SCIENTIFIC ABSTRACT KUZMIN, A.I. - KUZMIN, A.N.

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• Sequence Number: 9
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

29671
3 W/o S/169/61/000/005/034/049
leco (/VV/ My 6)
A005/A130
.t AUTHORSo Kuslmin, A.I. Skripin, G.V.
TITLE: On the decrease effect of cosmic ray intensity during magnetic
storms
PERIODICAL: Referativnyy zhurnal, Geofizika, no. 5, 1961, 13, abstract
5 G 104- (Tr. Yakutskogo fil. AN SSSR. Ser. fiz., 1960,
no. 3, 121-139)
TEM The authors investigated the upper limit and shape of the
energy spectrum of primary particles of cosmic rays subjected to the action
of the mechanism responsible for magnetic storms. For the analysis they
used data obtained from continuous recording of intensity at Yakutsk by a
neutron monitor, an ionization chamber and counter telescopes placed at
depths of 0-7, 20 and 60 m of water equivalent. The data were corrected
for the barometric and temperature effects. The presence of effects of
intensity decrease at depths of up to 60 m w.e. shows that the mechanism
which modifies cosmic ray intensity during magnetic storms affects par-
ticlee with energies up to 400 Bev. This being the case, the energy A-XI
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29671
S/16 61/000/005/034/049
On the decrease effect of cosmic ray intensity... A005X130
spectrum of primary variations has the formt
~D 0.11 t 0.03 , when 6 (7 t 2) Bev
D 0.22 t 0.03)-b-o' 7 t 0-2, when E (7 t 2) Bev
This form of the spectrum contradicts the concept of scattering of charged
particles by the magnetic field of the stream that has an intensity of
about jo-4 gauss in the earth's orbit. The authors assume that two me-
chanisms act in the decrease of cosmic ray intensity during magnetic storms%
one mechanism is connected with the magnetic field of the stream, and the
other with the electric field. What is more, the magnetic field plays an
inconsiderable role in the scattering of high energy particles, and its
action occurs in the main at the beginning and end of magnetic storms.
The authors point out the necessity of strictly taking Into account me-
teorological effects when estimating the effects in cosmic rays during
magnetic storms.
N, Kaminer
[Abstractor's note: Complete translation.] LK
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KUZ..1!,9N2 A.I.0 MDUK171, G.F., SHAFFR, G.V., SMIFER, YU.G., V RN011, 3.7~.,
"Cosmic Ray Outbursts on November 12-15, 1960,"
report presented at the Intl. Conference on Cosmic Rays and
Earth Storm) Kyoto, Japan) h-15 Sept 1961o

S/058/62/000/006/018/136
Ar,61/Aiol
AUTHORS: Kuzlmin., A. I., Yefimov, N. N., Krasillnikov, D, D., Skripin, G. V.,
-S_oR`313`v-,_7. ~D, Shafer, G. V., Shafer, Yu, G.
TITLE: A study of the variations with time of different cosmic ray compo-
nents by one-point observations
PEFIODICAL: Referativnyy zhurnal, Fizika, no. 6, 1962, 53, abstract 6B371
(In collection: "Kosmicheskiye luchi", no. 3, Moscow, AN SSSR, 1961,
64 - 79, English summary)
TEXT- A recording apparatus of the Yakutsk cosmic radiation post is de-
scribed, and the principal results Of a Study on variations of intensity are
presented. The following instruments are laid out on the surface of the Earth:
a neutron monitor, two shielded ionization chambers, and counter telescoper,
recording vertical and oblique cosmic ray components. In addition, counter
telescopes placed at depths of 7.20 and 60 m water equivalent record the muonic
component in the energy range of 2 - 109 -1 1011 ev, while the continuous frequeng
recording on latitudinal atmospheric showers yields ation or, 5 - 1013
n
Car-1 1/2

A study of the ...
S/058/W000/006/018/136
A061/A101
eT particles. The values of the barometric coeffioi-iLt of different comoonent-
are indicated, as well as the principal re::~ult-s of an Anv;~-stigatton of 27-day and
solar, day variations of intensity. Phenomena observed during magnetic storms
are.btiefly described. The interrelation factors betmeen Variatilons of intensity
of prf6hry and secondary cosmic ray components up to :rergles of -700 Bev are
detz-rmlned. These factors are utilized for the analysis of oome types nf varia-
tIons of intensity.
N. Kamilner
[Abstracter's note: Complete translation]
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3, 2,Y/O 7 0 5_1 7- 74 5;9 3/16 37 2 ~-C
9/62/000/004/075/103
S' 91 D218/D302
A"UTHORS: Kuz1minj A.tI.' Danilov, A.A., Krymskiy, G.F., and
18-k-rJ '-pin, G - V.
TITLE: Energy characteristics of cosmic-ray variations
during magnetic disturbances
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 1962, 14, ab-
stract 4G74 (V. sb. Kosmicheskiye luchi, no. 4, M.,
ALT SSSR, 1961, 16-24)
TEXT: The data obtained with a number of surface and underground
instruments at Yakutsk are used to analyze the energy characteris-
tics of cosmic-ray intensity variations during magnetic storms. It
is shown that the intensity recovery period after the Forbush-effect
minimum decreases with increasing depth of the recording device. Rr
some Forbush-type reductions there is a noticeable North-South ani-
sotropy in this effect. The method of coupling coefficients is used
to determine the energy spectrum of the primary radiation during
Forbush effects. Best agreement between experimental data and theo-
retical predictions is obtained with the following primary differen-
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S/169/62/000/004/075/103
Energy characteristics of ... D218/D302
tial spectrum
6D(E) = _ a fFO-7 at 6 > E,
D(E) 0 at ~, < F_1
Further analysis shows that the effective width of the corpuscular
stream should depend on the energy of the scattered particles. It
is suggested that the regular field of the stream carries with it
magnetic irregularities which give rise to scattering and diffusion
of moderate-energy particles. The parameters of the streamat and
the magnetic irregularities carried b them, are estimated. [Ab-
stractor's note: Complete translations.
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DOWNY L.I.; DZIMIN A I - SKRIPIN, G.V.
Sounding olactromgnAtic conditions in the interplanetary space
and in the vicinity of the earth by high-energy cosmic rays.
Geomag, i aer. 1 no.3:333-345 MY-Je 161. (MBU 14:9)
1. Magnitnaya laboratoriya AN SSSR i Laboratoriya fizichaskikh
problem Yakutskogo fili*la Sibirskogo otdeleniya AN SSSR.
(Qo~mic rays)

KUZIMIN't A.I.; SIMEER, G.V.; IRLMSMY, G.F.; SHAM, Yu.G.
.P- ------
Co3mic ray flares during Nov. 12-15, 10,60. Geomag. i aer. 1
no.4:510-5/2 J1-Ag 161. WIRA 14:12)
1. Sibirskoye otdeleniye AN SSSR, YakutsIdy filial.
(Cosmic rays)

M93
s/620/61/137/00/-/017/031
B100206;
30, (/b~ x7as)
AUTHORS: Krymskiy, G. F., Shafer, G. V-~ and
Schaferg Yu. G.
TITLE: Cosmic radiation flares from November 12 to 15, 1960
PERIODICAL: Doklady Akademii riauk SSSR, v. 137, no. 4, 1961, 844-847
TEXTt During the period of Nov6mber~12 to 17, 1960, intense cosmic radia-
tion, connected with events on the eiin, were observed in Yakutsk (geo-
magnetic latitude 510) by contihuous observations. The rec6rdin& are
shown in;the two figures. The duddei intensity increase of-the neutron
componezit started on November 12, at~13 hr 45 min (1345 UT)~Iuniversal
time an& coincided with the stait offa very strong magnetic3storA (1348 UT).
At.1630XT the intensity reached a maximum, which was 65 ~~ higher than the
normal value. At 1815 UT a second rise of the intensity started and
reached a maximum value at 2000 UT, 'which was 100 % higher than the normal
value. Both times radio waves 4ere totally absorbed in the ionoiphere
above Yakutsk. With the start of the second rise of the neutron component,
a drop of the Forbush type was indicated by all recording device3 for the
CaV 1/q. V,
E

