SCIENTIFIC ABSTRACT GALPERIN, Y.I. - GALPERINA, R.YE.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R000614130007-9
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: July 19, 2001
• Sequence Number: 7
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

25990
S/56o/61/ooo/oo6/008/010
Disc.overy of E032/E.3i4
is asumed. It in estimated that the energy flux associated
with these currents,-which may reach the lower layers of the
atmosphere, is at least I erg cm -2 sec.-1 . The discovery of
large currents of 10 keV electrons is.of particular importance
to the understanding of many geophysical phenomena. For
example, it is interesting to note that appreciable
intensities of such electrons first appear at the geomagnetic
latitude at which increased ionization was previously recorded
in t~e F-layer and which could not be explained by hard
electromagnetic radiation of solar origin.. The existence pf
these electron currents may lead to the explanation of ionization
irregularities in the upper atmosphere. Acknowledgments are
made to S.Sh. Dolginov, V.V. Beletskiy and Yu.V. Zonov for
determining the orientation of the apparattls relative to the
magnetic field. There are 11 figures and 15 references:
12 Soviet and 3 non-Soviet.
SUBMITTED: December 9, 1959
Card 5/7

GALP=) YU 0 1 0
"Proton Bombardmat in Aurora,?
report to be sulksitted for the Symposium of 2h~etle&l Interpretation of
Uner Atampbarla Jklaslow,, Paris lrmn,, 25 - 29 Jww 1962.
Dwt. of Phples of the Atmompherel, Aced. Sol* UM

.gAL,_pERIN, - yuri_y_ 11., -., ch - akovich; YAGLOM ,
,___~ZjjSHKOVICH, Aleksandr Isa
A.M., prof., red.; FAYNBOYM, I.B., red.; RAKITIN, I.T., tekhn.
red.
[Auroras]Poliarnyo siianiia. Pod red. A.M.Ikgloma. Moskva, Izd-
vo "Znanie,* 1962. 24 p. (Nowe v zhisni, nauke, tekhnike.
IX Seriia. Fizika i khiniias, n0.2) (KUU 16:1)
(Auroras)

J4~!B
S/04-9/62/000/002/004/005
.'7160 D21U-/D--"Ol
Yu. 1.
TL- T Ll On the proLlem of t1he sources off cncr,lry of the u?i.)er
atmosphere
-ZluDIC-'~L. 0
LiCa-demiya naul: lzvestiya. "criya
kaya, no. 2, 1962, 252-261
TIM: -I review off published information leLds tac author
to conclude that both direct measurements wad theoretical csti~ilates
indicate that tho `Iux, of solrr radiation which ionizer, the ~! layer
4.s of t-he order of 1-3 erg,/cm2sec. This result is loased on data
incIuding Sputuil- 1II measurements. if the source of heat in the
Ztmosphcre is only the incident solar r3iiiation, then L,,)ov(-2 the
bsorL)tion layer thc atmosphere should be isotherTial the tem,-)c-ra-
ture of the isotheiTiial laved- and the height of its base should de-
crease at night. If, on the other hancl, the atmosplacre cont- a i -,i S xn
appreciable additional source of heat in the --Form of cor~)uscular
Card 1/4

S/049/62/006/002/004/CO5
On the problem off the sources ... D2lU-/D301
radiation -,Aiich is rbsor*::)cd above 'Che '-' layer maximuta, then the
tel.-xpcraturc shotild incroase with altitude rio'lit: u--) to the up,x-,r
-ad arl17 o.-L"' the heat sourcc, and the t em-,.:)e r attire of t1he lower boun-
dary of Llhe e--ospnere shou": ell be highcr -than that Of 'the ---' layer.
'21ie different ter.,ipcrature variation preclicted by tlae two i.-Lccha-,-.-i,-mis
shoulcl have an effect on the (Icnsity variation with altitudc and
t',-ie latter can be deduced from the drag on satellites. In fact,
aal y f '-1 c latter
w- - --is of models off- the atmospla,2re lbased on ulata o- Lil L
.
type shuus that in the ra-inge 250-350 hm, the heat flinc al3sorbed i-L-1
daytime is about 0.2-0.6 er'r/cm sec I'Alich. Can hardly be c::plaincd
Q I
by the absorption of solar ultraviolet rL-Aiation. Un t".C O'Char
hand, the hc--t T'lux absorboO. at night above 200 lliii is I-ess ti-lan
0.05 err-*/cr,12sec. In independent criterion for cstimati-a~r the e-.ierZ;y
0 C->
'Llu:-c duc to the entry of corpuscular radiation may be the abscuce
+ L j -
o-E 1 'N-IGN emission --,*-,i the sl:)cctnim of the nil-1-it'FlOW WiJI-11, intcusicy
%2 0 0
,,-ereater than the detection threshold of modern hi',-:1-Ily sensitive
--o-j?,aratus it is estimated that for electrors the limit of
corpuscular radiation energy flux at night is 3 -1. 10- er.,:/-&
Card 2/4

