SCIENTIFIC ABSTRACT DORMAN, L.I. - DORMAN, L.I.

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• Collection: Scientific Abstracts
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• Release Decision: RIF
• Original Classification: S
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• Document Creation Date: January 3, 2017
• Document Release Date: July 28, 2000
• Sequence Number: 3
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

3. Mro (,W 4/ /J /0 4 LJ mrj)
V, 9 f,1/0
87h67
3/169/60/000/012/005/ov)
AOO5/A0Ol
translation from: Referativnyy zhurnal, Geofizika, 1960, No. 12, p. 219, # 16268
AUTHORS: Blokh, Ya. L., Glokova, Ye. S., Dorman L I
,'"TTLE: Investigation of the Nature of the Cosmic Ray Effect During the
Magnetic Storm on August 29, 1957, on the Basis of Materials From the
International Station Network of the IGY
PERIODICAL: V sb.: Variatsll kosmich. luchey pod zemley, na urome morya I v
stratosfere, No. 1, Moscow, AN SSSR, 1959, PP. 7-36
TEXT: The analysis is given of the great intensity decrease of the cosnic
rays which began on August 29, 1957. The investigation was performed on the bas-,s
of the materials of the imernational network embracing 50 observation points
(77 recording devices). I't was stated that the energy spectrum of variation of
the primary cosmic rays, W. .ich caused the intensity decrease effect, has the form:
A (EVNE) - 0.17 A,
where A I for < & min/4, A - -(2/'X) are sin (Emir/2t - 1) f or 6mid)i 4
Min/2, and A - 0 for E < S*min/2 and P-min - 90 Bev. The analysis results allow
Card 112

87467
s/a6q/6o/ooo/O12/0o5/bio
A005/AO01
Investigation of the Nature of the Cosmic Ray Effect During the Magnetic Storm on
August 29, 1957, on the Basis of Materials From the International Station Network
of the IG-f
the following Interpretation of the observed phenomena. A wide corpuscular stream
containing the frozen-in. regular magnetic field (H w., 1o-5 Gs) hit the Earth with
Its leading front on August 29. The scattering of the cosmic rays by this field
led to the observed Intensity decrease. The absence of solar-diurnal variations
during this period points out that the direction of the magnetic field in the
stream coincided apparently with the ecliptic plane. On September 2, the Earth
was hit by the second corpuscular stream having caused a -very intense magnetic
storm and a new decreas.? in the cosmic ray intensity. The analysis of the
diurnal variations, observed during this period, points out tha'. the magnetic
field frozen-in In the stream was oriented perpendicular to the ecliptic plane.
The investigation of scme phenomena Is presented, which accompanied the main effev~
of Intensity decrease: a soft decrease and following Increase in intensity before
the beginning of the me,in effect, the alteration of the variation spectrum wit*n
time, and others. - There are 16 references. It. S. Kaminer
Trazislator's note: Th.'is Is the full translation of the -_'~rlginel Ruz-;Ian abstract.
lard 2/2

87469
/goo Od"VI s/169/6o/boo/ou,/oo7/oio
.7;w a ' 106.Z.1 Ila) A005/AOOI
Translation from: Heferativnyy zhurnal, Geofizika, 19W, No. 12, p. 21% # 1627r)
AUTHORS: Blokh, Ya. L., Vernov, S). N., Dorman L 'L,,,2ut-rovin, M. M.
TITLE: Preliminary Results of an Investigation of the Underground Variationr,
of Cosmic Rays
PERIODICAL: V sb.: Variatsil kosmich. luchey pod zemley, na urovne morya i v
stratosfere. No. 1, Moscow, AN SSSR,1959 PP. 37-47 ~x
TEXT: The variations of the cosmic ray intensity are investigated on the
basis of data obtained from a counter telescope of triple coincidences, which was
located under the etrth's surface at the depth of 40 m of water equivalent. By
the simple- correlation method the value of the barometric coefficient A. (0.021 +
O.OC8) %/mb was obtained. The diurnal variation of the underground intensity
amounts to about 0.05%. By averaging the data it is shown that the average effe-;t
at the depth of 40 ri of water equivalent amounts to 0.39 during 11 events of
decreases of the Forbush type. The investigation of the di-sturbed diurnal varia-
tions in the cosmic ray intensity was also carried out. N. K.
Lranslator's note: This is the full translation of the original Russian abstract.
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87468
3 polo 00 Y/., '106'a ~ Mae) 811691601000101210061010
91 f d1149 A005/AO01
Translation from: Referativnyy zhurnal, Geofizika, 1960, No. 12, p. 219, # 16269
AUTFORS: Dorman, L. I., Feynberg, Ye. L.
MWWW=%WTW Awft"F
TITLE-. Some Problems of the Theory of Cosmic Ray Variations
PERIODICAL: V sb.: Variatsii kosmich. luchey pod zemley, na urovne morya I v
atriosfere. No. 1, Moscow, AN SSSR, 1959, pp. 49-57
TEXT: Ce:rtain consequences are described from the theory of the effect of N1
the solar corpuscular streams on the intensity of the cosmic rays, when the corpn-
cular rays carry frozen regular magnetic fields. It is shown that. this theory
explains well the observed decreases in the intensity oE the cosmic rays duriyur
magnetic storms; the variation of the intensity is totally determined by the
nature of the capture of the Earth by the corpuscular stream (by the leading
front or the by-side) . It Is known that the duratbn of the decrease In the inten-
sity of the coEmic rays is considerably greater than the duration of trie geo-
magnetic disturbances. For explaining this difference, the assumption is made
that the lines of force of the magnetic field frozen ir. th-S corpuscular stream
run out beyond the boundaries of the latter and are circuited at the Sun (if the
C ard 112

87468
S11691601000101210061010
Some Problems of the Theory of Cosmic Ray Variations A005/A001
general solar field is frozen in) or in the interplanetary spacp (if the field of
the sunspots is frozen In). In this manner, the region scattering the cosmic
rays increases, which leads to the in2rease in the duration of the decrease effe-,t
of cosmic ray intensity. In connection with the fact that the observed varialAx,5.
in the cosmic ray Intensity extend to energies of not lower than abou-. 100 Bev,
It is necessary to know the relation coefficient between 4-~Ie vartations of the
primary and secondary components of the cosmic rays for underground observations.
Basing on sufficiently accurate results of ratIrZ the relation coeffi,.,ient for
counter telescopes on sea level, the relation coefficients are calculated for
undergrou:nd Investigations at various depths down to 2,000 m, of water equivalent
,jnder certain simplifying assumptions.
N. S. K.
Translator's note: This is the full translation of th~, original Russian abstraTt,
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ZOANOV,,G.B...glavW red.;;IVAMMO, reipe, some glaynogo; red,; UTSVIN,
V,Je, otir.red,tome; 130MOT, B.A., samored.toma; GERASIKOVA. X.Mo,
rod.; HIKISHOW. A.I., red.; DCHKOI. L.I., red.; TULIROV, V.P.,
24id.; SrROVATSKIT, S.I., rer.-.1ma-Ro VX, red.; ITAV310T, U.N.,
rod.; ARROSIKOV, A.T., red.; GMV, I.P.. red.12d-va; BMMGAUI,
VoG., red.isd-va; BRUZGULI, Y.Y., takhn.red.
[Ixtensive air showers and cascade processes) Shirokie stmonfernye
ILvni I kaskadnye protsessy. Moskva. Isd-vo Akad.nauk SM# 1960,
331 ~. (Trudy meshdunarodnoy konferentaii po kosmicheskim luebam,
U302 0 (KMA 13:12)
1. IzLternational Conferenoe or Cosmic RadiatioLe
(cosmic rays)

ZhD)JiOVI G.B., glav. red.; IVANENKO, I.P.p pom. glav. red.; GMS1140VA.,
N.M., red. toma; VIKISHDV, A.I.; pom. red. toma; ZATSEPIN, V.I.,
red.; YJUMOV, V.A., red.4 DO; L. ., red.; TULINOV,,V.F.,
red.; SYROVATSKIY,S.I., red.; FEDOROV, V.M., red.; VAVIIDV, Yu.N.,
red.; ABROSIMOV, A.T., red.;
Proceedinim of the Moscow Cosmic Ray Conference. July 6-11,
1959. Moscow. VoLl. 1960. 333 P.
(No subJect heading)

ZHDAVOV, G.B., glav. red.; IVA)MHKO, I.P., pom. glav. red.;.-D-ORU_NlL-
L;L, red. tora; TULINOV, V.F.p pom. red. toma.-, GERASDUVAP
NIKISHOV2 A.I.,, red.; ZATSEITI, V.I., red.;
0=40Y., V.A., red,; 5VIOVATSM, S.I., red.; FMOROV, Y.M.,
red.; VAVILOV, U.N., rud.; ALIHOSIHaV, A.T., rod.
Proceedings of the Moscow Cosudc Ray Conferencop July 6-12p
1959. Moscow. Vol.A. Variations of comnic-ray intensity.
1960. 365 P. Va. Y -
(flo subject laading)

ZHUA OV, ".B., Slavayy red,; IVANZNK0, JoPaq zam,glavnogo red.;
SYROVATSKIY, S.L. oty.red,toma; KHREHOV, BOA&, cmm,rod,tona;
GNRASIMOVA, HoM.j red.; NIXISHOV, A.I., rod.; V.L.
red.~,~N~L.L# red.; TULZROV, V.F., red.; .;D0R0'1. V.M.;
VAVILOV, Tu.N. , ieia~.; ABRASIMOV, A.T., red.; FFX)KIH, H.I.,
red.izd-va; MWZGULI, V.V.. taklm.red.
[Radiation belts of the earth. Primary cosmic rodistion and its
proportion and origin] Hadiatsionnyi poles Zemli. Pervichnos
koomichaskoe isluchenie, ago avoietva I proiakhozhdenie. Moskva.
Izd-vo Aked.nauk SSSRO 1960. 2.58 p. (Trudy M02hdunarodnoi
konforentaii po kosmicheekim lucham, no.3)
WRA 14:2)
1. International Conference of Cosmic Radiation.
(Cosmic rays)

