SCIENTIFIC ABSTRACT PIKELNER, S. B. - PIKELNER, S. B.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001240820009-5
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: January 3, 2017
• Document Release Date: August 1, 2000
• Sequence Number: 9
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

PIKLI'f'~~h ;! k
=-=0- -..
flial Inveoti,at:cT: (~ ;-LuArescence c,,'
Lx I "Cl, 1~"G!-.Cow '--dr-r r,. ' - ', Ir.enl ' . 1. Lo-,rx~rror,-1, ',. "'. .
CM, 14 Dec 54)
Survey of cienti ,'ic ia.d Tlect.t.~ct-.Il :ds:,ertatl~-r... i~ofonded I* i .,:-
i if-I er iAuccticnal ;LnE (I. ,I
SC : Six- . 1% c . 5 '3 t- , 2-4 J u1, ~ 5

PinLIMM, S.B.
--ft
- 00a the distribution of Interstellax matter" (in Xngliobj. G.Alter.
Abstract by B.B.Pikellser. Topkosm* 2:325 154. (MBA 8:5)
(Interstellar matter)

PIKILIMM, B.B. -...
"Sow structural characteristics of gas nel"tlas and tbair relation
to the stars.0 V.G.Nsemkov. Abstract by SJL?ikellser. Vop.kosM6
2:325-326 954, (MM 8:5)
(fthase) (stars)

I ~-/ w - /~ ii~5 -
Plf,-~~ C
FIKILIMR, S.B.
wmwimoo~
Kagnetic fields in interstellar space. Vop-kosm- 3:85-93 154.
(Magnetism) WaL 80)

t i ~~ L- L-, N 1~ NI-,~)
ATUR, ~L.H.; - PIXEM Q lm
'Turbulence in the interstellar madlunm[in Zngllshj. Abstract b7
S.B.Pikellner. VOP.kosm. 3:317-318 154. O"A 8:3)
(Gases, Interstellar)

"I v\ f
I
-L- !m [ r) , - ~)
BLTRS. D.1 SPIT=, L.; PIKELIMM, S.B.
OThe density of molecules in interstellar spaceOCin Xnglishl.
Abstract bv S.B.Fikellner. VOP,koon. 3:318-319 '54.
(Gases, Interstellar) (MIRA 8:3)

~ I )~ i: - t v U t~ . -, "-~
SPITZER. L.; SAVIDDY7. M.; PIE131CLO S B
OThe texperature of interstellar matter*[in English]. Abstract
by S.B.Pikellner. Vop.kosm. 3:319-320 154. OaaA 8:3)
(Gases, Interstellar) (Temperature)

V I F, L L'JV LK) - -L .
HILTM, W.A.; PIEELIMM, S.B.
won polarization of radiation b7 interstellar medium*[in English].
Abstract by B.B.Pikellner. VoP.kosm. 3:320 154. (MLRA 8:3)
(Stare-Radiation) (Polarization (Light))

RMOCK, H.W.; PIKB Sa.- -WA
08tol1w -ago tic fieldow[in Xnglishi. AbBtract by S.B.Pikellner.
Vop.kosmo 3:321-322 154. Oaft 8: 3)
(stars) (magnetism)

IlCon'erencp !,evoted tr ~-ysics r Nehi.t v, ind rr IrterF-I't ir -itter"
Vor. osmor-ni I Ic,r4p c-161
Yhe crn'erenc- vis --r,r-ein st.rr
o f t,'- e 1 1 .':S~. I r s! - rs r i~ ve
r,ul7,.;ec* -.-rr, ~rrlar+sur-an, 117e , I I',
IrasewslAy, Yi. ~,T-per, V... r-71 r-w-l i v '.e~e ~ ins]- !y r,
V., 1 1 - vsl~ i-.,a nd Vn r r, t s -7 1-
(R:7fAstr, Ur 1 1
,ur . Nc If U-)

PIM169 MKR, S. B.
AltetrouWmtic phenowas in astrooWeles. Usp. "trea.mook 6:281-
322 154. (KERA 7: 8)
(magnstism)

PIMMITFIRP S. R.
"Spectrophotometric StudY of Dif fuse Nebula NMC 7000"
Tzv. Krymsk. Astrofi7. Observ., 11, 195", :1p 8-17
The study was carried oiit by means of the nehn-lar spectrof-r-aph of Maksutov-
loannisiani design. Relative intensities of 11 and N lines were corr,cted for
interstella absorption accordinr to the redenninr of the star HD 19Q579 of
class 07 which, as it was pointed out by (,. A. Shayn arid V. F. (,a.-.e id.
,,, of the nebula. Author cor- F to
3, (1951)), excites the lurrLinosit, same
conculsion. He also finds dusty a~jsoftinF matter between the Pelican ne~)ula
and the star IUM 199OV.1 of class P3. (RZhAstr, No.11, 1951j)
SO: 17-31167, 8 Mar

PIKELNER, S. B.
"Method for Studying 7kirbulence frDm Fluctuations of brightnesc in Neljuiae' ,
(Theoretical Astrophysics, Diffuse Nabulae), Izv. Krymbk,Astrofiz, CIL,--erv. N4-
11, 1954, PP 311-38
Abs
W-31146, 1 Feb 5",

PRELINER, S. B. and CHUVAYEV, K. K.
"The Probable Mechanism Governing the Luminescence of the Night Sky in the
Continuous Spectrum".
Izvesti-ya Krymsk. Astrofiz. Observ., U, pp 178-184, 1954.
The nature of the radiation of the night sky in the continuous spectrum is
considered on the basis of measurements of its intensity, in various regions of
the spectrum, which were carried out by K. K. Churayev by means of a photometer
with secondary-electron multiplier. It is shown that recombination of electrons
in neutral atoms of oxygen leading to the formation of negative ions 0- can give
radiation close in intensity to the observed radiation. Such a process can be effective
in the F layer of the ionosphere, whiq at night is about 250 km high add which has
and elecl6on creentration of nj 2 lo-, cm-3, concentration of neutral atoms of oxygen
no 5.10 am- . and electron temperature of T = 1500 . In the expression for the
energy radiated per unit volume containing n, electrons and no atoms is the quantity
k , which is the coefficient of absorrtion computed for one negative ion. The effectiv
thickness of the radiating layer is taken to be equal to 50 km. The computed inten-
sity of radiation is close to the observed intensity. Given the quantity T, one can
compute the behavior of k as a function of wavelength on the basis of the observed
energy distuibution. As it turned out, kv increases from the limiting series toward
the side of short wave lengths. The authors evaluate how esgential the other mechanisms
of radiation in the continuous spectrum can be. They conclude that the choice of
1/2

Continued:
possible mechanisms is extremely limited. Formation of negative ions must lead to
strong decrease of ne- Inasmuch as the concentration of electrons and the
intensity of luminescence do not decrease significantly in the course of the night,
it is necessary to assume that there exists a process that disrupts the negative
oxygen ions and restores the number of electrons. It is shown that in this connection
electrom collisions cannot be effective. The same holds for heavy particles. The
most probable mechanism of disruption of megative oxygen ions is consid1red by the
authors to be their collisions with ejdcited oxygen atoms in the state D 2' This
conclusion, however, is based on the as5umption that the energy of dissociation
of a negative ion is equal to the energy of a ouantum of the red line ,,f night-sky
luminescence. Therefore the presented evaluation only indicate6 that in principle
mechanism can exist which involve disruption of negative ions. (RZhGeol, No 1.1, 1955)
SO: Sum No 884, 9 Apr 1956
2/2

