or of protons of more than 30 Nev is said to be
I particle/cm2.sec. Furthermore, a radiation was detected which
consisted of electrons having an energy of the order of 10 6 8v,
or of protons of an energy of about 10 Nev. The first poesibili-
ty is considered to be more probable. This electron flux is
5 / 2
said to be 5-10 particles am aec.Theoxistenoo of electron
fluxes having an energy of between 20 and 50 kev (flux:
10 10 particles/cm2 seo), which had already been detected by
the first intercontinental rooketp were proven agains Thusq
Card 2/3 two essential groups of particle fluxes were found: electrons,,

67906
Radiation Measurement During the Flight of the
Second Cosmic Rocket
SUBMITTED:
8/020/60/130/03/oog/o65
B014/BO14
of about 20 kev and 106 ev electrons. The energy of the first
group is close to the mean energy of the solar corpuscular
radiation and allows to assume the existence of a thermodynamic
equilibrium between protona and electrons on their penetration
into the terrestrial magnetic field. It is pointed out that
the electron momenta of the second group are close to the pro-
ton momenta of corpuscular radiation and to the momenta of the
electrons arising from the decay of the reflected neutrons.
The existence of a lunar radiation belt could not be proven*
Constant radiation intensity was measured at a distance of
709000 km from the Earth, There are 2 figureeg I table, and
2 references, I of which is Soviet.
November 20, 1959
Card 3/3

B/020160/136/002/013/034
3019/W56
Tornov. S. X.. Corrospondtna Member of the AS USSR,
Chadakaw. A. To., Takulov. P. V.. e-h-k,r~ To. V.,
Logsob". To. I., &rA likolay", A. 0.
TITLE. adistion Mosouressents During %U Flight of %be Thard Coomdo
I
Rocket
PENIODICAL. Dotledy AW.mli msAk 35SR. 1960. Val. 136. NO. 2. pp. 322-324
raTt The ttlrd cosmic "4k*t launched an October 4o 1959 contained a
scintillation aountor And thr gas disc~argv counters. All a" diattarge
bad a sell strength :; 50 mg/c. .%.*I shoot. and -art. In .4di-
Tds. Ccantor I had a ;hl made fro.
me 2:w"und.4 by several oh
44 . I an alumIN11,01th counter ;;do :1.1, -blob was
closed by a 0.2 ma ths IL i"Immus 4be t. it. same hi*xd.
list without counter window$ and counter III was in an aluminum container
mode from 2.5 as thick alualnums. The scintillation counter recorded the
I.AlastIon of %b6 crystal (X&1) And the committee rat*. Preliminary results
of 4*91"tlon of the Instrument readings are given from the time from
Card 1/2
October 4. 1959. to October 10, 1959. The trw3sCtory of the rocket was in
Practical scrowswat with that or the first oad second cosmic rocket. ptos
& 00-Parls-a Of the readings of %he various counters. the author. conclude
that %he Intensities of the partieleM recort-4 by the Instruments d.pn4
an %ba absorptIcA In the container sells. Measurements In the
UrY GP4X* showed that the cosmic radiation An the boundary of the
tor"80-141 "gastla field I- very otrougg only Individual small fluctu4-
,,, 0 a war recorded. pleally, the Weea*nt existing bet-oott the recorded
Ist:nsilt 1:9 sad %b044 of 8 monitor are 44&1% with. rroa these considers.
tio" the authors draw the conclusion that the weak variations in the
t
I r otost
ime jTro Oct;b:,,.4 ta. 0b. ..r I- are I. .-..action with the waristiono of
%he Cm:t10 1 1 t lar system WO the interactions among %h*
letter Are connected with cosmic radiation&. There are I f1turo, i table,
And 3 3o-Iot references.
SUMITTEDs October 26, 1960
Cart 2,/?

VEMIOVJ S. N.,, GORCHAKOV, Ye. V., LOCIACHEV, Yu. I., ImTERoV.1 V. -,r,., PLIARENIM, N. F.,
SAVEITKO, I. A. and SHAVRIT4, F. I. -- -
"Investigations of Radiation During Flights of Satellites, Spa-.,~,
Vehicles and Rockets"
Report presented at the International Conference on Cosmic Rays
and Earth Storm, h-15 Sep 61, Kyotoj Japan.

8/169/62/000/004/067/103
D218/D302
AUTHORS: Bara'~zeyj L.T., Logachev, Yu.I., and Shishkov$ F.P,
TITLE-: A study of cosmic-ray variations at altitudes of
9 - 12 km
PERIODICAL:. Referativnyy zhurnal. Geofizika, no. 4, 1962, 13, ab-
stract 4G66 (V sb. Kosmicheskiye luchi, no. 3, M.,
All SSSR, 1961, 137-142)
TEXT: A report is given of the results of measurements of the ge-
neral, hard, and neutron cosmic-ray components at altitudes of 9 -
12 km, which were carried out from an airplane in 1959 and covered
the geomagnetic latitude range between 431 and 590N. The readings
of the instruments were recorded at intervals of five minutes. The
following values of the barometric coefficients were determined
from the altitlide variation of the intensity in the pressure range
750 - 220 g/cm~~ : (0 495 � 0.009)% g-1cm2 for the general component
(0 405 � 0.014)% g-l~M4 for the penetrating component and (0.654 �
O.i7)% g-1cm2 for the neutron component. At the altitude of 9 km in
the latitude range 520 - 600N, the latitude effect In the neutron
Vard 1/2

S11 6V62/000/004/067/103
A study of cosmic-ray variations D218/D302
component was (-2.4 � 1.1)%; the latitude effect was absent in the
general and hard components. At the altitude of 12 km and latitude
of 440 520N, the iatitude effect in the neutron component reached
(-14.7 1.6)%, while the result for the hard and general components
was (-9.0 � 1-3)% and (-6.3 � 0.8)% respectively. A reduction in
zhe intensity of all the components was found during geomagnotic
storms. In a number of cases the recovery In the Intensity of the
neutron component after the Forbush effect was incomplete. Moreover,
it was found that after the Forbush effect, the recovery of the in-
tensity of all the components to the normal level is faster at high-
er altitudeso (Abstractor's note: Complete translation).
Card 2/2

29879
(16 YF, In)) S/169/61/000/009/036/056
21, DO D228/D304
AUTHOR: Logachey, Yu. I.
TITLE: Determining the spectrum of electrons of the outer
radiation belt during the flight of the second cosmic
rocket (.11eptember 129 1959)
PERIODICAL: Referati-rnyy zhurnal. Geofizikap no. 9, 1961, 59
abstract 9G33 (Geomagnetizm i aeronomiya, V. 19 no* 1,
19619 30-33)
TEXT: A description is given of the apparatus,and the reaults of
investigation of the spectrum of electrons of the earth's outer radiation
belt by the second cosmic rocket are given. The recording of electrons
was accomplished by three gas-discharge meters of the type CTC -5
(STS-5). The differing thickness of the meters' screen permitted the
measurement of the intenaity of electrons with energies E ), 350, ',* 650,
and :~ 1100 kev . Simultaneous measurements by all three meters were
carried out in the altitu~de range of from 30,000 to 33,000 km from the
Card 1/2