21493
S/020/61/137/004/011/031
Cosmic radiation flares from... 0 .1 B104/B2o6 i
hard component of cosmic radiatVon. 'The energy speo.trum of-the drop is
satisfactorily described by Eqs.
CCAH P- < e1/4;
8D (a) 2 arc sin (ej/Ze ecAH e,/4 < a < el/2; (2)
D (e) n
0, ecnH P, > ej/2.
t 130- 170 Bev A second and .'.thirdflare of the hard component of cosmic
radiation was also observed, the third being described as Delling effect.
The coincidence of the start of the magnetic storm and the first flare
convinces the authors that the initial particle flare was a corpuscular
flow which then triggered off the 8magnetic storm. The velocity of the
corpuscular flow is given as 3-10 om/sec. If it is assumed that the
reduction of the Forbush type is caused by the regular magnetic Pield, it
can be concluded from the delay of this affect compared with the start of
the magnetic storm that ~he magnetic field was strongly dioturbod in the
front part of the flow. It is possible that the particle flow reached
there an energy comparable with the energy density of the magnetic field.
The relatively small second reduction of the intensity of the hard
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21493
S/020/61/137/00017/031
Cosmic radiation flares from... B104/B206
component of cosmic Vadia 'tion,and the absence of a neutron-component
reduction point3 towards the existence of accelerated particles in the
particle flow. Amplitudes and time of the maximum of the daily
disturbances agree with the velocity of the particle flow and the direc-
tion of the magnetic field in the flow (opposite to that of the earth).
The authors come to the conclusion that the ejection of the particle flow
was caused by solar cosmic rays, which partly produced the flares on the
earth and was partly captured by the particle flow. Particles of up to-
7 Bev were captured thereby. For a free incidence of the particles of the
second flare on the earth, it was necessary that t 'he direction of the
magnetic field of the first flow coincided with the axis of this flow.
There are 2 figures and 3 Soviet-bloc references.
ASSOCIATION:. Laboratoriya' fizicheskikh problem Yakutskogo filiala
Sibirskogo otdeleniya Akademii nauk SSSR (Laboratory for
Problems of Physics of the Yakut-sk Branch of the Siberian
Department, AS USSR)
PRESENTEDt December 16, 1960, by M. A. Lavrentlyev, Academician
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14?262
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0_0 E032/E314
AUTHOR: KuZ 1 1111 J,
TITLE: The role of the upper layers of the atmosphere in
small effects in the hard component of cosmic rays
during chromospheric solar flares
SOURCE: Akademiya nauk SSSR. Yakutskiy filial. Trudy.
Seriya fizicheskaya'. no.4. 1962. Variatsii-
intensivnosti kosmicheskikh luchey, 61-65
TF'1XT; Data obtained as a result of continuous recording of the
hard component of cosmic rays by surface and underground counting
arrays during 1957-1959 are discussed. The energy characteristics
of cosmic-ray variations were investigated at Yakutskaya
laboratoriya (Yakutsk laboratory) with-an array of triple-
coincidence counter-telescopes at sea-level and at depths of 7, 20
and 60 in of water equivalent. A re-examination of the
experimental results reported earlier (A.I.Kuzlmin, A.A.Danilov,
Tr. YaFAN SSSR, ser. fizich., no.3, 196o, 58), in the light of the
formulae given by L.I.Dornian et al (ZhETF, 26, 1954, 537) shows
that if there is a reduction in the temperature of the ozone layer
during small chromospheric flares, opposite effects should be
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s/845/62/ooo/004/005/013
The role.of the upper ... E032/E3i4
observed in the intensity of the hard component at sea-level and
at 60 m of water equivalent. Short-wave fade-out was used in the
experimental part as an indication of a chromospheric flare on the At
Sun (Dolbear et al, J. Ter. Phys., 1, 1951, 187). Analysis of the
data, corrected for the barometric effect and the average diurnal
variation, showed that there were no appreciable changes in the
intensity of IL-mesons at the three depths below sea-level during
and after the fade-out. It is estimated from these data that the
temperature oscillations in the 0 to 25 mb layer are of the order
of 5*. It is shown that this is, in fact, the maximum possible
change for the period 1957-1959. It is consistent with the data
reported by Kaininer (YaFAN SSSR, ser. fizich., n0.3, 196o, 92) for
1955-1956. Next, radio fade-out data were analyzed by the method
of superposition of epochs for the cases when the Yakutsk Station
was in the "zone of incidence" and outside it. "Zone-of-incidencell
calculations due to Kaminer (YaFAN SSSR, ser. fizich., no-3, 1960,
148) were used in this analysis. Although there were 37 cases of
radio fade-out when Yakutsk lay in a zone of incidence and 38 cases
when it was outside this zone, it was found that there were no
appreciable changes in the intensity of the neutron and hard
component in any of these cases. There are 3 figures.
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h2263
S/845/62/000/oWoo6/o15
E032/E314
AUTHORS: Kuzlmin, A.I. and Skripin, G.V.
TITLE: Underground variations in the intensity of cosmic
rays during 1957-1959
SOURCE: Akademiya nauk SSSR. Yalcutskiy filial. Trudy. Seriya
fizicheskaya. no. 4.. 1962. Variatsii inten51vnosti
kosmicheskikh luchey, 66 - 82
TEXT: The intensity of the ji-meson component was measured
with a system of counter-telescopes at different-depths below sea-
level (7, 20 and 60 m of water equivalent). Variations in the
intensity of the ~t-meson component at sea-level could b8 investi-
gated with this apparatus for an energy rhnge of 2 x 10 to
2 X 1010 eV, which corresponded roughly to average primary-pakicle
energies between 40 and 2oo-400 BeV. The vertical intensity in a
solid angle of ~-% and the intensity from the southern and northern
directions at 30 0 to the zenith were recorded at each level with
triple-coincidence telescopes. The accuracy was sufficient for the
detection of fine effects provided the recording was extended over
a period of some months or more. It was found that meteorological
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s/845/62/000/004/006/ol3
Underground variations .... E032/E314
effects in the intensity of the hard component at sea-level and
the above three depths were in agreement with the jt:~-meson scheme
for the generation of the hard component in the atmosphere,
suggested by L.I. Dorman (Variatsii kosmicheskikh luchey
(Variation in cosmic rays), Gostekhizdat, Moscow, 1957). The beat
agreement between experiment and theory is found to occur for the
following values of the exponent y in the effective integral
IL-meson spectrum:
sea level - Y = 0-3
7 m w.e. - Y = 0.5
20 m w.e. - Y = 0.8
60-m w.e. - Y = 1.
The meteorological effects at different depths below sea-level are
in good agreement with Dorman's theory (mentioned above). This is
confirmed by the fact that observed seasonal variations in the
ji-meson intensity at different depths and the expected changes due
to temperature effectswere identical to within experimental and
computational error. Analysis of solar-diurnal variations at a
fixed point again confirmed Dorman's theory of the modulation of
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Underground variations
S/845/62/000/004/oo6/oi5
E032/E,311,
the primary cosmic-ray intensity by the electric fields of solar
corpuscular streams. The lower energy limit for particles ' -
modulated by these streams is 12 BeV and the effective source of
these variations lies to the left of the Earth-Sun line at an
angle of 66 +- 110. The ratio of tho amplitudes of 27-day varia-
tions and th-C reduction in intensity during magnetic storms are
the same within a wide primary-:partic7le energy range
(2 x 109 - It x 101'eV)so that it is suggested that they are due
to a common mechanism. The energy spectrum of primary variations
is of the form:
6D(c) b C* < C
D(e) ac OL C > C
where e 7 + 2 BeV, a = -0.7 + 0.3, a = 0.22 and b = 0.11
for the magnetic-storm effects and a =-0.06, b = 0.03 in the
case of,the 27-day variations. This spectrum is consistent with
that expected on the Dorman theory due to the scattering of
particles by the frozen-in magnetic field of a stream with an
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Underground variations * ...
s/845/62/000/004/oo6/ol5
E032/E314
-4
intensity of 10 gauss at the Earth's orbit but appreciably
disturbed by the interaction between the stream and the inter-
planetary medium. The considerable change in the energy spectrum
of particles with E -'\ 30 BeV in the primary stream during
magnetic storms suggests the presence of irregularities in
the regular magnetic field of the stream and the importance of
the influence of electric fields. There are 5 figures and 5 tables.
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li?265
S/8lk5/62/000/OC,4/008/013
E032/E314
AUTHORS: Kuz'min, A.I. and Skripin, G.V.
TITLE: some basic properties of disturbed diurnal
variations in the intensity of cosmic rays
SOURCE: Akademiya naulc SSSR. Yakutskiy filial. Trudy. Seriya.
fizicheskaya. no. 4,. 1962. Varia-tsii intensivnosti
kosmicheskikh luchey, 91 - 102
T 1 ~"XT J. Sekido.and.SJoshido (Rep, Ionos Res. Japan, 4, 37,
1950), aud.thb present authors (Tr.YaFAN SSSR, ser. fizich., no. 2,
107, 1958) have found that there is an increase in the amplitude
of the solar-diurnal variation and a shift of the maximum towards
earlier hours during and after magnetic storms. According to the
theory of Dorman (Variatsii kosmichesklkh luchey (Variation in
cosmic rays), Gostekhizdat, Moscow, 1957), this is due to the fact
that during such storms the Earth enters a corpuscular stream
carrying a large frozen-in magnetic field. The source of the solar-
diurnalvariation is then displaced towards the Earth-Sun line and
the amplitude of the variations increases with the energy of the
recorded particles. This theory has not so far been satisfactorily
er~f!A. The aim of this work was to use the data obtained at
~
ar