PIKELINER, S. B.
"Electron Collision As One of the Possible Hechanisms Governing the Excitation
of Night-Sky Radiation of the Red Linen.
Izvesti-ya Krymsk. Astrofiz. Observ., 1-1, pp 185-188, 1954.
The possibility of the excitation, by electron collision, of the red triplet
of oxygen 6300, 6364, 6392 Angstroms which is observed in the spectrum of night-sky
radiation is considered. It is noted that form the viewpoint of "selective refraction"
one cannot completely explain the very co-iplex character of the behavior of the red
line. The rossibility of excitation of oxygen atoms b- electrom collisions strongly
depends upon the kinetiv temperature and density of the electrons in the upper layers
of the atmosphere. In recent years it has been established by means of raido methods
that in the F layer of the ionosphere the kinetic temperature T at night is equal to
about 150& and the electron density is approximately ne 2*165. Employing an
approximate expression for the cross section of excitation oXygen atom by electron
collision and assuming Maxwell distribution for t'e electron velocities and
effective thickness of the radiating layer to be equal to 30 km, the aut4or obtains for
-::1.43*10 quanta per cze. -
the number of quanta of the red line the value N' 7
see. steradian, which agrees with the observed value.
The gradual drop in the intensity of luminescence in the course of the night
can be 1 c?nse werce of the gradual cooling of the radiating layer, and the variation
from nigRt 0 night can be in consequence of the irregualr variations in the temperature.1

Continued:
For example, for a decrease of T Prom 1500 to 1300 the quantity N decreases by the
same order. Frop the computations it follows also that the kinetic temperature in the
F layer cannot exceed 1500 , since in the contrary case the radiation of the
red line would be greater than 'the observed radiation. (RZhGeol, No 1-1, 1955)
SO: Sum No 884, 9 Apr 1956

s T I
7,G
7
--c- PUP-
_T
llOT r,;D J -"JOIT~t
jo
-1-`-M,~ 'c

SEIATN. 0.A.. akademik; GAZS, V.F., kand.fiz.-miatem.nauk; PUBL'IM, S.B.
Presence of dust and gas in diffuse nebulae. Izv.Kr7D.aatro.'i2.
obeer. 12:64-87 154. (MIRA 11-4)
Olebula,j) (Interstellar matter)

PIULO NER. S. B.
USSR, A, t",

-c rz;
na ."I
(7, nil P' ke

D
P. -~d 1 3 r t) r, z u,- I M,
-rac' "r" 3S '.or.
Ing a' I type F n'.L)k:!:!" e mn e
c ame ra In c omb I na t I on w h one % a e,-
yellow fltl-pr. Porm 11 we.-,(-- -j,,
sumpt- '. onzi .9 re Tna e c f -1
on the distributIon ol- brlwhtn-~is r
inear, rf~"la tAor v-;~ zz f'cun,' betw(
bu' a e A ! -
tudes --,*- tht~ t-ml3slon n.,id - f
general a very complex c,f 'nt-pr'r; 3,
dus t exis ts i r, d 1 f f IIE: ed no bu I a - - -: to t, I es
10 references , 4 RuBs Ian ( q 1' n(,e ~ "j '-)) ~
Institution Academy of Sciences USISIT-1, Crimean Astrophysi
SubmItted January 4,

'16

PIKELIM, SOB.
Results of the observation@ of solar corona of June 30. 1954.
IZV.Kry'M.astrofig.obeer. 11:111 155. (KIRA 13t4)
(Sun--Corona)

-'-'-----.777
slid
-7-
7
7777
.0 us 0, tic fielcl
6f
an-Feb, 195_5
45;;47s
'Ar DYBUMIS
rac
:o .:su a
na
SUP
eous tali, mm
bad- 2:
I zo the'
-Cr anAst
Aclid a10 SOB YJSSR
j=D
rva-
Zr

SHAYN, G.A.;PIMINER. B.B.;MSAN(N. R.1.
Keazurement of polarization of the Crab nebrulas. Astron.shur. .32
no-3:395-4W 3-0 155- OIMA 9: 1)
lArymakaya astrofisicheakaya observatorlya Akadexii nauk SSSR.
(Nebulae) (Polarisation (Light))

PIKILIMM, S.D.; GIN33URG, Y.L.; SHKWVSKIT, 1,S.
Mechanism of particle acceleration IL envelopes of save* &ad
superseve.e. Astroz. zhur. 32 no.6:50-) 513 W-D 155.
(Star$, Now) (M72A 9:2)

PRELINER. S. -R., GIRS-MG, V. L. and SWLOVSKIY, 1. S.
"Radio Radiation of Discrete Sources," a report delivered at the Symposium on
Radioaatronoay held at the Jodell-Bank Experimental Radioastronomical Station#
Manchester University, Englan, is summarized in the account of this symposium in
an article by V. V. VITKEVICH in Vest. Ak. Nauk SM for January 1956.
St=. 900, 26 Apr 1956.

PIKICLINER, S.B.
?heory of magnetic storms and auroras. Izv.Kryn.astrofiz.obeer.
16:104-121 156. Ma 13:4)
(Auroras) (Magnetic storms)

PIKE41HER, S.B.
Dynamics of diffuse matter. Izv.Kr7m.antrofiz.obser. 16:1,W-14.-7
'56. (JURA 13:4)
(Interstellar matter)

AMIMM 3 B -S
. - - " 0 -to 6AM -- --
Symposium on radio astronomy hold at Jodrell Bank. S.D.
Astron.shur. 33 no.lo.114-120 Ja-P 156. (KUU 9: 6)
(Jod.roll Bank, Ragland-Radio astrousar-Coagressee)
'-I , ,

PIKIL'MM, S.B.
"I' ~
Spiral notion of prominence knots. Astron.shur. 33 no.5:641-
645 S-0 '56. (MLRL 9:12)
1. Krymakaya astrofisicheekaya observatoriya Akademit nauk SSSR.
(Sun-Prominence*)

PIKELIKER. S.B.
- .,-- .-- Ji~~etjb field of the Crab nebula and the central @tar [vith
summary in English]. Astron.zhur. 33 no.6:785-799 1~-D 156.
(KIaA 10:1)
1.Krymskaya astrofisicheekaya observatoeiya Akademit nauk SSSR.
(fiebulae) (Magnetic fields)

FIXILIMIR, S.B. doktor fiziko-matematicheskikh nauk.
Magnetic field of the Galaxy. Priroda 45 no.12:27-34 D '56.
(Magnetic fields) (Kilky way) (MLHA 10:2)

PIKELIMM, S.B.
Interstellar light polarlsation. Usp.fiz.nw, 58 no.2:2a5-320 F 156.
(cosmic rve) (Interstellar matter) (Polorlsation(Idght))(MUL 9:6)

PIKSLIMM S.B.
G.A.Shain; obituary. Astron.tair,,no.172:1-2 Ag 156.
(?U.RA 10:1)
(Shain, Grigorli Abramovich. 1892-1956)

Name: PIKELINER, Solomon Borlsovich
Dissertation: Investigation of the motion and
lumineacence of Interstellar gas
Degree: Doe Phys-Hath Sol
Affiliation: Crimean Astrophysics Observatory,
Acad Sol USSR
Defense Date, Place: 28 Feb 55, Council of Moscow Order of'
Lenin State U imeni Lomonosov
Certification Date: 9 Mar 57
Source: BIWO 13/57

AC.t NR, . Am6026m___ Monograph URT-7
Pikel'ner.-SolomDn Borinovich
Principles of cosmic electrodynamics (Osn*ovy kosmicheskoy elektrodinamiki) 2d
rev. and enI. Moncow, Izd-vo "Nauka", 1966. 1107 p -Illus., biblio. 5000 copies
printed.
70PIC TAGS: plasma physics, Plasma wave,
plasma stability, plasma interaction, -ovaz= electrodynamics, 6ftiftr,~'_
-;S=~ &qtdr=dP=_rA: ca ==a 04 magnetohydro-
dynamics, astrophysics , 006mokci6!
PURPOSE AND COVERAGE: This book is intended for the general reader interested In the
principles of cosmic electrodynamics and its relationship to astrophysics and geo-
physics. Emphasis is on the physical aspects of the problem. Mathematical
analysis is kept to a minirmim; it is used only to illustrate a point, and is
limited to relatively simple operations. The first several chapters deal with the
general properties of plasma, magnetohydrodynamics, wave phenomena in a plasma, and i
plasma stability. The subsequent chapters explain various plasma-associated
phenomena without going into too inuch detail or mathematical interpretation. There
are 331 references, more than half of which are non-Soviet.
TABLE OF CONTENTS [abridged]:
Card 1/2 UDCe 523,037