ACCESSION NR: AT3012740 S/2961/60/000/002/0005/00S7
AUTHORSs B10khe Ya. L.j Dorman, L. 1.1 Kaminer, No So
TITLE: individual cases of the influence of magnetic storms on
cosmic rays, and their interpretation
SOURCE: AN SSSR. Mezbduvedomst. komit. po prov. mezhdunarodn.
geofizich. goda. 7 razdel program. MGG. Koamicheakiye luchi. Sb.
statey, no. 2, 1960, 5-57
TOPIC: TAGS: cosmic rays, cosmic ray bard component, cosmic ray neu--
tron component# magnetic storm, sudden magnetic storm, corpuncular
strezan, solar corpuscular stream, cosmic ray intensity profile
ABSTRACT: An analysis is presented of the changes in intensity of
the bard and neutron components of cosmic radiation occurring in
about 50 different magnetic storms from 1954 through 1959 and ob-
servod- in ~he world network 'of stations. The profile of each case
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is classified (groups I# II, and III) and compared with the theoret-
1cally expected profile.under various assumptions concerning the
velocities of the corpuscular streams which carry frozen-in-magnetid
fields, concerning the manner whereby the earth enters the streams
(sideways, leading front at different distances from the stream
axes$ etc.), and concerning the field structure. It I's concluded
that the field intensity in the leading side edge of the stream is
much larger than in the remaining part of the strewn. A considerable
kinetic energy density dispersion is observed in the stream, de-
creasing on going to the trailing side edge of the stream. This ex-
plains why magnetic perturbations terminate after the resumption of
the cosmic-ray intensity. The pl~asma in the leading pa.-*t of the
strewn becomes highly c6ndensed and consequently the frt:zen-in field
intensity increases. This explains the sharp decrease in the inten-
sity of cosmic rays during the tine of some sudden magnetic storms.
The following general properties are found to be cornnon to all
strewns: the angular width of the stream is equal in the mean to the
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ACCESSION NR: AT3012740
angular width of the active region, the front oage of the stream
is characterized by a considerable increase of the magnetic field
(and'corresponding compression of the plasma), and the field is
somewbat more intense in the leading part of the stream compared
with the field in the lagging edge. it is assumed on the basis of
the analysis that during magnetic-storms the cosmic ray intensity
profile is determined completely by the manner in which the earth
enters the stream, by the stream velocity, and by the field distrib-
ution in the stream. A detailed study of this profile can therefore
yield important information on the stream properties. "in conclu-
sion we take the opportunity to express deep gratitude to Professor
Ye. L. Feynberg and-to 0. 1. Inozemtsova for a discussion of the
results. We are also grateful to the researchers who provided us
with the experimental data used in the present Work." Orig. art.
bast 39 figures, 17 formulas, and l'table.
ASSOCIATION: None
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ACCESSION NR: AT3012741 S/2961/60/000/002/0058/0073
AUTHORs Dorman, L. X.
TITLE: Mange in cosmic ray intensity during the entry of the earth
in corpuscular strGams carrying hoinogeneous and inhomogeneous froxaft-
in magnetic fields
SOURCE: AN SSSR. Mezhduvedomet. komit. po, prov. mex:hdunarodno
geofizich. goda. 7 raxdol program. MGG. Kosmic6skiye luchi, 6b.
statey, no. 2, 1960,. SS-,73
TOPICTAGSs cosmic rays, cosmic ray intensity, cosmic ray intensity,
variation, corpuscular stream, solar corpuscular stream, cosmic ray
neutron component, cosmic ray meson component, frozen in magnetic
field
ABSTRh'_T: The expected profiles of -the intensity variations.of the
neutro.a and meson components of commic'rays are -calculated for 40,
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ACCESSION NR: AT3012741
60, 80, 100 and 120 BeV. The calculations are made for front ve-
locities 2, 3 6"12, and 24 x 107 cm/sec. These calculations
5' f . F
are an extension Of an earlier investigation (L, 1. Dorimans, Tr.
Mezhdur.ar. konferentsii-po kosmicheskim lucham, AN SSSR, 1960, v.-
13) of the variations of the intensity of cosmic rays due to
4, p. I
the sca.%tering of particles by the magnetic fieldis of streams for
different cases of entry of the earth in the stretam, 'where only a
homogeneous magnetic field in the plane perpendicular to the field
was considered and the only energy value was 100 BeV. The profiles
expected for different characters'of inhomogeneity of the magnetic
field a.re also calculated. Comparison of these profiles with the
e*perintental data makes it possible to estimate the field distribu-
tion in the stream for each individual case. Thet profiles investi-
gated bave the 'forms of a drooping straight.line, a parabola, a
triangle and an inverted parabola. , The capture of the earth by the
leadinSt front, of the stream with 'the field having a higher intonsity
in the front part is also considered. CaVarison of tbo various

ACCESSION NR: AT3012741
Profiles with the *xperiwAmtal data makes it posisible to estimate
the dintribution of the field in tto stream for oach individual
case. orig. art. bass 30 formlast 5 tables, and.6 figures.
ARSOCIMTONS
SUB=' 00-
MEDs 00 DATS ACOs 220ct63 ENCLs
SUB CODEt PH 90 RZF GOVs 002 OTHMU 000
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ACCESSION NRt AT3012744 S/2961/60/000/002/0105/0109
AUTFIORa Dorman. L.
TITLE: Cosmic ray anisotropy due to the electric field of a cor-
puscular stream
SOURCE: AN SSSR.- Mezhduvedomst. komit. PO p"Ov. mezhdunarodn.
geoirizich. goda. 7 razdel program, MGG. K.osmic-heskiya luchi. Sb.
statey. no. 2, 1960, 105-109
TOP:fC TAGS: cosmic rays, cosmic ray anisotropy, corpuscular stream*
solar corpuscular stream, cosmic ray anisotropy spectrum, cosmic
parl;icle momentum, cosmic particle energy
ABSTRACT: The distribution over the earth's sphere is calculated
for the spectrum of the expected variations due to the electric
field under various assumptions regarding the structure of the regu-
lar inhomogeneous magnetic field. The momentum intervals at which
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ACCESSION NR: AT3012744
the-particles acquire or lose energy are also calculated, with allow,-~
ance for the effect of the stream magnetic field on the particle
trajectories. The calculations are made for different positions
of tho earth in the stream and for closed and open particle trajec-
tories. it is planned to take into account the influence of the
geomaStnetic field and to use the anisotropy spectrum obtained here
to determine the expected variations of different secondary compo-
nents under different registration conditions. Orig. art. has: 1
figure and 15 formulas.
ASSOCIATION: None
P I
SUBMITTEDs 00 DATE ACQ:' 220ct63 ENCL: 00
SUB CODE: PH
NO-REP SOVs 003
OTHER: 003
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ACCESSION KRi AT301274~
8/2961/60/000/002/0110/0130
AUTHORt Dorman# Lj.-_
.......... .............. .
TITLEt Diurnal variations 6f cosmic rays, due to anisotropic scat-*
tering of particles by inhomogeneous magnetic fijlds of corpuscular
streams
SOURCE: AN SSSR. Hezhduvedomst. komit.-po prov. inezbdunarodn.
geofizich. gods. 7 razdel program. MG. Kosmicheskiye luchi. Sb~
statey, no. 2, 1960, 110-130
TOPIC TAGSt cosmic rays, cosmic ray diurnal variation, corpuscular
stream, solar corpuscular stream, corpuscular stream magnetic field,
cosmic ray scattering, cosmic ray meson component, cosmic ray nou-
tron cosponent
ABSTRACTs Continuing earlier investigations (Variataii kosmichoo-
kikh luchey, M.o. Gootekhixdato 19571 Tr. Mezhdunar. konf. po kos-
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ACCESSION NR-. AT3012745
micheskim lucham, AN SSSRI 1960, v.-4, P. 113) the author considers
the diu:rnal variations of cosmic rays resulting from anisotropic
scattering of particles by the regular frozen-in homogeneous and in-
homogeneous magnetic fields. A general solution is obtained for the
case when the field is perpendicular to the strewn axis". The energy
spectrxua of the variations is determined as a function of the local
time for different distributions of the magnetic fteld in the stream,
with and without approximate allowance for the ingluence of the mag-
netic field on the particle trajectories. The e3q)ected vari 'ations
of the intensities of the neutron and meson cosmic ray components
are determined at sea level and at mountain altitudes for stations
with different geomagnetic thresholds, for-different distributions
of the frozen field, and for different positions of the earth in.
~.the stream. Numerical calculations are presented for the case of a
linear variation of the field from a maximum at the leading edge of 1
the stream to a minimu 'm at the iagging side edge. Comparison with
the experimental data yields information on the structure of the mag-
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ACCESSION NR: AT3012745
netic field in the corpuacular strewn. The effect of the orients-
tion-of the instruments on the measurement results is also discussed.,
A graph and tables make it possible to find the expected variation
of the cosmic-ray intensity and the solar-diurnal variations for
each specifi6 magnetic storm under various assum 'ptio'no. "I take the
opportunity to express deep gratitude to laboratory azoistant R. T.
Gushchina for help with~the calculations." Orig. art. bast S'
figures, 29 fornralas, and'3 tables.
ASSOCIMON: Nofie
SUMMED: 00 DRTR ACQt 220ct63 ENCL: 00
SUB CODEt PH NO REIP SOVS 004 OTHERs 003
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3,
AUTHORe
TITL&s
29665
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Aj05yAi3O
Dorman, L.1,
A method for detOrMiAiAg the temperature of cosmio rays from
the altitudes of isobaric surfaeos
PERIODICALs Referatiynyy zhurnal, Geofizika, no. -5, '1961, 11, abstract 5
0 94i) (Tr& Yakutskago fil. AN SSSR. Ser. fit## 1960t no* 3,
55-T5
TEX'Ps The author examinee the pce-iibility cf reylacing the atmo-
spheric temperature by the altitudes or slMad&rd isobario surfaces in order
to calculate the temperature effoot of the hard component of cosmic rays.
The intensity variation 6N/I of ocimic rays, which i's caused by temperature
variation# 6T(h) in the atmosphere at isobar!,-, leyel hf 449 deternined by
meting of W (h) ~T (h) dh , where W (h) is,,thedensity of the
T ' T
and h0 is the preseure at the observation level.
Uting into aaoount that the altitude of an isobaric surfaoe with pressure Ly
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29665
S/169 61/000/005/024/049
A mlithod for determining the temperature of ... A005/1130
h equals H - P dh' here ? (h') is the density of air at the h'
h T T7) , w
lev*l, for the variation of cosmic ray intensity that is caused by atmo-
sphtirio temperature variation the author derives the expression
N (h ) d (") dh. Having subdl~rided the entire atmosphere
N. AR WT dh
0 2
into sufficiently fine layers (about 100 g/,jm eaoh), one can determine the
dennity (%/km) of the teapera,ture ooeffi,,-Ieatn whii)h makes it possible to
caloulate the temperature effect from the var-'ation in altitude & R of the
isobaric surfaces. The author gives the values of the coefficients, oal-
oulated for the introduction of temperature aorrentions for the altitudes
of ,;he isobaric surfaces, for a shielded Lonization chamber (h. a 1,000 g/
OM2). The author points out that the proposed meth,3d, of taking into &a-
cotutt the temperature effect has several advantages; in partioular, it
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29665
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4
1 stethod for determining the tompsrstuzt, ~v A00,I)YI 030
enables one to avoid errors assooiated with xadlitlon hea,iing of the
temperature receivers in meteoruloglo acndeq.
N. Kaminer
[Abstractor's notes Complete
ICY
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2~3
6./OOO/OOt)/().;
1/039
97
A005/A 130
AUTHORs DQXma14,'111.14V,
TITIE8 T~e naturs~o soft radiation in the upper atmosphere
PERIODICAL& Referativnyy zhurnal, Geofizika, no. 6, 1961, 11-12, a!-dtract
6080., (Tr. Xezhdunar. konferenteii po kosmich. lucham, 1959,
Tot,~';. Jlosoow, Ali SSSR# 1960p 87-94)
TEXTs The author studied the nature of the increases in the intensi-
ty cf the low-energy cosmio radiation Bev) that is observed in th
stratosphere at high geomagnetio latitudes. Analysis of the experimenZal
data leads to the conclusion that three types of increase in intensity
exist. The first type in characterized by onset of intensity increase
immediately after an intense chromospheric splash. After attainin5,,a
maximum. the intensity decreases with time according to the law t- 2 or
t-2. T - second type is characterized by increase of radiation intensity
some hoaie after a ohromospherio splash. To the third type belong those
case- when the increase in intensity takes place after the onset of a
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29369
5/16 61/000/006/031j0301
The nature of soft radiation A005YAl 30
magnetic storm, and the decrease in intensity is characterized by an
expcnential correlation. To explain the first and second types of increase
it Is assumed that the pressure of partial6s accelerated in the splash re-
gion. is suffioient to throw out a oloud of magneti2ed plasma from the
sun's surface. If the upper energy limit of the accelerated particlee
is ~~ 10 Bev, they quickly pass through the sun's atmosphere and reach
the earth (type I). Particles of lower energy pass through ;he sur.'s atm
ophe-re and oorona via a channel formed by ejected plasma and arrire: with
a de-lay of bout 1o4 see (type II). Decrease of intensity according tc
the law t-3 2 (or t-2) follows from diffusion theory on considering the
scattering of charged low-energy particles by magnetic inhomogeneitiee
in interplanetary space. To explain the sharp inorease and subsequeai,
decrease of intensity according to exponential law (type III) it Ls
assu.med that at the instant of formation of a oorpuscular stream .)a the
sun a magnetio trap is formed in its frontal part which is capable cl
hoUing baok the captured charged low-energy particies for a long time
(- 10 see). In the absence of marked diffusion of particles In he zTap
volume the distribution of particles will reflect the time dependence of
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29 69
S/16 6110001006/0311039
The nature of softxadiation ... A0059PA130
th-e den$4,ty of pil. "in th*.-sone of generationt i.e., it will have an
exponential obaraq 9'!- to enoounter of the aorpuscular - treorr,
with the earth's m4petic fieldp the trap breaks up and the partiolee ar,-
otlerated on the sun penetrate into high latitudes and cause -rh-~ in,-rc:aee:
of' intensity observed in the stratosphere.
N. Kaminer
[,A.betraotorts notet Complete translation.]
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8/035/61/000/011/011/02B
AGOI/A101
AUMOR: Dorman, LJ
TITLE- On energy spectrum and duration of rising of cosmic ray intensity
on the Earth, caused by a shock wave of a corpuscular stream
P17RIODICAL: Referativnyy zhurnal. Astronomiya I Geodeziya, no. 11, 1961, 35,
abstract 11A262 ("Tr. Yakutskogo fil. AN SSSR, Ser. fiz.", 1960,
no. 3, 145 - 147)
T EXT.- The author investigates the problem of acceleration of charged
particles following a face-on collision with a shook wave front moving In a
m&gnetized plasma. Such a viave may arise in the motion of a solar corpuscular
stream carrying afrozen-in magnetic field. 7be shock wave effect must manifest
itself In a noticeable rise of cosmic ray Intensity prior to the beginning of tt-e
Fcrbush effect. The amplitudes of rising of the penetrating component (" 1%),
and neutron one (3-4% at latitude 500, and 1% an the equator) prior to-the be-
ginning to the Forbush effect on August 29, 1957, which were calculated theore-
tically, do not contradict experimental data. L. Dorman
[Abstracter's note: Complete translation]
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29673
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AO05/A1,30
AUTHORt Dorman, L.I.
--------------
TITLEi Determination of the entorgy spectrum of primary variation in
a very small energy range on the basis of a difference in
effects in Europe and Anerioa
PERIODICALi Referativnyy zhurnalt Goofisikat no- 5P 1961, 14, abstract
5 G 108. (Tr. Yakutakogo fil. AN SSSR, Ser. fiz., 1960, no- 3,
155-157)
TEXTs The author notes the possibility of determining the energy
spectrum of primary variations in the very low energy range by comparison
of tho intensity variations of cosmic rays at points that have the same
goomairnotio latitude but different cosmic ray outoff energies F-mino Such
a poenibility emerges on comparing variations based on observations in
Europo and America. If at geomagnetio latitude X incident to the record-
ing of a component of type i the amplitude of some variation on the ho
level in America equals Ni (h )IN' (h )
Card 1/2 16 X 0 A o j Am, VY"