s/845/62/000/004/008/013
On some'basic properties .... E032/E3i4
Yakutsk to determine the main properties of disturbed solar-diurnal
variations and to compare Dorman's theory with experiment. 'The
analysis is based on 1957-1959 observations with the apparatus des-
cribed in an earlier paper (the present authors and A.V.Yaryg in,
Tr. YaPAN SSSR, ser. fizich., no. 2, 34, 1958). The apparatus
consists of counter arrays and telescopes at the Earth surface and
at 7, 20 and 60 m of water equivalent. All the data were corrected
for meteorological effects. Magnetic data were taken from the pub-
lications of IZMIRAN. The analysis covers only those cases whe;
the reduction in the measured ji-meson intensity at the Earth surf-
ace was not less than 10,10. These data show that magnetic distur-
bances are associated with considerable changes in the solar-
diurnal variations of cosinic rays. The degree of disturbance in
the amplitude and in the position of the maxim4ffi diurnal variations
is greater at higher energies of the recorded particles. The
maximum change in the diurnal variations during magnetic storms
at all the four levels mentioned above iras recorded by the telescope
pointing in the direction parallel to the plane of the ecliptic
and at 300 south of the zenith at a geographic latitude of 600.
t was/~ound that the experimental data on the disturbed diurnal
ard 2
~