ACC NR, Am6o,,>6753
Foreword -- 6
Introduction to the second edition -- 8
Ch. 1. General properties of plasma - 9
Ch. 2. Interaction between a magnetic field and a moving conducting medium 58
Ch. '3- Waves in plasma -- 93
ch. 4. stability -- 14o
Ch -
Ch.
5. Certain forms of motion of a continuous medium -- 200
6. Magnetohydrodynamics of the galaxy and stars -- 259
Ch. 7. Magnetohydrodynamics of the sun -- 308
Conclusions -- 394
Internation system of units -- 396
398
FM co-,,,~
I . 201 SUBM DATE: igmar66/ ORIG REF- 161/ OTH REP: 170

ACC NR- APM01506 SOURCE CODE: UR/0033/66/043/006/lil-)/1142
AUT11OR: [Avshits, M. A,; Obridko, V, N.; Pikel'ner, S. B.
ORG: I ris t i t uL c of Terrr-sLrial Magnettsm, Ionosphere, and Radio~:-tve Propaga' 1111"',
AN SSSR (In-L zemnogo magnetizma, ionosfery i rasp ros t raneniya radiovoln A!~ -~,;SR)
State Astronomical Institute im. P. K. Shternberg (Goa. BBtronomicheskiy In-,)
TITLE: Radio emission and atmospheric structure above sunspots
MURCE: Aqtronomicheskly zhurnal, v. 43, no. 6, 1966, 1135-1142
'TOPIC TAGS: radio emission, sunspot, 1,hut(,sphere, chromosphereIA 1 f ve!i C! ;3 1
!corona
IABSTRACT: The circularly polarized radio emission on centimeter wave Jettj~lh: front tile
iregions above sunspots requires the presence of a magnetic field It 1, 1000 G ind ,)ronal'
Memperature a, 106 K. Direct observations of magnetic fields in the photosphore atid
jehromosphere as well as theoretical considerations on intense broadening oll I Lube of
lines of force in rarefied atmospheric layers show that field strength of 11 '-'- 1000 G is
found only at heights not exceeding 3000 km. This implies that tile corona iloparently
begins at a small height above spots. A model of a radio source it; computed using the
radio spectrum of sources and data on circular polarization. llydroatatic density dis-
tribution is assumed. The radio data allow reliable determination of tempvraLulc ('11
1height. The sharp boundaries of the source, its radiation directivity, and Ito coln-
Card l/ 2 UDC: 523.746

ACC NR: kP7001506
cidence with umbrae are also explained. The difference betweeti the chlrtnoq):~c~ri, a~,ove
!the spot and nor-mil chromosphere is associated with small dissipation of AlIveri and
!accelerated waves in a strong field. I'he slow (sound) waves fade in the low (hromo-
spheric parts, where they do not cause noticeable heating. Apparently on1v accelerated
:waves reach the corona, where they are transformed into other types of waves and fade
;at great heights. From there, the energy is passed by heat conduction to the low
,parts of the corona responsible for radio emission. Orig. art. has: 2 formulaH,
12 figures, and 1 table.
I
.SUB CODE: 03/ SUBM DATE: 22Mar66/ ORIG REF: 016/ OTH REF: 009
Card 2/-2

A _V" 7.1,TY,

PRELIM, S.B.
. q, .
G.A. Shain (1892-1956). let.-aetron, 1681. no.3:551-607 '57.
(Shaln, Grigorti Abramovich. 1892-1956) (MIRA 11:1)

?I!ML'JUQ-
Symposium ot radio amtrouonW. Top. koem. 5:279-?82 '57.
(Jodrell Bank, Ingland-Radio AstronoNW-Comeresses) (Y,;..rtA -.~ 9)

AUTHORs Masevich, A. G.
TITLEt The Problem of Cosmic Gasdynamics.
In International Conference in the USA.
(Problemy kosmicheskoy gazodinamiki.
Mezhdunarodnaya konferentsiya v SShA.)
30-11-23/23
PERIODICALt Vestnik AN SSSR, 1957, Vol. 27, Nr 11, pp. 140-143 (USSR)
LBSTRAM The physicists# interest ih these problems has constantly in-
creased, as the problem of the acceleration of cosmic rays and
their lives in the space of the galactic system, as well as
the investigation of the formation of interastral magnetic
fields is closely coni.ected with the motion of the so-called
interastral gases. Representatives of astronomy, physics and
mechanics met in Cambridge (Kembridzhe)o UBAI this was the
third international symposium devoted to problems of cosmic
aerodynamics. The report by the Dutchman Van der Kholst (ob-
mervations of the radioemission on the 21 am wave) caused
great interest. G. Vokuler (USA) reported on the observationB
made in Australia of the spiral structure of the galactic
system. 0. Vilson (USA) dealt with the new research data regar-
ding the inner kinetics of the planetary nebulae, G. Myunkh
Card 1/3 (USA) with the internal motions in the nebula of Orion,

The Problem of Cosmic Gaudynamics.
30-11-231/23
R. Minkovskiy (USA) reported on the investigation of the
group of fiber-like nebulae in the Swan, R. Devis (England)
thoroughly examined the physical conditions in the gas-dust
clouds on the basis of the most recent results of the observ-
ation of radio-radiation. Much attention in reports and dis-
cussio" was paid to the problem of the dissipation of energy.
Kh. Petchek (USA), L. Birman and A. Shlyuter (German Federal
Republic - FRG) talked on this topic. Some speakers dealt with
the nature of the magnetic field of the spiral extensions of
the galactic system. Very great attention was paid by the
conference to the problem of the gas-corona and of the forma-
tion of the radio-radiation (S.B. Pikellner). V.A. Ambartsumyan
talked on the genetic connection of-y_o-u-ng___Wtars with the di-
ffuse environment. By means of observations made he rejected
the hitherto existing assumptions with regard to the formation
of the stare from an interastral substance. The members of the
sovist delegation made themselves acquainted with the instit-
utions and the organization of the optical observations of
artificial earth satellites in the USA. The delegation visited
the astrophysical observatory in Cambridge (Massachusetts) and
Card 2/3 a number of other scientific institutions in the USA. Then the

The Problem of Cosmic Gaodynamics.
30-11-23/23
report deals with the details of the optical observations
of the artificail earth satellites in the USA. The delegation
showed great interest for the nr--nization and equipment of
the Numuhusetts Institute of Techpolosy.
AVAILABLE: Library of Congress
Card 3/3

AUTHORS: Pikel'ner, S. B. and Shklovskiy, 1. S. 497
TITLE: An investigation of the properties and energy
dissipation of the galactic halo. (Isaledovaniye
svoystv i dissipatsiy energiy gazovoy korony
galaktiki).
PERIODICAL:"Astronomicheakiy Zhurnaln (Journal of Astronomy),
1957, Vol-54-1 No.2., pp. 145-158 (USSR)
ABSTRACT: The distribution of the sources of nonthermal radio-
emission of the Galaxy is discussed. The division
into a homogeneous sphere and an "Oort-Westerhout"
sub-system is artificial. There is some concentration
of emission towards the plane and centre of the Galaxy.
The strength of the magnetic field,in the upper
(Hl','~3-10 t)) and'lower (H-;*6.l0-'j) layers of the
halo is estimated from the distribution of radio-
emission and two hypotheses: 1) the concentration of
cosmic rays is proportional to the field strength,
2) in the upper layers of the halo the magnetic
pressure is about the same as the pressure of cosmic
rays. The pressure of the magnetic field and cosmic
rays at the height z-10 kps is balanced by the
weight of the upper layer. Fro% thi condition the
density of the layer n> 0.6-10-4 cm-S is estimated.
Evidently the gas pressure does not play an essential
role in supporting the halo. To keep the cosmic rays
the field of the halo must be irregular. Hence the
strength. Some examples of halos, with incomplete
ionization and in rapid motion, are given. The Large

497
An investigation of the properties and enerry
dissipation of the galactic halo. (Cont.)
Magellanic Cloud is surrounded by an extenGed n&lo ~ cm-3
having a neutral hydrogen concentration n , 8.1u
on the periphery. High velocities did noL lead to
great ionization in the nucleus of our Galaxy, eviaently
because of the action of the field. Recent radio
observations show that the Coma cluster of galaxies
is surrounded by a halo, with a radial velocity
dispersion - 50u km/sec. The motions are undamped
and do not lead to a complete ionization of the gas,
because of the magnetic field. Radio observations at
low frequencies of galaxies 4enabled the esLimation
of n e--,j 0.01 and T - 10 in the lower layers of
the halo. 29 references, 11 of which are Russian.
Crimean Astrophysical Observatory,
Ac. Sc., USSR.
State Astronomy Institute
imeni P. K. Shternberg. Recd. Dec.11, 1-1L,-).