29879
S/18QJ61/000/009/036/056
Determining the spectrum*@* D228/D304
earth's center. The maxivRia intensity of the outer radiation belt was
located at a distance of 179000 - 182000 km from the earth's center.
The particle flow recorded by the three meters respectively amounted to
(1.4 � 0.1) -106 , (3.9 � 0.4) -10 5 . and (5.5 ! 0.3) -10 4 evi-2 sec -1
It follows that the integral spectrum of electrons N(> E),%, E - I( has
the indicator Y - 2 in the interval 350 + 650 key and tho indicator
Y-3.5 in the energy interval 650 1100 key . For energies E
1500 - 500 key , Y is evidently-7 Evaluation of the spectrum of
electrons In the energy field 20 - 350 key gives a value of - 4 for the
spectrum indicator Y . It is shown that the contribution of roentgen-
radiation quanta to the observed counting-rate is negligible and that
this effect does not change the character of the spectrum found in the
energy field 350 + 1100 key . fAbstracteroB notes Complete tranalation-7
Card 2/2

34350
S120 Y, 611001100610021021
D055 D115
AUTHORSt Vernovo S.N.; Chudakovt A.Te.; Vakulov, P.V*; Gorchakov, Ta.V.;
Logache-r, Yu.1. ---------
TITLEr Radiation measurements in the outer radiation belt on
February 12, 1961, during the rocket flight towards Venue
PERIODICALt Geomagretizm I aeronomiya, vol 1, no 6, 1961, 872-874'
7EXTs The article deals with data on the Earth's outer radiation belt
collected when the Earth-Vanus rocket launohei. on February 12, 1961, was
30,000 - 45,000 km from the Earth's center. The special equipment Installed
in the hermetic container consisted of a scintillation counter and an M -5
(STS-5) gas-diachaxSe counter. The distribution of matter around the 1TaJ(Tl)
crystal and the gam-discharge counter Is shown in a table. By reducing the
dimensions of the crystal and increasing the resolving power of the else-
tronio system of the counter, the radiation Intensity in the belt was cor-
rectly registered. Fig. I shows the overload characteristice for the
counting channels of the scintillation (1) end gas-dioch&rge (2) counters.
Card l/q
7

S12031611001100610021021
Radiation measurements ... D055/D113
These channels could register up to 106 end 105 pulzationa/sec. renpactively.
To penetrate the crystal of the scintillation counter and the working volu=*
of the gas-discharl;e oounterl electrons must have an energy of '*> 3 Mev,
protons - an energ;r of N 32 Ifey and the bremastrahlung quanta - an energy
of ~~oL 30 key. Cu:rves on fig.2 represent the counting speed of the ocintil.
lation counter (I)p that of the gas-diacharge counter after corrections were
made aczording to the curves in fig. 1 (3) and the energy relea3e in th e
crystal In relation to the distance from the Earthtn center (2). An all three
curves wore more or lone parallel, the moan energy release in the crystal
for one reading of' the scintillation counter was 130 key and remained
constant botwqen !,2,000 and 40,000 km and the mean energy or the broma-
otrahlung quanta did not vary with distance. Tito constancy of the mean-
energy release showed that no great changes occurred in the spectrum of else-
trono of the outer radiation belt. A diagrep Mg. 3) shows the paths of
the interplanetary rocket (curve 1) and those of another three Soviet rockets
(curve 2). A comparison of radiation and ionization data concerning the
interplanetary rocket and the space rockets no. I and 21showed that the
outer radiation belt was stable for a period of 2 years when no magnetic
perturbances were recorded. However, this period was not lone enough to
Card 2/6

S12031611001100610021021
Radiation measurements ... D055/DI13
evaluate solar effects on the outer belt, but could be taken as an indication
of the absence of ouch an effect, The space rocket no 3 was launched during
a moderate magnetic storm (the change in the vertical and horizontal compo-
nento of the torrentrial magnetic field was about 250 and 150Y respectivelA
The external aide of the belt was not moAoured, but the total eyorgy re-
lease in the crystal during the entire flit;ht coincided with that calcu-
lated for the rocket no 1 and was 1.5 times less than that of the rock,~t
no 2r i.e. no ohanSeu occurred in the mean state of the outer zone during
the flight of the rocket no 3 during a moderate maCnetio storm. Since
measurements were atmrted a few hours after the bei;inning of a caGnatic
ntorm, the radiation intensity in the belt had not yet decreased. On the
other hand, it in also possible that not all magrotic storms cause the
radiation intensity of the Farth'a outer radiation belt to decrease. There
are 4 fiKirea, I table and 5 non-Soviot references. The three English-
language references are: W.H. Ilene, J. Ceophyn. Hou.,1960, 65, no 10, 3107,
F. Rothwell, C.E. McIlwain. J. Ceophyj. Ran., 1960, 65, no. 3# 79);
R.L. krnoldy, R.A. Roffman, J.R. Winckler, J. Geophys.Res., 1960, 65, no 5,
1361.
Card 316

3120316110011006100210,",
Radiation measurements ... DO!5/DI13
ASSOCIATIONt Moakovokiy gosudaratyennyy univeraltat, Inatitut y.ldnrnoy
fiziki (Moscow State University, Institute of Nuclsar Physics)
SUBMITUDs Soptember. 9, 1961
Card 4/6

34352
S/203/61/001/'006/004/021
D055/Dll3
AUTHORS: Vakulov, P.V.- Goryunov, N.N. Logachev, Yu.--., and
V V -
Sosnoveta, E.N.
TITLE: Radiation registered during the flights of Soviet artificial
satellites and space rockets
PERIODICAL: Geomagnetizm i aeronomiya, v.1 , no.6, 1961, 880-887
TEXT: Methods of registerin- radiation, based on the use of scintillation
and gas-discharge countero and applied in Soviet artificial satellites and
space rockets,are described. The registration of weak currents (Up to 10-10a)
with the aid of a relaxation oscillator on a neon tube is described. The
scintillation counters measured the number of particles releasing more
energy in the cryotal than that determined by the thresholds of the counting
devices. Ionization caused by radiation in the entire crystal was also
measured. The gas-discharge counters registered charged pa:-ticles and
radiation to an accuracy of ~ 1%. The counters were located behind screens
of various materials to facilitate the analysis of radiation according to
Card 1/3

S/203/61/001/006/0()4//021
Radiation registered ... D055/Dll3
penetration. The devices with the counters werQ located both inside and
outside the container with scientific apparatus. For economy the photo-
multipliers in the counters were fed without a divider by leads from a high-
voltage battery direct to the electrodes. Ionization was determined from
the cur2ents of the anode and seventh dynode. By using two channels, thes'~
currents could be comDared in order to estimate how much of the energy pro-
duced in the crystal resulted from saturation of the anode current during
intense scintillation in the cry3tal. By this means comparatively high-
energy particles could be detected in the inner zone during tests with the
third artificial Earth satellite. The use of a single scintillaticn ~~ounter
to measure many parameters permitted the weight and size of the device to bo
reduced but required careful selection of photomultipliers, which had to
satisfy the following requirements: (1) there must not be more than one
sound impulse per 10 see. corresponding to energyliberation of above 30 keN
in an NaJ(TI) crystal and there must be practically no imnulses corres-
ponding to energylib 15 ral6on of > 300 kev; (2) leakage current of the
seventh dynode 1-10- a; (3) anode dark current 4 1.10-6 aW) leakage
current of the Sher dynodes of the intervals < 1-10-7 a. The le-5(STS-5)
Card 2/3