S/845/62/000/004/oo8/013
On sonic basic properties .... E032/E314
variations during magnetic storms were consistent.with a spectrum
of the form
6D(c) 0, C < C
D(c) ~,ac C
0
where a = -0.5 and c0 10 - 15 BeV o. -Moreoverl the experimental
data are also in agreement (to within experimental error) With the
variation spectrum accepted in Dorman's theory
1,
2
6D(c) f 2 -1 C 1 1
S in El < C, (2)
D(c) C 2c 4 2
0, C 1
where f = 0.30 andc1 = 80 108 BeV. The source of these
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S/845/62/000/004/008/013
On some basic properties .... E-032/C314
variations is found to lie at 35 + 5 0 to the left of the Earth-Sun
line. The source of diurnal variations during magnetic distur-
bances is associated with a mechanism whose position in space
varies continuously. A large number of considerable disturbances
in the solar-diiirnal variation was noted during 1957-1959, during
before and after magnetic storms. The general conclusion is that
the main characteristics of disturbed diurnal variations are in
good agreement with Dorman's theory, which explains them as the
effect of the electric and magnetic fields of solar corpuscular
streams reaching the Earth. There are 3 figures and 6 tables.
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42766
S/845/62/Ooo/oo4/oo9/Ol3
E032/E31.4
6)
AUTHORS: KuzImin nd Skripin, G.V.
TITLE: On the coefficient of absorption of, cosmic rays which are
responsible for solar-diurnal variation
SOURCE: Alcademiya nauk SSSR. Yakutskiy filial. Trudy. Seriya
fizicheskaya. no. 4. 1962. Variatsii intensivnosti
Rosmicheskikh luchey, 103 - 107
TEXT: Results of a comparison of diurnal variations in the
ji-meson component of cosmic rays at the Earth's surface with measure-
ments obtained with similar apparatus und 'er different absorbers are
reported. The PLK-1 (ASK-1) and C.-2 (S-2) ionization chambers
(Yu.G. Shafer, Tr. YaFAN SSSR, ser. fizicb., no. 2, 1, 1958) were
employed. It ifas found that there wex~e considerable differences in
the amplitude of the diurnal variations in Moscow and in Yakutsk.
It was established that these were not due to time variations or
1meteorological effects and the diference was therefore ascribed to
a change in the primary radiation. If it is assumed that the
diurnal variations are due to some localized source, it must also
be assumed that the properties of this source are very dependent
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S/845/62/000/004/009/013
On th,e coefficient of E032/r,314
on the level of solar activity and the dependence is such that
during the years of minimum solar activity the solar-diurnal vari-
ations are due to particles of lower average energy than during the
years of maximum solar activity. Simple numerical calculations show-
that the coefficient of absorption for t~ e radiation responsible
for diurnal variations is (0-5 +.0.10,0' cm /g for 1954-1255.A
V
similar estimate for 1956-L958 yields (0.23 + 0 .5)% cm /g. It
follows that IL"mesons undergoing diurnal variations at minimum
solar activity (1953-1955) have considerably larger absorption
coefficients than during high solar activity (1956-1958). This
difference in the absorption coefficients may be due to the follow-
ing effects: 1) it is possible that in 1956-1958 the threshold
energy , for particles undergoing the diurnal variations was displaoed~
towards higher energies so that the mean energy was appreciably
increased; 2) the energy spectrum of the particles reTonsible
for the diurnal variations in 1953-1955 was much softer than the
particle spectrum responsible for the - variations in 1956-1958
and 3) it is possible that both the above factors were operative
at the same time. There~ are 1 figure and 2 tables.
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h "1269
S/845/62/Ooo/oo4/012/013
r,032/E314
AUTHORS: Kuzimin, A.I. and Skripin, G.V.
TITLE: Electromagnetic conditions in the neighbourhood of the
Earth on May 10 - 24 , 1959
SOURCE: Alcademiya nauk SSSR. Yalcutskiy filial. Trudy. Seriya.
fizicheskaya. no. 4. 1962. Variatsii intensi.vnosti
kosmicheskilch luchey, 113 - 121
TrXT: The analysis now reported is based on experimental data
obtained as a result of recording the meson component of cosmic rays
with counter arrays at the Sarth'Ssurface a 'nd at 7, 20 and 60 m of
water equivalent. The apparatus employed has been described by
A.I. KuzImin (Diss. NIYaF MGU, Moscow, 196'0) and by the present
authors (Tr. YaFAN SSSR, ser. fizich., no. 2, 195, 1958). The-
apparatus included a neutron monitor, ionisation chambers RCK-1(ASK-1)
and C -2 (5-2) and a vertical counter-telescope at the surface and
'Vertical counter-telescopes at each of the above three 0depths. In
addition., there were counter-telescopes pointing at 30 north and
south of the zenith. blean diurnal variations, corrected for baro-
metric and temperature effects, were obtained for the cosmic-ray
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Electromagnetic conditions .... E032/E314
intensities and were compared with geomagnetic and ionospheric data
determined at 1/011HAN (Kosmicheskiyedannyy. (Cosmic-ray data),,May,.'jJ1
1959). Analysis of all the data showed that they were in agreement
with Dorman's hypothesis (Variatsii kosmicheskikh luchey (Variation
in cosmic rays), Gostekhizdat, Moscow, 1957), according to which the
cosmic-ray intensity is modulated by the magnetic and electric fiel:h
associated with solar-corpuscular streams which were respqnsible for
magnetic disturbances. The cosmic-ray data are consistent with a
lateral. capture of the Earth by the stream associated with the
magnetic storm of May 11, 1959 (9-13 hours Yakutsk.local time)
Analysis of the energy spectra of the variations showed that the
stream carried a frozen-in magnetic field of 10-5 Oe, 'and a'.
radial velocity of (4-6) x 10 cm1sec. It is considerea that the
magnetic field was not random although the stream did include
appreciable irregularities. It is possible that the stream trans-
ported cosmic-ray particles which were noted as an intensity burst
in-the low-energy region. However, the upper limit of the trans-
ported particles must have been less than 2 BeV in view of the
absence of a neutron-intensity burst at sea-level. There are
2 figures and I table.
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B/048/62/026/006/016/020
B125/B102
AUTHORS: Kuz'min._._Lt_I,.,.Krymakiyq G. F., Skripin, G. V., Chirkov,
N. P., Shafer, G. V., and Shafer, Yu. G.
TITLE: Some results of investigations relating to variations of
cosmic rays
PERIODICAL: Akademiya nauk SSSR. Izvestiya. Seriya fizicheakayal v. 26,
no. 6, 1962, 808-817
TEXT: The main results gained in the Yakutskaya laboratoriya (Yakutsk
Laboratory) concerning various meteorological effects-and primary
variations are here reviewed, covering papers published by Kuz'min et al.
in Tr. Yakutskogo filiala AN SSSR. Ser. fiz., no- 5, 1962. There are
12 figures and I table.
ASSOCIATION: Yakutskiy filial Sibirskogo otdeleniya Akademii nauk SSSR,
Lab~oratoriya fizicheskikh problem (Yakutsk Branch of the
Siberian, Department of the Academy of Sciences USSR,
Laboratory of Physical Problems)
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KUZIMIN, A.I.; KRECKIY, G.F.; SKRIPIN, G.V.
Angular distribution of cosmic ray intensity below ground
at deptbs equivalent to 0 to 60 meters of water. Trudy
IVAN SSSR. Ser. fiz. no-4:22-25 1.62. (MMA 15-12)
(Coamie'rays)'

KUZIMIN. A.I.
Role of the upper atmospheric layers in minor effects
of the hard comlJpnent of cosmic rays during chromospheric
solar flares. Trudy IAFAN SS34 Ser. fiz. no.4:61-65
162. (MIRA 15:12)
(cosmic rays)

KUZ.IMIN, A.I.; SKRIPINJ Gove
Variations in cosmic rays balow ground durring 1957-1950.
Trudy IAFAN SSSR. Ser. fiz. no.l+:66-82 162. (MIRA 15:12)
(Cosmic rays)

INUZOWNy A.I.; -MIFIN, G.V.
Some principal properties of distprbed solar diurnal variations
in cosmic r# intensity. Trudy IAFAN SSSR. Ser. fiz. no-4:91-102
162. (MIRA 15:12)
(Solar radiation)
(Cosmic rays)

KUZIMIN, A.I.; SKRIPIN, G.V.
Absorption icoefficient of the intensity of
responsible for solar diurnal variations.
SSSR. Ser. fiz. no,4:103-107 162.
(Ocamic rays)
(Solar radiation)
cosmiq rays
Trudy JIFAN
MIRA 15:12)

.KUZIMINp A.I.; SKRIPINp G.V.
Electromagnetic conditions near the eartb during the period
May 10-24, 1959. Trudy WAN SSSR. Ser. fiz. no4:113-121
162. (MIRA 15:12)
(Magnetic storms)

4KUZIHIN. A.I.; hIMIN, G.V.; SERGEYEV, A.V.; SKRIPIN, G.V.; CHIRKOV,
SHAM, G.V.
Flare-up of cosmic ray intensity on May 4, 1960. Trudy
WAN SSSR. Ser. fiz. no-4:132-137 162, (MIRA 15:12)
(Cosmic rays)

.. KUZIMIN, A-I.; SHAFER, G.V.; SpkM, Yu.G.; DUSL~'KKOV, - - -
KRI04SK-IY G.F.; MAMMOV, A.P.; SMIRNUV, N.S.; YAR114', V. I
.1 L,
July 1959 according to data of comprehensive geophysical
observations at Yakutsk. Trudy IAFAN SSSR. Ser. fiz. no.4:142-156
162. (MIRA 15:12)
(Magnetic storms)
(Cosmic rays)

A. I. KIJZ.MIDI
Modulation of Cosmic Rays by Interplanetary M2grietic Field
report submitted for the th Intl. Conf. on CosmLc Rays (IUPAP), Jaipw- India,
2-14 i~--c 1963

YERDFEYEV, N.M., otv. red.; MISHIN, V.M.0 kand.fiz.-matem. nauk,
red.; POLYAKOV, V.M., kand. fiz.-matem. nauk, zam. otv. red.;
KUZIMIN I A.I. kand fiz.-matem. nauk,, red.; NIKOLAYEVA, L.K.,
red. YU.V., tekhn. red.
(Studies on geomagnetism and aeronomy] Issledovaniia po geo-
magnetizmu i aeronomii; doklady. Moskva, Izd-vo Akad. nauk
SSSR, 1963. 149 p. (MIRA 16:6)
1. Sibirskoye soveshchaniye po geomagnOtizmu i aeronomii. lat,
Irkutsk, 1961. 2. Chlen-korrespondetn Akademii nauk Turkmenskoy
SSR (for Yerofeyev).
(Magnetism, Terrestrial) (Atmosphere, Upper)

KUZIMIN, A.I.; SKRIPIN, G.V.; KRIVGSHAPKIN, P.A.; KRYMKIY,, G.F.
Energy spectrum of the diurnal variation of cosmic rays and
the diurnal temperature fluctuations at an altitude from 20
to 40 km. Geomag. i aer. 3 no.5:830-834 S-0 '63-(IIIIUi 16:11)
1. Yakutskiy filial Sibirskogo otdeloniya AN SSSR.

