SCIENTIFIC ABSTRACT GINZBURG, V. - GINZBURG, V.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R000515130011-4
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: September 26, 2002
• Sequence Number: 11
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

At
33/65/040/003/0466/00.76
SAM
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~*Gta las.6tio space
i, sopdv: A i t" ~~h"X, V. 46,no. 3, 1963, 466-476
TO
M~stqkdaciid i plaotio cosmic rays, electron,
TO 0 Tpsii ~~smla
'604~ Q
to, il~ I I ,
ponemit oo, L0016 ~rldio emissions Metagalaotio g&MI erdsiion,
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pts an assessment of the po
TWTv Th ell a asible
th of, ibs. j41io~ssidn attem
(10) space within the framework of
lei
;Vv oil "obahilityt, the energy density of MG cosmic rays
taiti ~i Allai i thin -t 1 (0) cosmic rays; the latt
or
it
iimfttei 94 -z~h441 at' .~ooa :The best possible estimate for the energy
-sup-minus-16 to.10-sup-
Asnoliiy ouk ~~o t t4` time, approximates 10
of;10 themal
radiation is estimated at
s 3 0/06, A discussion is also.given of
114od lt in. vIub a 04 Ij Agy density is comparable with that of G
local sgargal or a local group of
rays *4
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GINZBURG, V..L.; SYROIIATSKIY, S.I.
Gamm& rays and magnetic bromnstrahlung X rays of galactic and
metagalactic origin. Zhur. eksp. i toor. fiz. 45 no.2:353-36)
All 163. (MIRA 16:9)
1. Fizichoskly institut imeni P.N.Labodeva AN 035SR.
(Cosmio rays)

BULAMSKIY, L.N,; GlffZBURG, V.L.
Temperature dependence of the shape of the domain wall in
ferromagnetics and ferroelectrics. Zhur. eksp. i teor. fiz. 45
no.3.772-,779 S 163. (MIRA 16:10)
1,, Fizicheakiy institut imeni P.N. Lebedeva AN SSSR.
(Domain structureY

GINZIZRG.,.-Y.,,.
-.- .. . ........-I-, .. ..
Whitt is provod by measurements of gravitational frequency
shifting?, Usp. fit. nauk 81 no.4:739-743 D 163.
(MIRA 17:1)

Al-~BARTSM,'.YAN, V.A., nkndevl; ~QjjjZjJQit_Q, V.L.; ZE1,11,0VICII, YII.H.'
A] Cadoir.Jk; )'ONT7--'KORVO, B.P.; vt.,.A.. "'ior
--nteg,. nauk, prof.; FOK, V.A., akider.,1k. UMNOV,
A.G.; FAYNDOYM, 1,13., red.
[birth and evolution of the galaxies and stars; the third
discussion] hozhdenie i evoliutsiia giilaktik i zvezd; be-
soda trettin. [BY] V.A.AMIxtrtsumian i dr. Vo;,kwi, Izd-vo
"hania," 1964. 27 p. (Novoe v Lhi,-,ni, nauke, tekhriike.
Scriia IX: Fizika, matemntika, astronomiia, no.12)
(YI U 17: 6)
1. Chleri-korrespondent AN ISS.M (for Ginziciurg, ~ontekorvo).

W 11ZHURG , ~'. 1'.
, my -results of radio antronominal re:jearch. Ve~.-O- AJ; ;SSH 34
no. 2:17-21 F 164. (!,',IilA 17:5)
1. ChImn-korrespondent AN SSSR.