29673
S/169J61/000/005/038/049
Determ.'.nation of the energy, spectrum A005/A13O
and at the same latitude in Europe equals &N i (h )/Nk (h )
I k 0 o ] Eur,
then the difference between the amplitudes of these variations will bet
N, 6D i -
0' 41Lk D W~ ho) (1)
k (b~
~N (ho)j Am NJ (ho)l Eur
[
where min min min Min
F-k )Eur - (f-?L )Am; 1~ )Am< )Eur (2)
Since the differential coefficients of the relation Wj h ) are known,
it is easy to determine from Eq. (1) the energy spectrum of tRe t D/D (E )
variations of primary cosmic rays, By wyDof exam 1e the author cites the
determination of the energ7 speotrum Of /D (e7variation in the
I-JI-5 .. 2.0 Bev energy range for the intensity decrease of cosmic rays
during the magnetic storm of August 29, 1957.
N. Kaminer
[Abstractor's notet Complete translation.
R--A M/P)

2967h
30,Y10, S/169/61/000/005/039/049
3, 1 if 49 0 ("A P Y/, Id VA) A0054110
AUTHM: Dorman, Lel.
TITLEs Determination of the eartblo point of Impact against a corpus-
oular stream, the oharaoter of the earth's motion within the
stream and stream velocity by detailed investigation of
variation of cosmic ray intensity during magnetic storms
PERIODICALs Referativnyy zhurnal, Geofi2iks, no. 5, 1961, 14, abetract
5 G 109. (Tr. Yakutskogo fil. AN SSSR. Ser. fiz., no. 3P
158-165)
TEXTs The author investigates the assumption that the differences
in observod deoreases of cosmic ray intenoity during magnetic storms are
not deternined by speoiflo properties -if the solar eorpuscular streams
but by tho character of the earth's capture by the stream. Calculations
based upon purely geometric considerations show that incident to capture
of the earth by the lateral side of a slow oorpuscular stream smooth de-
crease of cosmic ray intensity and similar smooth restoration should be
Card 1/2

296 46
S~l ki/oor,/oO5/039/049
Determination of.the earth's point of impact ... L005YA130
observed. This being the case, the amplitude of the effect will be de-
termined by tile magnitude of the magnetio field frozen in the stream and
the earth's distance from the stream axis. Incident to capture of the
earth by the ittream front, the character of the variation of cosmic ray
intensity is d.etermined by the velocity of the stream wid the point of
the earth's entry into the stream (distance from the edge or axis of the
stream). The calculation results enable one 'to determine the stream
velocity and magnetic field distribution in tits stream, from the decrease
profile of coomic ray intensity.
N. Kaminer
Abstractor's notet Complete translation.
Card 2/2

AUTHOR: Doman, L.I.
S/035/6 1/000/009/020/036
A001/A101
TITLE- Or, the nature of changes in intensity of cosmic rays during magne-
tic storms
FERIODICAL: Referativnyy zhurnal. Astronomiya I Geodeziya, no. 9, 1961, 38, ab-
stract 9A299 ("Tr. Mezhdunar. konferentsil po kosmich. luchani,
1959, v. 4", Moscow, AN SSSR, 1960, 113 - 125)
TEXT: The author considers the effect of mitgnetic fields of solar corpus-
cular streams on Intensity of cosmic rays and shouts that 'the profile of intensi-
Ly reducticn durlng magnetic storms Is determined first, by the form or Earth
capture by corptiscular streams and second, by electromagnetic properties of the
streams. Anisotropy of the flux of cosmic rays during motion of the Earth
through the stream is estimated. Calculations are performed for both uniform
and non-uniform fields frozen-in In the stream. A conclusicn is drawn from the
comparlson with experimental data that the field In the stream is non-uniform,
because it is weakened from the advancing side edge to the laFging one and is
intensified markodly near the front edge of the stream,
[Abstracter's no,*,e- Complete translatIon) L. Dorman Vn/
Clard 1/1 ~F

L/
Iq
AUIHOR: Doman. L. I.
3/035/6 1/000/009/021/0,36
A0011A101
TITLE: On energy spectrum and duration of increasing on the Earth of cosmic
ray intensity, caused by the shock wave and albedo from the forward
magnettzed front of a corpuscular stream
PERIODICAL: Referai;ivnyy zhurnal. Astronomiya i Geodeziya, no. 9. 1961, 38, ab-
stract 9A300 ("Tr. Mezhdunar. konterentsil po kosmich. lucham,
1959, v. 4" , Moscow, AN SSSR, ig6o, 132 - 1)9)
TEXT: The author calculates the energy spectrum of primary variations caus-
ed by the shock wave from the forward front of the corpuscular stream. An ana-
logous increase in intensity of cosmic rays must be also observed prior to the
beginning of the Forbush-effect as a consequence of reflection of charged parti-
cles from the forwaixt front of a magnetized corpu3cular stream. This intehsity
increase may attain several per cent in the neutron and penetrating components
on the Earth's surface, There are 8 references.
L. D.
[Abstracter's note: Complete translation] LAB
Card 1/1

28833 S/169/61/000/004/010/026
AOO5/A130
AUTHORSs Blokh, Ya.L.; Dorman, L.I.; Kaminer, N.S.
TITLE% Determination of the nature of earth's capture by streams, and the
properties of corpuscular streams from cosmic ray variations during
sundry magnetio storms
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 1961, 17, abstract 4 0 100.
(Tr. Mezhdune..r. konferentaii po kosmich. lucham, 1959, v. 4. Moscow,
AN SSSR, 196o, 154 - 171)
TEXT: The authors study the variations in intensity of neutron and hard
emission components of cosmic rays during magnetic storms for the period 1954
1959. The intensity variation profile was determined for eaah Individual in-
stance of Forbush effect &ad was compared with the theoretical expectancy for
different assumptions reg&-ding the velocity of solar corpuacular streams, the
nature of earth's capture by streams and the structure of the magnetic field
frozen in the stream. The results of analysis are compared with the nattree of
the geomagnetic disturbancos on the earth and the properties of the active area
of the sun that correspondo to these disturbances. The authors show that two
Card 1/2

28833 5/169/61/000/004/010/026
Determination of the nature oC eartA capture by.... AO05/A13O
types of stream exists 1) long-term extensive streams that capture the earth by
their lateral face, and 2) natTOW short-term streams carrying intense frozen mag-
netic fields. Often the narrcw streams move within the wide streams. The field
intensity In the lateral outstripping section of the stream is on an average -
twice as great as In the lagging section. The density of kinetio energy in the
stream decreattoe markedly for -transition to the lagging lateral etection of the
stream. In the front section of the stream, substantial compression (by a factor
of 6 - 10) of plasma and increase of the frozen magnetic field occur.
N.K.
[Abstracter's notes Complete translation.) UK
Card :q//n
2.

