SCIENTIFIC ABSTRACT DORMAN, L.I. - DORMIDONTOV, F.K.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R000411010005-9
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: January 3, 2017
• Document Release Date: July 28, 2000
• Sequence Number: 5
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

KC NRt AT6003524 SOURCE CODE: UR/3184/65/000/OOT/0039/0049
AUTHOR: Do 1.1. (Doctor of physico-mathematical sciences); Clikhetiji, A.M.
37
ORO: none.
TITLE: Electromagnetic conditions in interplanetary space
SOURCE; AN SSSR. Mezhduvedomtvep
.W geofizichesk!Z_kom1tet-. Kosmicheskiye
luchi , no-.-I 9
TOPIC TAM mi4petle storms active soNar, regiong central meridian, solar rotationg
'sunspot, chromosphoric flara.~ faculas flocculus, geomagnetic pole, cosmic ray,
neutron component
ABSTRACT: A me4metic- atormlid"ed with sudden commencement o.: 14 March 1958ithe
maximum activity of which lasted 4 br. Active solar region no. 12 passed the
central meridian on 6-14 March. This region was observed In ten solar rotations.
On the last pasnage, the active region contained groups of sunspots, thromospheric
flares, faculae, and flocculig which successively paused the central meridian. A
long-lasting sedimentation of protons in the polar cap star+,~d on 14 March.
Anomalcus absorption took place around the geomagneticpole to the 60th parallel-. The
influence of the magnetic storm on cosmic rays was studied from observation data of
44 stations. These data were compared with the rate of the intensity of the mag-
netic storm during its display. Two Forbush effect models were used for analyzing
1/2

L nelo-66
ACC NAs AT6003524
the corpuscular stream. The width of the stream was found to be equal to 1.5-1013cm.
Th;.intensity of the magnetic field In front of the stream was found to be equal to
2. 10-5 go and behind it to 1-5-10-5 go. The density of the corpuscular stream v"
determined to be equal to 3.2-10-23 g/cm3, and the coefficient R of the cosmic ray
diffusion into the corpuscular stream was found to be equal to I-T-1020=2/sec. Harm
monic analysis of the neutron component showed that the first harmonics for the
Northern and Southern Hemispheres were equal, and the maximum of the first harmonic
was shifted to the evening. This circumstance indicates that the magnetic fields of
the stream are opposite to those of the earth. An analysis of the state of the neu-
tron component of cosmic rays shows changes which are different in Europe from those
in America. Orig art. has: 6 figures and 32 formulas. JEG)
SUB CODE., 03/ SVBM DATE., none/ ORIG REPt 014/ OM REP: 005/ ATD PRMS:

KCC-Rkt-AT6003528 SOURCE CODE: UR/3184/65/000/007/OlhO/0144
AUTHOR: Dorman; L.I. (Doctor-of physico-mathematical sciences); Chkhetiya, A.M.
Olid: none
TITLE: the displiq of the surrounding of the terrestrial magnetosphere by Cosmic
rays
SOURCE: AN 8S8H. Meithduvedomstvennyy geofizicheakiy komiiet. Kosmicheskiye luchi,
no. T, 1965, 140-141r- A
TOPIC TAGS: cosmic ray, cosmic ray intensity, magnetic atom, terrestrial magnetic'
field, geomagnetic latitude, solar plasma, horizontal component
ABSTRACT: In some sharp decreases of cosmic-r Intensity,'increase peaks occur.
These intensity peaks differ from the increase of cosmic-ray intensity during the
main phase of a magnetic storm. Variations of cosmic rays are analyzed in detail,
but a final solution is not attained.. On 15 July 1959,.& special peak vas observed
which could not have been caused by solar cosmic rays because at that time large
chromospheric flarea did not appear and the spectrum of solar cosmic rays could not
create an increase in intensity. This peak 'was observed at many stations during a
sharp decrease in C013MI.c-ray intensity and the horizontal component of the terrestri-
al magnetic field. The intensity of the peak depends upon the geomagnetic latitude;
it increases from hilgh latitudes to the 55th parallel and then gradually decreases.
:Ord 1/2

L 3-1808-M
,ACC NRs. AT6003528
A graph in the orig~n~~aa-~ticle shows the correlation of the Ancrease of the horizon-
te-1 component 6f the gibimpetic field to the peak. The peak of the increased In-
tensity of cosmic reqs'appeared during the sharp increase of the horitDntal compon-
ent, indicating that the earthto magnetosphere was surrounded by solar plasma. This
caused.an inarease::in the geomagnetic field and a redistribution of the arriving
cosmic-rays. Orig.,art. has: 6*figures. IEGI
SUB CODE.: 03/ SUBM DATE: none/ ORIG REF: 004/ OTH REF: 001/ ATD PRWS
~Y- Peit.
2/2

AGC MRs KI:OVUJ;PZY uVub:
~0
.AUTHOR: (Doctor of physico-mathematical sciences); 13hatashvili, L. 1(h.
ORGi none
6V)
TITLE: 'Cosmic-ray 2T-day variations and general characteristics of electromggnette
conditions in inlerplanezary.-UpUv-
SOURCE: AN SSSE.~Heihduvedomatyinnyy-georisicheekly komitet. Koszic~eskiye luchl,,.
no. 7, 1965,"- - 64 %
TOPIC TAGS: cosmic ray, neutron oempennot, solar rotation, neutron spectrum, solar
activitr, geomagnetic,,%,.1 P&64gm, solar
plasmal Pno~ WJ~OA.1-
ABSTRACT: The neutron and the hard components or cosmic rays observed at mountai-m
and sea-level stations have been processed in order to determine -the influence of
solar rotation.on~the intensity of cosmic rays. Observation data used were world-
vide in scope. The 27-day variations of cosmic rays, vhich vere found earlier,
made it possible -to compute the spectrum of the neutron component from data of
mountain and sea-level stations. The study of apectral, variations during a 2T-der
period of maximum solar activity showed that the spectrum was neexly the same as
that of the Forbush effect during magnetic storms. Cosmic-ray vexistions with a
27-day period appsar, in the form of discrete waves. A map was composed representing

L 3.1809-66
ACC NRj AT6oo3529
correlations between the earth's geomagnetic activity, Wolf nudbers, and the neatma
components A dletinct correlation between these parameters was difficult to find.
It can be assumed that the 27-day period of cosmic-ray variations relates to abort.
lived vuriations. The 27-day period is similar to the lunar diurnal variationeq
which depend upon the lunar phases with a maximum during the frai-moon phase.
possible to conclude that the active element In 27-dq?,ccs-
Further analysis made it
mic-ray variations In the magnetized solar plasma which is ejected Into epaca. 12*1
SUB CODE: 03/ SIMM DATE: none/ ORIG MW: Oll/ OTH REP: 0061 ATD PrM t W 7
(~~212