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L 234011-65
ACCESSION NR: 0500210i
(institute of. Space Physics Researcn and Aeronomy of the Yakutsk
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Card 30

C'Elfullov, G.F.
~l . , 4.
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L `3399-65
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a n c r i b u t c d ch r oric, .5 1) it,,. rcc e s s a 1. a r
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n r k I t c h e s?c 4L'k h t s seo v a n i y i aeronomii
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L 1894-66 , EVIT(I)/FCC GS/G-14
ACCESSION NR: ATS022829
AUT11OR: Kuz'min, A. I.; F.
tIR/0000/65/000/000/0131/0136
TITIE- Cosmic ray bursts
ell
SOURCE:12 Vsesoyuznoye soveshchaniye po kosmofizicheskomu napravleniyu
issledova~niy koiiic' eskikh luchey. Ist, Yakutsk, 1962. c i
M _e _wi
r0 -k6-sd6-ft-zTk_i UCosmic rays and problems in cosmophysics); trudy
p
soveshchaniya. Novosibirsk,.Redizdat Sib. otd. AN SSSR, 1965, 131-136
TOPIC TAGS: cosmic ray intensity, cosmic radiation energy, ~!olar flare, space
maRnetic field
ABSTRACT- The paper gives a brief analysis of the frequency distributions and
temporal and energy characteristics of cosmic ray bursts, and reports on
principal results of experimental studies of bursts conducted for the purpose
of determining the structure of the interplanetary magnetic field. The fre-
quency of bursts in cosmic ray intensity declines sharply with the increase in
the minimum energy of the primary particles responsible for the increase in the
recorded component. Integrated spectra of the bursts versus energy and amplitude,'---
show that only a small proportion of chromospheric flares c~n produce an effect
Card 1/2

L 1894-66
ACCESSION NR: AT5022829
which can be recorded by earthbound cosmic ray detectors. The largest number
of cosmic ray bursts are due to chromospheric flares on the western side of the
solar disk. Solar corpuscular streams responsible for geomagnetic storms create
the necessary conditions for cosmic ray propagation. Differences in the in-
crease of the intensity of cosmic rays generated in chromospheric flares at
different solar longitudes do not result from differences in the condition of
generation, but reflect differences in the conditions of propagation of the
particles coming from the eastern and western portions of the solar disk. The
predcminant direction of particle travel from western chromospheric flares is
thought to be the direction of the lines of force of the interplanetary magnetic
field in the vicinity of the' earth. This direction lies in the ecliptic
plane 50-600 to the west of the sun, confirming the twisted character of the i
interplanetary field. Orig. art. has: 4 figures'and 3 formulas.
ASSOCIATION: Institut kosmofizicheskikh issledovaniy i aeronamii UP SO AN SSSR
(Institute of Cosmic Physics Research and AeroU10MY. YaF SO.AN_.SSSR)
~, 5
SUBHITTED., 290ct64 ENCL: 00 SM CODE: AA
NO REP S Oll
,PY: OTHER: 019
Card /2

~10-66 EWT(1)/EWT(m)/FCC/T/EWA(h) IJP(c) GS/(;W
ACCESSION-NR: AT5022836 UR/0000/65/000/000/0239/0245
35
A
AUTHOR: 4gj'W1.n 1,;KrIWshapj0n P. A..-,Kr G., V.~,
_ _w
TITLE: The study of upper atmosphere temperature variations from terrestrial measure-
ments of cRsm1c rqp
SOURCE: Vsesoyuznoye soveshchaniye po kosmofizicheskomu napravle tssledov4q!y
kosmicheskikh luchev. --I t. Yakutsk. 1962. Kosmicheskiye luchi I problemy koamofizik
(Cosmic rays and problems in cosmophysics); trudy soveshchaniya. Novosibirsk, Redizdat
Sib. otd. AN SSSR, 19651 239-245
TOPIC TAGS: cosmic ray measurement, atiRoppjjeriq_teTpei~atare
cosmic ray intensity,
upper atmosphere
ABSTRACT: Data concerning the dynamics of the mesosphere are necessary for the under-
standing of the coupling mechanism between the solar and terrestrial events and of the
general circulation of the atmosphere. However, systematic data about atmospheric dy-
namic,s at altitudes between 20 and 80 km are practically nonexistent. The present article,
consequently, gives results concerning the periodic temperature variations of the meso-
sphere asderived from the terrestrial measurements of cosmic rays at Yakutsk. The cos-
mic ray Intensity was measured continuously over the 1959-1960 period at 30 and 6W from
Card 1/2

L 4510-66
ACCESSION NR: AT5022836
the zenith on the Earth's surface and underground at 20 and 60 m. w. equiv. (some data
concerning daily variations are based on the 1958-1959 period). Experiments were carried
out under the assumption that the variations in cosmic ray intensity at 6(r and 20 (60) m. w.
equiv. depths were caused by temperature variations of the atmosphere only. The analysis
of da_J_- confirmed the accepted production mechanism for the hard cosmic ray component
via intermediate nuclear-active mesons. Significant periodic changes in upper atmosphere.
temperature were found at the height of the ozone layer. These seasonal variations were
between 35 and 50C, the 27-day variation amplitude was 5-10C, while daily variations were
within the 3-7' limit. The yearly maximum appears in the fall, and the daily maximum
during night hours. The observed temperature variations agree well with data from spec-
tral obse7vations of the night s1des. The spectral results referring to altitudes of 80-120
Ian have amplitudes several times larger than the corresponding results for the 20-50 mb
layer presented in this article. Orig. art. has: 2 formulas, 7 figures, and 2 tables.
ASSOCIATION: Institut kosmoiiztcheskfkh Issledovanly I aeronomff YaF 50 AN SSSR
stitute of Cosmic Physics Studies and &q_KqqqXpy., a SQ
SUBMIT TED: 290ct64 ENCL: 00 SUBCODE: ESt AA
NO REF SOV-. 005 OTHER: 000
Car, 0/2-

L 4481.-66 EWT (I )/F-d1(1a)/FCC/T/hEdA(h) IjP(c) Ut
ACC NRI
APS024635
SOURCE CODE: UR/0041;/65/029/009/1690/1692
Vernov, S.M.; Yegorov
A.I.
_1; YfUtMOV, N.M.; Krasil'nikov, 1).D.; Kuz'pin
Makstmov, S.V.; Nesterova, N.M.; Hikollgkiy s.1.; Sleptsov Ye. Shafer, Yu. G.
none
05
AVrHOR:
OnG:
TI TIR: Plan for a Jai-go installation at Yakittak for study of e tp
%VLtv~e
A , _gj~_A_ _.q ---
/Report, All-Union Conference on Cosmic Ray P~ystcj,held at Apatity 24-31 August 196V
SOURCE: AN SSSR. Izvestiya. Seriya flzlcheskaya, v. 29, no. 9, 1965, 1690-1692
TOPIC TAGS: primary cosmic r , secondary cosmic ray, extenqive nir rhower, spectrrl
energy distribution, cosmic radiation composition, cosmic radiation anisotropy
ABSTRACT, After a discussion of the significance of extensive air showers for tile in-
vestigation of ultrahigh energy primary cosmic rays, the authors hriefly describe an
installation to be completed in the next two or three years near sea level at latitude
620 N in the Yakutsk region; it is nnticipated that the installation will yield infor-
mation concerning the energy spectrimt, composition, and anisotropy of primary co.-mic
rays with energies up to 1020 eV. The installation, intended for investigation of ex--
tensive air showers, will comprise 65 stations spread over an area of 23 km2. Ench
station will be equipped with scintillation counters with a total sensitive area of I
m2 or 4 m2, and at the central station - 10 m2. The total sensitive area of scintil-
Card 1/2
0 ~/O/