28834 s/i6q/61/ooo/ooVoil/026
A005/A130
AUTHMs Blokh, Ya.L.; Dormin L,_IAj Kaminer, N.S.
__ j_
TITLEs The effect of oosmia ray Intensity increase preceding magnetic stam
PMIODICALt Referativnyy rhurna1. Oeofizika, no. 4, 1961, 17, abutract 4 0 101.
(Tr. Mezhdunar. konferentsil po koemich. lucham, 1959, v. 4. Moscow,
AN SSSR, 178 - 191) 1 ft~o .
TEXrt The authors study the effect of cosmic ray intensity increase pre-
ceding magnetic storms that in due to acceleration of charged particles Incident
to their collision with the fron*,. of the corpusoular stream traveling from the
am. It is shown that this effeat occurred prior to the magnetic storms of July
8, 19,98, and Au&st 29, 1957. The longitudinal distributions of t1ke magnitude
and of the time of onset of the offoot are elucidated. The authorv study the en-
ergy spectrum of the emission reisponsible for anisotropic increase of intensity.
Analysis of the increase In coemlo ray Intensity in the stratosphere on July 8,
1958, suggests to the authors thitt a magnetic trap may exist in the magnetized
frontal section of the corpuscular stream. This trap may carry particles with
energies of some hundreds of Mev that have been accelerated in the active region
Card 1/2 VK

28834 3/169/61/000/004/011/026
The effect of cosmic ray intensity 1norease.... A005/A130
of the sun. Incident to collision of the stream with the earth the tratp breaks
up and the particles arrive in the hAgh-latitude regions of the earth via the
lines of force of the magnetic field. It is shown in agreement with theory that
incident to capture of the earth by the lateral face of the stream the effect in-
crease of intensity prior to a magnetic atom does not occur. Capture of the
earth by the front section of the stream (stoma with sudden onset), on the other
hand, is always acoom.Panied by the effect. No effects of acceleration of cosmic
ray particles by the shoc'k wave generated by the front of the corpuscular stream
was detected.
N. Uminer LX
[Abstracter's note: Complete translation.]
Card 2/2

AUTHOR-
S/058/61/000/010/008/100
A001/AIOI
Dorman, L. I.
On the theory of cosmic! ray modulation by the solar wind
PERIODICAL: Referativnyy zhurnal. Fizika, no. 10, 1961, 94, abstract 10B480
("Tr. Mezhdunar, konfer*ntaii po kosmioh, lucham, 1959, v, 4",
Moscow, AN SSSR, 1960, 328-334)
TEXr- The problem of the nature of 11-year variation in cosmic ray
intensity is 'investigated. Experimental data are compared with effeot5 expected
from theories of-modillati6n of the galactic flux of cosmic radiation, advanced
by Parker and Singer; it is shown that these theories cannot fully explain
variations in the spectrum of cosmic radiation with the solar activity cycle.
If the broad speotrun of non-homogeneities of the magnetic field in the inter-
planetary medium is taken into aocouat, an agreement can be secured between the
experimentally observed and theoretically expected energy spectra of 11-7ear
variation of the primary cosmic radiation.
L. Dorman
(Abstraoterle notet Complete transl4stion]
Card 1/1

VEIINOV, S.Nop otv. red.; kand. fiziko-matem.nauk, otv. red.;
PODOLISKIY, A.D., red. izi-va; GOLUB', S.P.) tekhn. red.
(Collection of articles] Sbornik statei. Moskva, Izd-vo Akad.
nauk SSSR. No.4. 1961. :258 P- (MIRA 15.6)
1. Akademiya nauk SSSR. 143zhduvedomstvenryy komitet po provedeniyu
Mezbdunarodnogo geofizich)skogo goda. VII razdel prograuw 14GG.
Kosmicheakiye luchi. 2. C:olen-korrespondent Akademii nauk SSSR (for
Vernov).
(C-3mic rays)

S/058/62/000/010/0)W/093
Ao61/Aiol
AUnIOR: Doman, L. r.
T17"LE: Current concepts on cosmic ray variations
PERIODICAL: Referativryy zhurnal, Fizika, no. 10, 1962, 61, abstract 105154
(in collection: "Kosmicheskiye luchi, no. 3", Moscow, AN SSSR,
1961, 5 - 63, summar"I In English)
TEXV: This is a review of fundamental work done on the subject of~time
variations of cosmic rays In the Soviet Union and In other countries, particu-
larly during the International Geophysical Year. Discussed are questions of how
to improve methods of eliminating extraneous factors from time variation data,
and also studies concerning different categories o~ variations and electromag-
netic processes originating in the neighborhood of the Sun, In the interplahe-
tary medium, and In the neighborhood of the Earth. Special attention is devoted
.to two categories of cosmic ray variations: effects of modulation and effects
of solar flares.
rAbstracier's note: Complete translation]
Card 1/1

3/169/62 0 O/M/069/103
3, 0 'x0 5-j 'Z 7 10 ;7j 2 91 or) D218/D302
AUTHORS: Glokova, Ye.S., Dorman, L.I., and Kaminer, N.S.
TITLE--: On the method of introducing meteoroloLgical correc-
tions into the cosmic-ra-Y intensity data
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 1962, 13, ab-
8tract 4G68 (V. sb. Kosmicheskiye luchi, no# 3, M-P
AN SSSRj 1961, 149-162)
TEXT: A method of introducing meteorological corrections to the in-
tensity data for p-meson and neutron coemic-ray components is dis-
cussed. It is shown that it is 13UffiCient to introduce only the cor-
rection for the barometric effect, When the barometric correation
is computed, the exponential dependence of the intensity of the neu-
tron component on the atmospheric pressure must be borne in mind.
In the presence of large temperature variations, the neutron compo- LX
nent may exhibit variations of -;emperature origin, and in order to
take these into accountp the thooretical distribution of the tempe-
rature coefficients must be emp:.oyed. A detailed description is gi-
ven of the method whereby the barometric and temperature effects
Card 1/2

S/16 62/000/004/069/103
On the method of introducing ... D218YD302
can be taken into account for the hard component. Examples are gi-
ven of how tables of meteorological corrections, suitable for prac-
tical purposeep can be set up. The most accurate methods of extra- V~
polation of aerological data on the temperature of the upper layers
of the atmosphere are indicated. [Abstractor's noteoi Complete trans-
lation].
Card 2/2

37286
169/62/000/004/071/103
3, ~Y 10 (2,;z-os~ ';t- 2 or, )kor) DS/218/D302
AUTHOR.S: Blokhq Ya.L., Dormwi, L.Ip and Dubrovin, BI.V11.
TITLE: Meteorological effecto of cosmic rays under the
earth's surface
PERIODICAL:- Referativnyy zhurnal. Geofizika, no. 4, 1962t 13, ab-
stract 4G70 (V. eb. Kosmicheskiye luchi, no. 3, M.,
AN SSSR, 19610 166-169)
TEXT: A study is reported of meteorological effects in the p-meson
component of cosmic rays based on underground recordings in Moscow
(40 m) and Yakutsk (60 m~ in 1957 - 1958. The triple-correlation
method was used to determine-theA partial and total correlation and
regression coefficients a and 0 between the observed cosmic-ray in-
tensity variations, the barometric pressure and the temperature of
the atmosphere, (P is the baromatric coefficient and a is the tem-
perature coefficient representing atmospheric temperature variatiors
up to heights of 12 - 20 km). Although the values of a and P obtai-
ned for separate months exhibit a large spread, their average values
are quite reliable and are in good agreement with the theoretical
Card.1/2

S/169/62/000/004/071/103
Meteorological effects of cosmic ... D218/D302
results. For Moscow (40 M) : 0 = (-0.050 � 0.007) %/mb and for Ya- Or
kutsk (60 m): p = (-0.029 � 0.006) %/mb. Comparison of the values
of a shows that the upper layers of the atmosphere play an impor-
tant role in producing the temperature effect in the hard component.
LAbstractor's note: Complete translation].
Card 2/2

S/058/62/000/010/045/093
;06-11A101
~2 Ll
AUTHOR: Darman, L. 1.
TITLE: Calculation of the integr~ated.multiplicity of muon generation in
the earth's atmosphere for observations.under different bsorber
thicknesses
PERIODICAL: Referativnyy zhurnal, Fizika, no. 10, ic,162, 61 - 62, abstract 10B459
(In collection: "Koamicheskiye luchi, no. 3, ", Moscow, AN SSSR,
1961, 1711 - 198, summary in English)
TEXT: The integrated multiplicity of muon generation has been calculated
for observations at sea level and at different depths underground, using differ-
ent model representations of the elementary interaction event of primary parti-
cles with atomic nuclei of the air. It is assumed U-.-at the first interaction of 2
a primary particle with atomic nuclei of the air takes place at a depth ofxg/cm
where ,
'k denotes the interaction range, and the subsequent interactions take place
discretely at depths of 2 etc. The calculation of ionization losses
and muonic decay Is or essential importance in this connection. The fluctuations
in the depths of the first and following collisions, the spectrum of pion
C~~ 1/2

S/058/62/000/0 10/045/093
Calculation of the integrated multiplicity of... A061/A101
generation, their capture and decay Into muons are more accurately taken into
consideration. Once the integrated multiplicity has been found for different
versions and different cases of observatlon,.It is possible to determine the
differential muon spectrum at sea level and at different levels underground, as
well a5 the Intensity curve with depth. A comparison with observational results
pern1ts an estimate of the extent to which a choice of one or other value Is
essential for parameters determining the elementary interaction event of primary
particles with atomic nuclei of the air. Detailed numerical calculations are per-
formed for the cases where 20, 40, and 50% of the incident nucleon energy is
transferred to the muons. The muon spectrum found theoreticz.lly at sea level and
the curve of the Intensity change with depth are compared with experimental data.
The poor response of measurement results to the choice of elementary interaction
parameters within a wide range of the latter is noted. The nuon intensity is Cal-
culated as a function of the geomagnatic threshold for different absorber thick-
nesses. The expected changes of spectrum and muon intensity with a change of so-
lar activity (in connection with changes In the energy spectrum of primary per-
ticles) are also calculated.
(Abstracter's note: Complete translation]
Card 2/2

s,'058/62/000/010/039/093
o A0611A101
AUTHOR: Doman, L. 1.
TT11E: On the interrelation factors between primary and secondary
variations of cosmic rays in the high-energy range
PERIODICAL: Referativnyy zhurnal, FlAika, no. 10, 1962, 61, abstract 1013453
(In collection: "Kosmicheskiye luchl, no. Moscow, AN 5,35R,
1961, 199 - 204, summary in English)'
TEXT: Using the integral multiplicity functions of muon generation for
different absorber thicknesses, that have been calculated in a preceding paper
(abstract 1OB1159), the author determines the interrelation factor for the con-
version from secondary variations of muon intensity at sea level and at differ-
ent depths underground to primary variations of cosmic rays at the boundary,of
the atmosphere.
FAbstracter's note: Complete translation)
Card 1/1

s/169/62/ooo/oo8/068/090
E032/EI14
AUTHOR: Dormant
TITLEs Variation in the coefficients of coupling between
primary and secondary variations of cosmic rays with
changes in solar-activity. Som. practical problems
in the determinatign of the spectrum of the
variations.
PERIODICAL: Referativnyy zhurnal, Geofizika, no.8, 1962, 11,
abstract 8 G 81. (In the Sympo.-sium: lKosmicheskiye
luchi, no.31 ('Cosmic Rays. no-P), M.t AN SSSR,
1961, 205-210. (abstract in English)).
TEXT. Data on changes
cosmic rays with the solar
changes in the coefficients
sensitive to variations in
of the primary radiation.
for epochs corresponding to
minimum and may be used in
Card 1/2
in the energy spectrum of primary
activity cycle ar 'e used to calculate
of coupling between component 15
the low-energy part of the spectrum
The coupling coefficients are computed
the solar activity maximum and
the recording of cosmic rays from