S/203/61/001/006/004/021
Radiation registered ... D055/Dll3
gas-discharge counters used-were small and had a low operating voltage
400 v) and a thin wall, which facilitated the recording of low-energy
particles. The electronic circuits operating on semi-conductor elements
and the calibration method are described in detail. There are 9 figures and
5 Soviet references.
ASSOCIATION: Moskovskiy gosudarstvennyy universitet im. ?J.V. Lomonosora.
Institut yadernoy fiziki (Moscow State University imeni
M.V. Lomonosov. Institute of Nuclear Physics).
SUBMITTED: October 12, 1961
Card 3/3

S/058/62/000/0 10/0 42/093
Ao6 1/A 10 1
AUTHORS: Baradzey, L. T., Logachev, Yu. I., Shishkov, P. ?.
TITLE: A study of cosmic ray variations at altitudes of 9 - 12 km
PERIODICAL- Referativnyy zhurnal, Fizika, no. 10, 1~62, 61, abstract IOBII56
(In collection:: "Kosmicheskiye luchi, no. 3", Moscow, AN SSSR,
1961, 137 - PIP, summary in English)
TEXT: This is a report of results'obtained from measurements of the total
intensity, the intensity of the penetrating component, and the neutron intensity
at altitudes of 9 and 12 km (pressure 310 and 197 g/cm, respectively). The meas-
urements were conducted In two groups of airplane flights from March 20 to May
18, 1959, and from October 15 to December 21s, 1959.. An intensity drop for differ-
ent cosmic ray components, correlated In time with the magnetic storm periods,
is noted. The drop of the neutron Intensity is the greatest: (-16.~~ .)I) and
J-13.1+05M at altitudes o:? 12 and 9 km, respectively. The intensity drop of
total and penetrating radia-~ions is ofabout equal magnitude: (-12.0+0.3) and
(-8.740.5)% at 12 and 9 km, respectively. The intensity drop after magnetic
Card 1/2

S/057/62/000/010/042/093
A study of cosmic ray variations at... A061IA101
storms grows with altitude according to approximately the same law for all re-
corded radiations.
[Abstracter's note: Complete translation]
Card 2/2

LOGACHEV, Yuj.(translator); TRI.OFEYLV, G.Ajtranslator]; GC1110,11OV.0
Ye.V.T lator]; ASTAFITEV, V.A.[trarslator); SAVIN, B.I.
[translator]; SUBANSM, V.P., red.; FAFTAYIEVA, II.A., red.;
DUBKOVAp S.I.p red.; PAID,11ITSEVA, S.V.,, tekhn. red.
(solar corpuscular Dtreann and their interaction with geo-
ragnetic fiold]Solnechnye korpuskuliarnye potoki i ikh
vzaimodeistv:ie s ragnitnym polem Zer.-Ii. Moalma. I:A-vo
inostr. lit-ry, 1962. .438 p. Translated from the Englisb.
(1,11AA 15111)
1. hauchno-ionledovatellskiy inatitut yadernoy fiziki Mo-
skovskogo gosudarstvennogo universiteta (for Logachov,
Timofeyev, Gorchakov, Astaflyov, Sevin).
(Solar rndiation) (Magnotim, Terrestrini)
ij

PISARMO, N. F., SAVENKID, I. A,, CHUDAKOV, A. Ye., SHAVRIN, 11. I.J9
VERNOV) S. N., GORCHAKOV, E. V.,ILOGACEX-T---Y-u. I., NESTEROV, V. E.,
"Investigations of Radiation During Flights of Satelliteo, Space
Vehicles, and Rockets"
Soviet Papers Presented at PlenaryMeetings of Committee on Space Research
(COSPAR) and Third International Space sumposium, Washington, D. C.)
23 Apr - 9 May 62.

VFII!Irjv, "(''r V.,
CIMIAKOV, Alak Y'. VIA V. Y'-.
"Mm emrtls'n J-q.jjpjj.jr:n
report to be cubmittf-d to th- 13~lh TWA. TAF,
VeLrna, Dulgirin, 23-21) S-:1)

-" "";A, '1~
S/046/62/026/006/013/020
B125/BIO2
AUTHORS: Vukulov, P. V., Vernov, S. N.,Gorchakov, Ye. V., LoBachev,
Yji- T-, Neeterov, V. Ye., Nikolayev, A. G., Pisarenko ',
N. F., Savenko, I. A., Chudakov, A. Ye., and Shavrin, P. I.
TITLE: Radiation Studies during the flights of satellites,
spaceships and rockets
URIODICAL: Akademiya nauk SSSR. Izveatiya. Seriya fizicheskaya,
v. 26, no. 6, 190-2, 758-781
TEXT: This report deals with radiation measurements m!lde by the second
and the third Soviet spaceship, by the rocket launched toward the Venus
on February 12, 1961, and by the third Soviet earth satellite
(August 15, 1958). The spaceships were equipped with scintillation
counters, gas dii3oharge counters and elements for storing data through
24 hours. The northern and southern zones of increased radiation
intensity are undoubtedly linked by the lines of force of the geomagnetic
field. The increased radiation intensity is due to electrons of the
outer radiation belt, slowed down in the jacket of the spaceship. The
Card 1/3

S/048/62/026/000'/613/020
Radiation studies during the flights ... B125/B102
boundaries of this belt mere determined more accurately by the lower
orbiting Soviet spaceship. At 16 hours after the chromosphere flare of
June 17, 1958 had vanished but still a few hours before the magnetic
storm, charged particle intensity increased. The electron spectrum
of the outer radiation belt does not change much at an altitude-of
32,000-40,000 km, nor did the magnetic storm which occurred during the
flight of the third Soviet spaceship have any substantial effect on the
outer radiation belt. Except for a few percent, the proton intensity of
the inner radiation belt remained constant during the three weeks' flight
of the third Soviet satellite. The increased radiation intensity over
the Brazilian anomaly, observed on board of the second spaceship at an
altitude of 320 km, was due to the inner radiation belt. In this anonaly,
the proton component of the 'inner radiation belt is predominant at small
,-,eoma,jnetic latitudes. 4~he portion of X-rays increases with increasing
latitude. A zone of lower bromBBtrablung intenuity separLtea the outer
from the inner radiation belt. This zone is prautically absent in the
region of the Brazilian anomaly. T~e equator of cosmic rays determined
by 'he second and the third Soviet spaceship resembles remotely a sine
curve running between 110 of northern and 110 of southern latitude.
Card 2/3