F L
AUTHUR: Pikel'ner, S. B.
33-3-2/32
TITLE: Energy dissipation, heating and ionisation of i9terstellar
gas by shock waves. (Dissipatsiya energii, nagrev i
ionizatsiya udarnymi volnami mezhzvezdnogo gaza).
PERIUDICAL: "Astronomicheskiy Zhurnal" (Journal of Astronomy),
1957, Vol.34, No-3, pp-314-327 (U.S.S.R.)
ABSTRACT: In a previous paper (1) the author argued that the rare-
fied gas in the Galaxy is in the state of rapid motion and
fbrMB a spherical sub-system. However, Spitzer (2) has
pointed out that at ultrasonic speeds the kinetic energy of
the gas is rapidly dissipated into heat. The spherical gas
sub-system was discussed in another paper (3) where it was
shown that 6the field strengths in_g spherical system are
-1 6 x 10 Oersted and -,%,3 x. 10 Oersted in the upper and
lower_~ayer~ respectively, the mean gas concentration being
10 4 cm-2. The latter falls off with increasing radius.
It was also shown in that paper (3) that the presence of a
ma~pietic field whose energy is comparable wita the kinetic
energy of the gas should lower the dissipation of enerb-y.
atle 3./4 In the present paDer the d-issipation is calculated and
estimates are made of the heating and tnermal ionisation of
the gas due to magnetohydrody-namic shock waves.

33-3-2/32
Energy dissipation, heati J25 and ionisation of interstellar
gas by shock waves. (cont.
For simplicity, only perpendicular waves are considered,
i.e. waves in which the magnctic lines of force are parallel
to the wave front. It is shcwn that if, on the average,
the magnetic energy density is equal to the kinetic energy
density and is much greater than the thermal energy, then
the motion takes place with the velocity of sound and shock
waves are very weak. Rext, the effect of cosmic ray
pressure is estimated. In the galactic conditions the
cosmic ray pressure is of the order of the field pressure.
It is shown that the irreversible energy dissipation is
given by: q = 0. 044 E
iQ - 0. 040 E
where the first expression is derived by taking into account
the cosmic ray pressure and the second by putting pc.r. = 0;
B is the energy of the wave (magnetic + kinetic)
per gram. The velocity of motion of the gas, calculated
Caxd 2/4 by taking into account the cosmic ray pressure Pe.r. , is
subsonic:-
cl--%& 1-3v

33-3-2/32
Energy dissipation, heatin and ionisation of interstellar
gas by shock waves. (Cont.~
to estimate the temperature of the gas, or the degree of
ionisation of hydrogen, from observations, then the
calculations carried out in this paper could be used to
estimate the magnitude of the energy dissipation and to
obtain more accurate values of n and H. In the absence
of the field H, & Q and & T will be higher by a factor
of 20-30. In this case the first wave ionises the gas by
30 to 4M- and subsequent waves almost complete the
ionisation.
There is one table and 8 references, 5 of which are Slavic.
SUBMITTED: December 11, 195c.
ASSOCIATIUN: Crimea Astrophysics Observatory, Ac.of Sciences USSR.
(Krymskaya Astrofizicheskaya Ubservatoriya Akademii Nauk SSSR)
AVAILABLE: Library, of Congress
Card 4/4

1\ F v Toprogy kobsogm14 t. 6 (Problems In Cosmogony. V41. 6) Moscow,
Isd-vo AN SSSR, 1958. 367 P. 2,000 copies printed.
Sponsoring Agencyt A)r&4a&17a nauk SSU. AstronamIchowdy worst.
ARTICLU
Flagaltekly. W.A. Ca Uw Origin and fralatIce of ContLemU
arA O"ans 5
at,, V.1 latest Data in Determining the aar".8
ute 40
39
&*via, B. To. History of the Mom's Platatice =6 tkw
Meologleal Properties at Its Material 6
Safronov v. a. on the orowth or Terrestrial namets
~~)Alfvam. L On the Origin of tkW Solar 37219m
R1W A. Ta. wA14%oTlyt. DIslAtegratlem Preseason
t
ru
ati
i
im n
Eli;t
d
a
*swe
es
Quas
n
ai
v
0
"
s M
r
&
*
b
l"
V
u
SGb:
1~
v
ah
Ies of Planstary Nebulas
.
a
Oursadyan, O.A. Dynamles of Planetary Nebulas 15T
HIMA, I.M. Light Pressure and Uw Dynamic* of namstary
Nebulas 211
Agek7an, T.A. Interaction of Stars with Dimas Matter 222
Kaplan, 3. A. Magnetic Gas Dynamics and Prc,&ImW of
CoamogM7 238
PArkhomanko, P.O. On the Preservation of Contimammas
in the Pormation or ziewate 265
Parkh=�31kD P.O. Determinizz the Location or me -W-
P=d*rdMt* Theramwelma
M
Cl
r
o
um
ft"k-OLIP-r, 3-D. On the Tboories of the -WpvMdgrG&%- 269
273
In". 0- TU ft&tD Of Cosmology Today
R]LPORT3
MakarkLA, B-V. Conference cc Variable Stare apmas,
by ths Hungarian Academy of 3clenceo sma Bold in
Budapest an August 23-20
1956
,
Tarletaidy. T&. P. ayMoat- cc ftobjew In gimstpa. 333
magnetic Phemomema 3A Conde nVaLas
IbOlo
o
P
M
C 34
.
.
w.
ocrevense so Nor'n"d star*
p
V&PQftt90w-VGI1yam1ftvv, S.A. Coaferense an %be rhysiss 3
of Plow" mmudse 354
SUBUI, To. L. Conference at the Committee Co cc
60W
Dbvbted to RUXWM the PossIbIlitles at tm =
ve man
cc Extrawastis Astrononq " Coamc~W
812 !
3
h,
.
IC&I Coevers"s 3

4 ~_J_LJ,116
-AUTHDR: Fikellnev, 8,B.
TITLE: _ThEsa~sic C~oncep~s of Magnet o-Hydro dynamics .(Osnov-nyye
ponyatiya magnito-gicirodinami i)
PERIODICAL: Izvestiya Akademii Nauk SSSR, Seriya Geofizicheskaya,
1958, Nr 1, pp.46-53 (USSR)
ABSTBACT: This is a review paper giving a brief exposition of the
ideas lying at the basis of magneto-hydrodynamics and in
particular, the effect of the motion of the medium on the
magnetic field and the effect of the field on the medium.
The equations of motion of an ion and electron gas are
formulated in Eqs.(4) and (5), taking into account inter-
actions between them and following Schluter (Ref.1). On
the basis of these equations it is shown that if the plasma
is dense and the field not very large then the component of
the electric field relative to the system moviz4,r with the
gas and perpendicular to the magnetic field gives the same
current density as in the absence of tLe electric field.
If the contrary is the case, then the current in the same
direction is very much less and there appears a much
stronger current density component perpendicular to both
the above electric field e and the magnetic field H
Car,l 1/3 However, these are only very special cases. Next, the