L 4481-64'
ACC NR. AP5024635
lation counters in the whole installation will be 204 m2. Each station will be equip-
ped with photomultipliers (total cathode area 180 cm2 at each station) for recording
the Cerenkov flash accompanying a shower. In addition, there will be muon detectors
witti a total sensitive area of 22 m2. Pulses will be transmitted from the more rcmote~
stations to the central laboratory by radio. It is anticipated that this Installation
will record 2 x 10 showers per year with energies exceeding 1015 eV and 2 showers per
year with energies exceeding 1020 eV. Orig. art. has: I figure and I table.
SUB OODE: NP/ SUBM DATE: 00/- ORIG REF: 002/ OTH REF: 008

C ',,: - ". I ~ 1:, - ") "i, . .I`ii~
, ~ i . " . , r, _~ I IM i '1111- .
A;3y-r,m-,,. try in o-I ~rnl c ray I.,i i ..~r ~ili rA, " '.~ v. .-, , ", :f 7, . ~!,: , . f, -., .
21? no.10:2902.-I.906 () 165. (MIRA 18:10)
1. InstlLut 'fl-oimofi-?,i~!,:I~-.,,ki.el~ ir~variiy t Sibirskogo
otdeleniya AN S~Z_q.

L 4514~-bb F119T k 1)
ACC NRt AR6027538
RCE CODE: UR/0313/66/000/005/0043/0043
AUTHOR: Kuz'min, A._ I.; Krymskiy, G. F.; Krivoshapkin, E. A.; SjEhp!n V.;
Chirkov, N. P.; Shafer,_G,_ V.
TITLE: The nature of cosmic ray variations
SOURCE: Ref. zh. Issledovaniye kosmicheskogo prostranstva, Abe, 5. 62. 292
REF SOURCE: Sb. Issled. po geomagnetizmu i aeron. M., Nauka, 1966, 111-118
TOPIC TAGS: cosmic ray, cosmic ray variation, magnetic field, interplanetary
m.4gnetic field, magnetosphere
ABSTRACT: A review of stud ~7' s is presented on cosmic ray variations caused by
changes in the magnetosphere,~ the temperature of the upper atmosphere, modula-
tion effects, and flare effects. The role of the interplanetary magnetic field in the
generation of cosmic ray variations is emphasized and the characteristics of the
field are evaluated. [Translation of 'abstract [FMI
OW
SUB CODE: 03, 04/ SUBM DATE: none/
Card 1/ 1 6ZIt MV

L 04886-67 FW'r(1) /EW'r(Tr-) ,FCC I jr, GIVOW
ACC NR, AT6027221
SOURCE CODE: UR/0000/66/000/000/0111/0118
AUTHOR: Kuzlmin,,A,-!. Krymsidy, G. F.; Krivoshapkin, P. A.; Skripin, G. V.;
Chirkov. N. P. -, Shaffer, GG. V.
ORG: none
1 11
TITLE: The nature of cosmic ray variations
I-ddezLye, Sibirskly Institut zemnogo magnetizma, I
SOURCE: AN SSSR. Sibirskoyt o
I rasprostranenlya radlovoln. Issledovaniya po geomagnetizmu I aeronomil (Studies In
geomagnetism and aeronomy). Moscow, Izd-vo Nauka, 1966, 111-118
TOPIC TAGS: cosmic ray intensity, solar cycle, magnetic field
ABSTRACT: A brief survey Is given of available data concerning the variation of cos Ic ray'
intensity and the effect responsible for this variation. The effects of fluctuations of the
magnetosphere and temperature fluctuations in the upper atmosphere on cosmic ray variations
are examined. Cosmic ray flares with energies up to 10 Bev, and their association with
Forbush decreases are discussed in relation to 9pir effect on cosmic ray variations. The
1 1-year variations, 27-day variations, and solai~ diurnal and annual variations are shown to be
closely interrelated, and to have modulation of galactic cosmic rays by the radial inter-

L 048~c-67
~k Cc NR% AT6027221
planetary field as their common source. All existing observations an the variation of cosmic
ray intensity are seen to indicate the existence of an external (with respect to the fnm) radial
interplanetary magnetic field and the predominant contribution of the dynamic effects of the
field's disturbances to the modulation of galactic particles. An Important feature of the field's
configuration (deduced from observations of the variation of cosmic ray intensity, and also
from other unrelated data) Is Its oblateness with respect to the plane of the ecliptic or the
solar equatorial plane.
SUB CODE: 04/ SUBM DATE: 25Dec65/ ORIG REP: 026/ OTH REP: 009,i
Card 2/2

1, 040n'-'F~-o? LW'1 f"ci ~Aj
ACC NR: AT-6.02- 72-20 SOUR-CE CODE: 616-6/6-661066161-6-576i I
AUTHOR: Krymskiy, G. F.; Almukhov, A. M.; Skripin, G. V.; Krivoshapkin, P. A ;
Kuzlmin, X7 1. A-7
ORG none &t
TITLE: New method for studying the anisotropy of cosmic rays
SOURCE: AN SSSR. Sibirskoye otdeleniye,- Sibirskly Institut zemnogo magnetlzma, lonoofer,
I rasprosir--oneni
-ya radlovoln. IssTe-do-vanlya po geomagnetizmu I acronomil (Studies In geo-
magnetism and aeronomy). Moscow, Izd-vo Nauka, 1966, 105-110
TOPIC TAGS: cosmic ray anisotropy, cosmic ray Intensity, cosmic ray
ABSTRACT: A method is proposed for determining the instantaneous characteristics of the
anisotropy of cosmic rays. The method will make it possible to obtain the anisotropy dis-
tributiOlL in the merldional planes and to study the anisotropy of phenomena characterized by
abrupt changes in the Isotropic background (such as the Forbush decreases), all of which was
not possible using the method of diurnal variations. The method proposed makes use of the
fact that the world-wide network of stations establIE!hed during the IGY makes it possible to
determine the neutron component with an hourly statistical accuracy of 0. 1% and, thereby,
Card 1/2

_' u4ttt-b/
-Act _kk,__At_6_62_f2i6_
to determine the anisotropy characteristics over a 2-hr observational period, provided that
its amplitude exceeds the mean amplitude by a factor of more than 2. A distinctive feature
of the method is the representation of the distribution of cosmic-ray intensity over the celes-
tial sphere In the form of a series in spherical functions and the use of the first spherical
harmonic of the series. The expression for the first harmonic yields the amplitude of the
anisotropy vector and an expression for the intensity in an arbitrary direction at an angle to
the direction of the anisotropy vector. The spherical analysis reduces to the solution of a
system of linear equations with four unknowns. The solution of the system determines the
isotropic portion of cosmic-ray intensity as well as three components of the anisotropy vec-
tor. The coefficients at the unknowns are calculated and tabulated for 38 stations, Uddng into
account the effect of the geomagnetic field on the charge&particle trajectories, and also the
energy spectrum of the variations. Orig. art. has: 6 formulas and 1 table.
SUB CODE: 04/ SUBM DATE: 25Dec65/ ' ORIG REF: 012/ OTH REF: 002
Card