Variation in the coefficients of ... s/169/62/000/008/o68/ogo
E032/EI14
rockets and satellites, and also in the recording of the neutron
and ji-meson components at the earth's surface and in the
atmosphere. A brief description is given of the methods used to
determine the energy spectrum of the variations in the intensity
of the primary radiation. The effect of the position of the
cut-off due to geomagnetic disturbances on the results of
determinations of the energy spectrum of variations in the
primary radiation is estimated.
[Abstractorls note: Complete translation..]
Card 2/2

AUTHOR;
31238
1-i/169/62/000/004/073/103
D218/D302
TITLE: On the nature of the lunar diurnal variation in cosmic
rays
PERIODICAL: Referativnyy zhurnalt Geofizikaj no. 4, 1962v 14, ab-
atract 4G72 (V. sb. KOBMicheskiye luchi,, no. 3, M-P
AN SSSR9 1961p 253-255)
TEXT: It is shown that the observed lunar diurnal variations in
the cosmic-ray intensity may be associated with the amplitude and
Dhase modulation of the so.Lar-diurnal variation oy the 27-day wave.
~7-day variations in the solar-diurnal el ''fect should lead to the
apps-arance of two waves with periods of 23#2 and 24.9 hours in addi-
tion to the wave with a period of 24 hours. One of the harmonies
(24.9 hours) coes in fact have A period close to the period of the
iunar-aiurnal variation. When it will oe round experimentally that
ooth harmonics are preBentt This will indicate that the lunar-diur-
nal wave is spurious. If, on the other handt the experimental data
confirm the presence of the harmonic with a period of 23.2 hours,
Card 1/2

I
S/169/62/000/004/073/103
On the nature of the lunar diurnal ... D218/D302
then the lunar-diurnal wave will be expected to be real. [Abstrac- ~~
tor's note: Complete translation].
Card 2/2

J7,289
13/16 %000/004/074/103
3,91)-o D218YD30
J, 2. Y / 0 ( ~
AUTHORS: Dorman L.I., Blokh, Ya~L#p and Kaminer, N*S#
TITLE: The character of the increase in the cosmic-ray inten-
sity at the Forbush-effect minimum
PERIODICAL: Referativnyy zhurnalo Geofizika, no. 4, 1962, 14, ab-
stract 4G73 (V. ob. Koemicheskiye luchi, no. 4p Mov
AN SSSR9 1961P 5-15)
TEXT: The method of coupling coefficients is used to investigate
the increase in cosmic-ray intensity during the principal phase of
geomagnetic storms which is due to a reduction in the H-component
of the magnetic field, and the compression of the volume of the geo-
magnetic field by a corpuscular stream. A theoretical calculation
is given of the effects expected in the various secondary compo-
nents of cosmic rays at sea level and in the mountains. The results
of these calculations are oompared with experimental data obtained
by the world station network during the magnetic storms of Septem-
ber 13, 1957 and Pebruary 110 1958. It follows from the analysis of
these_~wo cases that the observed increase in the cosmic-ray intens-
Card (!,D

S/169/62/000/004/074/103
The character of the increase in the ... D218/D302
ity is in fact associated with a reduction in the geomagnetic cut-
off threshold during the principal phase of a magnetic storm. It is
noted that in the case of the hard component the effect is only par-
tly due to the change in the geomagnetic threshold. A part of the
effect is due to a disturbed solar-diurnal variation. It was foun6
that there is not only a latitude, but also a longitude dependence
of the amplitude of the increase, and hence it follows that the ca-
vity which appears as a result of the flow of the corpuscular stream
round the geomagnetic field is not axially symmetric in form. It is
concluded that geomagnetic storms with sudden couLmencement are pro-
duced as a result of the capture of the earth by the leading front
of a solar corpuscular stream which flows round the geomagnetic
field with ultrasonic velocitY- LAbstractorlq note: Complete trans-
lation].
Card 2/2

;t 7 -ON.; .7eos)- S/169/62/000/004/076/103
D218/D302
AUTHORS: Blokh, Ya.L.# Kaminert N.S., and Dorman? L.J.
TITLE; Cosmic-ray effects preceding a magnetic storm
A'OBRIOM CAL; Referativnyy zhurnal, Geofizikap no# 4p 1962, 14p ab-
stract 4G75 (V eb. Kosmicheskiye luchi, no. 4t Met
AN SSSRt 1961p 25-30)
TEXT: Discusses the interaction of the magnetized front of a cor-
puscular steam with cosmic rays which may give rise to the appear-
ance of certain effects just before the onset of a magnetic storm.
A corpuscular stream produces a shock wave in the interplanetary
space, and the magnetic field of this wave interacts with cosmic-
ray particles. Reflection of the particles from the wave front gi-
ves rise to their accelerationt and therefore the intensity of the
radiation should increase before a magnetic storm. The expected
spectrum of this variation is relatively soft. After the earth has
entered the disturbed medium behind the 13hock wave front, where the
magnetized interplanetary plasma is comp:~eesed and the field is
corre~q ndingly enhanced, the cosmic-ray intensity should decrease.
Card 1
1~
I-i-31

8/169/62/000/004/076/103
Cosmic-ray effects preceding a ... D218/D302
This effect is anisotropic and the character.of the anisotropy de-
pends on the direction of the interplanetary magnetic field. Reflec-
tion of cosmic-ray particles directly from the magnetized front of
the moving corpuscular stream shouid leact to an anisotropic increa-
se in the intensity, a few hours prior to the beginning of the r*eo- V~
magnetic storm# This type of increase in the intensity has in fact
been observed before a number of geomagnetic storms accompanied by
large Porbush effectso (Abstractor's note; Complete translation].
Card 2/2

37280
S,/169/62/000/004/065/103
~-Y 30 D;228/D302
AUTHORS: Kaminer, N.S., Blokh, Ya.L., and'Dorman,_1&I*
TITLE: The emission duration and the angular width of solar
corpuscular flows
PE'RIODICAL: Referativnyy zhurnal, Geofizik-a, no. 4, 1962t 10p ab-
stract 4G53 (V ab. Kosmich. luchi, no. 4, M., AN SSSRt
1961, 31 - 34)
TEXT: The width of solar corpuscular flows is determined from the
profile of Forbush-effects in cosmic rays; this is then compared
with the angular width (the longitudinal extent) of the active re-
gions on the sun that have caused the Generation of these corpuscu-
lar flows. A positive correlation .,ith a correlation coefficient of
--j 0.9 and a regressian coefficient of \j1 was discovered between
these two parameters. The estimation of the angular flow width acca-
ding to geomagnetic disturbances gives a considerably smaller angu-
lar width. The possible causes of the diverly.,ences in the estimation
of the flow.width by these two methods are briefly discussed. A
number of arguments are cited in favor of the fact that geoeffecti-
Card 1/2

B/169/62/000/004/065/103
The emisaion duration and the ... D228/D302
ve corpuscular -'Plows are continuously emitted by active regions du-
ring long intervals of time (several revolutions of the sun)# At
the same time it is Possible that plasma clouds are ejected from an
active region when the emission of a corpuscular flow has yet to be
completed. [Abstractor's note: Complete translation]. Ll~
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37293
S/169/62/000/004/078/103
3, 2. Y / 6 (,1 2,0-rfi 2 7 10 9, / 2- 0 a r) D218/D302
AUTHORS: Dormang 1~.I.,.~aminer, N.S., and Blokh, Ya.L.
TITLE: On the nature of the preliminary reduction in the
cosmic-ray intensity before a magnetic storm
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 1962t 14-15,
abstract 4G77 (V sb. Kosmicheskiye luchi, no. 4, M.,
AN SSSRt 1961t 49-58)
TEXT: A discussion is given of the nature of the preliminary reduc-
tion in the cosmic-ray intensity which is observed before the onset
of many magnetic storms accompanied by the Forbush e9fect. The mo-
tion of a corpuscular stream with a velocity of -_j10 cm/sec
through interplanetary medium containing a weak magnetic field,
should lead to the appearance of a shock wave moving towards the
earth with a velocity equal to 4/3 of the velocity of the stream.
The magnetic field of the medium behind the shock wave front is en-
hanced. flenceo the arrival of the shock wave at the earth should be
accompanied by a reduction in the cosmic-ray intensity. If the in-
terplanetary magnetic field is regularp and is directed at right
Card 1/2

S/169/62/000/004/078/103
On the nature of the preliminary ... D218/D302
angles to the plane of the ecliptic in the same sense as the earth's
field, then the maximum reduction in the intensity should be obser-
ved for particle streams arriving from the West relative to the sun
-earth line. In order to confirm these conclusions on the basJs of
the world station network data, an analysis was carried out of the
cosmic-ray intensity variations during periods preceding major geo-
magnetic disturbances and Forbush effects. A,study of the longitu- 01
de and latitude dependence of the preliminary reduction in the in-
tensity shows that the effect is particularly appreciable for those
groups of stations for which the particles arrive preferentially
from the direction of the sun, or from a direction west of the
earth-sun line. The spectrum of the preliminary reduction effect is
close to the Forbush decrease spectrum, although it is slightly sof-
ter than the latter. LAbstractor's note: Complete translation].
Card 2/2

S/15 Q2/000/005/071/093
D223YD3'07
Kaminer, N. S., Dorman, L. I. and Blokh, Ya. L.
TITLE: The magnetic storm in mid-May 1959 and cosmic ray
variations
PERIODICAL: Referativnyy zhurnal, Geofizilia, no. 5, 1962, 10, ab-
stract 5G83 (V sb. Koamich. lu-chi, no. 4, X., AN SSSR,
1961, 59-63)
LI -
TEXT; The intr4cate cOn2lex of phenomena, observed in cosmic rays
.Ln oonnection with the solar chromospheric flare of 10/V/1959, is
bein,ul sludied from the data of the world station network, These
"'i .nolude: the large increase in the intensity of soft
). enomena i. L, L.
1
cosmic rays of a solar origin in the stratosphere in high lati-
tudes, the Forbush-effect, the intensity increase before the be-;..'
ginning of the 6eomagnetic storm, etc. A marked increase in the
ln-uensizy of cosmic rays was noted for several days before -#;he
st.art of the Porbush-effect. The peculiarities of this pher.,~menon
-compel one -to assume that it is due to the arrival of an additio-
Card 1/3

3/169/62/000/005/071/093
The magnetic storm ... D228/D307 -
n1- 1 radiation f low, generated on the sun and comin, towards the
t:'
ear-,,h as a result of diffusion in magnetic i::-regularities with a
field in'tensity of-13 x 10-4 _ 10-3 gauss. The beginning of the
For;O,ush effect of May 11 occurred simultaneovaly throughout the
world. In the first place the reductionla effect started at sta-
tions where Particles, coming from westwards directions in rela-
tion to the line sun-earth, were recorded. ILI these stations the
reduction's effects began three hours before the outbreak of the
-wards direc-
geomagnetic storm. For particles arriving from east
tions in rela-cion to the line sun-earth, the Bffect commenced
2 - 3 hours after the beginninm of the storm. The epigenetic spec-
trum of the primary radiation's variation during the Forbush ef-
.ect was determined. This spectrum agrees with the supposition
that, cosmic rays are scattered by the regular magnetic field fro-
zen Lnl.o the flow. The parameters of the corpu.scular flow and of
the magnetic field I*rozen into it were ascertained from the pro-
file of the Forbush effect. The flow's width amounts to 5 x 1013
_cz, the mean intensity of the field in it being -,6 x 1070 gauss.
Card 2/3