Radiation studies during the flights ...
B/048/62/026/006/013/020
B125/B102
Between 600 western and (100 eastern lon-itude the equator of cosmic
U
radiation lies north of the theoretical sine curve. The General trend of
the lines of equal cosmic radiation intensity corre-aponds in general to
the distribution of magnetic rigidity. There are 16 fi,,~UrEs and 2 tables.
ASSOCIATIO41: Nauchno-isoledovatellskiy institut yadernoy
1.1oskovskogo Cos. universiteta im. _*.:. V. Lomonooova
(Scientific Research Institute of Nuclear Physics of the
Moscow~ttate University imeni MI. V. Lomonosov).
Fizicheaki,y institut im. P. N. Lebedeva Akademii nauk SSSR
(Physidd Institute imeni P. 11. Lebedev of the Academy of
Sciencea.USSR)
Card 3/3

VAKULOV, P.V.; VLTUIOV, S.N.; GOIRCHAKOV, Ye.V,,; ILL-aE-V, YRk.; NMThROVj
V.Ye.; NIKOIAUX, A.G.; ?1S1'-:U21KOj N.F.; SAVETKO, I.A.;
CIIUDAKOV, A.1e.; SHMMI., ?.I.
Study of radiations recorded In flights of artificial satellites,
cosmic vehicles, and rockets, Izv. AN SOMR. Ser. fiz. 26 no.6:75E~-781
je 162. OURA 15:6)
1. Nauchno-issledovateltakly inatitut yadernoy fiziki Moskovskogo
goo. universiteta im.M.14monosova I Fiziclieskiy institut im.
Lebedeva Akademii nauk SSSR.
(Van Allen radiation belts) (Artificial satellites)
(Spaceships)

L 0 6~-,oq-C- ff-'
V TZRNOV, S.N., OOWR&WV, 71.T.,,jPWFkV,_TV.I.
CNAMMU, T.N., CWJUMV, A. 71.
'Cooda rd" idtimi'stratoophere and their oormlmUon idth
solm 44uvity.
is"rt be sabod,ok for go&" lbseareb Constittes on OWAR 6th
PION17 "OUR$
Waromp IF*IsM U Jew 63-

F3F(h)1F35,-21E;v4(j )IFS( s) /"PA( b
-6 A
~7"
A 14 L
AUTHORt Vernov.- S~ ~,o r c h a k ov
Ye. V..' Lop-achav Yu.'I.; ~~L!n2v, P.; Hikolayev, A, G
TITLE: Investigation of cosmic radiation during the flight of the
1-fars-1 and Hoon-4 a &,ae stations
S01JRCEt Kosmichaskiya issludovattlye, v. 2, no. 4j 1964, 633-640
TOPIC TAGS: cosmic radiation$ space stettion, tiara 1,, tfoon 4, Earth
radiation baits scintillation counter, gas disch rge counter
-rY
ABSTRACTi Recordings of cosmic-radLation intensity beyond the Earth's
Magnetic field made during the ftightsof Hars-1 (20 Nc,vember 1962 to
25 January 1963) and Hoon-4 (2-1,4 April t963) ace discussed. Data an
the Earthes radiation belts received from :Hars-l and date on
the cosmic-ray intensity during various cycles of solar activity
are given. The equipment aboard Hara-1 consisted of two scEntillatior
and two Geiger gas-discharge counters. It Vag discovered that the
intengltv of cosmic zadiation remains practically constant beyond a
dt5tance of G.Z4 astionomical unkts. Duriag the fl'.ght of Koon-4,
--d 1/2

L 7o44-65
ACCESSION Nki AP4043504'!
0
slow and amoott--i variations in cosmic-city intensity connected vith
changes of the magnetic situation in the. solar syetem were recorded,
The particle ftwxes in Che radiation beLts recorded 13-y HarLx-l
are &Lven. The average energy yield In the crystal of the scLntit-
lation counters for a sirale count was about 2 Kev. 0-.Lg. art. hast
5 figures and 4 tables,
ASSOCIATIONt none
SUBMITTED: 30Jan64 ATD PRESSt 3104 ENCLi 00
SUB CODE: AA, SV NO REF SOVt 002 OTHER. 005
2~2

L 21116-65- ZZC-4/~"116 (,r)1bWA(h)1ViT(l)19ZC W/FS (Y)-31E&C (m)1FCC1FSF(h)1FS1S
pe-57p-C-4/pi-4/pl-4/po-,'+/Fq-4/Pae-2/Pob/Pb.4 A DC(b)/BSD/ArwL/S5D/AuD(s)-5/
AZDC(&)/AFI-',D(C)/AF=R/AFTC(&)/AYTC(b)/APGC(f)/ESD(B*i) TTIG'dlwS
ACCESSION HRz AP50021.06 S/0048/64/028/012/2038/2074
AUYHORI V4rnov, S. K.; Chud&kov,__&,_Xeg VAku'lqy orchakov.
V.; G
I rn4t y4v P. P. ; Kuzn a to ov, S. N. I j2AASUX6_Uo I- LYM~_km_*X,__
Okhlopkov'. V. N,j Tornovskay
ASV-4t t a _ks_
14. V.,
TITLE; Rsdiatio'.~f'itudy by qqgRFLq_l.7\:/ [Report presented at the Vat-
(All-Union
goyuznoye moveshchaniya po fL&Lke kossichookikh luchey
-Confarance an the Physics of CosmI4 Rays), hold at Hosaaw, 4-10 Oct-
~obar 19631
'S0URCZ3 AN SSSR. Isvestlys. .89riyA fisichookayas V, 25, no. 12,
1964, 2058-2074
!TOPIC TAGSs radiation m:aproment, spoesborne:lonLastion measurement, .;I
Iprimary cosmic radiation gas discharge cauikt4r/
.STS-5 gas discharge counter, Cosmos-17
ABSTRACTs The article describes equipment used In'the flight of
Cosmos-17 I (&pogaeo-788 km; perigee, 260, ka) for Investigating the'
Earth's radiation belts *ad prim vy cosmic radiation,. The equipment
.consisted of tva scintillation C:uators (with vat and GIZ crystals) and
Cavd.11 t

NEW
L 21116-65
AMSSION NRt AP5002106
a STS-5 gas-discharge counter. Ths, cylindrical Mal counter (20 X 20 an)
was mounted under the shell cif the satellite and was fitted with
aluminum shielding (I a/CS2). On one channel it recorded ionization
produced *in the crystal by radiation% on the two others, it registered
the number of pulses vLCh energy release in the crystal over the
specified threshold* (50 kav - and The effective cross
:&action of the Mal crystal for Particle$ rog"t"S d along the loniza-
ition and'.first threshold channals-was opprox.. 4.?_cm2j.for Cho secondi
;channel, it was roaghly 5Z smaller for particles with quadruple ioai~
:x&tion and 20Z smaller for relativistic particles.
The STS-5 gas-discharge counter has an effective cross section of
4.3 cmZ. It was placed inside the device containing the sciotillstioo~
counter and was not fitted with any special protection. Up to count-i
Lag rates of 3 x 103 pulse/see, the counter registered virtually all!
particles. At higher ratdj6 the count became less reli4b'.**
The flat Cal counle:(cryst&l dLattator, 6 nag thickness, 3 on) wag
mounted oucaLde the container. 'for protection from light, the crystal'---
was covered with aluminum foil (2 us/ca")o For protection against

