SCIENTIFIC ABSTRACT GINZBURG, V. - GINZBURG, V.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R000515130010-5
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: September 26, 2002
• Sequence Number: 10
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

6 -,- 6 9U
Nonlinear Phenomena in a Plasma Which Is Located 5/053/60/070/02/004/oi6
in a Variable Electromagnetic Field B006/BOO7
a i-A upon a -degenerate (classi-
E .0 non-relativistic and non
cal) plasma which may be kocated in a homogeneous and constant
(external)magnetic field 'ff0 is investigated, Macroscopic
(hydrodynamic) motione in the plasma are not dealt with. The
influence of the field upon the plasma in this case leads to
a chalige in the velocity-distribution function o th.% plasma
electrons, which is set up as a function of (ji, 1 0 , H0 and
of the plasma parametem The distribution function of the
heavy particles may in this case be considered to be a Maxwell
temperature function, which is justifiable in the steady case
under investigation. If the electron velocity distribution is
known, their kinetic energy (their temperature T e) and the
total current density it may be determined,, In weak fields
electron temperature is e_jual to that of the heavy particles,
and Stis proportional to E. Paragraph 1 deals with the elemen-
tary theory of the plasma in a homogeneous electric field
(electron current; dielectric constant and plasma conductivit
11a rd 2 14 electron temperature). In paragraph 2 the kinetic theory of a y)

6~~696
flonlinear Phenomena in a Plasma Which Is Located S/053/60/070/02/004/0 16
dn a Variable Electromagnetic Field BoM,'DO07
Card 3/4
plasma in a homogeneous electric field, l.e,. the description
v r
of the electron gas by means of distribution functions f(*Ult)
is dealt with~ Individual sections deal with the following:
The kinetic equationj the transformation of the collision
integral, elastic collisions with neutral pArticlea (moleculen);
inelastic collisions with neutral particles; collisions with
ions; collinions of electrons with one another; the solution
of the equation of motion for a highly ionized plasma; the
(Maxwellian) distribution function; the effective number of
collisions; the relative portion of transferred energy S eff
(table I gives the S -values for electron temperatures of
eff
between 500 and 15000 0for helium, hydrogen, oxygen, nitrogen,
and air; 6 eff equals 6 elast up to electron temperatures of
-1 ev, after which it increasee exponentially with T e.); elec-
tron current, dielectric constant and conductivity of the pl,Iama;
electron temperature; the weakly ionized plasma; elastic col-
lisions; the molecular plasma; inert gases; the electron cur-
rent and the mean energy of the electrons; the elementary theo iK

6~-,696
Nonlinear Phenomena in a Plasma Which Is Located S/M/60/070/02/004/016
in a Variable Electromagnetic Field Boo6/BO07
for an arbitrary degree of Ionization; transition from the
highly- to the weakly ionized plasma; and the conditions for
the applicability of the elementary theory (by comparison
With the kinetic theory these conditions are mathematically
formulated for highly and weakly ionized plasma). There are
8 figures, 2 tables, and 68 references, 35 of which are Sovie
Card 4/4

AUTHORS: Ginzburg, V. L., Gurevich, A. V. S/053/60/070/03/'001,,'007
Boo6/13014
TIFLE: Nonlinear Phenomena in a Plasma Located in a YariaLle Llectrc-
magnstic Field
PERIODICAL: Uspekbi fi%icheokikh nauk, 1960, Vol 70, Nr 3, pp 1Y15-428 (USSR)
ABSTRACT: This artiole is continued from a survey published in
"Uspekhi fiziehaskikb nauk", 1960, Vol 70, p 202. Paragraph 3
deals with the nonlinear effgcts occurr ipg in the propagation
of radio waves in a plasma 61onosphere,' eLar corona), per-
turbation of the principle o? superposition, influence of the
wave field on the plasma, Maxwell equations, Section 3-1 deals
with the propagation of radio waves in a plasma in considera-
tion of nonlinearity (self-action of the radio waves). In
thiB case, the.field at the plasma boundary (z-O plane) is
assumed to be E0 0) cosci S and the wave propagation is describ-
ed by At - grad div ? + 6)2 E 0; AII-5i
0
The amplitude and the self-action factor are studiedv and thfir-1-1)
Card 1/3 modulation of waves is discussed in detail. Section 3.2

Nonlinear Phenomena in a Plasma Located in a S/05 60/070/03/001/007
Variable Electromagnetic Field B006YB014
Card 2/3
describes the influence of self-action on the propagation
of radio waves in the ionosphere. This self-action depends
on the vavelength, and is separately studied for short waves,
medium waves (Table 4), and long waves. The resonance of self-
modulation near the gyromagnetic frequency, which amounts to
(6 - 6).106 in the ionosphere, is also investigated. The speci-
fic features and the causes of this greatly nonlinear effect
are discussed separately. Section 3.3 is devoted to an inves-
tigation of the interaction between modulated radio waves
(cross modulation). A theoretical study of cross modulation
in an isotropic plasma is followed by an investigation of
the influence of a constant magnetic field and of the resonance
effects occurring near the gyromagnetic frequency. Section 3.4
describes the results of experiments on cross modulation in
the Ionosphere (absolute cross-modulation depth, dependence
of the depth lip and the phase of cross modulation on the
depth p. and the frequency 9 , dependence of pQ on the intensi-
ty and frequencies of the disturbing waves, and cross-modu,

Nonlinear Phenomena in a Plasma Located in a S/053/60/070/03/001/007
Variable Electromagnetic Field B006/BO14
reeonanoe),, In section 3-5 the authors study the nonlinear
interaction of nonmodulated radio waves. At first, the varia-
tions of propagation conditions for a nonmodulated wave are
investigated, then so-called lateral waves, vizo waves with
combined frequenoiest and finally the nonlinear effects con-
nected with the variation in electron concentration. This
article is concluded with a few notes about future studies
in this field. There are 11 figures, 2 tables, and 65 r
erences, 21 of which are Soviet. 8r
Card 3/3