AccEssioN NRi AphwhW s/bl26Ah/a7/bo4/b63l/0633;
AUTHORSt Bulaywakiyr, L, No; Qjmburgj VeL
TIMEs Possibility, of the existence of surface f arroMpatiam
SOURCE: Mika metallov i metallovedoniye, v. 17, no. 4, 1964, 631-633
TOPIC TAGSs forromagnetiam.. surface property, rare earth, magnotio momenti
ABSrRACT: The possible existence of antiforromaginatic or paramagnetic crystals
whose surface layer in ferromagnetio is di8cuseedi such would be the case if there
were uncompensatod mgnetio moments at the surface, The particular case of helical
structure (structure type of rare-earth metals) is considered, with ther-axis of
the helix assumed perpendicular to the surface and the spins directed along the
surface. The angle between the directions of the average values of spins in
adjacent la.5%rz is 0 (neglecting surface effects). Considering only the inter-
action between neare.
st and next nearest fiaighbors, the exchange eneror is
x-2
E NrP F)RI cos I* + 1, cos + I
J~l A +
where 9is the angle between t e 'spins- of the k laM and those of the k + I
Card 1/3

ACMSION NRt IP4034067
layer,, No is the mmber of unit cans in a 'layer perpendicular to the helix axiso
S is the spin per cell,, 11 > 0 and 12 < 0 are the paramters of the exchange inter-,
action, and the thickness of the sheet is na,, a being the lattice constant in the
direction of the helix axis. Hinimizing E over all Ok results in'a system of n-I
ught in the form-
coupled homogeneous equations., the solution of which is so
Ok - 4 + OkAtIM 0. Areas
-_ '(
Assuming cKk" 3., a finite-.difference_equa~ion for CXk "a written froR.which
Olk - SII e f orI k <
rMh + I -")for. n1 >k> R/2~
where 2cosIO- and 0-rtain features of Cererj~R
which prov i d ed the bulk of Oe information , are discussed. Dif f iculties in the com-
parison of the ile'sults of -different researches -and the effect of the solar-
activity cycle and of the -individual solar flams are extensively dealt with. 7he
icorre,laticn with solar radio emission is also discussed in ccmection with the
jBlectrx:n-positrcn caR=ent of cosmic radiation. The section headings are:
Intirduction. 1, InveGtip,&tion of the nuclear cimponent of cosmic rays with Soviet
satelliten and sNoe pcbes. - 1. FYocedure. 2. Chemical =Wsition of cosmic rays,
flux?~s of different nuclear groups and their energy spectra. 3. Variations of the
flurx of the nucle-ar cosmio-ray omponent and nuclei of solar origin. 11. Use of
satellite3 and r:rckets to s t u d y primary cosmic radiation. 4. Nuclear ccFn-,=ent
0, galactic cosmic rayu;, 5. Solar comnic,rays and higb-latitude cAitoff. 6. klect-
rcn-posity-lon ccnqx:nent of ccisTaic rays. Bibliography, Orig. art. has: 31 figunas,
15 tables, anti 6 forqulas.

iACESSICN'KRs AP4031621
ASSOCLgI(li: H"
SUM=: 00 ATD* PRESit-13059 ENMt 0 0
SUB COM. SV, AA NO REV SOV: 063 0M., 074

ACCESSION NR: Ap4ol3323 3/0020/64/154/003/0557/0560
AUTHORS: Ginzburg, V.L. (Corresponding member); Ozernoy, L.M.;
SY*i4oVa:tbk1y' S.I.
TITLE: On the radiation mechanism of galaxy 3C 273-B
SOURCE: AN SSSR. Doklady*, v. 154, no. 3, 1964, 557-560
TOPIC TAGS: extragalactic, radiation source 3C 273-B, metegalactic
object, optical radiation, bremostralung, luminosity, Compton loss,
free-free transition, bound-free transition, relativistic electron,
pboton, visible frequency
ABSTRACT: The extragalactic radiation source 3C 273-B, identified
as an emissive star-shn7)ed object of the 12th magnitude (K. Schmidt,
Nature, 197, 1040/1963 , is one of the recently discovered new
types of metagalactic objects. The exceptionally high luminosity
and irregular changes in the brillance of that galaxy are indiea-
tive of an unusual nature of the radiating object. The latter is
Card 1/3