L 2ill6-65
ACCESSION NRt AP5002106
bramostrahlung, the photomultiptior and the crystal were shielded
with 5 mm of lead and 11 ma of aluminum, except for the front of the
photomultiVILer, which had a conical opening for particle Incidence
(aperture eagle, 40'). This counter carried out ionization measure-
meats and particle registration at energy release in the crystal of
45 and 160 ket and 5.4 and 8.5 Hav.. Both electrons and protons could
be registered along the first two (45 and 160 Kov) channels. Along
the other two 45.4 and 8.5 &Y) channels, the count'vae maAall of pro-
tons; at an electron path perpendicular to the crystal surface enerity
l'onaos* wars' about 2-)1*v*iod,*bl1qus-patb# ware-*-pro'cludiod by*;h*.thick--t
uses of the shielding.'. Tabli I of the-Enclasure gives the RLOLIEWti-
partlile
tablevand,4-foraulovz-
ASSOCIATION$ none
'Card 3/5--

;E,7, -, V,
VEITIOV) S.N.; CHUDAKOV, A.Ye.; GORCHAKOV, Ye.V.; LCGL[;IIET,' Yu.--.; 111 17".0
..
V.Ye.; SIMEMKO, I.A.; SHAVRIN, P.IO
Radiation belts of the earth. Geofiz. biul. no.~11:9C-108 164.
(mIRA 19:4)

VAKULOV, F.V.; GORCHANCV, Ye.V.; LOGAGREV, Yu.I.; CIIUDAKOV,
A.Ye., doktor fiziko-matem. nauk, otv. red.; ISAKOVICH,
T.D., red.
[Collection of articles] Sborn1k statel. MoAva, Nauka.
No.6. 1965. :-12 P. (MIRA 18: 5)
1. Akademiya rmuk SSSR. 1,ezhduvedoiTstvenrVy komitet po
provedeniyu %,',ezhdunarodnogo geofizicheskogo goda. VII raz-
del prograuxW IAGG: Nosmicheskiye luchi.

VAr"
-2
09977 'P 'C 'it)(
A
T504 jo. Q~
ri
jT110-R- VerApjv~!~!_ N.', ChiAS~_.tivA. Ye. Corchakov,_Ye. V., loqpchav, Yu. I., 6?j-1
Ye. so ko, E. A. ghav-rtn, P, 1.
th
T 1 YL E The radiaLion belts of the Ear
SOMCE, M SSSR. Mezhduvwfo=tvvnW geofitiz'~Xtskiy kamitet. GeGfi-siateskiy
_11TOPIC TAGS: radiation belt, radiation belt anomaly, cosmic ray measurement, Mars I
n& 4 satellite
iqatellite, 1~q_
ABSTRAXT- This survey article, based mostly on published Soviet and Western papera~
discusses the discovery and study of radiAtion belts, outlines their structure,
!describes the discovery of radiation belt anomalies, and presents so-me result of
the s tudy c-f con-mic rays be"ad the boundaries of the magnetoophere. This l#:t
~n-nr zrcph3 describing the intensity of cosmic radLaticn recorded by sta-
li__ M,
E~ I as - function of its dtaranc~, from the Sun, the couatLng rate of the
-3-uli-6charge counter STS-5 ort Mars 1 an,11 Lite Etr to ere 646 la,itwde) over
aph ht
v T&FuEi;:~)7r
fend rhe (ounting, rate OC- the STS-5 counter
t unn 4 cotellitc atetion and in the arrr_~au~phctrc durIng the ftrat haLf of
i ~,,f 1963. Orir,. art, hae- 16 figures and 2 tablea.

L 3281-66 FSS-21VE M73/FC~/DIA(d)/~'WA (h) V~IGSICjW
!ACCESSION NR: ATS0236111 UR/0000/65/000/000/0425/0433
'AUTHOR: Vernoy, S. N.; Chudakov, A. Ye.; Vg ~iv KuKq~~tso
':Logachev, YM. jg=yPts, E. X Stolpovskly, V. G.
TITLE! Irregular flows of high energy electrons close to the boundary of t"he
earthis,radiation belts
SOURCE: Vsesoyuznaya konferentsiya po fizike kosmicheskogo_2E2pjrans va. Moscow
1965. Issledovaniya kos-mfc-heskogo prostranstva (Space research); Trudy konferentsii.
~
Moscow, Izd-vo Nauka, 1.965, 425-433
TOPIC TAGS: geomagnetic field, satellite data analysis, radiation beltV_.1_
ABSTRACT: The authors analyze data obtained from "Elektron-111 and "Elektron-2" dur-i
ing their first month of.operation. The equipment used on the satellites is brief
described. Analysis of data pertaining to the midnight meridian indicates that th
intensity of thd electrons at the boundary of the oiiter*belt decreases by two or .`1_
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 terminates on quiet
days at L = 6.5-7.5i On th e day side, the boundary of the belt extends on the
Cord 1/2

L 3281-66.
.1ACCESSION NR: AT5023614
average to L 9-io. (Here L is the nominal McIiwain parameter calculated in the
dipole approximation and expressed in earth radii.) It is found that irregular
I
flows of electrons outside the boundary of the earth's radiation belts appear with
an increase in perturbatLon of the geomagnetic field both at the surface of the
earth and at distances ol 100,000 km from the earth. A theoretical explanation is
.1given 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-1, table. (14]
1ASSOCIATION: none
ENCL*: 00
SUBMITTED: 02Sep65 SUB CODE: ES.SV
10-REF SOV:' 002
I Card__ 2/2

L 1552-66 FSS-2/&n(l)/FS(v)-3/FCC/EWA(d)/EWA(h)-,---T,T/GS-/GW-
ACCESSION NR: AT5023628 UR/0000/65/000/000/0502/0506
AUTHOR: Vernov. S. I.: Valtulox... P. V. Zatsepin. V.-L; LoY_ache_v_,__Yu-
Okholopkov, V.'P ;4' tA-1c,~ 'i, (~o 0
I't 1 5 5" q Y'5 ir
TITLE: Primary cosmic radiation investigations&
-SOURCE: Vae'soyuznaya konferentsiya po fizike ko MLOjeskogg
__ 9 Mg!Lrans t'v'Moscow,!
1965. Issledovaniya kosmicheskogo prostranstva (Space research); trudy konferenteii..
Moscow, Izd-vo Nauka, 1965, 502-506
TOPIC TAGS: cosmic ray, coamic radiation, primary cosmic ray, primary cosmic
radiation, Elektron 2, qlektj rL4
ABSTRACT: Experimental data obtained by Elektron-2 and -4 on primary cosmic radial-
tion are presented and interpreted. The data, covering the period 30 January to
I November 1964, were obtaitted primarily by means of gas-discharge counters with
an average frequency of 20 pulses/sec. The apogee of the satellites was 68,000 kM'9__
keeping them outside the 'earth's radiation belts most of the time. The higher
count frequency as the thickness of the screens was.incrieased, made it possible tol
conclude that the primary radiation did not contain particle's within the 50 to
110 Mev range. Two types of radiation intensity variations were distinguished:
Card