81677
8/053/60/071/03/02/008
/goo B006/BO63
AUTHORSs Ginzburg, V. L., Syrovatakiy, S. I.
TITLE,4 The Present Stage of the Problem of the Origin of Cosmic
Ray _"A
PERIODICALz Uspekhi fizicheskikh nauk, 1960, VA. 71, No. 3, PP. 411-469
TEM TheInternational Conference on Cosmic Radiation took place in
Moscow in July, 1959. This review artiale contains a compilation and dis-
cassion of all known results, with special regard to the data obtained
after this conference. The authors proceed from concepts based on radio-
astronomical data~ according to which copic radiation mainly originates
from ~alaxieB, and is due to eruptions of Supernovae and possibly other
variable stars. � 1 is devoted to primary c-39-m-TF-r-Raiation on the Earth,
its chemical composition being described first. Table I lists data on
ZY 7, flux, number of nucleons, flux- and particle number ratios. The
energy spectrum is deveribed next. In general,
IA(" = KA~- 7+1 holdup where I A(>E) is the nuclear flux of group A with
Card 1/5

81677
The Present Stage~of the Problem of the S/053/60/071/03/02/008
Origin of Cosmic Rays 30061BO63
a total energy (per nucleon) greater than ~_. The values for XA and I are
given in Table 2. Within the limits of error I - 2-5 4 0.2. The differ-
ential spectrum exhibits a maximum with a steep decline, so that one may
speak of a "cutoff". The origin of this "cutoff" and the fact that itE
energy is independent of the nuclear charge are discassed. The spectrum
of the total energy per particle may be expressed by I A(> E) - KA(E/A
- (KAAT_.)/ET_1(cf. Table 3). For =1015 ev the spectrum has a singularity
whose nature and cause are discussed in the following. � 2 gives a survey
of radioastronomical data referring to synchrotron radiation, results and
interpretation of some observations on the structure of the Galaxy and its
sources of discrete radiation (galactic "lialo" or "corona", "radio-disk"
of the Galaxy (Figs. 1 and 2), and its "central radio range" (Figs. 3
and 4)). Data on powor, energy, and magnetic field strength are given in
Table 4 for numerous sources of galactic radiation. � 3 gives detailu on
the lifetime of cosmic rays and their motion in the Galaxy and metagalaxy
(the part played by cosmic rays formed in the early developmental stages
of the Galaxy; the motion of cosmic particles in galactic magnetic fields,
Card 213

8167
The Present Stage of the Problem of the S/053/60/071703/02/008
Origin of Cosmic Rays B006/BO63
the radiation yield from the Galaxy; cosmic radiation of metagalactic
origin; the origin of the electronic component of cosmic radiation in the
interstellar space or in the envelopes of Supernovae)- � 4 deals with the
sources of cosmic radiation, mechanism of particle acceleration and chemi-
cal composition (radiation sources, mechanism of acceleration, energy
spectrum, and the possibility of preferential ac~r?leration of heavy nuclei;
changes in the chemical composition of cosmic -radiation in the interstellar
space; chemical composition and distribution of elements in the radiation.
The article is concluded with three additional remarks in the proof cor-
rection of this paper. Mention is made of G. A. Shayn, I. S. Shklovskiy,
G. G, Getmantsev, V, A. Razin, and L M. Gordon. There are 6 figures,
8 tables, and 144 referencess 67 Soviet, 22 American, 1 Japanese, 2 German,
7 British, 14 Italian, I Belgian, 5 Australian, 1 French, 2 Dutch.
VX
Card 3/3

AUTHORSt Airlikurgi V:.~L.Corresponding Member, S/020/60/131/04/019/073
AS USSR-'-'F& At V. K. B013/BO07
TITLEs Possible Anomalies of the Magnetic Properties of Macromolecules
PERIODICALs Poklady Ak&demii nauk SSSR, 1960, Vol 131, Nr 49 PP 785-788 (USSR)
TIM Strong lines of electron paramagnetic resonance and anomalous magnetic
properties have recently been detected in a number of macromolecules (polymers).
In this connection it is essential that the initial links of the chain and the
short chains (monoters) are diamagnetic or ferromagnetic. Consequently, this
means a transition (with elongation of the chain) from a diamagnetic state into
a paravagnetic or ferromagnetio one. The authors give an explanation of this
hitherto unexplained effect. They assume that the finite, but not too short and
not too long chain of nonomers is antiferromagnetic. The electrons under
consideration then form two antiparallel sublattices. The antiferromagnetic
level is the lowest level of the whole system. It is further assumed that the
antiferromagnetio level is the lowest level in a chain of monovalent atoms with
-.11 --~* -%
the exchange interaction B 2 J1 3 3 at j Here, 8 denotes the
ex 2 Im M 1 m lm' 1
spin operator int units. When the chain is stretched, antiferromagnetiam may
Card 1/3

Possible 1nomalies of the Magnetic Properties of S/020/60/131/04/019/073
Macromolecules B013/BO07
at a certain frequency v- not only with a certain value of H but in a wide
frequency range. The lateral links which "cement" the chains into the three-
dimensional body, play a stabilizing part. Of special importarne is the deter-
mination of the temperature dependence of the magnetic moment of the samples.
It is possible that the spin waves play an important part also in biological
processes. The authors thank L. A. Blyumenfelld and V. A. Benderskiy for
experimental data and a discussion. There are I figure and 16 references, 7 of
which are Soviet.
LSSOCUTIONi Fizicheekiy institut im. P. F~ Lebedeva Akademii nauk SSSR
(Physics Institute imeni P. N. Lebedev of the kcadeM of Sciences
of the USSR) Nauchno-isaledovatellskiy radiofizicheekiy institut
pri Gorlkovskoa gosudarstvennom universitete imeni N. 1.
Lobaohevskogo (Hadlophysical Scientific Research Institute of
Gor1kiy State University imeni N. 1. Lobachevskiy)
SUBMITTED:
January 3, 1960
Card 3/3

- - -
Onmm, V. IL. XMSOVA, L. V. I ROSORMOV, L. A.) FRADKIN, M. 1.
"The results of meaLi;urementa of nuclear component of cosmic rays of solar
origin with Sputaiks and tunniks."
report to be submitted for the IAU Symposium on the Corona, Cloudcrbft, New
Mexico, 28-30 Aug 1961.