11,)- 1 -4/16
The Basic Concepts of Magneto-Hydrodynamics.
attenuation of a magnetic field in a hard conductor is
considered, following Cowling (Ref.?). An expression for
the rate of change of the magnetic field as a function of
the velocity of the medium, the magnetic field itself, and
the conductivity is derived in the usual way and the signi-
ficance of the various terms entering into this equation is
discussed. The basic theorem of magneto-hydrodynamics is
then formulated in the form: in a fluid with an infinite
conductivity (or with a finite conductivity but sufficient-
ly large characteristic dimensions), the magnetic flux
through any material contour remains constant during motion.
A discussion is given of magneto-hydrodynamic waves and it
is pointed out that they play a major role in cosmic
physics. Above all, they give a simple method of increas-
ing the field via the transformation of kinetic energy in-
to magnetic energy. Furthermore, they appear to be the way
by which energy is transmitted over large distances. By
means of these waves, energy is apparently transmitted from
sub-photospheric layers to the upper layers on the Sun.
There, the energy is transformed into heat and constitutes
Card 2/3 one of the main reasons for the high temperature of the

4 -)-i-4/ 1(-)
Basic Notiolas in Magneto -Hydrodynamics.
chromosphere and the corona. A mention is made of the wc-r1k
of Kaplan (Ref.10) and Kipper (Ref.11) who developed tkie
theory of turbulence in the magneto-hydrodynamic case.
Howeverp these phenomena are very complem and have only
been investigated in a first approximation. Somewhat
simpler phenomena are those connected with magneto-
hydrodynamic shock waves which were considered by Hoffman
and Teller (Ref.12) and Helfer (Ref.13).
There is 1 figure, 1 table, and 13 references of which 7
are Slavic.
SUBMITTED: May 14, 1957.
AVAILABLE. Library of Corpress.
Card 3/3

PIXEw nu
,"Oov
Theory, of the 'equilibrium' origin of elements. Vop.kosm. 6:271-276
158. (MIRA 11:10)
(cosmogony)

PIKEL11M, S.B.; ?CTIK. L.P.
,an cloudn. Izv.
Anisotropy of velocities of interstnilar I;
Krym.antro'fiz.obser. 18:198-201 '58. 0141Rh 13:4)
(Gases, Interstellar)

3(") Mk'A' I BnOK EXTIDTTATION SOV/3236
Pikellner, Solomon Bori-sovich
Fizika mezhzvezdncry aredy (Pt,yBir-z of' the Matter) Moscow,
Izd-vo AN SSSR, 1959. 215 p. ('74--ries: Akade-nlya nnW; S53B. Nauchno-
populyarnaya. serlya) 12,000 roples printed.
Ed.: V.G. Fesenkov, Academician; Ed. of Publishing HcruBe: Yu.1. Yefremov;
Tech. Ed.: L.A. Sushkova.
PURPOSE: This book is Intended for the general reader interested in astronomy.
COVERAGE: This is one of the popular science books devoted to Interstellar
matter. It gives background information on the stars and on our galaxy,
and explains the various complex processes taking place in Interstellar
matter and their relation to the processes In stars. It is concl-aded
that interstellar matter is closely associated vith the origin and
evolution of the stars. No personalities are mentioned. There are no
references.
Card I/# /

FMLIM, S.B.
Genetic relatton of star@ of various subsystems (with summary In
Inglish]o Izv,Zrym.astrofts.obser. 21:209-614 159. (MIRA 13:6)
(Stars)

AU'7'"O'~
1'ikellner, 3.B., Shklovskiy, I.:;. V 7
- . Ivanov-Kholodnyy, G. S.
TITLE: On Possible 1-'echanisms of Emission of Discrete Galactic Ob-
jects in the Spectral Region 1225 - 1350 X
PERIODICAL: Astronomicheskiy zhurnal,1959,vol 36,Nr 2,pp 264-268 (USSR)
ABSTRACTt The authors examine the possibility of explaining the emission
of discrete galactic sources, observed in the spectral region
1225 - 1350 A , by usual mechanics. However, this explanation
requiresthe assumption that the absolute value of brightness
of galactic sources in this spectral region were considerably
overestimated. The measurings of the H cc line necessary for
the investigation were carried out by R.N. Shefov and V.S.
Prokudina in the Zvenigorod station of the Institute for At-
mospheric Physics of the Academy of Sciences TISSR.
There are 9 references, 3 of which are Soviet, 3 American, and
3 English.
SUBMITTED: October '17, 1958
Card 1/1

A ( 7 )4
AUTHOR: P. 30V/56-36-5-37/76
T'.'TLE,- Th,!, 9 ~, --j o Yegrt~ -?.ohydrodynami c Shock Wave in a
P&-.fa'ly 1_):Az,,Q Gzx i3truk-~ura magnito-gidrodinamicheskoy
-1
-;ai-ncy vo-,%y ionizovannom gaze)
PERIODICAL~ ZAW-)h_. teoreticheskoy fizik.111959,
V~'._ ~f N7. 7, PP l'-36-154 ~UBSR)
ABSTRACT Tha fo.~lowing ?roblem io theorati3ally investigated in the
pspsi.- Vn ari only ps-rLlally ionized gas, which is
e.sir=ed tc It in a wa&i(itic fi,~'.d, a "piston" is assumed to
m,-ve in Ai Is to the H 0 -direction,
&r,d that produces a plane wave. Interaction between
-ed at,~,ms is assumed to be negligible, and two
is And yie~:ti
wa,~-es -7her, away 'L-~-)m the 'piston", the magnetohybmdyzxdc
onve In the :~Iasma and the orddna.-y one in the neutral gas. If
`h,~- f-5-,t ~Tariov.E, ldnda of purtieles have the same
j6Tp~~t:8SiO.71 Jn *,h#s plasma is lower than in the
th.! pr-_!se:nue of the electrons and
(--,f ra~q~r_t_'r, p-eEiaL_-0. In the case of gases having the
Card 1/3 s,~xno_ (in 10he, "laboratory system"), the wave front will,

The Structure of a Sho-~;- Wave :Ln a SOV/56-36-5-37/76
Ionized Gad
~rev m)ve- Y,,'-th greater speed in tne plasma than in the
bellow 100,0000 and 4 the case of
1 -,% I --.ni a ;11ro wheii the free lenft of path of
, n 'LOO oi 1000 -.i~jiwya less than theit of the neutral atoins,
+hV Stf-Jr,"OL e ~Ii Vio E,~,)~k .Fv(! is invmstigated within the domair
mo-i-_ or-,u..3 variation of the parameters. The
a~~o(,k wav,- In arach a gas consists of a thir.
&arm ac -,n'ini-. ty Lnd. a tranoition zone. Proceeding from the
if mcti..)n ir a sys-;am of coordinates that is
,-.ovne_-t,ed vril,~ -Oie fruxrn_ the aut.!ior derives an approximated
~f tne !'o:- tao turaLsltion zone with respect
A
'-f Kgi `-4). It is found that the charge
&k_1..hJ1Ar1 if~,-6cf, axezc's-s ~f,senttal influence upon the gene-r-.1
-,I' mo,.- in, L-.- ~. 'L-L reauoes the Beale. As long
the we.,e mev be considared to be steady within the zone of
-cran.cj't_or., the ordtr of nialmitude of energy dissipation is
indepene-ent cf the degroe of ionization. The author finally t
Ya. B, Zel'dc,~ich for 1-ds valuable remarks. There are 4 fimiret,
Card 2/3 And 7 -references, 3 of which are 3oviet.