S/01~ 62/000/002,/004/005
the -3roblovm o.-- the sources ...
D213yi)301
2 T,ie:-,c
waiI2 f"or protons the uPper limit is 6 x 10-4 cr,-/cri cec.
ures rcfer to 10W 1,1titLldCS. The concli--.;~o-a is, t`cre-
-t.3 I I - -
-z'L a,
kore, that it-low dlata indicate that corpuscular rad.LL cio ,
LL,(:-, for-ul 0-~ 2 tr 'ass and - rclons cannot bc an irq)ortant source of
Cl C 0 'D L
he -, - a~ 'L1- r"'at i~L t'L-~e middle low latitudes. At 'hi-h lat-itudes
I clL L LL) Q
the situatio-a may be di,.-'11crcnt. Ia the a-uroral zo-ac thc up,)Cr at-
mosplicre cout-inuously rcccj.vcs corpuscular raJiation and the cncrL,,y
cstimated for electrons turns out to be of 'the or(.'cr o" I cr~/
cm2sec. A.I. 'X-crsh.--.ov--'-ch is mentioned in the :Articl.c. Thcrc arc
I fi-1.1rc, 1 ttablc and 50 rclrorencos: 10 Soviet-bloc and 21 non-
Q
7oirict-'aloc. The 4 most recent references to tpub-
0 L3
lications read as follows: 11.1licolet. Plaziet Space Sci. , 5, no. I
(1961); 2. 1"lothwc1l an6 C .7- 111cIlwain. ].'-),-rnctic SitormS alld the Vail
--Ilen radiation bclts; Observations -from satellite 1953 cdsilon
(-~'-Olorer IV). Proc. Int. Space Sci. S"imp. , Nice (1960); L.G.
Jacchia. 21. variable atmospheric-dcusity model from satellite accel-
erations. Smitson. Contr. to astrophys. no. 39 (1960); H. Hinter-
egger, preprint. 1~rcliminary data on solar extreme ultraviolet rad-
Card 3/4

S/049/62/000/002/&A/005
on the probleta of the sources ... D21u-/D,3Ol
iation in tne upper atnos?hcre. Florence (1961)
ASSOCIATION: Ahademiya- naaul: "J30-R, Institut -2,iziki atmosil-ery
(Acadcmy of Sciences USSIII, Institute of Vhysics
of the Atmosphere).
SUM-1ITTM: !.~ay 25, 1961
Card 4/4

N-T4# MLTANGFIII, T.M.,
Soft Corpuffaur PAwdsuom
"r6 to be w&WtW ter as hfA ISU"NUOma gpan ftj~o
(OWAR) Van=, 2.22, j"m 63

L 18945-63 LUT (1) /UT (m) /FCC (w) IFS (v) -2/BDS/tS (V) AIMC/AFM/ASD/
..M tS TT/GW
ACCESSION NR: AP3007340 S/0293/63/001/001/0126/0131
Gal'pqrin,
Yu. I.; Krasovskiy,.V. I.,
AUTHORt
TITLE1 Study of the upper:atmosphere by means of the
and Cosnos,5 satellites. 1. Apparatus
SOURCEt Kosmicheskiye lssle,iovaniya, v. 1, no. 1. 1963, 126-131 1
TOPIC TAGSs count r, particle counter, ton counter, ion trap
a ;atelt
electron counter, ionospheric particle, ionospheric current,
lite, Cosmos satellite, Cosmos series, Cosmos 3, Cosmos 5, geo-
physical study, geophysical satellite
ABSTRACT: 1p the first of four articles on the investigation of
ionospherid\jfqh&rjed _particles by the Cosmos 3 and Cosmos 5 satel- it
lites, a detailed description is given of the parti e-sensing
'~,apparatus carried on board. Three types- of co -- Twere use
covering the energy spectrum from just above thermii up to hard
particles in the high-Mev range. The counters were as follows:
1) An indicator type, which consisted of a fluorescent screen laid 1--
Card 1/5

L-18945-63
ACCESSION NR: AP3007340
C)
on a glass bass and faced with a thin aluminum fail to eliminate
low-energy particles, the entire assembly being housed in a cylln-
der. Near the cylinder aperture were two girds, one grounded to
the case and the other biased at (-)40 v to block passage of ther-
mal. electrons. The fluorescent screen was isolated from the case
and could have stepped voltiges applied to it of 0, 0.15, 3, 6 and
11 kv in order to segregate the penetrating electrons according to
energy level. Screen illumination from particle impact was de-
by a photomultiplier whose output wao stored and telem-
tected
etered. On each satellite five such counters were mounted in
various attitudes and with differing values of phosphor composi-
tion and foil thickness. 2) An ion trap, which passed both posi-
tive and negative particles above a fixed threshold le~vel and
registered their algebraic sum. This was also a tubular cylinder
with a grid arrangement similar to the indicator type, i.e., two
grounded grids, a third at fixed bias, and a fourth at stepped
voltages of 0 to 11 kv as in the indicator-type counter. The col-
le-eting element was a silvered metal ring 0.43 cm2 in area, whose
output fed into an electrometer tube. The ring was located in the
annular air gap of a permanent magnet whose field diverted any
Card

L 18945-63
'ACCESSION NR: AP3007340
electrons arriving at less than 5 Kev, as well as ions with similar:r
Larmor radius. The ion trap thus could sensit selected ranges of
positive ions as well as electrons above 5 Kev. Two traps were
used on each'satellite# one with a fixed grid bias of (-)40 v, the
other with a bias of +24 v. It wits determined that the spurious
effect of photoemLssion caused by solar rays striking the collec-
tor ring was small (on the order of 10-11 amp), which verified the
suppressing action of the trap's magnetic field. 3) A standard
halogen-fill d geiger counter, type STS-5 which had an effective
area of 4.3 :m2 and was shielded by 3.4 g;cm2 of lead. With the
added shielding of the satellite skin this counter had a negligible'!
response to electrons below 400 Kev or protons below 50 Hev.
Sample recordings of the indicator counter are given which show
modulation in electron count caused both by the stepped accelerat-
ing voltages and by the rotation of the satellite. Degradation in
the Al foil*was detected, apparently caused by micrometeorite
erosion. A large increase in foil porosity occurred during the
launch phase, due either to frequent meteorite contact while rising'
i through the denser atmospheric layers or to sudden outgassing of
Card 3 / 5