PI 048:16 1 1XV003/001 !'004
1 (X)4! 1204
.kUI HORS Bjeniediktow, J A., Gittmancew, G. G., G1117burg, W L
1111.1: Radicastronornical investigations with the aid of artificial satellites and cosinic lockets
PERIODICAL Asltonaut~ka no, 3, 1961, 5-8
I'EXI , Radioastroncrilical observations by satellites can expand the range of wave Icngths at which extra.
t~jre,,trial signals can he reecked above 20-40 rn and below I cm Aleasurements (if the niicrov~ave separum
J the suit ma~ revival that the drop in its clTective temperature is caused b~ the fact that the
iadi at ion nasses through an inversc layer whose temperature is probably lo%cr than t fiat oft lie photophere.
Radiation of !he moon in the millimeter range and below may furnish information about the strLICIUN and
clemicand thermal proji~!rties (if the moon'ssoil. Rockelsvi,hich will pass in tile vicinity of Mars, Vellus, and
othcr plaiwts rna~ carr% out measurements of elect romagrictic radiation from lhese plancls over a wide
frcquencN range Sporadic eitiptions of the sun which are closely related to magnetic storms. ionospheric
hourhance~ affecting short wave radio communicztion. and other phenorneim can he ohwrVed morc
Irom salclhics Imotigalion of the sporadic cruptions ol'Jupiler hclo%~ 14 ML ina) tC%'Lal their CaUSC
Ca ril I I I

-to 0 (/461j)DIO);
E C,
I ORS ~Fl lc,ov. Ye. A. Getman! .9-
(itnif,,4rg, V.L.
I 'IT LE i fladc-'is!ronomical studieq
sciie t ! il cis and space rocke~!i
PEIR I 0i) I CA L. Akademiya nauk SSSR. Inkusstvennyye sputniki Zemli,
No,7, Moscow, 1961, pp. 3-22
I LXT In a provi.ous paper (Ref.. I
TIFN, 66, 1~;-.
k~l Earth ~,%t 11
Th-q-
,u I it -it I -Yr i ,,r, i o fiu~ d... me ni I
...- ionI. rJ specific forms
lit' t hE, ir, 1, ICA"1111r, QP( f I(Irl.85:
er.
r -id i.() pi~ii ss.,.en and the Y.i ~l
t~)Url' (.5k 4) radi-~ emission in tl:E I;t 1
11 la nr t s 1 2:, f u e1 i es o f t ii e L c, n,
fj I ILI Ili . ri,4, f part. of this oa p,
< M~ rl-e high-fi,equencv r~a,!t-
-.- d ~o

Ret-J,c -).it ronomi-c a! studies using

moon can be inve-q-. ~qated with the a iJ
wh a i,? t I-, F- of t I iis erni
Ili imet , F wa v e ! v ritv, I hs i ~s o f gr I, a
v - nt I rb t if . ri , lie t rn;~)-s JAI I i
erii,~~ ion r, I-, e wi v e J.e ri ~.- t h a shc.- I
P I ! o it, P i emlif?t'd t III 1~ 01' t he sun ti!,
W 1~ tle tha, -,.f' the M~ an Should be
inj.P.ide .hf.- sv)ichr-,t--on emission &.i-
c , rc%i la f ir a i I zc; ': a r m,-~ ane t ic f ie 1 JR
-, Pe z 1 r um (I i I h e S u 11 '_ I [nil v U e Po s." . ! -
th" 'erfe.~l 'empet"It ;lie on wave 1-n.,
passage o I the ra,diat ion throuc 'h
t empera ture is apparent ly lower than t f- j
The apparatus which should be set up - -, i i , ; -. . I -
in order to measure the high-frequen.N ii i luri_r r,1-f
emission need nct differ to any great r ii,_--
I,;tjrfa,-e" apparattis. The linear dime! o')*.'11:
(mirrors) need not be ver-j large since il i i!;* V I.-
moon and the sun are of the order of
A. = 0.1 cm the mirror diameter turrin I
Card 2/10

1.~~',(,57
S, 5 6o/6 I/ooo/ucq /(;(j I/ o I o
Hadio-astronomical studies using. . * 'E0321/E1 III
T:I--~ flux of Rolnr and lunar radio 4.-ii.9slan can only 1,,( i:t.;~;1ired
with antenmas having
., high directivity which woxild re(lilire
"orientnd" satellitpS. In the cilsoof space roclicts Jaunclied so
!hat they rench the neighbourhood 6t Nirirq, Vemi.4 and otill-1- I'li mets
ill tile solar !;ystellil, the radlo cm, I,( vut in
,I Wide frellw-,ocy r.mge. C.11. Mnyer, T.J. Xt'CllJI(-1'1.h '111d
Slon"al-l- 01717.51 Proc. IPE, V,-'I(I, :'(10, Pt5;)) ano J..K. A1.501),.
Y.A. GlorQ11111illp, C.H. Mayer and C.11. Towl-.t
;N.I'1j'oF-IuI1I oll '?'-Ijo Astronomy, Stanfol-0,
Inea-4111-f"d flip' radio ("Illissioll 4,11 ~ili-! On centinictre'
u:;Jllf- it 7-mijo telescope With 11 porob()IJ,c wirrur Ij In j 11
d-umieter. (In 3. 15 ell, tile ef(rct I'-, h,ml-or.itkii e. oi' I.,zirs was
found to b(' 1"20 i 75 OK, while I'm Vctm!- t1w corrc~spoiidini~~ .figrdre
Is 600 OK. Thnse. mcasurements repi v:-riot I Im. j t vsvi~t limit of radio
astronomical apparatum. oil the ol )111,- 11,11,1 ~~4 j r; I., I l'!: t o e, X t (In d
e me e Ili (I fl t S 10 1 o 11 g C 1, d e C v I V V C, I I Ine L r C W11 Ve 5
i,J1-I. izie,-t with -jerious difficulties, toct !;ilicc. the Omists-ion.
of Nars and V(Iiius in this riinge !.-~ ot charactcr its
iiitensity stioul(l I)e proportional to :,,i,l htncc ill order to
achieve the same power at the output (A' (Air, its in the case
Card -,/ 10