L 10924-66 EWr(l)/FCC
AwA(h) Gw
ACC NRt AP6002745 SOURCE CODE: UR/0203/65/005/0()6/1003/1008
AUTHOR: Dorman,_L._I.; Kolomeyets, Ye. V.; Sergeyeva, G. A.'
ORG, Kazakh State ~niversitY im. S. M. Kir (Kazakhskiy gosudarsivennyy
universitet)
TITLE: Solar diurnal and semidiurnal variations of cosmic rays and their dependence
upon 6)lar activity
SOURCE: Geomagnetizm i aeroisomiya, v. 5, no. 6, 1965, 1003-1008
TOPIC TAGS, cosmic ray, neutron,-_,M~, aampeaen.~.tns , diurnal variation,
v
gemjd-rltxnai varlab solar activity, energy spectrum, exponentlitl function
ABSTRACT:' Variations of the amplitude and phase of the solar diurnal changes of the
neutron component of cosmic rays~'tere investigated on the basis of date. frobi the
global network of stations obtained in the years 1957-.1958. Changes In the phase of
solar diurnal and semidiurnal variations are studied separately. The phase of di-
urnal variations changes slightly from month to month. The maximum of diurnal vari-
ations taken from equatorial stations precedes that of high latitude stations by
2.5-3 hr. A tendency for the phase to shift to a later time at high and low lati-
tudes is found with f. decrease in'solar activity. In 1962 the phase a,lift was noted
at earlier hours. The phase of semidiurnal variations changes markedly and does not
depend upon solar activity or particle energy. A table in the original article shows

1 10924-66
'ACC NR, AP6~~02/45
the mean yearly amplitudes computed for all latitudes by the first harnonics. The
amplitude in high latitudes increased during the period 1960-1962, and the amplitude
in middle and loo, latitudes decreased. The energy spectrum for each month has been
computed using the mean monthly amplitudes of the first harmonics and mean coupling
coefficients. The spectrum within the energy interval 3-15 Bev was computed by the
f ormula 6D (e) / D (e) = as-T., and y values are given in a table in the original article.
The mean amplitude of the second harmonics shows a wide range of valu(Is, which is
caused by charges of electromagnetic conditions in space and around the earth. The
energy spectrum of diurnal variations of cosmic rays within the energy interval 3 to
15 Bev for the neutron component may be represented by-an exponential function with
the exponent equal to approx. -0.5. The phase of diurnal variations changes in one
hour on the earth and at equatorial stations occurs earlier than at other latitudes.
Orig. art. has: 4 tables and 4 figures. [EC]
SUB CODE.,01. 4/ SUBM DAM 05jun64/ ORIG REF: 0051 OTH REF: 0071 AM PRESS.*
Card 2/2

DORMAN, L.I.; MAZARYUK, Ye.A.
Complex amplitude-phase modulation of periodic variations in
cosmic rays. Geomag. i aer. 5 no.6:1099-1102 N-D 165.
(KIRA 19: 1)
1. Institut zemnogo magnetizma, ionoofery i rasprostraneniya
radiovoln AN SSSR. Submitted May 4p 1965.

L 3A628-66, 2WT(1)1AWhVFW_-._ aw
ACC NR: AT6003522 SOURCE CODE: UR/3184/65/000/007/0005/0017
AUTHOR: Doman, 1. V. Dorman, L. I. (Dr. of Physico-Mathematical Sciences) 0
ORG: none
~TITLE: Investigation of the 11-year cosmic cycle (from data of obser'v'ationfr at!
sea level) 1C r9
SOURCM AN SSSR. MezhduvedomstvennXy poffzkogpKiy_.~qjn4e~. Kosmicheskiye luchi,
no. 7, 196.~_, 5-17
TOPIC TAGS: cosmic ray, geomagnetism, sun.pot cycle, magnetic rigidity
ABSTRACT: Data from a world-wide network of neutron monito--s, measurements of lati-i
tude effects in the neutron and hard components of cosmic rays at sea level, and
stratospheric measurements of proton and a-particle fluxes in the low energy region.
made from high altitude balloons are used as a basis for aralyzing the 11-year coa-
mic ray cycle. It is found that the amplitude of the 11-year variation increases
with a reduction in the geomagnetic cutoff hardness R which indicates that the pri-
miry spectrum of the 11-year variation decreases with an iacrease in R. The lag in
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L 16028-6
iACC NR* AT6003522
changes of cosmic ray intensity with respect to changes in solar activity increases!
wi-th a reduction in the penetrating power of the particles. There is a close rela-,
rtionship between cosmic ray intensity, the number of sunspots and radiation flux at
J0.7 cm. When considering variations for shorter periods of time, there is a closer
relationship between the intensity of cosmic rays and the K.-index of magnetic ac-
itivity, while longer time intervals show a closer correlatibn between intensity and
:,the number of sunspots. Hysteresis phenomena are studied on the basis of neutron
:monitor data and observations in the stratosphere. For R>3 Bev the energy spectrum-
~for the 11-year cycle is given in the form 6D(R)/D(R)-R-(W-8-0-9) hih is steeper
for R>13 Bev,with y>2. The spectrum of the 11-year cycle was considered together
~with delay phenomena 'to determine the scatteri'ng path as, a function of particle
.hardness and the dimensions of the modulating space. The magnetic field intensity
in scattering nonhomogeneities is determined for varioun assumptions on the rela-
tionship be~tween the average dimensions of nonhomogenei-ties and the distance between
them. The contribution Of variability in the.lag effect is evaluated. Orig. art.
has,-. 8 figures, 16 formulas.,
SUB',CODE., SUB14 DATE: 00f ORIG.IMF::_~ OTH IMF:. 019
Y

i5935-66 EWT(1)/FC0/E.M(.h). aw
ACC NR: AT6003525 SOURCE CODE: UR/3184/65/000/007/0121/0130
AUTHOR: Doman, L. J. (ft of Physico-Mathematical !3ciences); Tyastol_ M. I.
ORG: none
Ltia cutoff
TITLE: Effect of a fil&wntary e quatorial current ving on the jp~4~ma&!e
.hardness of directional cosmic radiation
SOURCE: AN SSSR. Mezhduvedomstvennyy geofizicheskiy komitet. Kosmicheskiye luchi,
no. 7, 1965, 121-130
TOPIC TAGS: magnetic rigidity, cosmic radiation, Seomagnetism
ABSTRACT: The threshold hardnesses are numerically calculated for particles arriving
at various angles tothe zenith. The results are given in the form of curves for
cutoff hardness as a function of zenith anglefor' eastern and western directions of
'particle arrival. Curves are also given showing t%ie relationship between threshold
hardness and geamagnetic latitude for various zenith angles in the east-west plane.
These curves show that a reduction in the radius cf the current ring or an increase
in-the ring current reduces the threshold hardnesses for both eastern and western
'Card 1/2