ACCESSION NRt AP3007340
the foil on entering the vacuum environment. The variations and
relative orientations of the indicator and trap counters are shown
in Fig. I of the Enclosure. Orig. art. has: 6 figures.
ASSOCIATION: none
SUBMITTED: 09May63 DATE ACQ: 210ct63. ENCL: 01
SUB CODE: AS, GE NO REF SOV: '003 OTHER: 001

AMC/F,SP-3APGC
ACCESSION NR:
(I-) jtwr(M) #CC (W) /FS(y)-2/BDS/ES (v) /t EC-2 AMC/ASD/
Pe--4/Pi-4/Po-4Aq-4 TTIGW
AP3007341 S/0293/63/001/001/0132/0139
AUTHORs Krasovskiy. V. I.; GallpAxLn-.-Yu. 1,,,: Dzhordzhio-, N. V.:
Mulyarchik, T, M#; Bl~-Iyunova* As D.
TITLEs Study of the upper atmosphere by means of the Coo mos 3
and Cosmos 5. 'satellites. 2. Soft particles
\,V
SOURCEs Kosmicheskiye issledovanlya, v. 1, no. 1, 1963, 132-139
TOPIC TAGS: Cosmos satellite. Cosmos 5, geoactive particle,
ionospheric particle, ionospheric current, ionospheric field,
ion, Lion counter,;,-patticle-counter, Cosmos 3
ABSTRAM This is the second in a series of four articles on geo-
active particle research conducted during the Cosmos 3 and Cosmos
orbital flights. This article,
,Ydiscu9ses the existence of currents
of electrons and positive ions\ in the upper ionosphere having
,a nergies that are relatively low but greater than thermal. This
was concluded from fluxes detected by the two types of particle
counters used: 1) a sensor formed of a fluorescent screen and
5
Card

/L, 1-894"3
ACCESSION NR: AP3007341
0
photomultiplier, which was biased negatively and also shielded with~
Al foil so as to register only electrons above 40 ev and positive
1 ions whose free path exceeded the foil thickness (e.go, proton of
the order of 200 Kev); 2) an ion trap which registered electron
of 5 Kev or more 'and positive ions. The trap counters showed r
'posted instances of anis6tropic positive ion flow in a direction
normal to the geomagnetic force lines; the fact that no simulta-
neous indications appeared in the indicator screen type counters
thus suggests that. these must have been "soft" positive ions; if
protons, thei.r-energy would be less than 200 Kev. This conclusion
is supported by the fact that when the satellite had turned 180*
the indicator counters in turn registered particids not sensed by
the -ion traps, which were evidently electrons below 5 Kev. There
thus are areas which exhibit local current flow, in which positi V e
ion energies are estimated to be several dozen electronvolts and
average density to 108 ion/cM2/sec/ster. These areas are in the
200-ID 600-km region and tend to remain at the same earth latitudesi
j for prolonged periods, sometimes as much as 9 hours. The authors
emphasize that complete determination of the orientations of the
j.Card 243- ------ -- -

L 18946-63
ACCESSION NR: AP3007341
Cosmos 3 and Cosmos 5 satellites during flight is not yet complete,:
but sufficient data are available to verify the above results.
Additional observations are made of some high-energy particles,
particularly those registered in the South Atlantic geomagnetic
anomaly. If these had been positive ions, the ion trap count, being
the algebraic sum of incoming particles, would have been phase op-
posed to the indicator count, which records the absolute sum; mined,
however, both counters registered such particles in phase, they
must have been electrons, estimated at between *50 Kev and 1 Mev
and at an omnidirectional density of 5 x 107/cm2/see. Regarding
electron counting technique, the possibility of spurious effects
caused by the fields of on-board transmitting antennas, principally
that of the telemetry transmitter, is rejected since no difference
in electron count was noted whether the transmitters were on or
off. The intensity and anisotropy of recorded electron currents
agree with earlier data from the 1958 Sputnik'~and from the U.S,
"Injun" rocket of .1961. Fig. 1 of the Enclosure shows examples of
electron intensity isolines over the South Atlantic taken by
Cosmos 3. Orig. art. has: 7 figures.
Card 3

L 11112 -63, EWT (1) /FCC (14) IFS (V) /BDS/ES (v) --AFJ)CAFFTC/kFMDC/ESD-3
-4/Pg-4/pi-h/P1-4/Po.4/P w
e
P
ACCESSION XR: AP3000792 S V(03_7~Z31~w 3/003/011 011VM
ATUMOR: Krasovskiy, V- 3: ; (12]L'perin, YU. I.; TC=Y-*Y. V. V. I
T. M.; Dzhordzhio, H. V.; 11C= 2~a. taty'dMova.
A. DO; Vaisberg, 0. Lis,
Potanay, B.~ P Bragin, M. L.
.TITIZ: Some characteristics oj.* geoactive particles
SOURCE: Gecmagnetizm i aeroacta1ya, v. 3., no- 3, 1963,401-407,
TOPIC TAGS: geoactivity, Cosmin-3, Cosmos .-5, satellite,' ;article co=ter,
ioaospheric particles, Kosmos-iL Kosmos-5
r/XSTRACT: Three types of q~arjzed-z_arbicle sensorslused 0:t1 th6 cosmos-3 and
axe d is sed. Oae
CoRmos-5flights are described and sane recorde& results, I CUS
type vas an altmiw= tube which housed a fluorescent ecrL-,en vhose lphotoemission
frcra particle impact was recorded by a photomultiplier. 1-7-he screen.was faced
with allym4nun fail of 0.4 to l..l rag/=2 thickness to prevent passage of
lw-~energy particles. , Grids placed at the tube entrance. included an acce3.eratinng
grid for applied stepped volta4res of up to 11 kv and a bias grid at -40 v to
prevent imj~act of thermal elecllrons on the foil. The Muores6ezt screen vus
made thin (1-4 mg/cm2) so as not to respond to x-ray radiation. Each such
Card