L 1552-66
ACCESSION NR: AT5023628 0
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 and the intensity of cosmic rays
were discerned in the sequence of monthly averages of the intensity of cosmic
radiation, the relative number of solar spots, and the 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 amplitude periodically acquire
a clearly cyclic character. ilie same observation was 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 obscure. 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 casas (rotations 1792, 1793, and 1794) there was a fair
indication of parallelism. The absence-of a conclusive connection with the*ounte
rotation suggests the posalbility.that the short-period variations have a common
Card_ 213

L 1552-66
ACCESSION NR- AT5023628
iorigin with the 11-year variations. It is also possible that the intensification
of coamic radiat'ion during decline of solar activity is not monotonic, but displ4ye
ups ajid downs stemming from changes in the condition of its propagation orAimansibno
of tho region of its effective scattering within the solar system. Grig. art. I
1has% 4 figures. (FP]
ASSOCI*,ATION: none T-n
SUBM11TED: 02Sep65 ENCL: 00 SUB CODE: AA, SV
NO REP SOV; 003
OTHER: 001 AT D P RE 5 SIf Pat -TL.
-4 If

L 1553-66 FSs-21owr(I)IFS(y)-31FCCIEWA(d)IF.4A(h) TT/GS/GW
ACCESSION KH: AT50236io uR /oooo/65/000/000/030/003
AUTHOR. YsxaQr,.,".; Chudakay. A. Tgj; Vakulov P. V
znetsov. S. K.- - ."Alk:
Ku E. N
=-Ju- .. Q,
W6jfn-9-ht-e-Yn= d1P'6vskiiV. 0.; Ellteko 5'Y) about 2-3 pulses were recorded
by the low-frequency circuit and about 1 by the high-frequency circuit., It is
noted that the number of magnetic field pulses with the amplitude t5 ~ is
generally greater in the frequency region of 1-10 cps than in the region 6f 30-300
cps and that the pulse intensity tends to increase in some geographical regions*
Normally, this increase is recorded by the low-frequency circuit but not by the
high-frequeney one. [041
iASSOC IATION t none
iSUBMITTED: 02Sep65 ENCLx 00
NO REF S071 000 OTHERt 000
Card 2/2
SUB CODE: E51 8V
ATD PRESS:

I h) TT/6W
iL 17777-66 EWT(l)/FSS-2/FCC/EWA(d)/hWA%
;Acu WK: AF 006652 SOURCE CODE: UR/0203/66/006/001/0003/0010
Logachev, Yu. I.;
AUTHOR: Vernov, S. N.,_Driatakly. V. M.; Kuznetsov. S. N.;
ISosnovets, E. N.; Stolpoy kiv,,Y._Q._
ORG:
111atiWC Qf ftc (Mosko'
vskiy goBudar
istvennyy universitet.Institut yadernor fiziki)
ITITIX: Behavior' of the radiation belts~lnd anomalous absorption of cosmic radio
,noise in the aurora borealis region during the magnetic storms of 12-14 February
.and 20-21 February 1964
SOURCE: Geomagnetizm i aeronomiya, v. 6, no. 1, 1966, 3-10
TOPIC TAGS: cosmic noise measurement, radio wave absorption, aurora, magnetic
storms radiation belt, magnetosphere
ABSTRACT: The authors make a direct comparison of electron fluxes with differing
energies in the outer radiation belt during various stages of geomagnetic disturb-
ances. The data used in this study were those transmitted by the glectron-1 -1~-and
' _i
Electron-2 ' satellites during the ma and 20-21 ebruary 1964d
Ine-t1c, storms of 12-14
VY
UDC: 550.385.41:621.391.81
!,Card 1/4

L 17777-66
;ACC NR; AP6006652
!These were relatively weak storms with an abrupt onset. The outer radiation belt
!behaved differently In each of these cases in spite of the fact that the storms
1were approximately Identical with respect to the amplitude of the main phase. Pc
oscillations with a period of approximately 40 seconds were observed on the day of
the first storm, indicating a quiet magnetosphere. During the first hour of the - I
storm, an electron flux of N,%,1.5xlO8 cm2/sec/kev was observed at a distance of
approximately 10 Earth radii. This region lies far outside the radiation belts of
the Earth,and the flux was apparently due to the storm. The magnetic field increas
ed in this region during the first phase of the storm. Electron intensity decreas-
ed somewhat after the initial phase. Electron-I data gave the boundar-
y of the
outer radiation belt on the night side as L = 6.5-7 before the abrupt onsei of the
storm, while the data of Electron-2 gave a value of L = 7.4. Data from these
satellites gave L = 5.5-6.8 and L = 5.9,respectivelylafter the initial phase of the
~Storm. This may be explained by compression of the magnetospbere. The period of
Pc oscillations after the initial phase was approximately 20 sec. The pe-riod.
of the Pc oscillations was reduced to 16 see when the boundary of the radiation belt.--
hifted to L,= S. There was a faster increase in the flux of electrons with ener
gies greater than 40 kev during the main phase of the storm than there was in the
;inte"nsity of electrons with energies greater than 150 kev. The basic data for the
'Card-2/.4

L 17777-66
,ACC NR: AP61006652
'storm of 20-21 February were those transmitted by the Electron-I satellite. Thes
idata show that the boundary of the outer radiation belt was at L = 6-6.5 before thei
~storm. The period of PC oscillations was approximately 50 sec. During the
Ifirst phase of the storm, the boundary of the radiation belt was registered as L=5
jand the period of PC oscillations was 14 sec. An intrease in the intensi 'ty oV
)the magnetic field was observed at a distance of approximately 10 Earth radii. Thes4
'data indicate compression of the magnetosphere. Low-energy'electrons appeared at
igreat distances from the Earth during the first phase of the storm. Data from 10
Istations were used for studying the absorption of cosmic radio noise in the r 'egion
:of the aurora borealis. The first burst of auroral zone absorption was observed
;on the day side of the Earth during the first phase of the storm. This may .,Pe due
~to the fact that the boundary of the magnetosphere was approaching theEarth.' The
Iamplitude of anomalous absorption *Increased from 0.1,db to.1%4.5 db when the bouna-
ary of the radiation belt moved from L = 5.6 to L = 9.6. Beyond this point)there I
was a reduction in auroral zone absorption. After the initial phase, no more such.
trong "bursts" of anomalous absorption were observed until the development of the
main' phase. Anomalous absorption was again observed during the main phase but thisi--
time with no clear relationship to L.- An analysis of thi data shows that ele tronsi
,s firatcph lei
Apour out of the radiation belts on the day side of the earth during the at
jCard 3/4'

L,177r
ACC NR: AP6006652
of a magnetic storm. This is indicated by the reduction in electron intensity in
the maximum of a belt and at higher values of L. Evaluations show that during the
first phase of a storm the mirror points of electrons in the outer radiation' belt
may move several hundred kilometers closer to the Earth. Anomalous absorption in
the auroral zone may be.observed between the first and main phases of a magnetic
storm. However, in this case they are accompanied by various effects in'the radia-I
tion belt region. A comparison of data on auroral zone absorption and the behaviori
~of radiation belts shows that anomalous absorption is sometimes accompanied by a
reduction in intensity in the belt and sometimes by no changes at all or even an inI
crease in the number of particles in the belt. More data are needed on auroral z=4
absorption around the -entire Eirth", and at L -e- 4. Orig. art. has: 9 figures. [141
SUB CODE: 08/ SUBM DATE., 03Aug65/ ORIG REF: 005/ OTH REF: 004
ATD PRESS. q.&oY
Card 4/4f0