ACC NRt AR6027539 SOURCE CODE: UR/0313/66/000/005/0044/oo44
AUTHOR: Krymskiy, G. F.; Altukhov, A. M.; Krivoshapkin, P. A.; Kuzlmin, A. I;
,Skripin, G. V.
;TITLE: A new method for investigating cosmic ray anisotropy
;SOURCE: Ref. zh. Iseledovaniye kosmicheskogo prostranstva, Abe. 5.62.298
,R=--' SOURCE: Sb. Issled. po geomagnetizmu i aeron. M., Nauka, 1966, lo5-lio
fTOPIC TAGS: cosmic ray anisotropy, linear equationt earth magnetic field, particle i
~Itrajectory, radiation spectrum, variational problem
1ABSTRACT: A method using the spherical analysis of data from a worldwide network of
!stations is suggested in order to obtain the instantaneous characteristics of cosmic
jray anisotropy. The analysis can be reduced to solving a system of linear equations
'with four unknowns. The solution determines the isotropic intensity and three compo-
I
inents of tne aiiisotropy vector. Introduced is a calculation for the coefficients
Ifor the unknowns in the equations for each station. The effect of the earth's magnet-'
1c field on particle trajectories, as well as differehoes In t4e energy spectra for iso;,L
itropic and anisotropic variations, is considered. Abstract'. LTranslation of abstrao
SUB CODE: 04
Card 1/1

ACC NR-I-AP603S494' SOURCff 'Cbbt;-IJRT04-13/667000/018/0116/0116-1
INVENTOR: Zhdanov, K. I.; Dubrovskiy, D. M.; Kazanskiy, B. P.;..~uz'min,'A. I.;
Kulikov, Ye. L; Bespechnyy, S, P.; Yevlakhov, L. A.; Meshchaninov, Ye. G.
ORG: none
TITLE: Aircraft-propeller test stand. Class 42, No. 186169
zz.-z:-zz- :=zbrcr prom obraz tov zn, no. 18, 1966, 116
TOPIC TAGS: aircraft propeller, admax=ft propeller blade, propeller test stand,
aircraft maintenance equipment,
ABSTRACT: An Author Certificate has been issued for an aircraft-propeller test stand
consisting of a pedestal and a propeller hub, equipped with dummy blade roots, and a
hydraulic pump which supplies working fluid to the stand's components. To simulate
propeller loading without rotation, hydraulic pistons, installed in the pedestal's
cylindrical housing, operate through the dummy blade roots to simulate centrifu3al
force and thrust. To simulate the aerodynamic forces produced by the propeller's
transverse inflow, it is equipped with movable hydraulic cylinders which consecutively~l
bend the dummy blade roots. Working fluid is supplied to the hydraulic cylinders
through a hydraulic pulser containing spring-loaded plungers; these are consecutively
displaced by a cam mounted on the hydraulic pulser's shaft by the use of an eccentri-
UDC: 620.178
Card 1/2 629 .13.01/06 -F

K7UZIMIN, A.I.; NATSUK, N.S.
Practice in plotting maps of underground %4aters as a basis for
designing wells; as exemplified by tho Chorltik AgricultUral
Administration$ Qnsk Province. Izv. Omsk. otd. Geog. ob-%,a
no.6:13-16 164. 18:9)

VASIL'YEVA,, G.N. , inzh.; ZALKIND, I.Y, .,, inzh,j ISEROV, D44j inzh.;, KORMER,
I.M., inzh.; KUZIMIN, A.I., inzn.- LAKHHANLUJ, A.I., lnzh.;
9
SHAKHSUVAROV , y . V. J, - Iiiih. ,
Determination of heat losses of boilers to an ambient media.
Elek. sta. 36 no.20-6 F 165. (MIRA 18j4)

-KUZIMINV A.M. (Novgorod)
Ways to increase theaftivity of students in the seventh grade
geometry lessons. M~t.v shkole no.5s26-29 3-0 162. (MIRL 15sl2)
(Geometry, Flane-Study and teaching)

te r i t s r e z!
C E t om n a a p n e r 7~ v a 1 7 o
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T-o a e I f z h - -p o w e r
o u t c t n e ume er)i
ne a c -
n c o re 'd a 5
Card 1/3

L 17636-65
ACCESSTON uR: AP4045332
power, core Volume, And Increaae in temnerac,irp rise )F tvie coolant,
n iz a t e r a I
e r -i
r a e s
0 r i g a r t h a 8 g 11 r e
A S , ! , f '- i A i I n o n e
Card 7 13

: 1 -7 6 ' 6 -.6 f,
~ I ! ;
ACCESS T(11~ NF - A74045332
SUBMITTED: V' 4.,o v 6 3 EN CIL : 0 0
NO REF SOV: 003 OTHE R: 0 0 1
, I/
s U B c 0 DE : 14 p
Card 3/3

KUZIMIN, A. M.
"AcaAel. Vladimir Afanaslyevich Obruchev" (On his 90th Birthday) General Geology,
Personalia, Izv. Thmskogo Politekln, in-ta, 74, No 1, 1953, PP 3-12
Abs
W-31146, I Feb 55

KIJZ 'MIN, A. M.
"Microcline" (Mineralogy, Silicates) Izv. Tomskogo politeklin. in-ta, 74, No i,
1953, pp 47-107
Abs
W-31140', L Feb. 55

XMIMIN, Ax.
..
The phenomenon of concentration streams observable during
crystallization. Isv, Sib. otd, All SSSR no.6:10-25 158,
(MML 11:9)
1,Tomakiy politekhnicheskir institut.
(Crystallization)

KUZIMI .
Mass crystallization. Part 1: Crystallization from supersaturated
solutions on several levels with rapid cooling. Izv. TPI 95:
378-383 '58. (MIRA 14-9)
(Crystallization) (Solutions, Supersaturated)

KUZ'MlN, A.M.
Mass crystallization. Part 2: Crystallization on several levels
with continuous feeding. Izv. TPI 95:384-392 ?58. (MIRA 14:9)
(Crystallization) (Solutions, Supersaturated)

KUZ IMIN. A.M.
Hoegbomite from Gornaya Shoriya. Geol. i geofiz. no.4:63-75
,6o. (MIRA 13:9)
1. Tomakiy politakhnicheakiy institut.
(Gornaya Shoriya--Hoegbomite)

KUZIMIN A.M.
Cleavage and slip planes in rock salt. Geol. I geofiz. no.6:60-
74 16o. (HIBA 13:9)
1. Tomskiy politekhnicheskiy institut.
(Dislocation In crystals) (salt)

KUZIMIN., A.M.
Upper Paleozoic gold formation i4 the vicinity of Tomk. Geo2.
rud. mestorozh. no.W30-131 Mr-;Ap 161. Off RAL 14: 5)
1* Tomskiy politekhnicheskiy institut.
(Tomsk region-Gold ores)

KUZIMIN, A.M.
Argon retention in mircoline. GeOkhi!nila no.5:456-458 161.
(MIRA 14:5)
1. Politekhnicheskiy institut imeni S. M. Kirova, Tomsk.
(Argon) (Microcline)
,i7-4

YERMOLAYEV, V.A.; KIJZ'MINp A.M. I
I
Microhardness of natural zirconium (ZrSiO4) crystals. Izv. vyse
ucheb. zav,;.fiz. no.1:63-68 164. , - (MIRA 17:3)
1. Tomskiy politekhnicheskiy institut Imeni Kirova.

FIffect of' flattening on ( ertal ... ......
charact(,ristics of a cylincricol Ptist
enr,rg. 1.7 no.3:199-201 S '64.