1,15935-66
'ACC NR: AT6003525
directions. This indicates that there should be a reduction in east-west asymetry
at lover latitudes during the main phase of a magnetic storm due to the change in
,cutoff hardness. Orig. art. hasi 5 figures, 6 formulas.
.SUB CODE: 08/ SUBH DATE: 001 ORIG FXF: 006/ -OTH REF: 006

D 16k8-66 EWT(1)/Fao 'law
ACC NR: AT6003526 SOURCE CODE, UR/3184/65/000/007/0,131/0134
AUTHOR: Dorman, L. 1. (Dr. of Physico-Matheinatical Sciences); Tyasto,,_M~J-
ORG: none
TITLE: Effect of a spherically distributed westerly current on geomagne
hardness
SOURCE: AN SSSR. Mezhduvedomstvennyy geofi-ticheskiy komitet. Kosmicheskiye luchi,
-no. 7, 1965, 131-134
JOPiC TAM: geomagnetism, magnetic storm, magnetic rigidity
~ABSTRACT: The authors consider the variation in cutoff hardness during the main
.phase of a ma tic storml~al'ssuming that an,equatorial current is generated which
.&nt_
flows along the surface of a sphere. The. !.-Following expression is given for the in-
tegral of motion
A
R cos X sip G +R cos X - 2,r.' (1) -
owhere R is the magnetic hardnessi A is the vector potential of the magnetic field;
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L i6W-66
ACC NR., AT6003526
:10 is the angle between the vector for thfj velocity of the particle and the plane of
the meridian; 2Y is the constant of integration. Curves are given for y as a func-
:tion of the square of the current shell -Padius in Stl5rmer units. The resultant data
are used for finding -the threshold hardnesses for vertically incident particles as a
function of the geomagnetic latitude for-positions of the magnetic field cm the
~equator equivalent to 100, 200, 300 and 400 y, and for current shells with radii
;equivalent to 3, 5 and 6 earth radii. -!:hese curves show that the cutoff bardness
for particles in the middle latitudes 1!3 affected not only by the drop in the hori-
zontal component (the force of the magnetic atom) but also by the iadius of the
current shell re3ponsible for this drop. Orig. art. has: 3 figures, 1 table, 8
formulas.
.SUB CODE: 08/ SUBM DATM 00/-- ORIG ICF: 002/ Oji-J REF. 002
Card

L16023-M EWT(I)IFCCIEWA(h) OW
ACC.NR: AP6006654 SOURCE CODE: UR/0203/66/006/001/0019/0026
orm3n L. I.; Mi~dvedey, M. Smirnov, V. S.
AUTHOR: D WW^k __1u
ORG: Polar GeophXsical Institute, Kola Division, AN S~_qk,(Polyarnyy geofiziche-
skiy institut Kol'skogo filiala.AN SSSR)
TITLE: Highly accurate trajectories of cosmic rays in a geomagnetic field
SOU11CE: Geomagnetizm Laeronoodya, v. 6, no. 1, 1966, 19-26
TOPIC TAGS: cnsmic ray Intenafty, magnetic dipole, geomagnetic field, anisotropic
motion, asymptotic direction, ispherical harmonic function
ABSTRACT* A study of planetary di6tribution of the intensity of si;zLQa& re-
vealed that the theoretical ccmputations based on the magnetlc dipole do riot
agree with the measured intencity of cosmic rays. This result indicated that the
higher harmonici; of a geomagnotic field influence the trajectories of coamic-rly
particles. The anisotropic motion of cosmic rays is associated with asywptotic
directions. These directions can be found by solving 'the potential of the geomag-
netic field by means of six t,armonic spherital functions. The solution was based
an two maps of the geomagnatl.c field with Isolines of its components. The one
Card 1/2 UDC: 523.165

L 1602).66
ACC NR: AP6006654
map was compiled by the Institute of Terrestrial Magnetism, Ionosphere, and Prop-
agatidn . of Radio Waves and the other by the British Admiralty. Asyriptotic direc-
tions . for the real and dipole fields were computed for two stations-Mirnyy in
Antarctica and Tiksi Bay on the shore of the Arctic Ocean. Results obtained at
Tiksi coincided*for both fields, but at Mirnyy the results are 20* apart. Asymp-
totic directions of particles of low hardness In a real magnetic field coincide
stith those in a dipole field.. Stormar's asymptotic directions pass through the
dipolets center, and each direction is associated with a shock-wave zone. Sta-
tions located in the second shock-wave zone receive particles of hardness lower
than 1.1 Bv. These stations receive a narrow cone of solar radiation particles
when they are located in tho main shock zone. The angle of Intersection of the
ecliptic with the earth's equator is under 23.5% A line was found, the effective
asymptotic latitude of which for solar radiation may be equal to 25' when the as-
ymptotic directions of the dipole coincide with those of the real field and are
shifted with the force lines in longitude. Results of computations are giveu in
a table in the original article for various hardnesses. Orig. art. has: 5 figurmi
3 formulas, and 1 table. JEGI
SUB CODE: 04/ SUBM DATEL 17Dec64/ ORIG REP: 002/ OTH FXF: 009/ ATD PRESS:
Card 2/20F--__-

L-ZI!L61-66- 54T(I)/
-ACC NR3 AP6012056
SOURCE CODE:
S.; Tyaqtot M. 1,,
AUTHOR: Asaulanko, L. G.; V.
ORG: Polar q~~qphysical Institute Kola Branch. AN SSM (Polyarnyy goofizichaskly
lnstitii)CA I skogo'
TII'U,'-. Ef f Oct of 3Ardtation or the ffl_.q;ja-&aat1c_fiold on cp1p~&.ray3
SOURCE: Goomagnotitm i aeronomlya, ve 5, no,, 5. 3.965, 809-816
TOPIC TAGS: goomagnetic 11old. cosmic ray, solar wind, magnetic storM
ABSTMCT: The earth's maj;notic field, oit least in the direction of t:ho sun, is limited,
and its axtent is depondout on the density and energy of particles in the solar wilic,
This articlo discusses tho effect of compression of the magnotosphoro caused by tha
solar wiivi on the cutoff rigvlitlos and asMtotic directions of cosaic ray-s" Lird-ta-!~
"lion of the magnotosphere influences cosmic rays not only in the period of the initiall
phase of a ma6notic storm, but also wh9n the magnatic field. is qlliot.. It is don3n- I
strated that '.he comprossion loads to intensification of tha influenco of the ma;Wticl
field on co5vdc rays and that tho joint effect of limitatlon of the nagnetosphez-3 axyll
the westerly current system loads to attenuation of the ird'luonco of external soarcat;
both on cutoff rigidity snd on asyriptotic directions. The authors Viank the workers
of the Computer Conterjj;9ja Branch, W1 SSSR for programxing the problems and calcula.
o; the oloctrordo aoi~~A-W*'-dRfg&-ir'L haal 3 figur43s. 9 formalu, aril 3 tables.
d Y : 08, 03, 04 / SUBH DATEt 2ASep64 / ORIG REF: 004 / ODI REFj 013
dk
Cgr ;" A&I