-SWRC-E --C O'DE--:--
ACC NR- iP603O0i6---
AUTHOR: Vernov, S. N. (Corresponding member AN SSSR); Vakulov, P. V.: Gorchakov. Ye. V.,-
Lo&achev,,Yu. I.; Lyubimov, G. P.; Nikolayev, A. G.; Pereslegina, N. V.
TITLE: Measurement of intensity of penetrating radiation on the Moon's surfaceNle, is
[Paper presented at the Seventh COSPAR MeetiN- held in Vienna in iiay 1966.1
SOLECE: AN SSSR. Doklady,--v. 16~, no. 5,--1966., 1044-1047
TOPIC TAGS: moons, radiation intensity, lunar probe, radiation measurement/
Luna-9 lunar probe
ABSTRACT: The lunar probe 'Luna-2 launched by the Soviet Union on 30 January 1966
maae''a soft landng on the Moon on 3 February at 24 hr, 45 min, 30 sec
(Moscow time); it was equipped with an instrument containing a 6 x 10-mm
d1scharge counter to measure the intensity of radiation. The minimum
shielding ;f the counter mounted inside the probe near its jacket was 1-1 gni/CM2.,
The instrument was switched on immediately after "Luna-9" was put
Into orbit and was kept in operation until the pro%~topped functioning. The
data on the intensity detected with the gas counter\ averaged over 14 time
intervals are shown in Fig. 1. The first five time intervals are those for the
flight from the Earth to.the

It k R:__ A-P-6-0-3-0-0-1-0--
Moon. The next (sixth)
interval
is that for the flight near the
coum/~_
Moon (beginning with at a dis-
tance of %,50, 000 km from the
Moon), the landing, and the
first 5 minutes on the Moon' s
surface. The subsequent eight
Intervals are related to operations
Time of on the Moon' B surface. Table I
landing shows the accurate values of the
Measurements du Measurements time intervals and the mean-
the f bight tIo the Moon Ion the Moon count rates recorded in these
jIt IS 29 liff /is I mod intervals. The basic errors in
determining the count rate are
statistical.
Fig. 1. The mean-count rate of "Luna..;9"
discharge count *e'r
The data In Table I show that the mean-count rate recorded on the
Moon, s surface was about 6316 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
much as during the flight in free space. The detected excessive radiation
Card 2/8
~Nffl==X_ RR twl WTEV
OW
~TM

~R_,'~_-,A-P6030010'
X
tc
Interval boundaries Averaging interval Mean-count 11
rate Note
31 Jan 1966 18 h 38 min 40 aec 10 h 12 min 3
0 sec 3.2290.010 Duringthc
1 flight
1 Feb 1966 04 h 51 min 10 see 10 h 54 min 20 see 3.2770.010 to
' 15 h 45 min 30 see
23 h 01 min 45 oce 07 h 16 min 15 see 3.2670.011 to
2 Feb 1966 16 h 29 min 00 see 17 h 27 min 15 see 3.278'0.007 to
3 Feb 1966 15 h 34 min 15 see 23 h 05 min 15 sec 3.28610.006 if
21 h 50 min 00 sec 06 h 15 min 45 -sec 3.24510.012 Near the
Moon and
on to M~on
4 Feb 1966 00 h 06 min 54 see 02 h 16 min 54 see 2.0650.016 Da the Hx)n
06 h 35 min 04 see 06 h 28 min 10 sec 2.0690.010 it
17 h 02 min 00' sec 10 h 26 min 56 see 2.07410.008 it
19 h 52 min 30 see 02 h 50 min 30 acc 2.07710.014 Is
5 Feb 1966 04 h 00 min 40 sec 08 h 08 min 10 see 2.05810.009 to
19 h 01 min 40 see 15 h 01 min 00 see 2.05510.006 to
20 h 37 min 30 see 01 h 35 min 50 see 2.05910.020 to
22 h 42 min 20 see 02 h 04 min 50 see 2.059t0.017
The mean-count rate during the flight is 3.27Z'0.004
The mean-count rate on the Moon is 2.06410.004

ACC NR; AF6030010 ------
is 0.43 count/see or .261/o 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 rndintion In
the matter on the Moon' a surface region closest to the station (cosmic-ray
albedo).
Until nowi no experimental data have been availa'ble on the radioactivity
of the Moon's surface. The "Luna- 9" measurements make it possible ko
evaluate the zadloactivity of the Moon' s gurface in the landing area near the
Ocean of Storms. Assuming that the total detected additional radiation is due
to the radioactive gamma radiation from the Moon' s surface, the radio-
activity of the Moon' E; surface may be -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 multiplica-
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 2076 of the total cosmic-ray flux or 4076
-of half the cosr.,iic-ray flux. Additional considerations show that at least
,in the region of the "Luna-9" landing, cosmic rays will be the m*a'ln source
Card 4/8

ACC NR, AP6030010
.of radiation hazard and that the radioactivity on the surface of the Moon is
iclose 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 from the Moon' a
surface, the intensity of the radiation trapped by a possible lunar magnetic
field does not exceed 1076 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 rate 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 radiation de-
tection on the Moon's surface (this correction is about 176), the resulting
count rate is 3.28 count/sec. This practically coincides with previous
measurements. The time required for the "Luna- 9" to cover the last 1000 km
,to the Moon' s surface was '- 2% of the time measured in the given interval.
At the measuring accuracy mentioned above, an increase of 5076 in the count
rate during this time interval would be noticeable.
Card 5A
0;~

ACC NR: AP60300!0____________ 7
Thus the upper limit for the possible radiation -flux penetrating the
"Luna-9" 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 no 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 th~_A~g4t
.of "Luna-4.,'~his makes it possible to assume that' dur-i n--gt-he period of
-the 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. ChKaWjq_4yqR and T. W. _Chat~*hchvan (unpub-
lished) revealed any considerable decrease in the cosmic-ray Intensfity.
Card 6/8
777777~-.'