161 d j o-as tro no iii I c.1 I S I, 1A d iPS US ill /J .14 (11(i(; 7100 1/0 10
of' the short er wave I engths the area (i iilie II)ll:,t be
Incre(ised in propcsrt itin to X2 A it; I ivor li,i%-inil a 6,w.uter of
itholit 150 ill is ~klrf!.Idy 11crestillry ot ill -In Oil- vik:w of'(ii
.sp,lce Eocket, on thi! O,her hand, thc ti,t( jillik (11mc-11'.. iolin Can be
r,r~duced very coro;iderably, e.g. down t u L The sporadia solar
radlo ej,.ij..,5_qiun )%-is been extensive1y !;Illdied :Iii ii wide wavulongti)
ron,ge bfmg.tnnlii!~ :it I few cm right ill) to lu m. It hali beew
established that Hie i0owly varying (Jn t ime) component is
associated with sunspots. The other couilon(itt tit the lipuradic rAdio
entission tnkes the forin of short burst.-i. are due to the at
radio emirision wbich is largely as-qot- ioted i-i th !joJ.11: corl-usculnr
streams and also !3olzir cosmic rays emitt-ed from chro;uu,-ij heric
f lares. The Study of the spectral characterjzAicL of th(-se bursts,
and also the time dependence of the Intensity is of major
importance to any (jotolled theory of the ~,por,kdic radjo eii;issivn of!
tile Sun. The a )oradic' solar radio eutj:ision j.,i al-Ijo of Frcat
interest from the geophysical point of view. The corpuscular
Streams which arv responsible for these bur.,J.,i are al!io responsible
for geoniagnetic disturbances, radio fadt~out on sliort w.4v(_S,.
ionospheric disturbances, etc. A consideration of the expcrimental
Card 4/ 10

s 61/000/007/01-11 It:
;~~td Jx-as t I olmmi cal il tu d ies X.18 ill g . . . . L
iii.,'.c-rial nvailtible vo far shows that in tll(~ clise of ~ '4 It 1: - 5 o ,I
t h~! n tudy of so Ii, r rild io b iirm ts r1irl otily J)e ~rriad out with the
oid of nrtific:ial rmrtll Satellit.8 nith orl) i v i n -Q :,bovi., the
F -layer maximum. .-.,.atpJ lites wil i olso be f (,I' :I C I::.
ava:il-ible data (C.W. Alloil, Anti-p: t-;, I 'tll*-J -L r: r,
j At 11 low! -m - .1953 He f. Pi , iind D. F - I :I li w c 1, 1:o I I till
:'cjt - Roy. Astr. Soc . , V - 116, iO , V '1-)6, iiec. i6l) , ii un tit the
I'lldio hursti oil X 1,-' 40 In should b4 gnil-l"O r'! it t t.!,.,e!y ],w
.,!It !3 4 11 t I 1,L, Corolilt , IvINW-1v ~Vlq (.I I ~~vr 1.:"wl the
irr so A,- r c,.)x-on.i i.~; hnown to e., t n I,,', -it
Ii ~'.-C'S.S ib I y t o e v 4- rt gr e a t e r d j n * a i ~ c (,!~ .I t be
_C V rot
_:cted that tbe burst nomponent of, th- dio
'.---~;ion !ihould be observable up t- ~ r"" '~ t t- I" t ".. i ~ n. '111),
~,~.cvniatjon on bun~3ts on wi'volvil,th in oxcp~-' be of
j .-P ra b I e j. nt e ren t from th p 1 1, f v j ~_ v (. f I f, Cs of thc
!iolar corona. Satellite al,; -i 'J.i 1(:,i 1 '.-,1 c r 1 :3 o I nr
could n1so bfl used to dvi c c t !it it -r.
~11-11,1 t!j 1,1 t T fj~ nts would
--_~llarlv int. Crest ing ilifortitiO i
!)11(1 to the %,;, (! I e 1, AE, I
! avelength rltllg'~ the
'i.c radio emission and the rixdJo eini! I (.,I cA .id .- cr, ;_-7_;rcesj

f)IIIi CZI 1S t 11 d i e 13 US i llL~ . . .
F () 7,
it [.I out t hat. present I y w,,-, 4 1:1 Ll 11, dt, t t
11 L, spectrum of' tilk c. I I c 1--
30 ill obt~iirjed with !hi iv-iJ c[ -,~-t -~l .;I'tll
11 1 d 10 A 0 t 0 11101'0 it C C L1 V ( V i 111 I'l- I I I ,.,I (.I., Ic I B
oj,~ CYt.1, 1 1 2 lit er-p J '111(itary 0. i. fo I kjk~jl,lj I.I., L -11~' C 1 .1 e I (Is
. I - , it d - -,:~ t c c 1! 1 - a t c
~ C, 3! v those measkirorlie lit ;)(-I) 101 t o 1,~f,, .
t I XA C ! ' A ~ ~ h e 1zw4 cone e D t r b (I I Ic ~-i I) bi 0 1: t c I-;- ific (I
i ndc p(! I S It r C I'll I ."1r
-C('Ilritte. !;Ixtellitc if t1.( bl)(ct:. a
f L, 1~, Ac rndlo emission ,ihould Le carri( k: oUt from
h 4
"D ~.F to ionosp)liiric G-1 i E-cts. No-cerit rocket
d I ~!w 1- 11 ~, I s how t hit t t he ci 1e c t ron corcczAr;t t ion
iibovc the t. r (is wi t h a It j t Udo rather ,-, lowly
Yo. L. A). -c r,~ ;)obr3,akovtl, E . I.'. chudic's c l1ko, piro
v.63, ab-1, 11 of - 2 7 It IS C-Stillhitfl- that in t0
nninimi Be cffects. the slica surciiim-, nts of c-xtra-
terre4trial 1,acli.o i-J!*;sion on wavelent:ths grea ter than I -.i ~,Ilould
be carried out frogi satellites having an apogee in cxc-s-'s of
1000 Jim. lnter-plan~: tiiry absorptictit Lit' radic) ivavcs iziziv bcconle
Amportant in sa t jj' Ii te measurements . Table :' (fivcs th;-.. (--,,Aji.;ated
absollitioji in ;9pac(! for 1(w, 1, i%nd
'd /IC
C, Ex I