L 20464-66 eq
ACC NR, AP66121 17
r06RC9 019: 16,
AUTHOR: Dorman, L. -I.,; Miroshnicheriko, L. I.
j013
ORG: Institute of Terrestrial Mapetism, the Ionosphere and Radio Wave Propagat
TITM: Dotermination of the duration of OMi3s.-Lon of so cosm4p
lar y; from the gone-
, --ra
ration region
SOURC:,': GoorAgnetizu, i aeron*W~ratt v, 5, no. 5, 1965, 910-913
TOPIC TAGS: cosmie ray, solar radiation, solar corona, solar chromosphere
ABST0,ACT: A diffusion model usually is used in the investigation of the
Propa-ation of so:La-- cosmic rays in interplametary space. 7ne density
c~an,ga of solar pirticles in space and change with time is d13scribed
approy-4matlely by & nonhomogeneous equation of the parabolic Typo. A
solution is easily obtained. Source density is thlo quantity of parbicloe.!
e:aittled from the source (from the region of generation) Ln a unit time
apa -,5-. general. is a function of c., kin and t. It i:; determined by the
character of generation of particles on the sun anti their propagation
in the solar corona and 6upercoronat At present there is no detailed
:L-iformation on tho'character of the dependence of r on 6 kin and t (f
is source density');' it is only known that f (f, kins t) rapidly attains
a maximum after the onset of a chromospheric flare and then drops off
steeply approxim.-itely exponentially. In the case of -low enorgies
Card 1/2 Mc.. '523.16J

;- 2W
XCC NR:
f rL kin, t-) "-i be drawn out cons-iderably in time, which is partly
responsible for the considerable lag of low-energy particles. Expres-
.sions; are derived for approxim&vin~g f. Since recent data indicate the
possibility of accumulation of low-energy solar parLicles in inter-
planetary space in years of high solar activity, the authors have in-
vestigated the noyihowogeneous parabolic diffusion model equation in'
combination with Vleir proposed expression for f for. the case when
emission occurs uniformly over a finite interval of time, 'Ath an in-
crease of T (enission period) the maximum of the density curve is dis-
placed in the direction of larger values to The density increase occurs i
quite smoothly-and the decrease after the maximun, is quite steen. TWhen
t :,>, T the don3ity decrease conforms to the diffusion law "t-372; this
is applicable to an instantauneous source. In the case of prolonged
e;.usslon density increases to a maximum more slowly and then begins to
decrease much more rapidly. 11he results make it possible to use the
temporal variation of intensity change of solar cosnic rays to determine
duration of their emission fr= the region of generation. They- also
sh~ra that for study of the duration of emission of solar cosmic rays it
is most important to have detailed measurements of the particle flux near
the increase n, axinum., where the influence of T is manifested most. strongly.
The authors thank Yo, A. KorDjtWW;L, To L. YinnIkmw_. UtkUwa, and D
a. To N
Fishchuk for ca pyiii ~ST fig- at 8 r0im,
,g out the calculation* Orig, art* ha
and I table iW .I
SUB CODE: 04 SUEM DATRt 29Doo64 / MIG REF: 004 / OTH.REFt 001
Card 2L2

ACC NRs AM19296 SOURCE CODE: UR/0203/65/003/004/0673/0678
AUTHOR: Dorman, L. I j Ivanov, Vs io; K21omeyets,, Ye, V.
ORG: Kazakh*St te UdyersitX JM, By M,-- roy (Kwiakhskiy gosudarstvennyy universitet]
TITIE! Effects of small bursts in the hard component. of coMjg_r"s on quiet and
magnetically dititurbed days
SOURCE: Geomagnetizm i aeronomiya, v. 5,. no. 4, 1965,, 673-678
TOPIC TAM cosmic ray shower, diurnal variation
ABSTRACT: This paper presents an analysis of cosmic ray bursts occurring on
magnetically quiet and disturbed days. The bursts are classified into three
groups. Statistical accuracy was increased by double averaging: by stations
and for all-bursts. Solar-diurnal variations were excluded. Data for 19 stations
(210 bursts) were used (120 observations on magnetically quiet days and the others
.at the time of Forbush decreasesa Orig, art. hai3l figures and 1 table. (JPRSj
SUB CODE: 04- SUBM DATE: O5Jun64 ORIG RIEF: 008 / OTH REF: 003
UDC:

ACC W AP6019101 SOURCE CODE: UR/0203/65/005/004/0760/0762
AUTHOR: Dorman, jL,; Kolowntep- yet y.; Pivne ap Vo, .; Sergeyeva, G. A
ORG: Kazakh,Sta~.,e University im. So M. Kir (Kazakhakiy goeudaretvennyy universitet~,
TITLEs Mature and energy spectrum of solar-diurnal and semidiurnal variations at
the time of some Forbush effects
1,SOIRCE: Geomagratizm i asronamiya, v. 5, no- 4. 19659 760-762
TOPIC TAGS: diurnal variationt solar spectrum, cosmic ray intensity, geomagnetic
field
ABSTRACT: This paper discusses solar-diurnal and semidiurnal variations on
11-2 November,'11-13 April 1960 and 29-30 April and i May 196L The
,study was.based; on data from the world network of stations recording the
ineutron compontint of cosmic ra ntensity, corrected for the barometric
,effect. The harmonic analysis was based on data corrected for the For-
tbush effect. .1the plotted.data show*that there is a clearly expressed
6diurnal variation of both cosmic rays and the geomagnetic field. Cosmic
ray data hav-it~ ii well-expressed inverse correlatinn with, the H component
:in the fArdt t1lo'cases, considered, when there were moderate magnetic
stormri;','in the third-'rass' therb was, a direct correlation, when; the geo-
'Yiagnetic' fietd:was: restored afteri the Forbush effbct., Analysis of the
Card 1/2 UDCi 523.165

L 29290-66
ACC NRs AM19301
p- he time of the maximum of diurnaL and s'iidiurnal varia-
ds endence of t e
o
.;tions dn'the cutoff energy revealed that' the time of the maximum of the
.diurnal,variation is displaced gradually to the early hours with an in-
hcrease of cutaff energy. Nothing definite can be said concerning tha
Iphase'af the aemidiu~nal variation. It is shown that the first two cases
:can be attrib,ited to a close source'andthe third case can be'attributed
ito a distant soureb.' In these cases the energy spectra are tomewhat dif-
Iferent. In the case of a near source the spectrum is somevhat'hairder
than for the case of a distant source. Orig. art. hast 2,figures and
1 tables [JFRS3
SUB OODE 1. 04.0 08 SUM4 DATE I '13kug64 ORIG REP: 007 OTH RLP 1 001,