M
L =21-63
ACCESSION M. AP3000792
indicator subtended. about 1/12 -.-ateradian and had its. axis.: awmal to the
sate3.lite rotational axis; each satellite had several Indicatoxs, A second
tubular device, acting au a traj~ tor. high-opted protons wbi eloatwo=.. AMIS
similar in construction but had an annular,collecting electrocIt placed in. a
permanent-magnet field rather Uan a screen., Tho bias gria in this case
eliminated electronz of less tMa 5 kev. AaguLw- coverage of -the :trap counter:
was about 1 steraaian. The third collector used was a standard Geiger caMter
type STS-5, ithich was inside the satellite aldn and had P. 3-=:laad ;shield. to
minimize x-ray effects. This counter responded only to electrons abo-v-e 0.4
i Mev and protons above 50 Mev, but is described as too prinitive to distingld::~h:
"recorders are
their relative contributions. Results from the three types of-
discussed as functions of sete.Uite altitude., latitude, and day/night exposure*
C= ev.
Three general energy groupings appear to exist: 1)ele~tr of 10*_104
at maximum flux density of 109 el/cm*/sec/ster, observed at levels above 300
Im over the USSR (30-35- N); 2) electrons of about 100 Imv, urith a Maxiwaz
density of 2 x 107 ei/cmp/sec/ster, noted maln3,y in southern latitudes at
altitudes of 600-700 lm aver the South Atlantic; and 3),the verr high enerMr
protons and electrons registered by the Gaiger ~ counter at jxaloro of - 100
pulses/ca:3/sec/ster' (not
associated with any particular geograj~,Acal region).
Orig. art- has: 7 fia=es-
Card 2/A

ACCESSION NR: AT4034383 8/2662/63/000/010/0070/'0079
AUTHOR: Gal'perin, Tu. I.
TITLE: Proton precip'itation in auroras
SOURCE: AN SSSR. Maihduvadomvtvenny*y geofizicheakly komLte4. IV razdcl program-
my* mGG: rolyarny*yc o~yaniya i Gvecheniye nochnogo neba. Sbornik atatey, no.
.10, 1963, 70-79
TOPIC TAGS: aurora, proton, proton precipitation, hydrogen line glow, meteorologyq
geophysics, proton energy spectrum
ABSTRACT: The article is in two main sections: a discussion of experimental
results and the theory of auroral hydrogen line glow. In the first of these
sections the author considers such factors as the morphology of proton precipita-
-tion, intensity distribution as a function of height, hydrogen line profiles, tho
Balmer attenuation decrement, hydrogen line intensity levels and correlations
with emissions of other specific character and direct measurements of proton
precipitation into the auroral atmosphere. In the second part of the article,
which deals with theoretical considerations on the glow of hydrogen lines under
auroral conditions, the author has diacuoned the dependence of glow on the velo-
Card 1/4

ACCESSION NR: AT4034383
city of the particle and the role of protons in the excitation of auroral glow.
Theoretical considerations on proton flux anisotropy and corresponding cross
sections are briefly reviewed. The author claims that the problem of deducing
the initial proton energy spectrum from profile observations is still unresolved.
This brief survey of certain aspects of the problem of proton precipitation into
the atmosphere indicates that, despite the considerable successes that have been
registered in this area, the study of proton auroras still resolves itself
basically to a compilation of experimental facts. The material discussed in this
paper leads to the following conclusions; 1. The fact of a broad dispersion of
velocities on the part of simultaneously precipitating protons is established.
The energy spectrum stretches even to hundreds of kev and is variable. The
maximum differential energy spectrum lies in an area of I - 30 kev, with the lower
limit the more probable. The directional intensity of protons -,,t (0) above the
atmosphere is practically isotropic. The refinement of this data requires in-
formation on the function Fnn'(v) for upper atmospheric components and direct
measurements of soft protons (with energies of less than 30 kev), as well as a
height-dependent distribution of the glow intensity of the L.I. lines in the
nuroral regions. 2. The typical form of proton intrusion into the upper &tmos-
phere is a band I - 150 in width, extended along the geomagnetic parallel and
arranged to the South of the basic region of the brilliant auroral forms, excited
rad 214

ACCESSION Nit: AT4034383
by electrons. As the marnatic perturbation increases, tile area of proton pre-
cipitation shifts from the auroral zone toward the equator, but later returns,
Such precipitations are characteristic during a substantial portion of tile obser-
vational time in the auroral zone. The maximum observed intensity of It-- is an
the order of several thoocand raylaighn. For the auroral theory, an explanation
of the character of proton precipitation is of undoubted interast. In this
connection, the author calls ittention to the following pointas in the first place,
in order of magnitude, the energies which correspond to the maxima of the dif-
ferential energy spectrum are close to one another. This coincidence is hardly an
accident. In the second place, the proton energy distribution normally has a
considerably longer tail in the high energy region than the electron distribution
(although during rare, particularly low, type B auroras a large number of elec-
trons with energies of several hundred kev do occur; however, at such times protons
are generally absent). This fact must be considered when analyzing the possible
mechanisms of corpuscle acceleration in the upper atmosphere. In particular, this
situation would scarcaly take place in the event of acceleration by an electrical
field and, possibly, points to some statistical mechanism of acceleration. . Orig.
art. has: 2 figures.
Card 3/4