2~
Radio-astronomical studies using .... S/5 OV6 1/000/007/001/010
E032/E114
cm3 where f is the path length in cm. The optical thickness T
given in Table 2 was calculated from a formula given by
If.P. Ginzburg (Ref.28s"Propagation of Electromagnetic Waves in
Plasma", Fizmatgiz, 1960). This formula reads:
-2. 312
T = 10 N 17.7 + ln Te
Te3/2 . f 2 1 f
and holds for rarefied plasma for which (n 11. The values
given in Table 2 are very approximate but nevertheless it is to be
expected that the absorption should become appreciable beginning
with X- 500-1000 M. Another interfering effect in the range
X'?j 200-300 m may be due to corpuscular streams. A consideration
of available satellite and rocket data (Ref.1; as above. Ref.2:
194,
F.T. Haddock, Amer. Rocket Soc. No.i 1959. Ref.3: A.C.D.Lovel
Proc. Roy.Soc. A253, 494, 1959. Rer.4. J.P.J. Tvas, C.A.Franklin,
A.R. Molozzi, Nature, 184, 785, 1959) suggest that the satellite
antennas should be of a simple form. It is estimated that there
should be no intensity difficulties and arifenna dimensions of the
order of a few metres should be suffici,!nt. As regaids the radio
Card 7/ 10

26657
Radio-astronollitcal studies using .... S/560/61/()()()/()07/()O 1/0 10
F 0 1:.,/ E 1 14
emission of discrete sources the wavelength range 20-50 m is of
particular interest since it is in8cccs4iblO t', telrestrial
measurements. Here antennas having I inear d imens ions of' the order
of the wavelength are estimated to be adp(juairt. In order to
dchieve angular localization of discrete sout-ct!s and to determine
the details in the distribution of non--thermiA cosmic radio
emission, one could use the diffraction of extta-terrestrial radio
emission by the moon and the earth. r5timateg of the radio
emission of terrestrial and planetary radiation belts are more
difficult. Nevertheless,very rough calculations indicate that the
intens4ties involved should be detectable from artificial earth
satellites, and it is precisely because these estimates are
difficult that the satellite experiments should be carried out.
Finally, satellite and rocket measurements can produce information
about the radio emission of the terrestrial and planetary
atmospheres and also about the inter-planetary medium. It is
suggested that the most promising method of measuring the electron
concentration in the ionosphere and in inter-planetary space is the
method involving the measurement of the group delay time of audio-
frequency modulated nignals transmitted from artificial earth
Card 8/ 10

26657
Radio-astronomical studies using .... S/56o/61/000/007/001/010
E032/EiA
satellites kE.Ye. Gershman, N.A. Mityakov and V.0. Rapoport,
Ref-37; Izv. vuz, Radiofizika, Vol-3, 949, 196o). it is suggested
that a review of available information indicates that the above
radio-astronomical observations can be carried out with relatively
simple apparatus (this refers to thp radio apparatus and the
antennas). The authors therefore expect that satellite and rocket
radio-astronomical observations will attract considerable
attention in the near future.
There are I figure, 2 tables and 39 references: 19 Soviet and
210 English. The four most. recent English langungt- references read:
llef.3: as above.
Ref.10: A.R. Tompson, A. Maxwell, Na'l.jre, WS. 89, 1960.
Ref-31: J. Van Allen, Nature, 181, 41(j, 19=9
Ref-39: A.G. Smith, T.D. Carr, H. BoIll.-tizen, N rhatterton and
F. Six. Nature, 187, 568, 19WI.
Card 9/10

W10111 upwl"IMOV, S (11 C - 7,-) C-
Vit:lly Corresponding Acadony of S,,-Icn:!cs USSR
Kcll;rdclu'--'~i-~Ie luchi it Zomli i v0 VE;Clennoy (Comuic ll~,.yr, at, the wd in the
UriVOM?) 14001~01;1 L:d-VO "ZParliyC," 1961. 46 P. (SeriCS: VC-eSO~U7MOYC"
-po nu*,p7o9t---=erJju politiclhellkh IE -r.4 V. Se y
naw:N)vkh Ir 1. r1 a IK
tA,
FLAM i !!Miaiya~ no. 11) 26,000 copies prin d.
E,!. 1. 13. Paynboym, Tech. Ed..: Y,-,. V. Saw,,henka.
FMI-POVE: This boolc~t is intended for readers intcresu,!d in the phenorw-non of
coimlt: rays.
CUrMS: The boo?.Iet discusses bricfly the migin, llaturcl rind prowrtios of
,~osmir rayn. Tlvi theory of the phenomnon of co5mic rayn Is exudzif-Ill
ud wthodB of investigating nuch rays axe dpncrlly~d. inc"Alded itn- a
,I
-iscussion of our and other galaxieu aa the tmurco mid origin of cosmtc
ya, an arzilysin of their chemical composituion anel cnar-gy spnti-am. imd
balrucey illid rm Inventigation of the mchantsm of pa;7ticlo ac.L-,-Ienktio!,.
C::~-A 1/2

CnSrdl~ HUYS 'Lt th4! EW71.,h (COTIt.
Th~ prii:ciples of vuUomrixonomy as the mst inq)ort!vlt tooln of'
comir rnys axe (lAsciumel. Vo Tx-rsorvil.i 9 an, m,rtior-~~. Th-r-
CC, re r i c e r, I
!Lll 30v~e t.
OF CXMIMS:
Introduf"Idwi
Pi-iroxy Cosmic tbf, ElLrtll"I
Climical corgionitlon
I-,,-,i:.rt3y sly--Arm. . Inotropy of cocirdc rays
ilL,I[oastronomy axil Cosmic Rays
1; of -omdc M, diation and comxtc rcty.,;
Cc
rays in file liniverile
01-ir"In 0~ Cosmic Rays
Eii,n~gy ~mlQice. SollMcs 01' coando rayn,
lmcaarlun,
Conclusion
BitliolT,niphy
AVAILUME: Libmr-y of Congnesr, JAlrrT4~rn-
C%rd 2/2