L 30973-66 EWA(h)/EWT(1.)ZFCC
C NRt AF6018098
AUTHOR: Dorman,L.- Is
ORG: Institute of Terrestria
SOURCE CODEs
UR~0203/66/006/002/0231/0240 ?V
s
A SSSR (Institut zemnogo magnetizma, ionoefery, rasprostraneniA i1iAovolnWS$4
TfTLE' om-etry of the solar system
: kole 0-t -ge- in costw-W ray -variations observed at
the earth,
SOURCE: Geomagnetizm i aeronomiyap ve 6p nos 2v 1966p 231-240
TOPIC TAGS: geomagnetic fieldp cosmic ray# solar systemi, asymptotic propertyp
cosmic ray anistropy. angular distributi 3-naction and eight parts. 1-
ABSTRAMThis papqr consists or an intro
t Asymptotic directions in the geomagnetic fields Asymptotic direc-
tions relative to the plane of the ecliptic- WFlormation of diurnal
variation at the earth despite its absence in interplanetary spaces 4..
Distort.-Lon of true anisotropy. 5o./Possibilities of investigating the
transverse gradient of qosmic ray~fntensity in interplanetary space and
;seasonal variations. 6o Effect of ellip3oidal configuration of the
-earthfa orbit. 7. Effect of noncoincidence of the plane of the
ecliptic and the plane of the-sun's equator. So Transformation of the I
diurnal and semidiurnal variations symmetrical to the sun's equator. It.
is shown that allowance for the relative position of the earth and sun
and their axes of rotation makes it possible to obtain additional infor-~
mation on the angular distribution and transverse gradient of cosmic ray
intensii~y in interplanetary spaces The author considers geometrical I
effects leading to the modulation of solar-diurhal and sidereal-diurnal.
variations and to the formation of annual and eaniwmal cosmic rayjvar;iations~',
Orxio" 34 rofm-ffa-i.
1 Card 1 USIM CODE: 03, 04t 08/8411 VMt OAM&;r 65/ORIG tWt_ 00`7107~H BEFt 003
GW

L 3905-66 FAWZEWA(h)/P~r, 0WAM-2
1 A~C__NR,__MJF018097 SOURCE CODEj UR/0203/6()/006/002/0215/0222
AUTH OR: Dorman, L. I.; Miroshnichenkoj._j!.,_j.,
ORGs Institute of Terrestrial Magnq~t_~Rj~,.Jopqsphere and Radio Wayej)~opa~utimfil 9FSR
(Ins t Rt~if- z-em'-n'o gm- - -m-a-g--n--'e'-ti-z'-m-'a-,-I--o-nosf ery I. rasproatraneniya radiovoln)
K'
TWLEi Method for determining the spectrum of solar co-s-mic.rays In the high-energy
region
SOURCE: Geomagnetizm I aeronomiyap ve 69 no. 2p 1966v 215-222
TOPIG TAGS: cosmic ray# cosmic ray shower, cosmic ray measurement. solar radiation)
ionization. chamber, solar spectrum
ABSTRACT: This paper presents the results of computations of the integral
multiplicity of generation for a neutron monitor and an ionization
,'thamber.. 7ho computations for the neutron monitor were made using the'
latitude effect of the neutron canponent at sea level. The Integral
,multipLxity of generation for the ionization chamber was computed on
,the bas:Ls of the latitude effect of the burst of 23 February 1956. On
~the basis of the computed generation multiplicities the authors deter-
mined the spectrum of solar cosmic rays at the boundary of the atmosphere
,for the burst of 23 Februs--y 1956 in the region of rigidities 1-15 BoV-
Thd oiig'. art. s97a--3.-ngui6s and 27 formulio. a-pr,,
a _7
SUBM DA,rE O4Jan65/ ORIG REFs 00
Card DE: Q3, 04 5/ (YTH HEF: 011/

AqC NRI'All-7007046 SOURCE CODES UR/0203/66/006/004/0782/0785
AUTHORs- Alanlya, H. V.; Do ian, L. I.; Shatashvili, L. M.
ORGs Institute of Terrestrial ~~gr6imlsm, Ionosphere and Radio
Wave Propagation, AN SSSR (Institut zemnogo, magnetizma, lonoefery I
rasprostronenlya radlovoln AN SSSR); Institute of Geophysics, AN GruzSSR
(Institut goof izikI AN CruzSSR)
TITLE: flathematical expectation of the distribution of the harmonic
coefficients when determining them using 12 ordinates and comparison
with experimental results
SOURCE: Geomagnettzm I aeronomiya, v. 6, no. 4, 1966, 782-785
TOPIC TAGSs diurnal variation, cosmic ray
SUB COM: 04
ABSTRACTI The method of harmonic analysIs is used frequently In
investigation of stellar-diurnill solar-diurnal, semidiurnal and other
cosmic ray variations of a periodic character. The frequency distributions
of the zmplitudes and phases of the first and second harmonics of solar-
diurnal variations show that the amplitude and phase of the harmonics
have a definite distribution caused by two factors of a different
physical nature: 1) actual changes of electromagnetic conditions in
interplanetary space and In the earth's magnetosphere, determining
periodic variations of cosmic rays; Z) fluctuations of the values of
cosmic ray Intensity caused primarily by errors of a statistical and
InsLrumontal character. The purpose of this paper to to determine the
relative Importance of the first and second factors. The quantitative
solution of this problem Is important for study of diurnal variations
,:ard UDCt 523.165

j~dC NR: AP7007046
over short intervals of one or two days, especially in analysis of
changes of the diurnal variations from day to day and In periods of
Forbush decroasos. In this paper emphasis Is on the second factor
its influence on the frequency distribution of amplitude and phase of
tho first harmonic In a harmonic analysis using 12 ordinates. It is
shown that comparison of the theoretical and exparimantal results makes
It possible to then determine the contribution of the first factor.
The results obtained In this paper can be generalized easily for the
case of determining harmonics using any number of ordinates. OrIg# art*
has 1 2 f Igures and 7 formula LJ-PP.Ss 38,677
r..j, 2 12