ACCESSION.NR: AT4034383
ASSOCIATION: Mezhduvedomstvanny*y geofisicheakLy komitat AN SSSR (Interdepart-
mental Geopbysical Cemmittso# AN 856R)
SUBMITTED: 00 DATE ACQ: 13Kay64 ENCL.- 00
~SUB CODE: ES NO REP SOV: 012 OTHER: 033
C.,d 4/4

L 10799-63 EWT (1)/1Fcc (w)lFs (v)IBDslEs (v)--AEDcAMcASD/MMC/9M -31 145-
APOC-Pe-4 g-4/Pi-4/PI-4/P.o-4/Pq-4-TT/Gw
ACCESSION ~R: AP3000793 s/=3/63/0o~/003/0408/0,416
Temn _X. V. V
OR: Krasovskiy. V. I.; Gal']Lerin. Y'U chik. T-M
_X*
Pzhordzhio, N. V.; Ma-rov. M.
TITM. Soze new results of geophysical studies made Upp-OS-_1 and Fosm os-
satellites
S OURM: Gecmagaetizm i aeroncmiya,, v. 3, no. 3, 1963, 408-416
TOPIC TAGS: Yosmos-3, Mosmos-5, radiation belt,- paiticle coiiiter, upper
atmosphere radiation, radiation, upper atmosphere Cosmos~-3, C oslaos - 5
AESMCT: Uncentrationa and intensities of Paiticles as measure& by
the Kosmos-3 and Kosmos-5 satellites are analyzed. The satellites used
ordersV"l) a aolleeto~ tub 'v~itb fluorescent
ccmbinatioas of three typea o~ ree e
screea sensor and photomultiplier, 2) an ion trap with a:ring, electrode
collector located in a parmatent magnetic fieIAI and 3Y a Geiger counter vith
a 3-mn lead shield', Which r .egistered caly.electrons abov6 0.4 Ifev and protons
above 50 Mev. Particles recorded W these sens,ors fell into three energy,
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ACCESSIM M: AP3000793
groups: 1) high-energy protons and electrons recorded by the! Geiger coun~ter,
2) electrons of dboat 100 Kev; and 3) electrons of the 6raer O~f 1-10 Kwi- 3~0
observable correlation appears to exist ar~ong these grour-S. -Isoline'contomrs
in earth coordinattes are given for groups I and 2 . shcrxing their energy!
distribution over the South Alantic region,, where Intewlty v" m=im=..
'These data are in the 650-im altituae region &a shov that the coordinatea of
=dmm intensity areas shifted with succeeding puses cif the ~ satellite.1 Scme
:possible explanations for this shift are suggested which ampostulated on
the lifespan of the particles relative to satellite orbit time. In equatorial
latitudes at a 200--400-1= altitude the Geiger count did, not average overt 1.8:
1?ulses~/sec. In contrast., the Oxeiger count recorded'~y KOSMOS.5 in the vicinity
of apogee (1600 1=) exceeded 1,300 pulses/aec and* showeda'stmg periodicity
with satellite rotation, indicating that these high-energy particles are, trapped.
in the geomagnetic field and miwing normal to its lines ocr force. Group, 3
electrons,' which were sporadic in appearance and, located xminly in the polar
latitudes, varied in intensity proportionally %dth altj~tjiAeo Me reUrUng of'
the satc:1lites due to particle friction at the par1gees (200 Im for Kos=06-3y,
was noted to be less than for Ile 1958 sPutniks, vhich indicates less
.Card 2/3

W14kt
Fc
'178
34
(h); 'Jowh 4/i~-4/Paii', /Psb/Pi4~.'.~ASD(414A /G
(T)TEWA
6 74 2,
ACCEMON N R: AP4046779 S/02.93j64/Q012~/0O!,jb7 3/0
,Iyunova, Aj Do
AUTHORS G&I'VeXia. Yu#_1 Bp
WMW
TITLE:t Registration w ttud4' nu'cle
of the effects of ithe k~~* V~" ar
XL July 9j 1962 by satellite
~_Oaion-of
G
-772
,SOURCE: Kosmicheekiye issledavianlya, v.. 2. Roo 4964 i ~763
ai
Isla 4 :nucle*r::expj#s or#,, gamma
TOP1C:TAGS1 Kosmos 5, J'ohnstoln,
a 'OR
radiation, nuclear ~tes.t. nucle. r radiation,: radiatt
ABSTRAM Kosmos-5. launched 18 Nay, M21,:with W466.41 plane: i,
inclined 49' to the 3qustor,.ois an spopsa of 16004M anif a perig'sis
of 241) kmt registered the hlRh-altituda American nucleat xpl 1ol~iool
which took place above Johnston Island ion 9 Julyo; tfi bent 0 tfi~
ft m mom
explooion, a hard-radiation burst was detecte& far;~!Vsy~id: ihe Iii.01tsi
of tho satellits0s lineof 910t, This ;bUf3.t Was ppariintly the.
registration of (P-radistion caused by :the explosion, ;4ind ~was
named: (f -glow. In the f L re t minutes f ol lowing thfl~ OXV tos ton
positiLvely charged particles (protons), M -particieso :a:nd ftssi~ a
fragmionts (positrons) drifted.to the vast to be detectOd by the
113
Card

L 17830-65
!ACCESSION NR: AP4046779
:;,'cussion of the radiatLon sensing; a#paratuse OvLg#.;l4rt'-:haqi 03 f; guresli
-JASSOCIATION: none

114ar64

CL i
~OO~

Ei 0 W.
c0
'00 REF SOVv
004
OTHERI.
t: . 010

Card
3/3 ::'t'.
F

G-kLPZRIN, Yu. I.; TWNYY, V. V.;
NAtmospheric scale height in the 200-400 km range according to radiation belt data."(USSR)
Report submitted for the COSPAR Fifth International Space Science Symposium, Florence,
Italy, 8-20 May 1964.