The Structure of a Magnetoohydrodynamic Shook 'gave in a SOV/56-36-5-37/76
Partially Ionized Gas
ASSOCIATION: Krymakaya aBtrofizicheskaya observatoriya Akademii nauk SSSR
(Crimean Astrophysical Observatory of the Academy of Sciences,
USSET
SUBVITTED: November 30, 1958
Card 3/3

AUTFOR: S. E.
T i T !-I--- L-ette- -o th. Ed o- Gz v
Sound
PERIODICAL: n oy I t,~ o i t.,
Vc ' i-.' pp -18-17-]F~,'~, (TY--i,)
ABSTRACT- -~I( pll op~,.,,,'A-'o -~ o!' :io-ma th-ouf-,h th,
y Cow- di , ~d , t~~c ord A rif, to r- ~I lip-
!Ty(lr~)dynam-l - T,

,-- ~ - r, .. - - "r 7,~ 1 . " ., . ,
- - r. - - -:1 '7 , - -

Letter to the Editor. Grav!~atlona! 77011
Attenuation of Sound
The weakening of the flow is defined b:i the
lifting the gas:
d (rc-1)I(/-' ----
From this it fol ows that
This means "hat w.1thl n the of
atmosphere (,L~ z
extinct-'on '-s t r,:
extinc,fon ,XP(-nent_,a,
p_~rt- Ic ipated in t~r~ d -Iscussicn of5
The -,e a-k~ 2 Soviet -efercnces, .
ASSCCIATIOY: ~-_'~nean AstrDp-ys 0 b s -a t o ryc

Q -7
Ca:-d 4/,,

-PIKELIZIERO S.B.v-red.
[Third Symposium on Coamical Gas DynamicB; June 24-29, 19571
Tratil sinpozium po tossicheskoi gazodinamike, 25-29 iiunia
1957 gods. Pod red. i a predislovier S.B.Pikellnera. Moskva,
Izd-vo inostr. lit-ry.) 1960. 360 p. (MIRA 14:10)
1. Symposium on Cosmical Clan Dynamics, 3d, Cambridge, Mass., 1957.
(Astropbysice) (Aerodynamics)

PIKUI NER, Solomon Borisvich
Physics of the interstellar mediwn. dright-Patturson Air force Ba~~e,
Prepared by the Liaison Uffice, Techical Information Center, 1960.
1, 224p. il;us., diagrs., graphs, tables. (MCL**66Vl--I,)
Translated from the original Russian: Fizika mezhzvezdnoy sredy.
Moscow, 1959.
Bibliography: p. 222.

89803
S/169/61/OW/0G3/G2.!/_-22
6 0.? V V/j AGG5/AOG5
Translation from: Referativnyy zhurnal, Geofizika, 1961, No. 3, p. 44, # 3G352
AUTHORS: Dvoryashin, A. S., Pikellner, S. B.
TITLE: On the Fine Structure of the Sudden Beg Ing of a Magnetic Storm
PERIODICAL: "Izv. Krymsk. astrofiz. observ.", 1960, Vol. 22, pp. 144-149
(English summary)
TECT: The momentary decrease in field intensity (pri) preceding the magne-
tic perturbation with sudden beginning may be caused by the dynamoeffect connected
with the increase of ionization of the lower ionosphere. The compression of the
magnetic Earth's field which begins at a distance of about 7 Ro propagates with
the speed of a magnetic-hydrodynamic wave. Simultaneously, the energy of the fast
particles surrounding the Earth (induction acceleration) increases. These partic-
les moving along the lines of force reach the polar regions of Earth and there
they increase the ionization. It is possible that the perturbation furthers the
permeation of particles into the atmosphere. The increase In energy of particles
reaching average latitudes is less. Hence the latitude distribution (pri) is
explained. Author's summary
Translator's note: This is the full translation of the original Russian abstract.
Card 1/1

PIMIMM, S.B.
Reviev of "Interstellar gas dynamics" by S.A. Kaplan. Astron.
shur. 37 no.3:593-594 My-Je 060. (MIRA 13:6)
(Gases, Interstellar) (Kaplan, S.A.)

S/033/60/037/cD4/002/012
AUTHOR. Pikellner, S.B. E032/E314
TITLE: Mechanism of Formation of Active Regions in the
Pres.nnce of a Magnetic Field
PERIODICAL: Astronomicheskiy zhurnal. 1960, Vol. 37, No. It,
pp. 616 - 621
TEXT: In order to explain the presence of plages. floccull and
r.oronal rays, it must be assumed that the presence of a weak
magnetic field can lead to the amplification of motion in upper
layers of the convective zone. Since the convective currentq
have a large Reynolds number, they should be unstable and givi~ rj~,
to turbulence. Usually, the velocity of major turbulent pulqatici,
is of the order of 100,'v of the velocity of the main stream., Fcr
large Reynolds numbers, turbulent viscosity is much greater than
molecular viscosity and determines dissipative forces. The
appearance of convection '24determined by the Rayleigh number
given by; 9P
R - (V T V T)
Card 1/4 X~ ad

S/033/60/03 704/002/012
%31~EAII
Mechanism of Formation of Active eg o s in the Presence of a
Magnetic Field
where g is the acceleration due to gravity,
is the volume expansion coefficient which. for a ga-s
is equal to T_ 1 .
is the thickness of the layer, if it is thin or
comparable with the height of a uniform atmosphere
)L is the temperature diffusivity, and
NJ is the kinematic viscosity.
Convection will take place if R > 0 If the numbf-r
R~/,~ is large, say. of the order of 10 then stationarv
convection is unstable, the motion is unordered and cells ar(- net
formed. For lower values of this number, non-stationary conve-c-11"il
takes place, i.e. cells are formed but are irregular. Solor
granulation resembles this type of convection. It would theref-)rc
appear that R XAJ is not too high. However, a simple estimat(-
shows that R -%~ 10 10 and, moreover, e. C onv e:V
Card 2/4

S/033/60/037,604/002/012
EO~2~E~11
Mechanism of Formation of Active e i ns in the Presence of a
Magnetic Field 12-'
cells should not be formed on the SUp at all, Schwarzschild
(Ref.13) has pointed out that this contradiction can be avoided
by using N) turb instead of V. The former is larger by
several orders of magnitude and hence R is relatively low.
Moreover, X is only slightly greater than \j turb ' " that if
convection is present it must be quasi-stationary. Thus, the
velocity of convective motions is determined by the equilibrium
between the upward forces and the turbulent viscosity force. if
the viscosity is reduced, the upward velocity should increase.
The intensity of a weak magnetic field is not sufficient to have
an effect on the convective stream but may influence turbulence.,
A few tens of Oe should be sufficient for this mechanism to takc-
place. It is argued that any field, independently of its origin
and character, should give rise to active regions whose properties
depend only on the field strength. In particular, a weak field
tends to decrease dissipation and increase convective velocity
Card 3/4

S/033/6o/037,4o4/002/012
E03fi/E314
Mechanism of Formation of Active egions in the Presence of a
Magnetic Field
since, as mentioned above. it does not affect the main stream
but damps turbulence This is illustrated by polar plages which
are closely connected with the Sun-s -)olar magnetic field The
low value of the latter field is the reason for their low
brightness and the great depth of the upper boundary, Heating
due to polar plages gives rise to polar coronal rays and possiblv
the permament solar wind. Complicated spectral variations in
magnetic stars may also be related to the influence of the magnetic
field on convection. There are aO references 5 English
6 German. I Swedish and 8 Soviet.
ASSOCIATIONi Gos, astronomicheskiy in5titut im P,K Shternber 'ga
(State Astronomical Institute
SUBMITTED. Aptil 10. 196o
Catd Li/4

PIKELINER, Solomon BorisovichiKULIKOV, G., red.; LUIUCOVA, L., tekhn.
rea. --
[The aun) Solntse. Moskva, Gos.izd-vo fiziko-matem.lit-zT, 1961.
82 p. (Popullarnye lektsii po astronomii, no.11) (MIRA 15:1)
(Sun)

PHASE I BOOK EXPLOTTATION SOV/5732
Pikellner, Solomon Borisovich
Osnovy kosmicheskoy elektrodinawiki (Principles of Cosmic Electro-
dynamics) Moscow, Fizmatgiz, 1961. 295 P. 5POOO copies printed.
Ed.: B. Ye. Gellfgat; Tech. Ed.: L. Yu. Plakshe.
PURPOSE: This book Is intended for nonspecialists interested in
cosmic electrodynamics.
COVERAGE: The book is an attempt to present in a systematic and
simple form the fundamentals of cosmic electrodynamics and their
connection with astro- and geophysics. The main emphasis is on
physical rather than on mathematical concepts. 'The author thanka
D. A. Frank-Kamenetskiy and S. I. Syrovatskiy for their advice,
A. B. Severnyy for his photographs of solar formations, and B. N.
Gershmar. and R. Z. Sagdeyev. There are 258 references: 135
Soviet, 95 English, 14 German, 7 Swedish, 2 French, and 5 other.
Card-1/_4