ACC NR. V7008936 SOURCE CODE, UR/0203/66/006/005/0922/0923
AUTHOR: Dormin, L, I.; Kovalankol V, A.
ORG: In-,:trt-u-t-a-0'rT8Yr0s trial Magnetism, Ionosphere and Radio Wave Propagation,
AN' SSSR. (Institut zemnogo magnotlzma, Ionosfery I rasprostranonlya radiovoln. AN
SSSR); IrLstituto of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation,
SO AN SSSR. (Institut zemnogo magnettzmaq lonosfory I rasprostranenlya radiovoln
SO AN SSSR)
TITLE: Method for Introducing barometric corrections into data on cosmic
ray intensity
SOURCE: Geomagnetim I neronomlyaq v. 6, no, 5, 1966# 922-923
1 TOPIC TAGS: cosmic ray intensity, cosmic ray
SUB CODE: 04
ABSTRACT:
31 now is customary to define the rolatiqh between comic ray
intensity and pressure at the level of obsorvat on by the expression
i - io exp C- A (h - ho)-7
whore I and To are the intensities of cos=aic ays at the pressures h
and ho rospoctivoly* p is the barometric coofFiciont. However, str.Lctly
speaking formula (1~ is not procisoo The fa t is that the barometric
effect consists of two parts: a) a negative absorlZon effect,, charac-
torizing the decay and absorption of tho ooldax7 component or comic
1 rays in the atmosphere; b) a positive effooq caused by the oh~ngo of the
Lc--,dlz~- UDC: 523.165

ACC NR, Al-7008936
generation of the secondary component. In genoral.,, th4 quantitative
rolation of those effects changes with a chango of he The barometric
cooffiniont ~ is a function of h and is dotorminod b ho expression
7 t
dl/,dh - 6 (h). (2)
From (2), with tho boundary condition Ith ho 10, it follads
h,
exp ~tp (h)dh]
0 (3)
ho
Using A' (h) (3) can be used for computing the anticipated chan.-cs 1/1,0
fol- difforent gutoff rigidities R vfilcn ho - 760 rxi fig. Theso results
for R -- 3, 4.5'*. 6.4 and 9*5 BoV are given iq,Ya tablo. For comparison
the same table gives the predicted changes X110 for 'R - 3BCV, on the
basis cof fomul4 (1) with constant Vfor h.,,- hoe The errors in this
ca.:,o 'ar 5 h - 10, 20
30# 40, 50, 60 mm.Hs are 0..1, 0.2, 0.4, 0.7,
104 and 2.1%o ~iose errors are rathor large in comparison with the
accuracy of roaZi-ding the neutron compon6nt, by mcKlem instruments*
Orig. art. -has 3 figures and I*table.' RSs- 38*,6'
Li-P

ACC NR, SOURCE CODEt UR/0203/661006/003/0959/0959
AP7008940
AWHIOR: Dorman, Lo I*; Inotaintsevaq Ov Is
ORG; none
TlTLE: Ihird all-union school of space physics
SOURCE: Geomagnotlzm I aeronomlya, v. 61, no. 5, 1966, 959
TOPIC TACS: solar wind,, solar activity, cosmic ray, solar flareq
supernove
SUB CODE: 03
ABSTRACT,~
The Third All-Union School of Space Physics was hold at Bakurani
during the period 15-26 February 1966. It, was sponsored by the Cosmic
Rays and Radiation Belts Siction of the Interdepartmental GeophysicUa
Co=:Litteo. Mich of the work in organizing the school was done by the
AcadcrW of Sciences of the Georgian SSR and the Geophysical Institute
at Thilisi. It was attended by about 80 t3oiontists from moro than 20
Soviet observatories and institutes* The program covered a -;--"de rage
of problems in space physics* A total of 39 lectures were prc:;i-.rtcd
on several themes. The first-group of papers was devotbd to the origin
of cosmic rays and the acceleration of charged particles to great
energie;3 under different apace conditions (in solar chromospheric
flares, quasars# supernovaep and in the tail of tho eax-th's magneto-
sphere , The main lecture was given by S. 1. Syrovatakiy, who told
in detail of the now mecha~iism of acceleration associated with tho
dissipation of magnetic fields. He demonstrated that the acceleration
of.particles can occur under very different physical conditions. H(r,,-
rnrd _14~ UDCs 002,704,31

I-ACC NRI ---Aj?7008940-- ------
ever, most of the lectures were,on the physics of cosmic rays and their
variations. L. I. Doman gave a claisification of variations and their
possible reciprocal interference and discussed the problems of the
nature of comic ray variations of difterent types, On the basis of
data on the 11-year and 27-day variations of cosmic rays it now has
been possible to estimate bhe dimensions of the region of the solar
wihd and their change with the cycle of solar activity. It is found
that on the assumption of a opherically symmetrical model the radius of
.the region of modulation, attaining about 100 atu. at the maximum of
solar activityq decreases by about 2-3 times in the period or dec.Line
.of soL-Lr activity., G, M, Nikolfskiy,.Vo Vo Vitkovich,, Ao Zo Dolginova
and V, I. Shishoy discussed studies of the solar corona, solar wind and
intern, lanetary jupetic fields by' study of oomet a and use of.. radioastro-
n=ical methods** LJPRSt 38,6777

ACC NRi j%?7000517 SOURCE C'O-DE-: -UR/00-118/66/0--io/oll/.-L-15,7/1759
AU-11'rHOR: Blolech, Ya. L.; D OR44.,_L. I.; Xurnosova, L. V.; Razorenov.,
.U. A Raychenko, L. V.; Suslov, K.'A.; Fradkin, M. 1.
ORIG: rionze
TTME: 11, study of time changes of nuclear flux in orimary cosmic
rad4_ation on Elektron-2 and Elektron-4 satellites /Taper presented at All- 1
Union ConAl"crence on Physics of Cosmic Rays held in Xoscow fi-o-M 15 to 20 November 19~57,
SOURCE: AN SSSR. Izvestiyq. Seriya fizicheskaya, V. 30, no. 11,
1960", 1755-1759
TO?TC lp.,'^S: primary cosmic ray, cosmic ray-measurement, cosmic ray
Lr
Intensity,
ABST.R~CT: Some results of a study of primary cosmic radiation conducted
using the Elelctron-2 and Elektron-4 satellites are given. An Integral
Cherenkov counter was placed in each satellite to measure fluxes of
nuclei with energies greater than 6oo mev/nucleQn. Those nuclei be-
longirr, to groups Z a 2, Z --- 5, z ,> 15 were measured by the Elektron-2.,.l
and.those of group Z -- 20 by the Elektron-4. Average flux values
measured for the above groups of nuclei relative to the average flux
Viluez; obtained during July 1964 are given in Fig. 1. The above data 1-
!.-c'over.s the period from 30 Jan 1964 through 9 Feb 1965. The fluxes
1 -11 1----

ACC NRt AP7000517
J
W'N?N.- VT
v4
4A OW
1. Relative values_of primary cosmic ray flux obtained by
El~'ktron-2 and Elektron 4 satellites and by a ground station
1, '2, 3, 4 - Relative fluxes of nuclei with Z --e 2, Z ?: 5, Z ~t 15
(right-hand graph) and magnitudes of statistical error of the
mid-day values; 5, 6 - cosmic flux values obtained by the neutron
-monitor, and flux caused by c4romospheric flares (the sizes of
vertical lines correspond to flares of particles 1, 1+, and 2)
registered at the Climax ground station.
CGEL-2/3