ACCESSION NR: AP4013323
probably a "super star" rather than a cluster of stars, but the
word "galaxy" is used here for want of a better tem. It would be
interesting to find out whether the continuous optical radiation
from the Plan 3C 273-B is due to magnetic bremBstralung. The
optical radiation of galaxy 3C 273-B is not polarized, and could
therefore easily be characterized also as non-magnetic bremsstralung.
A contrary assumption would of course be wrong Inasmuch as magnetic
bremsatralung can, for a number of reasons, be completely depolariz-
ed. If the radiation from the object is of a braking nature (free-
free and bound-free transitions), it cannot be considered as black
body radiation in view of its spectral characteristics. Although
the possibility of the bremestralung nature of the mentioned radia-
tion is not excluded, the spectrum of the other star-shaped extra-
alactie sources makes such a hipothesis considerably less probable
in the opinion of 1. Shlovskiy . Orig. art. has: 11 formulas and
t
I table.
ASSOCIATION; Fizicheskiy institut im. P.N. Lebedeva Akademii rauk
Card 2/3

ACCESSION NR: AP4013323
SSSR (rhe P.N. Lebedev Physios Inatitutep kCademy of Scien.ess &MR)
SUBMITTED: lOOct63 DATE AOQ: 26Feb64 ENCL: 00
SUB CODE: PH NO REP SOV: 002 OTHER: 009
Card 3/3

ACCESSSIM NII: AP4039)0( ) S/0020/64/156/001/0043/Oo46
ALMIOR. Gin-"burg, V. L. (Corresponding member)
TITIZ: On Magnetic Fields cof CollapBing Masses, and the INature of Superstarn
SOURa: AN SSSR. DoUwIIr*, v. 156, no. i, l964, 43-46
TOPIC TAGS: sup~:rotai., collapainG protostzLr, superstar ma(-,netic field, general
relativIty theory, coumic x ray, cosmology, coonic radio wave
AECTRACT: The juthor p7)1.nI-i,'v out that the obser-.,,ttion of a prutost&-r (a E;as C101a
Idth a mass of ;:uzny milliov Uzer, tbtLt of the !j,, 3n adv:,%ced staze of I
collap:;e will be 1"Ifficult, if aot L-mossible, `)CC'au:;O. of, t"~c dezn,-ase of surface
and the cul-,"Iture Of t, ',;a%reS. '21-,erefC--~e, 0-.Ic fo-r Other Inhenomena,
that riignt be (!o:'Lnec-V:!d wit'a a collaj)sino siAperotr--i, suc'Zi a~3 ~. :zag.,-2tic field. A
fiel.1 uxiuUnji, befDre the colla-j),~e, i-~iy be expeoted to bo preserved
dUTing ti!O COIJ.1661)ue if it r-~usoaabla electri)eolaductivity of tho neditz is assi=ed.
.The presence of a magnetonnhere may cause a noticeable Zeeman splitting of spectral
,lines and a rotatioa of tluj p1me of polm-ization of radio waves. Particles In
thia field will be t1w Bouxve of electrauguetic waves in the radio, Optical,
Card

!ACCESSION NR: Al)W35W6
and x-ray range (cyclotron radiation). This may explain the recently discovered
.discrete source of x-rayu. Orig. art. luw: no figurea, I table, 3 equationa.
1ASSOCUTICU, Fizicheakiy Institute im P. N. labedeva Akademii nauk SSSR
(Physion Institute, Academy of Sciences SSSR)
SuMa-LM', 3Wana DATE ACq: 2&XaYQ MiCL: 00
SUB CODE: J; AA;' NO 1w sav: oo6 OTM: 004
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L ~1888-66 tWTW/91VT(m)/FCC/T/EWA(h) IJP(c) GS/M
ACCESSION NR: AT5022822 UR/0000/65/000/000/0008/0022
AUTHOR i L.; Kurnonova, L. V.; LP Razorenov, L. A.;
TITTZ:
_gof cosmic rays
1 SOURCE. Visesoyuznoye soveshchaniye po kosmofixicheskomu napravlaniyu iseledo-
vaniy kosmi6hiskilch luch~y'. 19621j6smich6sklye ludhi i problelay
(Coiiffl'ic i~yi-and' problems in cosmophysics) ; trudy saveshchaniya.
Novosibirsk, Radizdat Sib. otd. AN SSSR, 1965, B-22
TOPXC TAGS: primary.epsmir- ray, cosmic ray particle, cosmic ray measurement,
cosm
ic radiation composition ,V
ABSTRACT: The article is a survey of reported experimental data on the composi-
tion of cosmic rays. The following groups of nuclei (other than protons and
alpha particles) with charge Z >3 are considered: (1) light nuclei with
charge 3 < Z 4 5 (group 1); (2) nuclei of the middle group with 6 4 Z < 9; (3)
heavy nuclei with Z >10 (group 11). The symbol S is also used and designates
nuclei with Z ~*6 W! H-+H), It is shown that fluxes of different nuclei
(including protons) should be compared for a given value of their hardness. As
a rough 111 neral rule, nuclei of elements with atomic number Z are Z times more