3 05
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11 2 ~[ Oo D299/D302
AU"HORS:
L., Kurnosova, L. V., Logachev,
V, L., Razorenov, L,. A., Sirotkin, L A,,, and
Fradkin, M, I~
TITLI-I': '._Audy of charged-particle intensity during the
flight of' the 2nd and 3rd Sputnikn
SOURCE Alcademiya nauk BSSR. Iskusstvennyye t3putniki
Zemli, no. 10. Moscow, 1961, 22-33
TEXT: During the 1.*Jiirtlt of the 2nd and 3rd Sputniks, the flow
of charged particles at 111titudes betiveen 187 and 339 km and
latitudes of -65 to +65 was recorded by mems of a telescope
consisting of' 2 rows of gas-discharge counters; the telescope was
part of measuring equipment for coamic rays, As a result of the
measurements, the intensity of the charged particles and its
latitude dependence were determined. The counting rate NC and
Cards

Vi ~05
S/560/61/000/010/003/016
Study of charged-particles,-, D299/D302
the global intensity J gl at various latitudes are listed in a
table, It was found that at all latitudes the recorded intensity
was several times higher than the intensity of cosmic rays re-
corded in the stratosphere and in free space beyond the earth's
magnetic field. This difference is particularly noticeable in
the region of the geomagnetic equator, where the measured inten-
sity was six times that of cosmic rays, Several regional anoma-
lies of intensity were observed, apparently related to the anoma-
lies of the earth's magnetic field. For the entire track of the
space-ships, detailed graphs were made of the time dependence of
the intensity and hence of its dependence on geographical coor-
dinates and altitude of the space-ship, From these graphs, maps
were made of the intensity distribution on the earth's surface,.
It is noted that, with repeated pasoage of the space-ship above
the same terrestrial point and almost same altitude, the recorded
intensity differed sometimes from that on the first passage; in
some cases, the irtenBity was almost double,, This difference
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Study of charged-particles.-, D299/D302
was particularly noticeable at high latitudes, As the orienta-
tion of the apparatus changes during the second passage, this
difference in intensity may not be real, The obtained equi-
intensity lines for the south-Atlantic and southern anomalies
constitude a slight refinement to the earlier obtained data (in
the references); the maximum number of counts in the southern
anomaly was 60 per second, and in the south-Atlantic anomaly it
was 70 per second. The anomalies are particularly great in the
Southern Hemisphere. The intensity distributions in the anomaly
regions, recorded at altitudes of 306 - 339 km and at altitudes
of 187 - 265 km during the two flights, differ from each other,
This difference is apparently due to the different flight-
altitudes. The connection between the anomalous structure of the
radiation belts and the anomalies of the earth's magnetic field
is evident; it would be premature, however, to assume that the
regional anomalies of the magnetic field on the earth's surface
have a substantial influence on charged-particle flow up to
altitudes of 200 - 300 Im. The many anomalies in the South- and
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Study of charged-particles..- D299/D302
North-Pole regions, their disposition and variation, suggest
that these anomalies are the edges of the outer radiation belt
of the earth. The latitude dependence of the intensity is shown
in a graph (for the Northern Hemisphere); It is noted that,at
high latitudes, the increase in intensity ceases,, The obtained
data on the intensity distribution give evidence of the edge
effects of the radiation belts at 200 - 300 km altitude and of
certain peculiar features not observed previously. In particular,
the great temporal anomalies are noted; thus, the "northern ano-
maly" recorded on August 20, 1960, at 7 hr. 40 min, (worid time)
and the south-polar anomaly recorded on December 1, 1960, at 14
hr, 22 min, These anomalies are apparently due to solar activity-
The line of least intensity (the "radiation equator") is shovin
in. a figure. With regard to the composition of the radiation,
it is 'Likely that the increase in the counting rate (as compared
to that from primary cosmic rays) is due to protons with E p 11
60 Mev; although no definite conclusion is possible as yet, it
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Study of charged-particles- D299YD302
is assumed (as a working model) that the Inner radiation belt
if formed by protons and that the number of electrons of energies
higher than --,2 Mev is small. The above results confirm the
existence of a high-intensity region down to 200 km altitude
(from 1000 km),. On the other hand, the radiation at 50 - 150 km
1B practically independent of altitude. The altitude dependence
of the intensity (for 200 - 2000 km) is shown in a figure.
Tentatively, the altitude b and the atmu8pheric density p can
be expressed by the value:4-
h, km 100 150 200 300 400 500
P) gm- cm-3 10-9 10-11 10-12 10-13 2 x 10-14 2 x 10-15
h, km 600 700 800 900 1000
gm 'CM-3 6 x 10-16 2 x 10-16 6 x 10-17 3 x 10-17 10-17
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Study of charged-particles- D299YD302
On the basis of the incomplete data available, the internal
radiation-belt in the equatorial region for altitudes above 400
600 km can be approximated by a very simple model, where only
ionization losses are taken into account. At higher latitudes,
the pattern is more complicated; it becomes necessary to render
more precise the composition, spectrum and altitude-variation
of the charged particles. At altitudes below 400 - 600 km,
considerable deviations from the formula J occur. This
is due to diffusion of the particles in a direction transverse
to the magnetic field; this diffusion mechanism is related to
collisions between particles, A second diffusion mechanism
exists, related to the presence of electric fields E which
cause particle-drift,. The diffusion processes require further
investigation,, Finally, the radiation dose is estimated beneath
a layer of matter of the order of 4 gm/cm-2 at an altitude of
200 - 300 km. Assuming recorded proton energies (in the equa-
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33,ic)5
S/560/61/000/010/003/016
Study of charged-particles.- D299/D302
torial region) of EP >,60 Mev, the daily radiation dose consti-
tutes approximately 30% of the permissible dose. In the region
of the south-Atlantic anomaly at 300 km altitude, the radiation
dose Is by an crder of magnitude higher than at the equator.
There are 10 figures, 1 table and 10 references: 7 Soviet-bloc
and 3 non-Soviet-bloc (including 2 translations). The reference
to the Englieli-language publication reads as follows: S.
Yoshida, 0. H,, Ludwig, J. A. Van Allen, J. Geophys. Res., 65,
807, 19W
SUBMITTED: May 15, 1961
Oard 7/7

GIMBURG) V.I,,; SY14VITSKIY, S.I,
Origin of cosmic rays. Geomag. i aer. 1 no.4:479-48" il-Ag :(,I,
14:L~)
1. Fizic~ioskly institut imard II.N. belvedeva AN
(cosmic rays)