ACC N5j A?7000517
mcast-.red at midday by the satellites are in close correlation with
those measured by the ground stations for quiet ground conditions.
is noted that nuclear flux Increased by a factor of 1.7-2 durin3 the
nariod from 1959 to 19611. During the same period the flux registered
~y a neutron monitor at the Climax ground station increased by about
20~'5. Druring 1964-1965 as was anticipated the nuclear flux Increased
by about 15;'j for nuclei with Z -:!- 2 and Z "-~: 5. The accuracy of meas-
.:vemonts of the flux increase of nuclei with Z > 20 during tho flight
of the E'lelctron-4 satellite was impaired by several rises In flux and
by s,16-nificant statistical errors. Orig. art. has: 3 figures.
(WA-751
(IV)
SUB XDE: Oq, 19
V ?0/ SUBM DATE: none/ ORIG REF.- OOT/
OTH REP: 007
card 3/3

ACC NR& AP7013721 SOURCE CODZ; U,(/0203/65/005/006/1099/1102
AUTHOR: Dornan. Lt If Hazaryuk, Yo. A.
CIRG: Inntitute of Terrestrial Magnetism, the Ionosphere and Radio 'Java
Propagation, AN SSSR (Institut zermol;o nagnetitnag ionosfery i rasp ros traneni ya
radiovoln AN SSSR)
TITLE: Complex anplitude-phass modulation of periodic cosmic ray
variations
SOURCEt Geomagnetlzn I aeronomlya, v* 5. no. 6, 19659 1099-1102
WPIC TAGS: cosmic ray, amplitude modulation, phase modulation, solar
variation, earth rotation, solar telescope, cosmic ray telescope
SUB CODE: 04,03917
MTRACT:_F,ar3.ie*r 'studies by L.'I. Dorman have discussed the simultaneous
amplitude-phase modulation of periodic cosmic ray variations *Waic.h
occurs with.a period much greater than the basic period. Dorman also
has used exiwrimental data on the rolar.,diurnal variation obtained
with crossed telescopes and a neutron monitor to invostigate the sat-
-ellites, determine the modulation ParaMOterb and detect the true
-sidereal-dournal wave,. In these studiesJt was assumed that there-,
Cord 1/ 2 UDC% 523.165

ACC NR: AP7013721
,is one kind of amplitudo-phase modulation with a definite period (one
.yeax). ftwever, in actuality the phenomenon is far more complex, when
~there is modulation of the periodic variation simultaneously with
.,several periods, This modulation is related primarily to the rotation
,of the earvh about the sun (with a period of about one year) and the
.rotation of the sun on its axis (with a period of about 27 days). In
a general case the depoWdence of intensity on time for such complex
modulation can be represented in the form,
f (t) = AO/1 + S.,l sin(Olt + Val)11l + a2s in(4)2t + Va2)1 X.
a In lwot + 0. + S. f a WO .lt + (Pfl) + r2s in(102t +Vf2YR.
itude, frequency an
vhe.re Ao, Wol, VO are the ampL d phase of the
prkacipal,waveof w and w2 are the modulating frequencies; Sa and
-S f is the intensiiy of amplitude and phase modulation; ~Pa and yr
are the phases of the amplitud and phase modulation. The authors
then expand f(t) into satellit:3)o It 'is shown that. with an increase
of the order of th4 satellites their amplitude decreases sharply in .
-comj*z~ison with thd.amplitud;.of the main wave. Therefore, at present#
due to the relatively low accuracy of experimental dat.j, it scarcely
makes sense to use satellites of a higher order than-indi 'cated in the
art-."-cle for finding the modulation. parameters. The authors thank 0. 1.
Inoll, iseva for dUcussio results. Orig. art. hass I figure
C r/ ormulas. Lipits: 340S99'

ACC 14R: AP7002197 SOURCE CODE: UR/0203/66/006/006/1096/1098
AUTHDR: Dorman, L. I~.
ORG: Institute of Terrestrial Magnetism, Ionosphere, and Propagation of Radio Waves,
AN SSSR (Institut zemnogo magnetizma, ionosfery i ras pros traneniya radiovoln Ali SSSR)
TITL7: The barometric effect of cosmic rays with variation of the primary spectrum
and the rigidity cutoff taken into account
I i
SOURCE: Geomagnetizm, i aeronomiya, v. 6, no. 6, 1966, 1096-1098
TOPIC TAGS: -barometric - coefficient, cosmic ray, magnetic storm, solar cosmic ray,
mfft!!m- magnetosphere, primary cosmic ray, cosmic ray intensity,
iatmos-oheric pressure
ABSTfiACT: A correlation between the barometric coefficient of cosmic rays and the
enerj7, spectrum of the primary rays, and the coefficient's variation during magnetic
stormis and the arrival of solar cosmic rays on the earth are established. An attempt
is*mz;do to associate the barometric effect with the change of the spectrum of pri-
mary rays and the rigidity cutoff caused by the instability of the
magncttosphere. The integral equation for the cosmic ray intensity at a selected
level with a constant pressure is given on the assumption that the energy spectrum
and the ridigity cutoff are constant. The variation of the intensity of cosmic rays
is associated with a change in the barometric pressure. The final integral equation

:At C _NRS---iii-06ii-47
for the intensity of cosmic rays can be solved 'by successive approximations. Orig.
:art. has: 15 formulas. CEGI
I
.SUB CODE: 04/ SUBM DATE: 25Mar66/ ORIG REF: 003/

ACC NRt 1,P7002198 SOURCE CODNI: UR/0203/66/006/006/1098/1100
AUTHOR: Alaniya, M. V.; Dorman, L. I.; Shatashvili, L. Kh.
ORG: Institute of Terrestrial Magnetism, Ionosphere, and Propagation of Radio Waves
i AN SSSR (In-stitut zemnoso magnetizma, ionosfery i ras pros traneniya radiovoln AN
SSSR); Institute of Geophysics,AN GruzSSR (Institut geofiziki AN GruzSSR)
TITLE: Quasi-spiral changes of 27-day variatior. -f cosmic rays with the solar
activity
SOURCE: Gecmagnetizm i acronomiya, v. 6, no. 6, 1966, 1098-1100
TOPIC TAGS: cosmic ray, magnetic field, interplanetary space, harmonic analysis,
neutron comp3nent, solar activity., 11,17'FA,~.Slrtl
ABSTRACT: 1-:: is pointed out that the eleven year variations of cosmic rays are
41 usually determined from the mean monthly intensities of cosmic rays. However, the
fine structure and the longitudinal distribution of cosmic rays cannot be determined
from these d4xa. Using the 27 day variation of cosmic ray intensities, the asymmet-ri
of the magnetic inhomogeneities on the solar surface and their duration in the inter-
planetary space can be detected. The amplitude of the phase of the 27 day period of
variations in the intensity of cosmic rays was determined by haronnic analysis from
the mean values of the intensity of the neutron component. The obtained results are
presented gra3hically. The graphs show that the amplitude of 27-day variation
diminishes nonmonotonically with the solar activity, completing a full cycle (12 to