1-1 1888-66
ACCESSION NR: AT5022822
frequent in cosmic rays than in nature. Difficulties involved in meaSurimente
of fluxes of the different groups of nuclei are described. High-altitude ex-
periments definitely indicate the presence of lithium, beryllium, and boron
nuclei (20-30% of the quantity of heavier nuclei) in the primary component of
cosmic rays in the vicinity of the earth. Findings concerning the electron-
positron component of cosmic rays are discussed, and the chemical composition of
solar cosmic rays is considered, Differential energy spectra of protons and
nuclei and their hardness spectra are analyzed. On the basis of the body of
datst accumulated thus far it is now possible to state that not only protons,
but also multiply-charged nuclei are accelerated on the sun; however, this
mechanism of particle acceleration is still unknown, and several such mechanisms
may exist. Orig. art. has: 14 figures and 3 tables.
ASSOCIATION: lizicheskiy institut iw N. P. loebedeva AN SSSR (Physics
Institute, AN SSM
SMITTED; 290ct64 ENCL: 00 SUB CODE: AA1 NP
NO REP SOV: 014 OTHER: MO

-,NT ( IFC, G IM 4 A ( hGS/GW
AT5OP3626 UR/0000/6
5/000/000/0486/05011
AUTHORS: inzbur&jL.4 1(14rAQqqX#1J!.V-1 SYrqYkt44j__P. L;
Fraft M. I.
TITM Soma problem and perspoctiYes in the investigation of primar
ot _~
y_
;SOURCEs V~eaqyu~~p konforenti4ya Po fiaike kosmioheskq _. yrostranetva. Moaoowf
,1965. Insiedovaniy'-a IE6_iiiaiiik~j~
_E~_c~ow, Izd-vo Nauka, 1965, 06-501
TOPIC TAGSs cosmic rayt gamma ray, x rayt solar activity, antiparticle
ABSTRAM Problems associated with the investigation of primary cosmic rays and
gum rays are presented in a three-part report. Part I deals with the proton-
,nuCICILS component of the cosmic rays, Part II covers the electron-positron component
'and Part III diocusmes connie gamm- and x-rays. Although the proton-nuoleus
~component of prijoary cosmic ray-9 has been studied qtLite completely, a group of
problems still remins unanswered, Eigbt such problems discussed in Part I arel
;1) energetic spectra of protono and nuclei in the energy interval below 100 Mev/
inuoleon. These spectra are represented by the form X(E)-vEI-8. 2) The relation-
~ahip between fluxes of 4ifferent nuclei groups (Lj N, H) in the energy range 55 to
5O.Me olson, which in still not well known. 3) Isotopic components of primary
i CoM 1~~u