S/1 69/'62/000/005/0'71/093
D223/1;307
,.qe nature of the increase in the intensity in the minimum of the
23rbush effect, observed on IMay 12-14, is dis.-ussed. It is shown
that only a small part of the effect of the int"en3ity's increase
u
by the change in the geomagnetic trim-ning threshold;
main cause of this phenomenon may be the anisotropic screening
of -.he earth by the corpuscular flow. Z-Abstracter's note: Com-
'e
te translation-2
Card 3/3

:i729L.
S/169'62/000/004/079/103
D2187D302
AUTHORS: Blokh, Ya.L., Dormanp L.I.p and Kaminert N.S.
I---------------------
TITLE: On the superposition of Forbush effects in July 1959
PERIODICAL: Referativnyy zhurnal. Geofizikap no. 4, 1962t 15, ab-
stract 4G78 (V ob, Kosmicheakiye luchip not 4l Mot
AN SSSR9 1961, 84-95)
TEXT: A detailed study is reported of the character of the super-
position of Forbush effects in July 1959. Analysis of world station
network data showed that the observed phenomena may be explained by
assuming that the modulation of cosmic rays is due to regular nagne-
tic fields frozen into corpuscular streams. The second and third
Forbush decreases occurred as a result of the simultaneous capture
of the earth by two or even three corpuscular streams. The proper-
ties of these streams, their dimensions and the intensity of the
frozen-in magnetic fields are determined, The energy spectrum of
the increase in the cosmic-ray intensity observed on July 17 is de-
termined, Analysis of this effect is used to estimate the intensity
of the magnetic field of the stream which is found to be in good
Card 1/2

B/169/(;2/000/004/079/103
On the superposition of Forbush ... D218/D'02
agreement with the value obtained from an analysis of the profile
of the Forbush effectolAbstractor's note: Complete translation].
t./,
Card 2/2

') 72 95
S/169/62/000/004/080/103
D218/D-4102
AUTHOR: Dorman, L.I.
TITLE: On the effect of a solar corpuscular stream in the
form of a magnetized shell on cosmic rays
PE'RIODICA1: Referativnyy zhurnal. Geofizika, no. 4, 1962, 15, ab-
stract 4G79 (V ab. Kosmicheakiye luchip noo 4p Mar
AN SSSRv 1961p 96-121)
TEXT: A study is reported of the modulation of the intensity of.
the galactic stream of cosmic rays by a solar corpuscular stream in
the form of a thin-walled magne:,:,Red shell Omagnetic sack'). The
importance of the following'factors is estimated: Absorption of
cosmic-ray particles by the sun, change in the intensity as a re-
sult of the expansion of the shell, exchange of particles through
the surface of the shell leading to equalization in the particle
densityt change in the reflecting properties of the shell on expan-
sion. The solution of a differentiai equation for the particle ba-
lance, which simultaneously takes into account these factorep was
Card 1/2

S/169/6,2/000/004/080/103
On the effect of a solar ... D218/D302
used to determine the energy spectrum of the variations for a shell
in the form of a.aphere and a spherical sector. Im addition, the
General solution is obtained for a shell of arbitrary form and an VI(
incompletely closed shell. Numerical results are given for diffe-
rent values of the velocity and dimensions of the shell, and vari-
ous assumptions regarding its properties. The calculations were car-
ried out both for relativistic and non-relativisl;ic cases. [Ab-
stractor's note: Complete translation].
Card 2/2

37 25~6
S/169/62/000/004/081/103
I)218/D302
AUTHOR: Dorman, L.I.
TITLE: The earth as an absorber of cosmic rays and its role
in producing Forbush-type effects, and 27-day and
11-year variations
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 3, 1962, 15, ab-
stract 4G80 (V sb. Kosmicheskiye luchi, no. 4, M-9
AN SSSRt 19619 122-127)
TEXT: A theoretical discussion is given of the effect of a local
ausorber on the particle density in a scattering medium. It follows
from the calculations that if the earth is surrounded by a scatte-
ring medium consisting of magnetic irregularities, then the cosmic-
ray Intensity near the earth should be reduced. This reduction de-
pends on the properties of the nedium. In particular, during nagne-
tic storms and also during changes in the level of solar activity,
the scattering properties of the interplanetary medium near the
earth should chan-ge considerably and this should lead to changes in
the cosmic-ray Intensity at the earth. The dependence of the ampli-
Card 1/2
vy,

The earth as an absorber of ...
tude of the expected effect on the mean
and the intensity distribution near the
ned. Special cases of the capture of the
with finite and infinite dimensions and
to particle exchange), semi-transparent
discussed. [Abstractor,s note: Complete
S/169/62/000/004/081/103
D218/D302
free path for scattering
absorbing body are determi- /
earth by clouds of plasma
transparent (with respect
and opaque boundaries are
translation].
2/2

3,),qi 0 (7 7e. 5, -A-7 C)S~ 28 0.1;
AUTHOR: Dormang L.I.
37297
B/169/62/000/004/082/103
D218/D302
TITLE: Cosmic-ray variations due to an expanding turbulent
magnetized cloud
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 1962, 15, ab-
stract 4GB1 (V sb. Koemicheskiya luchi, no. 4, M.,
AN SSSR, 19619 128-131)
TEXT: Cosmic-ray intensity changes at the earth due to the capture
0f the earth by an expanding iurbulent magnetized piasma cloud ar-
riving from the direction of the sun are discussed. The problem is
solved for the stationary spherically symmetric case on the assump-
tion that the range to a scattering event depends on the distance
to the cen-Ger of a cloud. The expected reduction in the cosmic-ray
intensity at the earth's orbit is found for a cloud velocity of u
3 x.10 cm/sec and particle velocities of v = 101C am/sec and v =
3 x 1010 cm/sec. A considerable reduction in the intensity is to be
expected for rglatively small values of the mean free path for scat-
tering (X -j1O11 am), i.e. for low-energy particless Moreoverp the
Card 1/2

S/16 62/000/004/082/103
Cosmic-ray variations due to an D218YD302
deceleration of field irregularities by the interplanetary medium
is taken into account in the stationary case. Here alsot appreciab,
le changes in the intensity are only possible for values of which
are much smaller than 1013 cm. Hence the magnetic fields which are
necessary at the earth's orbit to give rise to ef ,fective scattering
of particles with t -,~ 1010 eV are H ;~-,3 x 10-6 g1lusse [Abstrac-
tor's note: Complete translation].
VI(
Card 2/2

3725.8
o)
6;1 0'7 S/169/62/000/0041/083/103
3,1 ~60 D218/D'302
AUTHORS; Kaminerl N.S.0 Blokhq Ya.L.9 and Dormanp L.I.
TITLE: The cosmic-ray flare of May 4, 1960
P.'"4"RIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 19629 15, ab-
stract 4G82 (V sb. Kosmicheskiye luchip not 4, Met
AN SSSRv 1961, 146-167)
TEXT: The world station network data are used to investigate the
increase in the cosmic-ray intensity on May 4, 1960. A chromosphe-
ric flare of importance 3 was observed on the vrestern limb of the
sun at 10 hr- 5 min. It was accompanied by a series of radio bursts
on 92.209 and 600 111c/sec. By acting on the ionosphere, the ultravio-
let emission from the flare gave rise to a reduction in the criti-
cal frequency of the P2 layer and the appearance of a bay-like dis-
turbance in the H-component of the geomagnetic field. After 15 to V,
20 minutes, there was a rapid increase in the cosmic-ray intensity.
It fullovis from the analysis of the data that in the initial stage
of the increase in the intensity, the additional radiation was ani-
sotropic. The method of coupling coefficients is used to calculate
Card 1/2

S116SV621000100410831103
The cosmic-ray flare of ... D218/'D302
the distribution of intensity over the earthlij surface. The real
spectrum of the additional radiation and the Tinite extent of its
source are taken into account. Comparison with experimental data
shows that on the first approximation the intensity distribution It
corresponds to the position of the shock zone3. However, better
agreement between experimental and theoretical results is obtained
if it is assumed that the shock zones are considerably wider, or
that they are displaced by 30 to 400 to the East. The possible rea-
sons for this displacement are discussed. The energy spectrum of
the emission of the flare and the time variation in the intensity
are determined. The dimensions and the intensity of the magnetic
field of scattering irregularities in the interplanetary medium are
estimated. 32 references. LAbstractor's note: Complete translationj.
Card 2/2

312 v 3D
37299
S/16SV62/000/004/084/103
D218/D302
AUTHOR: Dormant L*Is
TITLE: Cosmic-ray flares in connection With the properties
of corpuscular streams and electromagnetic conditions
in the interplanetary medium and the earth's neighbor-
hood
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 1962, 15-16,
abstract 4G83 (V ab. Kosmicheakiye luchit no. 4, M-t
AN SSSRp 1961, 168-172)
T13M The main energy and time characteristics of cosmic-ray fla-
res are briefly discussed in connection with the electromagnetic
properties of corpuscular streams and the interplanetary medium.
Possible mechanisms of generation of fast particles in solar chro-
raospheric flares# the character-of propagation of these particles
in the solar super-coronat and -the possible :paths of their transport
to the earth (magnetic traps of corpuscular .3treams, diffusion in
interplanetary magnetic fields) are discussed. (Abstractor's note:
Complete translation].
Card 1/1

S/169/62/000/005/073/093
-3. A WO D228/D*2107
IAI U T.H 0 2-3 !)orman, *..I.- and Shataah,viliq L. Kh-
T Lnvest4gation of the 27-day cosmic ray variations from
C~
the da-.a of the world network of IGY stuations for the
-Decer-ber 1957
period July
?%-jTODICAL: 2,cferativnyy zhurnal, Geofiz-ka, no. 5, 19621 11, ab-
stract 5G85 (V sb. Kosmich, :.uchi, no. 4, M., AN SSSR,
19061, 179-201 )
T7-XT: "Iie properties of the 27-day variation in the cosmic ray
are investigated, as are -'%-,he changes in the solar and the
~eoma6n-etic activit in ' he period of the solar activity maxinum
~
j-aly-Dacenber 1957~. Itis sh-own that the terdency'to a 27-day re-
currence during the period under consideration is better-displayed
in cos--4L-- rays than in the solar and the geommagnetic activity. Mag-
netic which are accompanied by Forbush-effects in the cos-
--ys, are observed near t.he minimum of the 27-day wave. Dn all
the 27-day reTet'-''*ion is bect di,p',ayed if days with
Card '1/2