ACC NR: AP7002198
"8 solar rotations) at the minimum of solar activity. Thus, the 27 day variations of
cosmic rays exhi'At a spiral-shaped run. The spiral twists during the minimum of
solar activity and untwists at its maximum. Variations of cosmic rays are caused
t-y asymmetric fluxe!! of magnetic inhomogenei ties. The asy=,.etry decreases with a
decrease in solar activity. Orig. art. has: 2 figures. (EGI
SUB CODE: 04/ SUBM DATE: 08Dec65/ ORIG REF: 004/

ACC Mi AP7002199 SOURCE CODE: UR/0203/66/006/006/1101/1103
AUTHOR: Dorman, L. I.; Kolomeyets, Ye. V.; Sergeyeva, G. A.
ORG: Kazakh State University (Kazakhskiy gosudarstvennyy universitet); IZMIRAN
TITLE: Seasonal var-rations of solar diurnal and cemidiruanl variations of cosmic
rays
SOURCE: Geomagnetim i aeronomiya, v. 6, no. 6, 1966, 1101-1103
TOPIC TAGS: cosmic ray, ecliptic plane, ==d= diurnal variation, solar variation,
solar physics Cc'-~;/77 / C_ R14 C/ 1M7-V,0:-Y17-Y e'e?Z,0-nj. 0
-ABSTRACT: The seasonai variations of solar diurnal and semidiurnal cosmic ray
intensity were analyzed using the 1958-1962 data from the global network of
stations. All stations of the network were divided into three zones on the basis of
the mean cutoff energies: E - 1.5, 4.2, and 12.0 Bev. The mean solar diurnal
variations representing the amplitudinal deviations from the mean yearly values
were deterndned for each zone. The results obtained were tabulated and plotted on
graphs. The change :1n the amplitudes was computed using harmonic analysis for
annual and semiannual seasonal variations of amplitudes. In 1958, 1959, and 1960
these variations were equal at all latitudes; however, they were different at dif-
ferent latitudes in 1961 and 1962. It was established that two sources of aniso-
tropy of cosmic rays, (tangential and radial) are almost always found at the same
1/2 UDC: 523.165

ACC NR: AP7002199
time. The intensity and the relative importance of each source varied considerably
during the period of investigation. (EG]
SUB CODE:
04/ SUBM DATE: 06Sep65/ ORIG REF: 002/

DORKU, M.I.; NIMDIAYZVSKIY. A.A.
Now data on the geology of the V1lyW syneclise. Geol. nef ti I gaza
4 no.1:13-18 Ja 160, (XIBA 13:10)
1. Yaltuta4ve goologicheskoye upravlent3re,
Ofilruy Lovland--Geoloa)
(Prospecting-Geophysical methods)

88382
,q- .2~8 7
~', 3 2.4 o(0 /so /0 4 7
S/108/60/015/010/010/016AX
B012/B077
AUTHORt Dorman, M. I.
TITLEs Characteristics oJ* Oscillation Phenomena When the Frequency
Passes Through the Zero Point
PERIODICALs Rad:Lotekhnika, 1960, Vol. 15, No. 10, pp. 27-32
TEXTs In the present work, the characteristics of the origin and the
fine structure of the "zero beat" are investigated. For this purpose, the.
influence of two oscillations e (t) and e upon a linear or nonlinear
1k 2(t)
system with variable parameters is studied. It is assumed that the in-
stantaneous frequencies of these oscillations are positive and can be
represented as derivatives of the. phases with respect to time. Only
"zero beats" are investigated, and it is assumed that the load of the
mixer is a low-frequency filter, and that the initial oscillations are
not amplitude-modu2ated. The formula
t
(t) - (!2(t)dt + f. (5)
Card 1/4

88382
Characteristics of Oscillation Phenomena When S/108/60/015/010/010/016/XX
the Frequency Passes Through the Zero Point B012/BO77
clearly expresses the relation betwean the instantaneous phase 4(t) of
the resulting oscillation and the difference frequency SZ(t). Since the
difference frequency is a steady funation, also f(t) has to be steadyl
that is, there can be no jumps near t - to. sz (t) - W 1(t) - (.)2 (t) -
The function J (t) is investigated near the stationary point to. Two dif-
ferent cases can be distinguished if _Q (t) is considered an arbitrary
functions 1) 2(t) Passes through zero without changing the signt 2~ the
sign changes. It follosis that t - to, the stationary point of I (t , is
a point of inflection in the first case and a maximum or minimum in the
second case. It is pointed out that the widely used representation of the
frequency of difference oscillation b;T 101(t) - 02(t)1 can only be applied
to determine the absolute value of the difference frequency 1.2 (t)1
because the real characteristic of tho change of the oscillation phase is
not taken into consideration. It is noted that the two definitions of the
frequency: 1) as a derivative of the phase and 2) as a positive quantity
2jr/T are in some cases incompatible. Ls has been shown, the contradiction
of such a double definition can be seen at the zero point. In order to
change this, it is sufficient to take the first definition
Card 2/4

Characteristics of Oscillation Phenometa When S/ 1 OB/ 601015/010/010/01 61XX
the Frequency Passes Through the Zero Point B012/B077
E~(t) d4 (t)/dt as an exact definition of the frequancy. and the second,
12 (t)l - 2r/T? as a definition of the absolute frequency value. It is
pointed out that the sign of frequency has to be considered when investi-
gating oscillation phenomena related to a passage of frequency through the
zero point. The author thanks Professor I. S. Gonorovskiy for his sug-
Gestions. There are 4 figures.
SUBMITTEDt February 24# 1960
-pig
I-C3 rr-C3
C~rd'3/4 Qj%

S
08/60/015/010/010/016/XX
/I
B010077
to
ts q,
IV vv uv
Psc. 2
Pvc. 3
Card 4/4

BOIO/BO59
AUTHORt Dorman, M. I.
TITLEt Energy Spectra of Random Sequ,ances of Overlapping Pulses
PERIODICALt Hadiotekhnika, 1960, Vol. 15, No- 12, PP- 50 - 52
TEXT: The energy spectra of random squences of overlapping pulses can
be calculated by conventional methods. The mathematical procedure is shown
by an example. For a pulse-like random process without storage and overlap
(in accordance with the terminology used by I. N. Amiantov and
V. 1. Tikhonov, "Radiotekhnika", Vol-14, No.4, 1959), the energy-spectrum
formula (1) as given by B. R. Levin boldst
12 + f( 2 X 00 21)
F(&~') - 'ffK(Cj) - JH(c-) C.3) + III (C.) 1 2 _F T 6 (cAj - r-with the
r_-oo I
same notations that were used by B. R. Levin. However, with the amplitude
condition ~M(t) =-= 0 , t