:Ai~ NRi AT5023626 C.
.cosmio rayfi. Thio would require the measurement of three Independent paramoters
such as dt/dx, E, and p0 . 4) The presence of high speed antiprotona generated by
the interaction of oosmia rays vith interstellar media. Some measurements place the!
.percent compoultion of amt1particles at 0.23%- 5) The verification of the presence I
~cf superhnavy nuclaij Z 1 30. 6) Estimates of the time rate of change of the fluxes,
in primary nuolel. components whLch have their origin either in oolar barste or in
,modulated galactic coamic rays, These intensity variations should be recorded
continuously, outolde tho terrestrial atmosphere- 7) Intensity gradjents of cosmic
raya in tho solax system as evidenoed by data from Pioneer-5 and Mariner-1. 8)
Aniootropy among prArtlelo fluxes of low, near-threshold energies. Two similar
;problems are diBousued in Part II. Here the flux and energy spectra of primary
cosmic, ray electron-positron components are analyzed f Irst, where data are shown to
b,:- rather scant. Next, -the relationship between positron and electron fluxes is
conBidered by measuring -the choxge composition of the primary cosmic rays. In Par
III, aalculation resulO of expeoted Y - and x-ray intensities from important
galactic sodroes aTe considered. The y-ray generation is attributed to processes,
such as 10-menon decayp brematrahlung radiation of relativistic electrons and
positrons, and Oompton *r-raye by the scattering of photons on x-ray electrons.
Fxper iments indl oats I y (:~ 50 Rev) j 3 - 5 1 1 e4 photons/ 2
am /eeo/stere which in
'larger than expected galaotio estimates. This then implies Y-rays of
Card 2/3, .... . . ....

11326-tM
meta-galactio origin.
lbotons/om2/oso/sters.
ASSOCIATIONt none
!U'WWTTEJDi 028op65
;90 RHF 8M 020
For lower energies (0-51 Nov) 1 1.2 to 300 x 10 -6
Orig, arto hast 6 tables, 2 flAfes; and 4 formulas. 104)
IMOL 1 00 M CODEs Up NP
OTM 046 ATD PRESS I
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Amcit, I Gin L V,14aMIjA-U-~
M: --Plff&U-o UgAtd6_jrj Ps N~ J&Wgym AN SM (FidahesIcLy institut AN Maj
TIM Relativi" O'Sa).iAtOle Wdels of Sim Adale P This - paper wal giren
4 '.q
at thi 14th AmWa ~C ftum-mm"Offic W-O Thiliftip ebr
SOMt, Taderftyti Mika, vo 2, not 6i 1963, nO3-n:L4
TOM TAGM a0loar PwrtAOIS, nulosr son
Awm=t Relativistic, lm~.iA squtioba are"emidered for partirles
~d oribed by ths "center of six N coordinatoo zi W three 4-vactors
V
.u (I a 1#20304#1 C< 40903)1 z am the Intrinsic variables which obeyi
tie oscillator *qmtLmp4 Tho i44ims of these equations mTress the
9mP SUM In th* rwk Optau :4 1$ P06sible to wits the *qUALOI'W4h
=WIUUM cornspohUngtoltho octet and deom4lat for the am of
Or- and 0 the octet MA ki*et for- t.be Gas of lnt*W
, - --l- I" " . _apb! i
Tba smthars MkAwLiOt-, & OAS, art, hus. 25 formilas &M
tables& J56Z.On"." thors, IM*
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A.CC Nki AP 5026225 SOURCE CODIC: UR/0048/65/029/010/1819/1824
AUTHOR: Gint, 8.1.
ORG: EV.10--insti~-ute in. P.N.Lebodev, Academy Of Sci8nC88,SSSR(FIsich*skiy insti-
tut Akedeall nauk M)
TITLR: Funtlemantal problems In cosmic ray astrophysics /Report, All-Union Conference
On Cosmic Ray Physics bold at Apatity, 24-31 August 1964/
SDURCB: AN $881. Izvestiya. Serlys fisicheskaya, v.29, no.10,965,1819-1824
TDPIC TAGS: Primary cosmic ray, gglWypoemology, astrophysics
VY
ABSTPACT: Recent literature on the astrophysical aspects of cosmic ray physics is
reviewed and some roilated questions, particularly that of the origin of cosmic rays,
are discussed. Advatness in astronomy and redionstronomy in the past decade have
attracted attarAtion to the possible cosmological significance of cosmic rays. Cosmic
rays, for example, might serve as a mechanism for carrying off the energy released
in the gravitational collapse of stars or galaxies. There is convincing evidence the
the energy density of oossic rays is much less in metagalactic space than in our
Galaxy. Arpments to the contrary by G.R.Burbidge and F. Hoyle (Proo.Phys.Soc.,84
141 (1964) Wre spjO,flcally criticized. Most of the galactic cosmic rays, therefore,
must be of galact c origin. The electron component of the primary cosmic radiation
has been shown to arise mainly from the direct acceleration of electrons rather than
Cara