89319
S/033/61/038/001/002/019
7 3 2-6, // Z 7.,// 2.17) E032/E314
AUTHOR: Pikellner, S.B.
TITLE; Th`eiff7elt ;fcl~lml --Rays on the Character of the
Magnetic Field and the Formation of Filaments in the
Envelopes of Supernovae
PERIODICAL: Astronomicheskiy zhurnal, 1961, Vol. 38, No. 1.
PP. 21 - 27
TEXT: In the plane of the Galaxy the cosmic-ray and magnetic-
field energy densities are roughly equal. 1.S. Shklovskiy
has frequently pointed out that this cannot be accidental it
is possible that this is connected with the retention of
cosmic rays. Radio data show that magnetic fields and cosmic
rays are also present in the galactic corona but the intensity
of the radio emission gives only the retktion between them.
The quantity KH 1.8 is roughly 20-30 times smaller
the"disc" (K is proportional to the concentration
particles or their energy). in a previous paper (Ref.
present author and Shklovskiy assumed that both K
decrease so that the energy balance is preserved.
Card 1/8
than in
of the
5) the
and H
Kahn and

89319
S/033/61/038/001/002/019
E032/E314
The Effect of Cosmic Rays on the Character of the Magnetic
Field and the Formation of Filaments in the Envelopes of
Supernovae
Woltjer (Ref, 6) assumed that since the distribution of cosmic
rays it, a closed stationary system should be uniform, only
H decreases. In that case, the particle energy should be
5-10 times greater than the magnetic energy. Hoyle (Ref. 7),
on the other hand, considers that the cosmic-ray energy is
several times greater than the magnetic energy. The problem
therefore arises as to whether the retention of the cosmic
raysis possible. The present author argues that the magnetic
energy should be comparable with or greater than the cosmic-,
ray energy. Moreover, magnetic forces should be comparable
with the cosmic-ray pressure gradient and hence the field
cannot be force-free in the entire region if the cosmic-ray
energy is comparable with the magnetic energy. The
equilibrium of' gas in gravitational and magnetic fields is
described by~
Card 2/8

~93i~
S/033/61/038/ool/oo2/oig
E032/E314
The Effect of Cosmic Pays on the Character of the Magnetic
Field and the Formation of Filaments in the Envelopes of
Supcrnovae
(!g + 7 P + V p+rot H x H - 0 (1)
I k 41r
where p is the pressure of the gas
Pk is the cosmic-ray pressure,
9 is the acceleration due to gravity,
H is the magnetic field and
indicates that the gas is subjected to the
component of the gradient which is perpendicular
to H .
The problem is therefore reduced to the investigation of the
stability of this equilibrium for P < Pk and
H2"Ti< Pk - If the system is stationary and cosmic rays
are retained by it, their density should remain constant.
Card 3/8

89319
S/033/61/038/001/002/019
E032/E314
The Effect of Cosmic Rays on the Character of' the Magnetic
Field and the Formation of Filaments in the Envelopes of
Supernovae
In this case V p k = 0 inside the system but at the boundary
the gradient increases considerably. However, the Galaxy
is hardly a closed system with sharply defined boundaries.
Ginzburg and Syrovatskiy (Ref. 8) have shown that the
chemical composition of cosmic rays and some of their other
properties can only be explained if it is assumed that the
particles do not return to the plane of the Galaxy from its
boundaries, i.e. that they gradually diffuse in the outward
direction. In this process, the particle density gradually
decreases and ~7pk / 0 inside the galactic corona. More-
over this result suggests that the field inside the Galaxy
is not quasiregular and curving only at the boundaries
since otherwise the particles could easily be reflected back
into the galactic plane, If the cosmic-ray density decreases
Card 4/8

`9319
S/033/61/038/ool/oo2/oi9
E032/E3i4
The Effect of Cosmic Rays on the Character of the Magnetic
Field and the Formation of Filaments in the Envelopes of
Supernovae
gradually within the corona, then the equilibrium of the gas
is only possible if the lines of force are sufficiently rigid
so that the magnetic force (last term in Eq. 1) should not be
smaller than 7p k * This defines a lower limit for the field
strength and means that the field cannot be force free in the
region where the cosmic-ray density is not constant. Inside
a closed system the cosmic-ray pressure should be constant
but should decrease within the limits of' a thin transition
layer, In order to retain the cosmic rays a large force
concentrated in this layer and directed inwardly is necessary,
If the magnetic energy is smaller than the cosmic-ray energy
then even in the case where the magnetic force is concentrated
in the transition layer it cannot balance the particle pressure
and the latter will penetrate the layer in the outward direction.
As a result, the system will cease to be stationary and closed,
Card 5/8

89319
S/033/bl/036/001/OU2/019
E032/E314
The Effect of Cosmic Rays on the Character of the Magnetic
Field and the Formation of' Filaments in the Envelopes of
Supernovae
the cosmic-ray density gradient will appear and the instabilitv
will be propagated in the inward direction, Even when the
magnetic energy and the particle energy are equal, the
transition layer will only be able to retain the cosmic rays
when the magnetic force is comparable with the pressure
gradient. A force-free field within a closed system should
give rise to surface currents responsible for the discontinui~v
in the tangential component of the magnetic field, These
currents cannot compensate the pressure due to relativistic
particles since for these particles the magnetic force is
also equal to zero. A single force-free field of the type
described by Woltjer (Ref. 11) for the Crab nebula would be
unable to retain the cosmic rays in the nebula. Retention of
the cosmic rays is only possible because the filaments are
massive formations capable of withstanding the pressure upon
them, Thus the cosmic-ray density in the galactic --orona
cannot6Y constant because tiiis wou Id Icad to instabi lity
Car

S/033/bi/o38/ool/002/019
E032/E314
The Effect of Cosmic Rays on the Character of the Magnetic
Field and the Formation of Filaments in the Envelopes of
Supernovae
at the boundary where all of' the cosmic-ray pressure
gradients would then be concentrated. Since a cosmic-ray
pressure gradient should exist insiae the corona,the field
in that region cannot be force-free and quasiregular. In the
envelopes of supernovae the cosmic rays are enclosed and
their pressure gradient at the boundary is large, The
main mass of theawelopeis also concentrated at the periphery
and if a tangential field is present a peculiar type of
instability is produced, in which the field is forced out
by cosmic-ray pressure in the form of isolated loops and
the gas is ejected by the accelerating field along the lines
of force and forms filamets. The curvature of the arcs formed
by the lines of force between the filaments suggests that
the magnetic and cosmic-ray energies are roughly equal,
In principle, the cosmic-ray pressure can be determined
from the condition that it is equal to the pressure in
Card 7/8

89319
S/033/61/038/001/OU2/019
E032/E314
The Effect of Cosmic Rays on the Character of the Magnetic
Field and the Formation of Filaments in the Envelopes of
Supernovae
interstellar gas condensations which are
envelope. Such condensations have been
in Lassiopeia. However, a detailed calculation
become possible when photometric data on
available, There are 14 references: 5
9 non-Soviet.
observed within the
found in the source
will only
the spectrum become
Soviet and
ASSOCIATION: Goa. astronomicheskiy institut imeni
P.K. Shternberga (State Astronomical Institute
imeni P.K. Shternberg)
SUBMITTED: September 17, 1960
Card 8/8

1.!3.; pa~Ll: 'I" j.".
--
On ',.' c--l- I- article c,: - clio Lci.:-c :..I' J G: .
' :* 3j c.- 1 1, - - "11. "
z a. r E .~ . i:JC,6-11 [ Ja-7 Ia. ( 7. 1
(;Lltr(.Ilc,!:Y)

- PIKELINER., S.B,
Formation of corowd condenoations a+e active regiona. Astron.zhur.
38 no*3:552-553 MY-Je 1619 (VM 14:6)
1. Gooudaretvennyy astronomicheskiy institut imeni F.K.Shternberga.
(BuD--Corona)

V,71L'NIKOV, O.A.; UHL'NER, S.B.
"Course of Practical -strophysics" f~y D.1A.Fart *ynov. Rpviewed ~'v
O.A.Me.Vnikov, S.B.Pikel'ner. Astron.zhur. 3P no.5:10(14-1Vr(
S-0 (I. (MIRA 14:9)
(Astrophysics)
(Martynov, D. IA.)