S/181/61/003/006/024/0~1
7 (d 3 B102/B214
AUT-HORS1 Ginzburg, V. L., Rukhadze, A. A., and Silin, V. P.
TITLE: Electrodynamics of crystals and the exciton theory
PERIODICAL: Fizike tverdogb tela, v. 3, n6. 61 lo,61, 1835 - 1850
TEM The preBent. paper gives a detailed theoretical treatment of the
general problem of the application of the electrodynamics of matter With.
spatial dispersion to crystals. The*authors confine themselves particu-
larly to t~e inveatigat'.on of the approximations one obtains when one
norks with E the tensur of the cotplex dielectric constant.
ij
First the fundamental equations of the electrodynamics of matt'er with@
spatial dispersion are written down. They are in the usual notationss
1 1 8B
curn - our19 - _T Tt ; divB' - 0;
cjo; di'D'-4'Qo c Ly B]
the force acting on a point char e moving with velocity ~; for the
electric induction one has T/at - af/at + 413. For plane monochro-
matic waves, D' and are interrelated byt
Card 1/7

2 i-91 7 3/101/61/003/006/024/031
Blectrodynamics o~... B102/B214
9, (k, W) lij (to, k) Ej (k, to); E((k, t-1 (w, k) ~Ij k), (1, 6)
tij ((0' k) dt I dRe'(kR-.,)j,1 (%R). (1,7)
For crystals one has
D',(r, to)= fdr'a,1(-, r, rl)E,(r,
U, (k, j dk'#,, (w. k. kj E, (W,
It is shown that in cr ystals in the optical region the tensor
can be reduced to the tensor 'ciic(w,k) in the usual way. If the normal
electromagnetic waves have the form E e B Bo,le
1 01
E constant, B., - oonstant (spatially homogen'eau.9 med um) on'e has
for j - 0,
Card 2/7

5/161/61/oo~/006/024/031
102/32 U,
Electrodynamics of.., B
D'= (U], B (U],
D' PE k (kE)),
OF, k,kjFj = 0.
17, y5j
1 2 2
or, in the doterminantal representation tj("'-k') (",r-.)-k 6 +k k
2 1 j ij i J1
k k, 1 ( A or j~ denote the
0, or 2 ('~' ((, + ki. 1ij
') _jLtl~ij_ -ij k " ,
c
determinants of the a ys t e:.-. of linear homogeneous equations~ Starting from
these equations the authors investigate in the following the properties
of the tensor Ei in cryBtals, as well as the possitraity of calcu-
lating this tenser ~JURntuzn-mochanically. Pirst, the effect of taking in-
to consideration the space inhomogeneity is investigated. (1.8) may be
4' c rm
I . ) 7e n
written in the _i4(,t~,kI whe- i i
v b :L7 1
is an arbitrary v,~,ctor of the reciprocal lattice. The relation between
Card 3/7

S/181/61/003/006/024/031
Electrodynamics of .. B102/B214
D' and ~E is given by
k,kjF.y (-, k) -- PF, k) 2- b (,, k) Ej (k -f- 2,rb, to)== 0. (2, 3)
CV ii
whose determinant ieaEs to the dionersion equation A(ttyq) . 0 with roots
W . il~, (V) . if ail terms with b / 0 are eliminated from (2.3)'Yihich is ju&-
tified for thoreaion vith k,,b-1/ar.:/~cb.;~c/a) considered here one ob-
tains for ana2agous (1-13): k,(~E) - OEi + (_2/c2)Eij((.j)E -0
2
Here ~_ ii("),Z) differs from ~-i3 only by terms of the order of (a/,kd.
In optics, not only is ~fif Q ~1, but it can also be assumed that ab.
1 0)
a nA 0 (a-lattice constant, A -vacuum viavelen~th). This is done in
0
the following, i. e., t he spatial dispersion is.assumed to be small. One
may then expand (to, ) in series of powers of V and neglect 'termp of
higher order than the second. Near the absorption lines where some com-
ponents of ~. (w) become very large one must expand analogously the recip-
ij 1 1 . , !,. 2,q2
rocal tensor oil (1 .6): E7 ((",-k,) - E- W ig n (,)/C)
Ii ij i j 1!c'! , I ijlM TM,
flard 4/7

Llectrodynfird.c:~ ~jf
/( r,~,/024/031
J
v.-here "' r. n I -in",-. n+i-i. v F, P f-, x v a n q i c. n. n in. r e n~ o t j u o t i f id i n
C
all the case~i (e. for by ii r4un.0rupole tranni-
tion) . In tho! f- I ~o I Orr~-' ~i(;! na_'
are studicL 11 'n C. i `!, ~u' II v s
0
there exist oth(-_- f i (.L.-_-,s,.)ord.`ng to
"fA4Ct it iVf~"' 101'.;; ! t, U . 4~ !.:1 7 t to obof'rve in
the dcmain of c la ic -'- c ryf; tal -p- op, th:~t th 0 become
longitudinal when n2-0,). E,:. (1 .-1 is i n v es
f orr. -I . I / - , -~," 'n this case in the
~2 at` on
I't"i C I; ~j I G
1~ s On' - i n. '21 !~nd are Ii`ferent
fr~m' zer'o~ 'iIf 'E-' a :-. d 0, 0 -ust be
P
satisfied. The inst; case ;-s that of 'Ipciarization All three,
the lon,~itudinal, the fictitive longitudinal, and tlne ro1arization waves
(). Finally the authcr,) liscuss some prob-
satisfy the ccin~ition 'd ~, v I;
lems of the ~.,iuantum of tho dizi~f~--sicin nf li,,:ht iln crystal's during
which the chotce ol thm, ::,.(!'shod of calculating the
r.
tensor ~ is also TLnking intc ccns.-I'deraticn the trans-
ij %
lational symmetry of the cr.,,stal a result is obtaincd for t-e current
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s/181/61/005/006/024/031
214
Eloctrodynamicc of...
do is ity in the ~on of t ~ie pert urbp t iecrv. Thi.9 renult int
(k, k) Ej (k -t- 2T-b, w),
(4,4)
b
vhtre w", k)
w - W, -0- W.
te f P,
Js determined by exciton
It may be assunmed that the vulue -o f j
transitions, J.. v., the freouenciesj- and in '4.5) are the frequencies
n
of "mechanical excitons? in the crystal. The exciton 54 ates are quasi-
stationary, i. e. -.he are compl ex. One can expand or the tensor
0ij into a series of no,,-, -~rs of k anO thur, obtain!3.fcrmu-'as analosous to
Card 6/7

r dy n a
1 A
fit 1
t;~ ry Fi n
t
a k
--s cm En,~, c n
Th~,:~r
ASSOC LATT"N F A,;
3 1 TP "'T I TT E T)
ra r J 7 / 7