L 6946-66
NR. AP 5026225
0
from meson decay. The stationary model of cosmic ray origin given by the authors
(Proiskhozhdeniye kosmicheakikh luchey, Izd. AN SOSR, 1963), according to which
most cosmic ritys originate In supernovae, has not encountered any difficulties but
cannot be rognrded ms proved. There Is no convincing 9evidence that an explosion of
the nucleus of our Galaxy has occurrod in the past 10 years. The explosions ob-
served in M82 and WtC $128 do not indicate that such explosions are probable in our
Galaxy, for M 82 and NOC 5128 are not spirals and differ considerably from our Galaxy,
It has been argued that if. all cosmic rays originated simultaneously, the relati-
vistic particles would have travelled farther and encountered more interstellar
matter than the low-onergy particles, and would therefore contain a larger fractiou
of light nuclei, whereas siuch observational evidence as exists indicates that the
higher energy socmic rays have a smaller fraction of light nuclei. This argument is
not decisive, howerver, because the high-energy cosmic rays any have travelled through
regions in whiah the densIty of interstellar matter is less than in those through
which the low-energy cosm1c rays passed. It may be possible soon to determine
whether the cosmic ray Intensity was significantly greater some 108 years ago than
now by investigating meteorites as proposed by the authors (Proc. Internat. Conf.
Cosmic Rayo,Jaipur, 3 301 (1964); Izv- AN SSSR. Ser.fiz.,28,1910 (1964); Astron.zh.
41,430 (1964). Although the authors do not see any real arguments in favor of a non-
Eltationary model for the origin of cosmic rays in the Galaxy,they agree that further
Investigation of this matter is Justified. Orig.art. has 2 formulas and I table
SUB CCIDB: AA SIMM DATRI 00/-OWS ORIG. RV: 012 OTH W: 007

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3616-66 EWf(m)/EWP(vt) Vf !Tf 0 ... JD
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AC.0=10N NR9 JY5021085 UR/0020/65/163/006A332A355
:i AUTHORS i 6,.Oprresponding member AN SSSR) so Notuleviobi
FitNmvsk !r I'
TITM ti%~ ro rties Of P04-Mlont metals and interelectronic interaction
7_4 SOURCEt AN MR. Dok)Adyj Y, 163, no, 6t 19650 1332-1355
TOPIC TAGS: Fermi surfics, optical electron, valence electron, polyvalent metal,
polmlent metal eleetran
MiTRACTs A critical, examination of literature data pertaining to tl* ratio of
Dr "Au I V#41 Sn, and Pb is presented#+
optical eleoltwrona to valowe electrons Z
The data are axwnited in terms of the Fermi our4aee integral
v M
F are the mass atj4 momentum on the Fermi surface of the free elsetroA
ii uhare x andp
I the nwdwr of v&lence electr d
aud Nval oti per cm:3. It is concl ad that the ob-
1"'Ind FbT most proba
I: amed decreitas of V optical from N valence in A' lv%r
Hdue to interelectronic luteractions, Koveverp Tvo ~Uficul_tles regarding the
C'rd
1/2

L 3676-64
ACCESSION NRI AP502IM5
abbvo explamAtion ar* noted. For iLll polyvalent metals, the number of optical
electrons pat atom n opt --'1p % fact the authors are unable to explain. The
tion that imtereliDotron interaction exerts a strong influence on the ratio,
`
7 not supported by wq existivg theoretical model, The authors thank
nop n,., in
ra, Azbe~!6*nd D a Sor their helpfW. criticism. Orig, art. has 1 2 tables
and 7 oqust~ohe* J
ASSOCIATIOM Fiddhookiy institut it, P, N, Lebodevay Akademii nauk SSSR (Phys
Ical Institute, Acade# of Sciences, SSSR)j Institut fizicheakikh problem,
Aladezii va~k SSSR (Institute. for Physical Problemax AcadeW
of Sciences,
EXCLI 00 SUB GODEs MMoP
BUM=Ds i
NO MW SOV 1, M3 OTHIRt 04
Card 2
01"2"t- W, m"~~M P 10