GALPE-UN, Yu. I. ; .60LYUNOV.A, A. D.;
"Study of drastic changes of the radiation in the upper atmosphere in -Tuiy 1962!(USSR)
Report submitted for the COSPAR Fifth International Space Science Symposium, horence,
Italy, B-20 May 1964.

GALFERIN, Yu. I. and TETWY, V. V. (Acad. Sci. USSR)
"Atmospheric Scale Height in the 200-400 IGT Range."
report presented at the OOSPAR , 5th Intl. Space Science Symposium,,
Florence, Italy, May 1964.

1, 2796-66 FSS-2/&iT(1)/EWT(m)/FS(v)-"-/FCC/EWA(d)/WA(h) TT/GS/al
........... .. ... ... _.._ --------
tACCESSION HR: ATS023608 UR/0000/65/000/00010388/0393
.fk-v
'AUTHOR: Gallverin, Yu. I.
*TITLE: Physical description of the artificial radiation belt'created by the Amerl- I
:can high-altitude thermonuclear explosion on 9 July 1962
.SOURCE: Vsesoyuznaya konferentsi a po fizike kosmichesko 0 rostranstva. Mosc&Q.'
.'1965. Issl7ea_(5Van1y_Y prostranstva (Space research); trudy konferentsii.
-Moscow, Izd-vo Nauka, 1965, 388-393
TOPIC TAGS; nuclear fission, radiation belt, nucle.ar explosion
,ABSTRACT: Direct observations by 11Kosmos-511 and other sources indicate that the
;rinal radius of the plasma cloud accompanying the American higb-altitude blast of 9
~July 1962 did not exceed 600 km and may have been even less.' This is less than the
final radius for a plasma cloud expanding in a vacuum, which indicates a consider-
g in a vacuum close to the r-region
:able dissipation of energy in a plasma'expandin .1
,maximum. Theoretical. calculations show that an hour after the explosion there were
A1.5*1025 electrons with energies >20 kev in the artificial radiation belt formed byl
the blast. It is estimated that decay of fragments from u,025 fissions was
Card 1/2

L 2796-&
tACCESSION MR: ATS023608
25-
Irasponsible for this number of electrons in the belt. This decay took plade above
'Johnston Island at altitudes of more than 1200 km, i. e. within limits of direct
~visibility from the "Kosmos-5.1~-/About 2.1026 fissions took place during the explo-,
osion. Experimental data show that the Ily-glow" and radiation belt are caused by the
Isame mechanism--decay of a small number of radioactive fission fragments in' the geo-1
!magnetic field beyond the limits of the blast cloud. Three mechanisms are proposed'
;fo,v this particle ejection beyond the boundaries of the cloud:' 1) diamagnetic ejeci
of plasma clots due to instability at the interface between plasma' and field;
j2) free separation in the magnetosphere of fission fragments neutralized in the be_
Iginning stages of cloud expansion, i. e. before the stage of "inertial separation;11~
;3) free separation in the m *agnetosphere of fragments neutralized by charge exchangel
ibetween ions in the plasma cloud and neutral particles in the atmosphere. "In con-!
I
;clusion I take this opportunity to thank I. Krasovskiv, S. H. Pikellner, A. S.
~Strelkov and Yu. V. Kukushkin,for.,useful discussion.of the results." Orig. art.
lhas: 4 figures, 3 formulas. [14)
IASSOCIATION: none
'SUBMITTED: 02Sep65 EXCL: 00 SUB CODE- ES, NP
:NO, REF SOV: 007 OTHER: 005 ATD PFGSS:*,6
Card
13Vkl

;.r. N-1 JIN'l I F.",
UP 1. r., i 1, 1!-
L 3107-66.
ACCESSION NR: AT5023611 UR/0000/65/000/000/0406/0417
r
jggM~n,-Yu. I., Potapov, B. P.;
AUTHOR: Zolymnovi-IL D. V4yabgrg,_,Q~1.; C
Temnyll, -'V. V. ; Shylskffa, F. K. b7
TITLE: Preliminary results of particle studies using the "Elektron-l" satellite
SOURCE: Vseso uznaya konferentsiya_Ro fizike kosmicheskow rostranstva. Moscow
1965. Issledovaniya kosmicheskogo prostranstva (Space research); trudy konferentsii.~~
Moscow� Izd-vo Nauka, 1965, 406-417
TOPIC TAGS: particle physics, artificial earth satellite, satellite data analysisl
electron, proton
ABSTRACT: The authors analyze data from th "Elektron-111 to determine the distribu-,
tion of radiation~'Ien the &~ ~ma et~c trapr?1on`g'fh--e-orbTt of the satellite in Janu-
ary-Harch 1964. At lower latitudes (L < 2) close to the equator, the dominating
particle flux i6 from electrons of natural origin with bnergies of.20:m-200 kev and an,
intensity of up to 2.109 particles-cm-2.sec-1, and from electrons aftificially in-
jected by the high-altitude explosion of 9 July 1962 with energies of several Mev
and a flux of Up to 2-108 particles-cm-2 sec-1. There are also trapped protons in
Card__
7