GINZBURG, V.L.; RU111ADZE, A.A.; SILIN, V.P.
COXTOCtiOn to the article "Electrodynamics of cr-jutals and
exciton theory 0 Fiz. tver. tela 3 no.9:2890 S 161. (MIRA 14:9)
jGrystals-LIectric properties)
(Excitons)

S/141/61/004/001/007/022
E133/E435
AVTHORi Ginzburg, VA.
TITLE: On the law ;Fiiiergy conservation and the expression
for the energy density in the electrodynamics of an
abtorbing and dispersive medium
PERIODICALt. Izvestiya vysshikh uchobnykh zavedeniy, Radiofizilea,
1961, Vol.4, No.l,'PP-74-89
TEM There seems to ba some doubt, from the macroscopic viewpoint,
as to what constitutes the energy density of a medium when
absorption is present. On the other hand, a physically
comprehensible expression for the energy density can be formulated
In the microscopic approach. The author first considers the .
macroscopic approach in the fo&w of electromagnetic waves passing
through.& non-magnetic, isotropic medium. It is known from plasm
theory that the following equations hgld:'
4::e'JV
4- ni
(where N electron concentration andV is the number of
Card 1/6

25947 -t-
S/141/61/004/001/007/022 V
On the law of energy E133/E435
collisions of electrons with other particles). It can be seen
that two simplifications are possible: if w2 0 group is 53 � 15
5) The intensity maximum of the outer radiation bell shifted 104kni towards the surface ofthe earth during
the time interval between the launchings of orbital spaceships I and 11 (front January to September, 1959).
Card 1/2

Some invest igat ions of die cosmic ray...
S/203/62/0021'002/001/017
1046/1246
6) At altitudes of 200 to 300 kni in the 65N to 65S belt thc radiation count is in excess of what could have
been expected front primary cosmic rays; on the equator, the global radiation intensity is 6 to 7 times as high
as the cosmic ray intensity. This phenomenon remains still unexplaimd 7) Two radiation-intensily ano-
malies were di%covered,viz.,the South-Atlantic anomaly at an altitude of 340 km and the Southern anomaly
at 194 to 340 km above the Antarctic coast, both being closcl) associated with the geoniagnetic anomalies.
In August and December 1960, the lower boundary of the Soul h- Atlant ic anorna1v was mapped at an alti-
tude of 265 to 306 km. There are 15 figurcs, 7 tables and 70 references.
Card 2/2

GUMBURG, V.L*
IAw of the conservation of energy in the electrodynamics of media with
ape.tial dispersion, Izv. vp. ucheb, savj radiofiz. 5 no.3.*473-477
162, (MIRA 15:7)
1. Wauchno-issledovatellskiy radiorizicheAldv institut pri Gortkovskom
universiteU
(Eleci M"d3mamice) (Field theory)

S/051/62/012/003/003/ol6
E03 2/ r,-:, 14
AUTHORS: Gi nzI) and Glukhovetskaya, N. P
------ juj.,Z... . V. L.
1'." L 1.1, Dopendence, of the intensity of spectral lines on
the O'Coctive ionization potenti,,xt- of an arc
iya, V. 12, 1)(2. 19 G-2
PFRWDICAL: Optilia i spol(troshop
T 71KT: The authors roport an experimr~zitil studs,, of' the
~ 1
1 2' o 1 2 0 1 0
for H, 2 1)
0, IT-1 - I, j- - cli,/OtAr, i + 60 -1 where S is the
OA_
area ana I the perimeter of the cylinder croon section. It is further
shown that a s tate, wi th a given n #z 0 is attained when the flux of the ex-
ternRl field throug 2H Lc (n - 1)
,h the opening is given by ~2 - nr 1 2 ' 2e 2 .
Thin result is in agreement with experiments. There are 1'3 references:
6 Soviet and 7 non-Soviet. The four most recent references to English-
language publications read as followst J. Bardeen. Phys. Rev. Lett., _7,
162, 1961; L. C,isager. Phys. Rev. Lett., 1, 50, 1961; R. Doll,
1961; N. Byers, C. N. Yang. Phys.
M. Nibauer. Phys. Rev. Lett., 1, 51,
bett., 1, 46, ig6i.
ASSOCIATIONi Fizicheskiy institut im. P. N. Lebedeva Akademii nauk SSSH
(Physics Institute imeni P. N. Lobedev of the Academy of
9cionces, USSR)
SUB:,'.ITTED: September 12, 1961
Card 4/4

GINZBURG, V,,
--* -- - --------- .-
Voices of remote worlds, Av, i ~Oam~ 45, no,9 SP-89 `62
(MIRA 15~10)
1. Chlen-korrespondent All SSSR,
iCoamiQ rayal'

S/053/62/076/004/002/004
B102/B104
AMIM. A,;;ranovich, V. !"I., and Ginzburg, V.L
TITLE': Cryotal optics with reference to spatial dispersion and
exciton theory. I
-IL1116DICAL: Uspekhi fizicheBkikh nauk, v. 76, no. 4, 1962, 643 - 682
TILXT: This paper is the first part (introduction, � it ~ 2, and first part
of ;eferences) of a longer work. The present state of crystal optics in
the light of recent years, literature is reviewed. The following topics
are discussed: j 1. The tensor of the complex dielectric constant
i~ ij and normal waves in a medium; properties of ~. ip-,k), normal
electromagnetic waves in matter, transverse and longitudinal waves, ghost
longitudinal waves and "polarization waves", energy and other relations
for waves propagated in an anisotropic medium. � 2. 6ij (t~,-k') in crystals;
introduction of 6ij; weak spatial dispersion (a/A