ACC NRi - A116019473 SOLTRGS- COLE-~-UJV0269/66/000/002/0037/0037
AUTHORs Ginzbwgi V. L.
TITLEi Space-phyeics trend in Oosmic-ray research
SOWWEt Refs the Astroromiya, Abs, 2-51*313
I-LEF SOURGEt Sb, Nosmich. lucht i probl. kosmofiz. Novosibirsk, Sib. otd, AN SM,
1965, 5-6
70FIC ThGS: comio rayp electromagne-tism, radiation bolt 1115/019 e e-
ABS-1AACT3 A brief historical review of cosmic-ray research is given. It in noted that
in the 1955-57 period a new era in cosmic-ray research began, i.e., a study of the
origin of cosmic rays and the relationship between the variations of cosmic rays and
electromagpetic phenomena in interplanetary space, in the radiation belts of the 6A
and of the planets. The significance of the new space-physics aspeot of cogmic-ray
research is stressed in conjunction with the launching of artificial eatellitea and
space rookets. No K. Lfranalation of abstraqt
7
SUB 0018 1 04/
Card 1/1 UDGI

MG: Ln. P. N. Lubadova, Acadway of ',~;iuncu-- SS5,~j !c'-"kiY
.'"kadumii niaulc ~'SSR)
~.ITIZ: ray om~ -,Lion of radio galaxies
SOUTICF: k;tronxi-Ichoskiy --hurnal. r. 43, nc,. 5, 897-9D2
TOPIC TAGS: galactic radiation, x ray bro-.~;strahlun-
ABISMIACT: 'A7ie C-~U,~o of 'L.'-,o LntamO x MY radio galaxioo V--'-Zo and
cygnw, is di5cus5,x.. G3jections aro mado '~-o i.nQ' Com-pluon mochanisms and to
quasar typt, n=joi :Ln radkio gal--~y or '.,D ~,;,oups as oxplanationz of the
-ource of t-o x Instoad, t'ho n, mochnism i,
proposed. In
tao case o--' z;uch c~-.ission L'-,O'i larCe clouds of ~.ot Ews, intumal onorgy of the gas
would be of -ao orior of ma-niLLde as tho tota'. cosmic ray onargy Ln the source
zmd tho Ca5 co-"-'d be heatcd by he c.-'.a.-q,o in t, o onarCy of tha coamic rzys during
',~aeir L-otro:)izat--~ :,.). '!~.o difficuIV ,kith -Lho ',vonosucl Mccnani=n is t1hat for an
Oytondod -,ourco tho ho-6- Zar mass should be lz,.-Flr. X ray emission of tine Crab nebula
is also discussod ~n the of t1ho proposed -mall hat gas cloud. coed for
additional measuro.,,.wats of -,ol-=-iza-.-ionj diraons~~ons, snap3 and spoc',,-,a of -,he x ray
:,-Card-

ACC NR, AT6027583 SOMICZ
AUT_--~074 Gin*urg# V. L. (Corr6al*nding ma;zber AN SS_S;Q
ORGi none
IITI.Es I;cw trends in astroxiouq
S5'V'-i'0Ls '4',vcuIy i vs6leLnayu (Staxis und the UnIvorso). %bqcow, jzd-va Zni)x.'p,, 1966)
15-20
WPIC TACiSi doticxiptivo astronomy, ruillo arstronoruy, primary rtk;(, ri-jut.rino,
acintill&tion, j~,Iaotla nebulaj euporrova
A:1111'17~u'.(;'~'I 740 fivnl. rovolutIon in by R C.IlicA cf
2cierica, occx-rea In 162.0 when Galileo O'b"Jorl"';L 1,;J0 r"'rY fur th") _`irj;" o ~~AI'.
LrME:d eye. Tail cpanod up trio optical ora in astronoi~q Tiiu quc-onu
in 3.945 wher, optIcal astronorv becama urdvo,-,,ial. Now, twenty yearc afte:- t-is
rovolutionj nix now brancbes of astronoV have bean davolopc;d; U~-.Z'OnCMy Of
CIU0,10y VUVOS; x-ray and gaima-ray aatronomy; qtucy of primary cormic r&ys; cptical
a9tronomy from sate]'Llites in visible, infr&red, and ultraviolet ray:,; diroct
uDing sataLlitas leog., photographing 'ho )-bon and MrE; from short distalx6s) &nd re-
capLion 'of noutrinos (thoy pass throuoi tho ~ &nd E&rth in Fmall 'b"A detectaIJIG
amc;untsj. -Zhose rew methods have already yjold(,~d oignifioant reaults. Tao cicialo;ZaLt
Cord l/2