L 3107-66
:;ACCESSION NR: AT5023611
thiL; same region with enerfies of tens and hundreds of Mev and an intensity of up'tj
1 4 particles-cm -sec
-2 (E > 50 Mev). At middle latitudes (2 < L < 4) there is
a sharp increase in the flux.of soft protons with energies of a few hundred kev to
in v108 particles-cm-2.sec-I
intensities of no less thi at latitudes of 30-500 and ap
parently to no less than n,3-108 close to the plane of the equator 'at L 1- 3. Their
spectrum is softer at higher latitudes. Both protons and electrons are observed at!
higher latitudes', the low energy electron component (E > 20 kev) being extremely
of the
variable, especially during increased geomagnetic activity. The boundary
t ines of
capture zone in the geomagnetic field during magnetic calm matches the ou 1
the "momentary" p6lar aurora zone which reflects the diurnal asymmetry of the mag7.
netosphere. "In conclusion, we are sincerely grateful to V-I. Krasovskiy, T. M.
IMulvarchik. N. V. Dzhordzhio, M, L. Bragin, G. N.,Zlotin,-1,H,-Kiknadze, I. D.
-Tb;-ijtjrKR-~, T. N. Zagiyadimova, A. K. Nazarova and G. Ai BordoVskiy for gri-a-tas--
Isistance in the work and for useful discussions." Orig. art. has: 8 figures and
I table. (341
ASSOCIATION: none
SUBMITTED: 02Sep65 ENCL: 00 SUB CODE:. ES, NR
~
r sov opq OTHERi 008 kD PRESS:
q

L 62104-65
ACCESSIOWNRs AP5015670
iv. 162 5 kJ,
injdction:~holdsat-about one half ipproximnte smionli '~nlst at!suf
ficient height, where the artificial radiation:belt is formoo in order i for #o
indicated number of electrons to belnjeot6d'by means beta! di~cAy. Cariput4tion
of the intensity and time depohddnce:of~'glim.'radi~tion~.of th6 hasion P"~Pdud,ts
that rise to great height indicates a correspondeme iiii~, ~ the i iAon~ity.:ahd time
dependence of gamma flashes. r9corded on Cosmos V at th~ ~,tbne ~bf this
cts Of 1045. fissions app ed above V
means that the produ elthe horizon of Goomos'
within three seconds after the expldsion,, i.e.i' the prdd6tS'2',0.'J8 itb a ~eAghtlof
12CO kn or more in that time,,and.their gamma and. beta ~rhdiatfbij ~ausedvimma!
flashn and an artificial radiatilon1elt of:.ha~d elbetroA44 1W 'iipor I
6f
6
t
otal fissions during the --plosion wad 2' or x6re, ab. a
Tohnston loland qx -er-
sV about ;26 idn~tiis after 'tie ei'710-'I
mined by, Ole-Igor counter measurements on Co6moi .
-1 sion. "In conclusiong I am happy to express my thane ti~-i Gt~lol
;he ~group at
fiziki varkhney atmoofery 1FA AN SSM. (Departmont of Ph~4 ion ';'y'C th U ;Atm~s-
! ~ .0 . ppe~
pherej, ~A
AN~-SSSR), in partioular.to its diredtoi Vt. r't4r"6fjki ~or his gireat
aid and numerous - useful discussions on interpretation of ~16&awrements frot arti
ficial satellites*0 - Oridd art* bass 4 figures
ASSOCIATIONt" none
~6ii 60DE
SUBMITTEDs 25Feb65.
E'NCLs GO.,
NO REF SOV It,- 005, -
OTHEM .007
Card 2/2,
;2-

I ACC NR, AP7007042
SOURCE CODE: UlU0203/66/006/004/0633/0649
AUTHOR: Gallperin, Yu. I@; Poleuktov, 1, A.; Sobellman, 1. 1.
ORG: none
TITLE: Flux and energy spectrum of protons responsible for hydrogen
luminescence in auroras
SOURCE: Geomagnettzm I aeronomiya, v. 6, no, 4. 1966, 633-649
TOPIC TAGS: aurora, solar wind, magnetic anisotropy, geomagnetism
SUB CODE: 08,04
ABSTRACT: The author draws on 65 Soviet and foreign sources In review
of the proton spectrLa, responsible for H luminescence in auroras. It
Is concluded that soft protons, penetrating In a broad zone into the
polar latitudes, play a very Important role In the energy processes of
excitation and Ionization.in "proton" auroras and In the energy balance
of the upper atmosphere In the polar lati.tudes, Howeverl at present
there Is no well-developed hypothesis on the origin of powerful low.
energy fluxos of protons. Due to the regularity of appearance of the
proton flux and Its slight dependence on geomagnatic activity It can be
postulated that these protons penetrate into the atmosphere from the "solar
wind". The mean energy of these protons Is close to the mean translational
energy of the solar wind-In the case of conservation of magnetic moment
of a proton the increase of magnetic field strength with motion from
the boundary of the magnetosphere to the region of luminescence should
lead to an appreciable Increase of the Isotropy of the flux of penetra-
ting protons. Computations of the proton flux reveal that with ad-d-line
I trylity greater than 300 rayleighs the energy density of protonsj even
____UDC., 550.388.8
Z :7 - P, ell", 1~~_3'