KHALFIN, L.O.: Prof.y OtV. red.; T,,IA..
A dot3.0
geol.-L.iner. nauk, red. Tn,-ra; jAZ-,'-;R;Cl,fT
BULYNNIKOV, A.Ya.) Prof. GORUJIM, LlOtS.,
rC4.
geol.-riner. Ilauk, red. KU k a nd
D.S.p prof., red.; ROG04- I ~"' "~ A-1U.,,,prof., red.;
V, G. j., dots., kand. geol.-sdnor
nauk, red.; SU1,AKMIN, S.S., iots.g kul!J. Leklin. nmik, r,d.;
KHAKHLOV, V.A.., prof.p red.
[Materials on the geology and mliior&l o f ~10 ~j t.'~ 1~11 L 4 J~
reports
I ~tate'ria]Y FO geQ100i i polezyWin J~qkoijaemvm, Zapndno-i
Sibiri; doklady. Tomsk, Izd-vo Tomskogo univ., 1964'. 424 p.
(MIRA 180)
1. Konferentsiya) posvyashchezinaya 100-jetiy,,j so ~jnya j-,,zhdc,--
niya akademika M.A.Usova, Tomsk, 1063.

L 25438-66
ACC NR: AT6005814 SOURCE CODE.i UR/0000/65/000/000/0051/0069
AUTHORS: Khromov, V. V.; Slesarev, I. S.; Shmel 4, A. N.;
e
S,
Kuz'min, A. M.,
ORG:
TITLE: Effective method of calculating two'dimensional and.three~
dimensional reactors
SOURCE: Moscow. Inzhenerno-fizicheskiy institut. Nekotoryye
voprosy fi_z_1_kf__f_tekhnik1 yadernykh reaktorov-mome problems in the
bysics and engineering of nuclear reactors). Moscow, Atomizdat,
p
1965, 51-69
TOPIC TAGS: nuclear reactor characteristic, computer application,,
algorithm, neutron flux, gas kinetic equation, iteration,
neutron distribution, nuclear reactor technology
ABSTRACT: The authors present a possible simplified method, with a
much smaller amount of the computation, for designing two dimensional
and three dimensional nuclear reactors. The algorithm for the cal-
culation of the neutron fields Is constructed.and the assumpti&n that
Ca rd-

L 25438/~6
ACC-NR:--AT6005814
the spatial components of the neutron field can be separated in each sl
zone. The purpose of the investigation was to develop a simplp and
reliable algorithm, which would make po3sible to perform with suf
ficient accuracy a whole series of different variants of calculation
without requiring an excessive volume of computer memory. The forMal4
~'Ism of separating the variables ts used not for a detailed descrip-
Ition of the neutron field in different parts of the reactor, but to
lobtain integral characteristics of the field along selected layers of
'the system. This simplifies the equations, yet makes it possible to
icarry out detailed calculations of the neutron distribution along any
'line which is parallel to a coordinate axis. The computation scheme
'includes an iteration procedure for successively calculating the one
t
idimensional systems whAch correspond to different layers of 'e re
!actor. The section headings are: 1. Derivation of the equation oi
!the effective method. II. Scheme of calculation of the neutron field
lin problems of external sources. III. Calculation of a neutral field,
:!in a nuclear reactor. IV. Concerning the formalism of the method
V. Generalization of the method for the case of the gas kinetic
equation. VI. Verification of the method. The method was checked
Card
-13

25438-66
ACC NR: AT60058i4
with several reactor variants and provided good accuracy withi
n
10 -- 20 iterations, using 15 to 20 minutes of the M-20 computer
N. Yurova for useful
time. The authors thank & 13, ablAbqv and
discussions during the devel(~pment of the method. Orig. art. has:
4 figures,, 39 formulas, and 6 tables.-
SUB CODE:18,09,tl SUBM DATE: 05jun65/ ORIG REF: 0021 OTH REF: 003

L 25430-66 EPF (n) -2/E'WT(m)/gTq(f )/EWG(m) aj/(Z
,ACC NR: AT6005815 SOURCE CODE:--UR/bobo/65/000/000/0070/0077z
!AUTHORS: Slesarev, I. S.; Sk:Lkkqv
~B.
IShmelev., A. N.; Kuzimin, A. M.; Shishkov,
ORG: none
Khrqqqyj_~ 6z,i
L. K.
~TITLE: Design of fast reactor using electi-onic computers
1 7e,
SOURCE: Moscow. Inzhenerno-fizicheskiy institut. Nekotoryye
voprosy f izikl i Ee--Rniki yadernykh reak-t-or6v(Tome problems in the
lphysics and engineering of nuclear reactors). Moscow, Atomizdat,
11965, 70-77
nuclear reactor technology, nuclear reactor operation,
TOPIC TAGS: A nuclear reactor characteristics., fast reactor, computer
application, algorithm , electronic computer/ M-20 electronic computer
!ABSTRACT: The purpose of the paper was to develop a computer algo-
Irithm which, on the one hand, is sufficiently simple and requires few
!operations, and on the other hand'displays the quantitative and
!qualitative characteristics of different reactor variants, so as to
'permit the best design choice. A comprehensive computation pngram
Card,

L 2543046
1ACC NR: AT600591_~__ Oj
lintended for the M-20 computer is described. Thie program, which is
based on a single-group method proposed by one of the authors.
I(Shikhov, with A. I. Novozhilor,.Atomnaya energiya v. 8. 209, 196o)
'Jin conjunction with the method of conditional separation of variables,
makes it possible to determine the critical load for established di-
mensions of the reactor, to determine the reflector saving, and to
i
evaluate the Integral of many-group fluxes and the neutron importancel
in all the zones of the reactor. The program also includes thermal. I
icalculations which yield the diameter of the fuel elements, the heat
~flux to the surface, and the main heat exchange parameters and the
ratio of the volumes of the components of the active zone to the totai,
~volum In addition to this program, there has been developq4 at them;
!Moscow Engineering Physics Institute a program, based on a dlffusion-~
~transport approximation, for calculating the critical parameters of
ia cylindrical reactor by the method of conditional separation-of
.!variables. This calculation.is carried out by a multigroup method
!with an electronic computer, and makes it possible to calculate the
'critical parameters of a many-zone reactor. It Is used essentially
Ito calculate the finally chosen optimal variants of the reactors,
since it requires more computer time than the for~egoing comprehensive:--
Card-- 2/3

L 25430-66
AdC NR: AT6005815
program. Mention is also made of a program developed under the
leadership of G. I. Marebuk to solve the cylindrical problem by
conditional separation of variables with a single refldotor saving
for all groups. This should lead to a more accurate allowance for
the edge effects in the lower part of the.neutron spectrum. Orig.
art. has: 7 formulas and 1 table.
SUB CODE: 18,09/ SUBM DATE: 05Jun65/ ORIG REF: 001/ OTH REF: 001

ACC NR-.
AT7005603 SOURCE CODE: tTiZ/0000/66/000/000/0033/0052
AUTHORS: Kuzlmin, A. M.; Khromovf V. V.
ORG: none
TITLE: A few-group method of designing multi-region reactors
SOURCE: Moscow. Inzhenemo-fizicheskiy institut. Inzhenamo-fizicheskiya voprosy
yadernykh reak-torov (Problems of nuclear reactor engineering and physics); sbornik
statey. Moscow, Atomizdat, 1966, 33-52
AI#X4 F,~94 ieLC1-.7C_' 70,e- D.F-31 G AJ,
TOPIC TAGS:, nuclear reactor, approximation method, boundary value problem,
differential equation, neutron diffusion, mathematic matrix, gas kinetics, neutron
distribution
ABSTRACT: A method is proposed for designing multi-region reactors in a diffusion
I approximation based on reducing a large number of neutron enerey groups to small
groups~ without taking into account the importance of the neutrons. The initial
system of multi-group equations is:
(v1l, 0
under the boundary conditions
Card 1/2

-ACC NRt AT7005803
This system is reduced to the following system of differential equations for fL, (r):
2-1
-(D'> Af- (r) + W h W
M