ACC' NRI AT604,758.5
of 110W tociiniqUol hatj oliminated U46 diqadvrrtifa 6f the cmall i;nular of
rad-lofrequenoy a:%trono.-iy and made its angular re,-olution evi'n '-Grater th-;~T. of
optioal antrorDMJ. TLis is done by tbree raothodst the use of ra~ilofre(~ueLc,.,. intcjr~'ero-
MOLry (placing several long-vave toloscopes at lago diFt&ncos from Oac~2 ot2,6i;, use
of ovarlappiLg Lho Pources o~ radio fro quen oy-wava radiation by the %brL, scin-,.illa-
tion twinkliz~ ber of si.-plf eLrt
of very ez&ll radiation sources. A Lum ~ Lft
were made in 1965 1doed on now astronomical methods. 7ne small rou-.co, osz~acizdly
powerful on lorjr, wavos, was u1scovorod by the British (and confirzze~ in t~-D
a nebula remaining from a supernova star, tho envelope of which oxl~ancod ~it tho rato
of IOW km/sac. It is pDnsible that this source is a remnant of the rupoi:-,-.ova j3tzz.
This fact could possibly solve the problem of the nebulae. other importfLnl, disc")varller,
made in 1965 Included the detection of quaoiastr&1 galaxies, among them t~,O 3S-9
quasarp Vaicb in moving away from us at a velocity equal to 80% of *~Go speed of llept,
i and a most speot&cialar disoovery of radiation that was emitted 10 billion years alP.
Dole) 031 SUBM DAM 224c66
Cord -2/4__

s/n5/6z/ooo/oil/O02/008
E.192/F38,~,
AUTHOR: Ginzburg, Y.M.
i, rr 1. L: Relationship between information and energy during
measurements
PERIODICAL,: tzmeritelInaya tekhnika, no. 11, 196a, 6 - 8
T EXT: The quality of measuring equipment can be estimated by
the formula , ~ 11W , where I is the. desired information and W
is the energy consumed during measurement leading to the recovery
of information. 'lite problem consists of calculating Tj and deter-
mining the conditions for which n is a maximum. The measured
system is in the form of material particles which are either
stationary or mobile. It is found in the case of stationary par-
ticles that: 1) the quantity of energy required for measuring the
position of a finite number of particles in an enclosed volume is
independent of the number of particles and is directly proportional
to the quantity of' the resolution elements in volume; 2) for a
known number of particles in the observation volume the information
per unit of energy is a maximum when the number of particles n is
approximately equal to the overall number of the resolution elements
Card 1/3

S/115/62/000/011/002/008
Relationship between .... F192/r382
N in the volume; 3) if any number of particles from 0 to N
is equally probable, the information per unit energy decrea-leR. inono-
tonically with increasing N from I - 1/2 hit; 11 ) if* it probability
distribution p(n) is given, where 0 -' n " Nanrl its maximum occurs
at n = n. . the inl'ormation is a maximum ror N slightly smaller
than 2n In the came of' moving particles, the measurement. is
efrected by equipment producing probe pulses of' duration and
a period 't;:. Two cases are possible. In the first case, file
character of motion oCthe particles is not known and nach of the
particle.-; can be found in any of' the N elements contained in the
volume under observation. The measurements are conducted for thi.9
case in the same manner as that used for the stationary particles.
In the second case the particles can appear only in a portion
N,