S/16 62/000/005/073/093
V- Lration of the ...
D228YD307
ex-~re-.ie values of the intensity of the neutron cosmic-ray component
are chosen as the zero days (wher, Using the epochal imposition zie-
~.hod). r2heepigenetic spectrum of the 27-day variation is determined
-from tfe latit-udinal change ir, the effect's ampiitude by m,~ans of
the coupling factor meth.od. The epigenetic spectrum :Calls as the
Oarticle energy increases and agrees with the results of measure-
ments o,~' the tolal component in ihe atratoaphere and of the hard
L U
con"ponent underground. It ia conclud..-d that in this period the
27-day variation in the intensity was rela*,,ed to the stable region
of e_c-:;4_ve lon-itudes on the sun. /-Abstracl-.er's note: Complete
tran3lation._~
Card 2/2

>70
AUTHOR: Dorman, L.I.
37300
S/169/62/000/004/085/103
D218/D302
TITLE: On cosmic-ray variations due to asymmetric solar wind
PERIODICAL: Referativnyy zhurnal. GeofizikELp no. 4, 1962, 16, ab-
stract 4GS4 (V ab. Kosmicheakiye luchi, no. 4, M.,
AN SSSRt 19619 204-208)
TEXT: Assuming that -the radial, flow of magnetic field irregulari-
ties from the sun may be spherically asymmetric, a calculation is
made of the cosmic-ray intensi-.y variations associated with an asym-
metric transport and diffusion of particles. An approximate solu-
tion is found for the equation of diffusion with transport for the
case where the asymmetric field may be represented in the form of a
spherical sector whose leading front moves with a constant velocity.
This asymmetric field is characterized by a diffusion coefficient
which may be very different from the diffusion coefficient in a
spherical region in which the magnetic irregularities move with the
so,me velocity. Cosmic-ray intensity variations in space and time
are calculated inside this region. [Abstractor's note: Complete-

37301
S/169/62/000/604/086/103
D218/D302
AUTHORS; Dormant I#L.p and Inozemtseva, 0.1.
TITLE: Experiments with crossed telescopes and the nature of
the eolar-diurnal variation in co8mic rays during the
maximum and minimum of solar activity
FE"RIODICAL: Referativnyy zhurnal. Geofizika,-no. 4, 1962, 16, ab-
stract 4G85 (V sb. Kosmicheskiye luchit no. 4, Mot
AN SSSR, 1961t 2C9-224)
TEEM A study is reported of the solar-divirnal cosmic-ray intensi-
ty variations on the basis of data obtained with crossed counter te-
lescopes. It is shown that the introduction of temperature correc-
tions into the data recorded during minimun solar activity conside-
rably modifies the observational results. If during the period of
a solar-activity maximum, the phase of the diurnal variation from
the I-East' leads the phase from the 'West', and the phase from the
'North' leads the phase from the 'South', -then during the years of
minimum activity the opposite situation occurs, namely, the phase
from the 'South' leads the phase from the 'North', and the phase
Card 1/3

s1/1()9/62/000/004/086/103
Experiments with crossed telescopes ... D218/D302
frorr the 117est' leads the phase from the 'Bast'. The results obtai-
ned are used to determine the properties of the sources of the diur-
nal variation at the minimum of solar activity. The method of coup-
ling coefficients is used to find the sensitivity of crossed tele-
scopes for primary particles of various energies. Next, corrections
are introduced for the deflection of primary particles with ener-
Gies between 7 and 200 BeV in the earth's magnetic field for vari_ VY
ous directions of arrival of the particles. This enabled the authors
to discover two sources of diurnal variation during the period of-
minimum solar activity. The first source is responsible for the mo-
dulation of the.particles arriving only from directions close to
the piane of the ecliptic; it is capable of explaining completely
the diurnal variation from the western and northern directions. The
diurnal variation from the western and northern directions is*part-
ly due to the first source and partly to the second. In contrast to
the first source, the second is a high-latitude source and provides
a good explanation of the experimental diLta if it is assumed that
cosmic rays with energie- in excess of 50 - 100 BeV are associated
--he low-latitude source is localed to the left of the sun-
7- 'A -
earth line and is apparently connected wi*:h corpuscular streams,
Uard 2/3

8116 62/000/004/086/103
-'Experimentus with crossed telescopes D218YD302
The second source lies to the right of Tb.e 8un-earth line and is
associated with the preferential arrival of particles of galactic
origin frow the center of the Galaxy. The: strength of this source
si,.ouid be variable and should depend on i,he degree to which the in-
Lerplanetary space is filled with iaagnetized turoulent elements, i.
e. it should depend on the level of solar activity* [Abstractor's
note: Complete translation].
Card 3/3

3 73 04
S116 62/000/004/089/103
3, --kLJ 10 ()"-Po r, -k70 r, ~.Cos) D218YD302
AUTHORS; Dormang L.I.p and Inozemtsevat 0.1.
--------------------
TITIZ: On the nature of the diurnal. variations of cosmic ra-
diation arriving at the earth from various directions
which are disturbed during magnetic storms
PERRIODICAL: Referativnyy zhurnal. Geof12',ika, no. 4, 1962t 16, ab-
stract 4G88 (V ab. Kosraicheekiye luchi, no. 4, M&p
AN SSSR, 1961, 237-250)
TEXT: Using the directional properties of crossed counter telesco-
pes, and data on charged-particle trajectories in a geomagnetic
field, a study is made of the disturbed solar-diurnal variation in
the cosmic-ray intensity. Use is made of continuous measuremen. 4, s of
the hard component at sea level (south-north) and at depths of 7,
20 and 60 m below ground (southrnorth) and also neutron-conponent
measurements. The method of coupling coefficients is used to deter-
miine Ihe diurnal variation in the intensityt depending on the direc-
tion of arrival of the particles before the onset of gecmagnetic
storms accompanied by the Porbush effect, during the period of the
Card 1/2

S/16 62/000/004/089/103
On the nature of the diurnal ... D218YD302
principal phase of these storms, and also during the recovery in
the intensity following the Forbush effect minimum. It is shovin
that in order to explain the observed properties of the solar-diur-
nal variation it is necessary to take into account the effect on
the cosmic rays of not only solar corpuscular streams but also pro-
cesses in the immediate neighborhood of the earth. In particular,
analysis of the data shows that during geomagnetic disturbances the
magnetic field at large distances from the earth's surface is not
spherically symmetric. [Abstractor's note: Complete translationj.
Card 2/2

37305
S/169/62/000/004/090/103
D216/D302
AUTHOR: Dormant L.I.
TITLE: On the nature of the source of the diurnal variation
in cosmic rays with the direction of the sun
PERIODICAL: Referativnyy zhurnal. Geofizika, no. 4, 1962, 16, ab-
stract 4G89 (V sb. Kosmicheskiye luchl, no. 4, M.,
Ali SSSR, 1961t 251-252)
TEXT: It isshown that independently of the structure of the magne-
tic field frozen into a corpuscular stream, cosmic-ray particles
entering the stream will drift xvith the velocity of its plasma in a
radial direction relative to the sun. As a result, a cosmic-ray
anisotropy will be observed at the earth. When the corpuscular
stream velocity is ,,jlO8 em/see, the amplitude of the diurnal varia-
tion for low-energy particles is a few tenths of a percent.' For par-
ticles with an energy ev3 BeV, the amplitude Yrill be about 0.03
K
,oreover, as a result of driftv there is a change ir. the article
energy and this enhances their anisotropy still further, rAbstrac-
tor's note: Complete translationjo
Card 1/1

L 19443-63- EWT(1)/EWT(m)/FCC(w)/BDS/ES(v)/EE);-2. - AM/AFFTC/&D/.
AMIEW-31APGG Pi--4/-Po-4/Fq-4/Pa--4 MVGWIN
ACCESSION NR: .'AT3007837. S/2961/61/000/004/025310255.
AUTHOR: Dorman,-Lo To
TITLE: Ch a ra c t er c(fj diurnal variations of cosmic a s
raLS-4
'424-MA111
r -E
A-1
u zich. komitet. VII'razdel
SOURCE: AN i
programmy* MGG: Kosmich askiye luchi. Sbornik r-tatay, no. 4,1961,
253-255
TOPIC TAGS: cosmic ray, lunar culmination, lunar shadow, pseudo-
lunar diurnal variation, amplitudinal"modulation, phase modulation',
interplanetary plasma, tidal wave, magnetic force line, geomannetic
throshold
ABSTRACT: The existence of a period of lunar variations of cosmic
--tay-li, coinciding with thi period of lunar diurnal culminations, Is
difficult to prove experimentally, as the lunar shadow is too
narrow to permit detection of its influence. Two possibilities
for pseudolunar diurnal variations of cosmic rays arise. . The
first is related to the amplitude modulAtion of solar diurnal
variations L~ the 27-dAy period. Mathematical analysis of
card I I)

L 19443-63
ACCESSION NR:- AT3007837
amplitudinal modulation yields two periodx, 23.2 hr.and 24.9 hr,
the latter coinciding with the lunar 24-hr period. The second
possibility is related to phase modulation. HathematLcal analysis
in this CA6G yields two p4riods identical to those determined in
the first case. Experimental proof of the existence of the 23.2-hr
period would establish the falsity of lunar diurnal variations.
If experimental investigations do not indicate the existence of
such a period, the reality of lunar diurnal variations would be
established. Such variations can be explained as the reault.of
a tidal wave in interplanetary,plasma with frozen magnetic force
lines. Such a wave causes periodic changes in the geonaRnetic
threshold which act.- on earth as the lunar diurnal variations.
.orig. art.-has: 6 formulas.
ASSOCIATION: none
SUBMITTED:, 00 DATE ACQi 220ct63 ENCL: -.00
SUB CODE: AS NO REF SOVt 002 OTRHR-r -06'i
r-,A

DORMANp L. I.
Cosmic rays and aeomapetism; a survey. Geomag. i aer. 1
no.3:293-313 My-Je 161. (NLU 14:9)
1. 14agnitnaya laboratoriya AN SSSR.
(Cosmic rays) (Magnetism, Tmestxial)

DORMANP L.I.; KOLOHEYETS, Ye.V.; SERGEYEVA, G.A.
Investigating variations in the intensity of cosmic rays and
properties of thq corpuscular stream during the magnetic
storm of July 1958, Geomag. i aer. 1 no.3:326-332 14y-Je
161. (14IRA 14:9)
1. Magnitnaya laboratoriya AV SSSR i Kazakhskiy gosudarstvannyy
universitet imeni S.M. Kirava.
(Cosmic rays) (Magnetic storms)

DDRMAN L I ; KUZIMINo A.I.; SWPINt G.V.
Sounding electromagnetic conditions in the interplanetary space
and in the vicinity of the earth by high-energy cosmic rays.
Geomag. i aer. 1 no.3:333-3/+5 MY-Je '61. (MIRA 11+:9)
1. Fiagnitnaya. laboratoriya AN SSSR i Laboratoriya fizichaskikh
problem Yakutakogo fili4la. Sibirskogo otdelaniya AN SSSR.
(Co=de rays)

DORKAN, L.I.; KOLOHEYETS, Ye.V.
Individual smll noutron intensity flares of cosmic rays according
to the data of the world station network. Geomag. i aer . I no.4:
500-506 Jl-Ag 161. (MIM 14:12)
1. Magnitnaya laboratoriya AN SWR i Kazakhakiy gosudarstyannvy
universitet imeni, Kirova,
(Cosmic rays)