ACC NR: AP7007042
with anisotropy of the flux ta;en
with or even exceeds the energ,
--,.30Y- . Therefore, the injo
luminescence of hydrogen emIss
measurements of the contours sLould
near the boundary of the magne:osphere,
moment of a proton can be expe:ted
path In the magnetosphere. On
of the region of the zone of t.,apped
that the injection of protons
Into account, probably Is commensurable
density of a magnetic field with a strength of
~tion of protons responsible for the
on with an Intensity adequate for precise
considerably distort geomagnetic field
so that constancy of the magnetic
only In a limited segment of Its
the othet hand, the diurnal asymmetry
particles (outer zone) suggests
-,an occur from the plasma tail of the
magnetosphere (where the field is not greater thin 10-301-) ... It Is
entirely probable that the region of injection of protons lies directly on
the boundary of the zone of trapped particles (to be more precise, the
zones of closed geomagnetic lines) and is associated with "frictione
between this zone# participating in diurnal rotation with the earth, wW
the region of unclosed geomagnetic lines (emanating from the polar caps
into the tail of the magnetosphere), twisted during this rotation.
This hypothesis harmonizes vith the morphological characteristics of the
&one of Injection of protons and vith the pattern of Its movements ac-
companying change of magnetic activity. OrIg. art* hass 7 figures, &W
23 formulas. LrJPRSt 38,93V
CWd
2

ACC INR,
JU7000551
SOURCE CODE:
Lo
AUTHORS: Gal~pqrin Yu. I.; Mulyarchik, T. M.
ORG: none
TITLE; On the altitude distribution of photoelectrons
UR/0293/66/004/'-,06/0932/0935"
SOURCE: Kosmicheskiye issledovaniya, Y. 4. no. 6, 1966, 932-935
TOPIC TAGS: photooloctron, electron (iistribution, ionosphoro, scientific satellite,
upper atmosphere, solar radiation, ele(:tromagnotic wave, geomagnetic field / Kosmos
5 scientific satellite,-IMP-1 scientiff.c satellite, LMP-421 scientific satellite
ABSTRACT: The results of measuring photoelectrons with energies of >, 40 eV (at the
ma.dnum of the F region and above) madu uith the Kosmos-5 satellite in 1962. are dis-
cussed. The distribution of photoelectrons with altitude for the domain of the open
ma-ganetic field must be close to curve :~ or b (see Fig. 1). Time variations of the
magnetic and electric fields in the corresponding tubes of force, electromagnetic
waves in them, and also macroscopic diztortions of the shape of the magnotosphere,
intrusion into its hot plasma, etc, ean affect the properties of photoelectrons
propagated through the corresponding tubes of force. Study of the characteristics
of photoelectrons is seen to play an important role in the investigation of the
topology of the geomagnetic; field.
UDC: 525.7:551.590.21

ACC NR, AP7000551
x +
x x
u3
V
N
9 X X
x
x xx
x x
0
r-I
+
b
to card 3/3

-T-

t;
A4

ACC NRt AP7000551
from card 2/3
Fig. 1. Altitude distribution of-photoolectrons with ;~~ 40 eV
obtained frog Kosmos--5 satellite: 1 - measurements for
L >,- 1.20p 914 ':!~ T 15h; 2 - L >
., 1.20, 8h 4- Tl.c
loc
< gh 3 - data of Ifintoroggor for electrons with Z 30
eV; 4 data of Shea, at al for >, 40 eV- 5 - calculated
equilibrium flux of photoelectrons with 40 eV; 6 - quali-
tative estimates A and B of high-altitude course of photo-
electron flux; 7 - results of calculation of flux tor Cole;
8 - b-d seat -1; 9 - C-1 (12)
~-.Orig-.- art. hast. I graph and 2 formulas.
,`~"SUg-X01E: 04P 20/ SUBM DATE: 11'~".2%ug66/ ORIG REF: 004/ OTH REF-. 018
C.,d 3/3

4 FF, R. b'4- -'s .0
(KIRA -18:10)
Iviv. kand. med.
t;
Yii.',,,. cta,!. ~.n M, -
ine-ii, VIR-.11m~fSkag) Wir.

GAL' PHUN, Yu. X.
"The Role of the Central 14)rvous Systen, in the Restoration of
the Blood Circulation During Raiuscitation.11 Cand 11W. Sci, Kazakh
State Medical Inst iment V. M. 1folotov, Alma-Ata. 1955. (KL, Ho 10.
Mar 55)
SO: Sun. No. 670, 29 Sep 55--5-irvey of Scientific and Technical
Dissertations Defended at LSSR 4igher Educational Institutions (15)

USSR/Human and Animal Physioloey - Blood. V-4
Abs Jour : Ref Zhixr - Biol., N ) 1, 1958, 3863
Author : Yu.M. Gallperin, Kandell
Inst
Title : An Analysis of the 4echanism. of the Effect of Intra-
Arterial Transfusioas.
Orig Pub : Fiziol. zh. SSSR: 1)56, 42, No 7, 559-564
Abstract : The authors studied the role of peripheral mechanisms
in the cardio-vasciAar system stimulation in cases of
intra-arterial blocl transfusions after a complete and
prolonged anemia of the central nervous synten
They applied a modJfication of I.P. Pavlov's cardiopul-
monary "preparat" L'.preparation 7_7. Blood was circu-
lating only in the small system and in the artificial
system. In the lalter, blood pressure was recorded.
At various times aUr the beginning of the C143 anemia
(from 20 up to 105 minutes), the animls were receiving
Card 1/3

USSR/Human and Aninal Physiology - Blood. v_4
Abs Jour Ref Zhur - Biol... No 1., 1958, 3863
through the femral artery 20-25 ml/kg of physiological
soluzion, or 1-1.5 ml/kg of hypertonic solution (20 %
NaCl) to stimulate the receptors of the vascular bed.
The experiments were carried on under morphina-hexanal
narcosis. Under the invluence of the mechanical. stret-
ching and the chemical excitation of the walls of arte-
ries separated from the heart by clamps on the aorta
and the inferior vena cava? the cardiac activity was
increasing - which was reflected by an increased blood
pressure in the artificial system and by changes in the
pulse rate and amplitudee Additional experiments with
decapitation and total removal of all the spinal cord,
which were perfoinuc