'!M, ~.V4 .1Q
ACC NRs AP600500
I'count/sec II count/sec
Time of~ ~ianding
Time. of landing I.Vq
Mpaiurements dur tbelHea9uremento 0 a Z02
$,to f light to t~e M0401 the Nbon'
J_
.Pig. 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 Moon's
surface has been reduced to the mean-count rate during the flight, and the
.scale has been changed in proportion to the mean-count rates during the
-flight and on the Moon's surface.
The absolute flux of the cosmic-ray particles detected by "Luna- 9" was
,equal to 5.35 � 0.5 cm-2 sec-1. The great error in the determination of the
absolute,fluxes is due to the 101/6 uncertainty in the operational dimensions
a-71t,,and IIL
of the counter. Analogous measurements from "Lun una-8"
~emb~_A
stations performed on 4-6 October and 3-6 De er iV66 have shown the
:particle fluxes to be 5.4 and 5..9 cm2 sec, respectively. The cosrriic-ray
.intensity in February 1966 decreased compared to December 1905. This
Card 7/8

ACC NR,
is likely to be associated with the beginning of a new cycle'of solar acti,.qty.
Thus the cosmic-ra intensity maximum occurs durin
g the period
December 1965-January 1966, andthe lag in the cosmic-ray intensity
maximum behind the solar maximum detected for the protons of energion
.higher than 30 Mev is about 1.5 years. This conclusion Is also confirmed
.by the data of the,"Zond-3," "Venus-2," and "Venuig-,3" space probes.
[FSB:''v.'2,'no. 101
SUB CODE; 22
SUBM DATE: May66 ORIG REF: bO3 OTH REF: 001
f v

~3
BoURCE; Ref. zh. Issledovaniye kosmiche(skogo proBtranstva, Abe. 8.62.238
AUMOR: Vernov.-S.H..; Cbudakov, A. Gorchakov, Ye-V.; Loga ev.14-.J.; Hea'teroy.
Y.Xe.; &kveALo., I.A.; fL I.
TMUB; R%4j%jjonj-vjts of the earth
CIM SOURCE: Geofiz. byal. Hezhduved. geofiz. kom-t pri Prezidium AD OSSR,
no. 14, 1964, 96-iog
TOPIC TAGS: satellite, Tocket, radiation effect, cosmic radiation
TIMSIATION: A short outline is given of the results obtained from otmues conducted
using Soviet artificial satellites and cosmic rockets of the radiation belts and of
primary cosmic radiation beyond the limits of the magnetic spbere.
SUB CODE: 04M ENCL: 00

ACC NR S_ /0 8;,
A OURCE CODE: /0583 5 0
AUTHOR: Vernov S. N. (Corresponding member AN SSSR); Chudakov, A. Ye.
I(Corresponding member AN SSSR); Vakulov, ?. V.; Logachev, Yu. I.;
ILyubimov, G. P.; Pereslegina, N. V.
1,ORG: Moscow State University im. M. V. Lomonosov (Moskovsky gosu-
darstvennyy universitet)
TITLE: Cosmic ray variations according to data from Zond-3 and
Venera-2
SGURCE: AN SSSR. Doklady, v. 171., no. 3, 1966, 583-586
TOPIC TAGS: cosmic ray, cosmic ray Intensity, cosmic ray measurement
ABSTRACT: At the end of 1965 and beginning of 1966 two Soviet space
stations, Zond-3 and Venera-2, were in space simultaneously measuring
cosmic ray intensity. The first was In motion away from the Sun and
the second toward the Sun, which made it possible to determine both
variations in the intensity of cosmic rays and their dependance on the
distance from the Sun (i.e., their radial gradient). Data obtained by
STS-4-type gas-discharge counters onboard the spacecraft revealed the
radial gradient as S = (3-1 +0.4)% per 1 astronomic unit. The radial

1 ACC AP7001-54-9-
gradient was irregular; this phenomenon was attributed to chan~,es in
the character and magnitude of the Forbush effect. Detectors 011' the
n-p type onboard the'space stations measured the radial gradient of
protons with energies of 1-5 Mev. In addition to a sharp temperature
Increase, the detectors revealed a very stable and time-independent
noise which exceeded by about 10 times the possible noise of high-
energy particles. It was also found that the intensity of protons in-
creased in moving away fromthe Sun. Whgn the distance from the Sun
was increased from 130 x 10' to 190 x 101 km, the intensity of 1-5-Mev~
protons, whose origin Is known to be solar, increased 5 times. A mech-1
anism is proposed for explaining this paradox. The nature of the radial
gradient may possibly be explained by Parker's diffusion theory.
Orig. art. has: 4 figures. (WA-751
SUB CODE: 04/ SUBM DATE llAug66/ ORIG REF: OOR/
OTH REF: 002 -ATD PRESS: 5111
Card ?/2

--~-07G_67f_j-f[0J0*470 8 47 /0 6 50'
AC'C--NR, _'_AP'(00 169 4 :~OtflfCE CoWfi 0 1~;rO 0
AUTHOR...- Vern ov, S.N. (Corre.sponding member. Ali SSSR); Chudakov, A.Ye.
(Corregipp,nu` in (;'member kN SSSR); Vaktilov, P.V.; Log~achelr; YU.I.; LoVimov
G.?. ; !Jilcolaye A.G.; Peralegina, N.V.
ORG: Moscow S tate University im. 14. V. Lomonosov (]4oskovskiy
gosud-,rstvenrzyy universitet)
TITLE': Measurement of solar protons with energies of 1-5 Mev by the
Venera-2, Venera-3, and Zond-3 space probes
SOURCE: AN SS,5R. Doklady, Y. 171, no. 4, 1966, 847-850
-TOPIC TAGS: S'olar.radiation, solar radiation intensity, proton counter i
AB ST RACT :,During the flights of the Zond-3, Verena-2, and Venera-3 space 'probes,
the counting rate of proton detectors and Geiger counters on board in-
creased markedly on six occasions. The semiconductor surface-barrier
2
'proton'detectors had an area of about 0.2 cm ; the p-n junction was
:35 p thick. On the side of free space within a solid angle of ^-l sterad,
'the detectors were shielded with 2 mg/cm2_thick aluminum foil; on other
sides the shielding was more than 1-g/cm2 thick. The detectors were
.tuned to record protons with energies v.~rying from 1 to 5 Mev. The
Intensity Fange measured corresponded to 1.1 x 10-~ pFlse/sec.
2 UDC: none

t. AP7001
An analysis of the recorded data indicates- th~_t_ th~; protons -are ac'celer-
:ated on the Sun and are propagated withott hindrance along the magnetic
Jorce lines in interplanetary space. The width of proton fluxes with
energies of 1-5 Mev was estimated at.3 x 1012 cm. It is concluded that*'
these protons of comparatively low,.. energies are generated periodically
from the active areas on the Sun. They reach distant regions in
~interplanetary space'through a "tunnel" produced by the corpuscular
.streams. [WA-751;
SUB CODE: OC4)Z);/ SUBM DATE: 11ju166/ ORIG REF: 002/ OTH REF: 0021
ATD PRESS: 5113

BANDMAN, M.K.; LOGACHEVA, A.A.
Transportation and trade relfitions of Krasnoyarsk Territory and the
outlook for their development. Trudy Transp.-energ. inst. Sib. otd-
AN SSSR no. 10:23-46 160. (MIRA 14: 1)
(Kra,inoyargk Territory-commerce)

CHERMENSKIY, M.P.; LOGACHEVA, A.A.; BANDMAN, M.K.
Main trends in the dev~I-Oim-ont of transportation and trade relations
and the transportation system of the Angara Valley, within Krasno7arsk
Territory. Trudy Transps-energe Inot. Sib. otd. AN SSSR no. 10:47-
68 160. (MIRA 14i1)
(Angara VaII07--Transportation)

LOGACREVA _A.A,--
- ---t
Development of transportation aud trade relati*ns of Siberia with
regions of Central Asia and Xaza