31802
S/203/6 1/00 1/00~/005/028
los-~L70,r/ -t-10 A006/A101
4/ 0(-q
AUTHORS: Dorman,_.jtL_, Kolomeyets, Ye.V.
TITLE- Statistical analysis of "small" bursts of costpic radiation during
quiet days of the period of maximum solar activity
PERIODICAL: Geomagnetizm I aeronomiya, v. 1, no. 5, 1961, 652 - 657
TEXT: Although a number of studies has been devoted to large and small
bursts of cosmic radiation, two main problems have as yet not been solved, namely:
1) whether all chromospheric flares produce increased intensity of cosmic radia-
tion incident on the Earth, 2) whebher there is an effect of small bursts in cos-
mic radiation during the period of maximum solar activity. The authors studied
the dependence of the effect of increased cosmic radiation intensity on the index
of chromospheric flare using data from observations ofthe neutron component dur-
ing the IGY at 6 stations, located on geomagnetic latitudes 48 - 880c (climax,
Upsala, Churchill, Mauson, Resolute-Bay and TWO. Three groups of solar flares
were determined from July 1957 to January 1959,. namely I. flares of 3 and 3+ in-
tensity (4o); II. flares of 2 and 2+ intensity (225); 111. flares of 1 and 1+
Intensity (186). The effects were found for each group, It was stated that durirg
Card 1/2

Statistical analysis ...
31P,02
3/203/61/001/005/005/028
A006/A101
the maximum of solar activity, in spite of the presence of magnetic clouds in in-
terplanetary space, solar cosmic radiation reaches the Earth witfiin several hours;
solar flares of intensity number 2, 2+, 3 and _3+ produce, on the average, the same
stream of high-energy particles and substantially different low-energy streams.
The dependence of the effect on the location -of stations was investigated (within
and without the zones of incidence). No substantial dependence was revealed dur-
ing the maximum of solar activity, contrary to the minimum. This indicates a dif-
fusional nature of distribution of solar particles during the period investigated.
There are 4 figures, 1 table and 18 references: 9 Soviet-bloc and 9 non-Soviet-
bloc.
ASSOCIATION: Magnitnaya laboratorlya AN SSSR (Nagnetle laboratory of AS USSR)
Kazakhskiy gosudarstvannyy universitet imeni S.M. Kirova (Kazakh
State University Imeni S.M. Kirov)
SUBMITTED: july 4, 1961
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gL"061
AUTHORSs Dorma Shatashvili, L.Kh.
~Li
TITLEo Lunar-diurnal variation'of the neutron component of cosmic radiation
and the problem of its origin
PERIODICALI Geomagnstizm i aeronomiya, v. 1, no. 5, 1961, 663 - 67o
TEXT: The authors investigated the lunar diurnal variation in intensity of
the neutron component of cosmic radiation, using observation materials from high-
mountain stations during the IGY. The authors established the existence of lunar
diurnal variations of cosmic radiation and their latitudinal dependence, It Is
proved that these variations depend mainly on the mutual position of the Sun, the
Moon and the Earth, attaining a maximum during the full-moon and a minimum during
the new-moon period. At the same time substantial changes in the phase take
place. Tke origin of lunar diurnal variations can be, explained as follows: The
gravitation forces of the Moon and the Sun affeo-t the plasma of the terrestrial
magnetosphere. As a result, terreatrial magnetic force lines frozen in the plasma
at high altitudes are shifted. The effect of the deformed geomagnetic field on
the cosmic radiation entails the appearance of lunar-diurnal variations. It can
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be,expected that this effect will be the higher, the more the corresponding layers
are remote from the Earth. The results obtained prove the reality of the tide-
forming movements of the plasma and the magnetic field in the outer layers of the
terrestrial atmosphere, bordering the interplanetary medium. These phenomena
should be studied by observations with artificial satellites and rockets. There
are 5 figures and 10 references: 7 Soviet-bloc and 3 non-Soviet-bloc.
ASSOCIATION; Magnitnaya Laboratoriya AN SSSR (Magnetic laboratory, AS USSR) In-
stitut Geofiziki AN GruzSSR (Institute of Geophysics, AS Georgian
SSR)
SUBMITTED- August 22, 1961
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AMORS: Doman, L. ;E..,.Kolomeyets, Ye. V.
TITLE: The dependence of solar cosmic ray intensity on the earth on loca-
tion of chromospheric flare in the Sun
PERIODICAL: Oeomagnetizm i earonomiya, v. 1, no. 5, 1961, 830 - 831
TEXT: The authors studied the effect of solar cosmic ray intensity on the
helio-latitudes, of flares, using data obtained from observations of 149 chromo-
spheric flares with magnitudes of 2 or higher, which are effective in the inten-
sity.of the cosmic ray neutron component. The range of solar latitudes was di-
vided into 3 zones: I - from 0 to 100 (17 flares); II - from 10 to 200 (75
flares); III - from 20 to 500 (57 flares).. The analysis shows that the intensity
of solar cosmic rays produced by flares between the solar equator and 100 helio-
latitude, is 1.5 times greater than the intensity of radiation from flares between
10 - 500 helio-latitude. A study of cosmic-ray neutron data obtained at the Cli-
max and Churchill stations Indicates that conditions for the propagation of re-
latively high-energy particles (several Bev) toward the earth are independent of
the longitudinal distribution of chromospheric flares. Data from the Thule sta-
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The dependence of solar cosmic ray intensity... A006/AIOI
tion confirm that about twice as many low-energy particles were incident an the
earth when a flare occurred on the western solar limb as when it occurred on the
eastern limb. There are 3 figures and 5 references: 3 Soviet-bloc and 2 non-
Soviet-bloc.
ASSOCIATION: Magnitnaya laboratoriya AN SSSR (Magnetic Laboratory AS USSR)
Kazakhskiy gosudarstvennyy universitet imeni S. M. Kirova (Kazakh
State University imeni S. M. Kirov)
SUBMITTED: July 21, 1961
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AUTHORS: Koyava, V.K.
TITLE: Effects of magnetic atoms in cosmic rays during the minimum of
solar activity
PERIODICAL: Geomagnetizm i wronomiya, v. 1, no. 5, 1961, 839 - 841
TEXT: The authors analyzed the decrease of intensity of cosmic radiation
during magnetic storms (Forbush effect) in 195-3-1955, using data on magnetic
storms obtained at Tbilisi and data on cosmic radiation gathered with the aid of
an ionization camera. An analysis of the effect of magnetic storms of different
intensity and nature of commencement on the cosmic radiation leads to the follow-
ing preliminary conclusionsi The Forbush effect Is observed only for-big storms
commencing sudde'nly. Consequentlyjthe corpuscular streams causing these atoms
carry frozen-in magnetic fields of large extent and high strength. These fields
scatter effectively cosmic raya~with an energy of dozens of Bev. For big storms
beginning suddenly, an effect of Increase before the commencement of maghetic
storms apparently takes place. This shows that the corpuscular streams, causing
the storms in the minimum of solar activity, are magnetized and that a magnetic
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cushlonwas formed in their front section. In the minimum of solar activity no
substantial changes occur In the nature of correlations between the corpuscular
scream and the g'eomagnetic field, as fat, as changes in the sharpness of cut-off
are similar to those in the maximum of solar activity. The authors thank N.A.
Katsiashvili for the materials submitted. There are 3 figures and 7 Soviet-bloc
references.
ASSOCIATION: Magnltnaya laboratoriya AN SSSR (Magnetic laboratory.. AS USSR),
Institut geofiziki AN GruzSSR (Institute of Geophysics, A2 Georgian
SSR)
SUBMITTED: july 4, 1961
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34359
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AUTHORS: ~o an(fKolomeyets, Ye,V.
E~L. ~1.' ~
TITLE: Small flares of cosmic rays on quiet and ma&netically-
disturbed days, connected with solar radio bursts of
types II and III
PERIODICAL: Geomagnetizm i aeronomiya, v. 1, no.6, 196i, 1015-1016
TEXT: To discover the nature of solar radio bursts connected with chromo-
spheric flares Iit is important to know whether relativistic particles are
generated during these flares. Cosmic ray flares on Earth may indicate
that this is so. In any case,an increase in intensity is a direct indi-
cation of particle generation in the solar atmosphere. Relativistic
particles are usually generated in flares which are accompanied by radio
bursts of types II and III, but the effect for flares accompanied by type-
Il bursts is considerably greater than for other flares (Rell. 4: L.I.Dorman,
Ye.V.Kolomeyets. Geomagn. i aeronomiya, 1961, 1, no. 5, 653). When the Earth
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is in a corpuscular flow, during days of magnetic disturbance, the Earth is
effectively screened by the magnetic fields frozen -in the coLpuscular car-
rents, which accords with another study (Ref. 5: L.I. Dorman. Ye-V. Kolo-
meyets. Geomagn. i aeronomiya, 19629 2, no. 1.). If it is Z43sumed that the
partiole apeotrum which causes the increase un quiet days is the same as
during large flares (Ref.6t L.I. Dorman, G.I. Freydman. Tr. Yakutsk. fil.
AN SSSR, 1958, 2, 129) or flares in the stratosphere (Ref. 7: A.N.
Charakhchlyan, V.F. Tulinov, T.N. Charakhchlyan. Zh. eksperim. i teor.fiz.,
1960, 39, 249) then the additional flow of particles to the Ear% is:
~1' D ( E ) ~ E_', (n=e- 4-.7). (1)
Acoording to numerous data (rapid attainment of isotropz( in the adil'tional
flow of solar particles, decrease in intensity by the 0/2 law,etc.~
particles are distributed in interplanetary space by diffusion, The
intensity of particles on the Earth after emission from the Sun at a moment
of time t will be (Ref. 8: L.I. Dorman. Sb. "Progress in physics of cosmi15
ray elementary particles"9 1961, 6):
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2
cf D t) N4rl V - - exp 3r 0 1 (2)
8 51~v t 3/' 4 v t
3 )
where N is the total number of particles generated in the flare, - the
mean effective distance for scattering, r - radius of the Earth's orbit,
v - velocity of oDlar particles (for relativistic particles v--ac). If
formula (2) is ured in conjunction with coupling coefficients for the neu-
tron component and the spectrum in the form of (1) is incluOled, the flow of
particles in a flare can be calculated for every actual case. As a result
of nuclear reactions in the solar atmosphere, these oarticle3 will generate
fast secondary electrons, whose motion in magnetic fields will cause
synchronotronic radio-emission. Flows of fast relativistic particles
through the solar atmosphere outwards will excite the plasma and cause it tc
generate radio bursts Both processes may be associated witli the creation
of solar radio bursts connectod wich chromosphoric flaroo in 0iich relativ-
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istic particles are generated at the same time. There are. 2 f 16-ures Find 8
references: 6 Soviet, and 2 non-Soviet. The two English-language refer-
ences are: Monthly bulletin of solar-geophysical data. Boalder, Coloradc,
1957-58; Quart. bull. on solar activity. Zdrich, 1957, no. 7-12; 1958, no.
1-12 [Abstracter's note: Esnentially complete translation]
ASSOCIATION: Magnitnaya laboratorlya AN SSSR.Kazakliskiy goaudar3tvennyy
universitet im. S.M. Kirova (11agnetic Laboratory)AS USSR,
Kazakh State University imeni S.11,1. Kirov.)
SUBMITTED: July 4, 1961
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