PIKELINER, S.B.; KOGANS V.I.
OPhysical processes inside stamm by D.A.Frank-xamenatilkii. Reviewed
by S.B.Pikellner, V.I.Xogan. Uap.fia.naak ?4 no.1:181-18.4 iV
o61. :. (KERA 14:6)
(Astrophysics) (Frank-Kamenstskii., D.A.)

0 42
%1523/090/0 .3/00.5/0

S/03 VUZ/03 9/006/00't /0~-' 't
AUTHOR: Pikc-llner, S.B.
TITLE i Formation of a chrOITIOSP110riC net,~ork i,i,i tho
of the in.ignetic field
PERIODICAL: Astronantichesitty zhiirnn I , v. 19, no.h, 1962, ~7-)-)70
TEXT: A model is con.-,idered in which it is fibsmaod, for th,
sake of simplicity, that the lines of force passinS tht-oil.,;h a
section of the siirface are vertical. It is further supposed t1i it
there are two Inyers of convective cells. The upT)er layer ~;iv(-
rise to granulation nno the lowor one contains motioi)m
energy i- appreciably higher than the field energy so t;iot t;1- lo--
er layers deforming the lines of force, may be ignoreu. Ti.- ,i-
velocities in the cells are directed from the centre tt~ th~ (1-1~1-~'
fortaing close lines passing thr~jugh the lower parts of the c(-1 Is.
In this way tlv~ gas flows townrds the networl-, formt-(i 1j'. tliv
boundaries of thr, convective cells. This gives rise to a
displacement of the linen of force so that their number pcr unit
area becomes greater at tho!se boundaries. This "condensat ion"
of lines of force is transmitted in t)i-- forin of
dynamic waves into the upper layer itntl then to thf- photo,
Card 1/2

Formation of a chrot-riospheric 5/033/6 2/0!q/0o6/o(, If /o-,'i
r, 0 -12 /r 1. 4
chromosphere aii(I cor,ina. The arts aL~,) )rop;ii;atf_-(; it, -t
clownward direction -!wre t!ie ilvdi-o'lVililmit -Ire
tile magnetic forces so tiiat tiic 1:tttvr do ni)t dotf-rriiiiie f!i- i.
Judging fro.n the tiiitj of exist(~iice t)f f,i(. fiett-ork, t,1)(' (:!-.,ft -r-
istic time of oxistr ice of a cell 14 'Ibollt 2"1 11WIt'.4. Diii-i ; i i i
time tile gas i il a pa r t i cu I ik r c f, I I c twip I o t o.-3 a s i;ip, L v c y cI o
( revolu t i on ) a rid is w-w c P I 1 1) 111.,4 t,, fo riii i n (J v r) -n,: nii tI y' It:w
ori~jtial cell (,ion-st.-,tic) iory wivi-c t toji) . Tit(, litiefo; ol ,,. c
then redistrio.-te thei;tselve!, ag:iin into ri new net-oj-%. I t I
that tile I)er:L,i(; if Cie w.ives prop.-ivatirig iii tho . I ""( I
Is aboij t ;iwi i - . I',t1:111Y)CWl CIMVPC tit-11-1 IV-4 1-1.14V t-) .1 !1 1 1.1
in chromospheric ettii.4 iion and fiv,i( e tit(, notwork (_ovt,rii- tit,
surface of tit(, un accurrli,ice witli thf- ibokv I!, -11su
observed in Call ancl If Cx lines. rh e pro!.; Pric P C C. S ')!I tile
entire solar sur!.-cc i7l (jicatvs tilat .. wealk M.1trietic I'l (.11 1 i
present everywiiere.
ASSOCIATION: G0.9 . a S t ronomi chesk i V i 11.9 t i tit t im . p Sit t p
(State %Str-')?101T11c.1I lrititiite Iiiii-ni 11.1%. Slit -tw- r,~
SUAMITTED t ff , V 0 , 1 90
Card 2/2

PIKELINER, S.B.
Okerodynamic pbenomena in stellar Atmospheres; proceedings
of the Fourth SympcAium on Cosmical Gas Dynamics, Bologna,
196108 Reviewed by S,B. Pikellner. Astron zhur. 39
no.6:IIJ&-IIAI N-D 162. IMIRA 15:1-1)
(Stars--Atmosphere)

~A036547 BM EXPLOITATION a/
Kaplan, Savull Aronovich; Pikellner, Aft'low Awlauu.
Interstellar mediva (Mezhzvezftaya sreda),, Moscow, Fismstgiz, 1963v 531 P.
illus., biblio. Errata slip inserted. 3,50D copies printed,
TOPIC TAGSt Interstellar medium, interstellar g",,-interstellar bydrogen,,
interstellar dust, interstellar magnetic field, Interstellar gas dynavics,
galactic evolution, radio transadesion
TABLE OF CORMTS [abridgedli
Foreword 9
Ch. 1. Interstellar hydrogen - n
'Ch. Il. Physical state of Interstellar gas - 105
Ch. Ill. Interstellar dust - 191
Ch. IV. Interstellar magnetic fields and radio transmission - 277
Ch. V. Interstellar gas dynmioa and evolution of the Interstellar sedium - '1072
Appendices - 480
Bibliography - 510
cod 2./2

AN4036547
-SUB ODIZI No AS
281
LoctO
SUMTM
ACQS 06Ayr&
MR JW 3DVI

PIKELINERV S.B.; GINTSBURG, M.A.
Mechanism of type-2 bursts of Bolar radio emission. Astron.
zhur. 40 no.5t842-846 S-0 163. (KRA 16:11)
1. Gosudarstvennyy aBtronomfbht*kiy institut im. P.K. Shternberga
i Institut zemnogo magnetizma, ionosfery i radio AN SSSR.

KAPLAN, Samuil Aronovich; PIKELINER Solomon Borisovich;
=4 - Zl------,--, - -
AMBARTM-TYAN, V-.A., red.; KffSTELI , E..T1. Fea. ~ S-Vm"~-Y'
.9 p
A.B., red.; SOBOLEV, V.V., red.; i7~LlKcy, G.S., red.;
AKSELIAOD, I.Sh., tekhn. red.
[Interstellar medium] Mezhzvezdnaia sreda. Moskva, Fiz-
matgiz, 1963. 531 p. (MIRA 17:2)

ACCESSION NR: AT4019685 S/2555/63/009/000/0060/0069
AUTHOR: Pikellner,S. a.
TITLE: The diffuse medium and formation of stars and stellar systems
SOURCE: AN SSSR. Astronomicheskiy sovet. Voprosy* kosmogonil (Problems of
cosmogony), v. 9, 1963, 60-69
TOPIC TAGS: astronomy, astrophysics, stellar system, diffuse medium, star, star
formation. hyperon star, cometary nebula, globule, galaxy
ABSTRACT: Arguments in favor of the origin of stars from gas are given. Gravita-
tional condensation of systems of different orders is considered. The paper be-
gins with a refutation of the Ambartsumyan hypothesis that stars are not formed
from. diffuse matter, but from dense bodies of an unknown nature, possibly hyperon
stars. The hypothesis that stars originate from globules is explored next and it
is noted that cometary nebulae are an indirect confirmation of the validity of this
theory. The evolution of a compressing mass, real time of compression and inter-
mediate and extreme cases of compression are considered. The Importance of taking
.rotational and magnetic fields into account when computing gravitational compres-
sion is stressed. Star formation must be considered as occurring in large groups
.r..plusters,oot in an individual group of cluster; this viewpoint is emphasized.
Card 2

ACCESSION NA: AT4019685
The breakdown of spherical clusters into a great many stars Is important because
the formation of stars in spherical clusters is occurring at the present time.
The final problem considered Is the fact that star formation Is still continuing
in spiral and irregular galaxies but already has virtually.ended in elliptical
galaxies. Orig. art. has: 2 formulas.
ASSOCIATION: ASTRONOMICHESKlY SOVET AN SSSR (Astronomical Council AN =R)
SUBMITTED: OOOct62
SUB CODE: AS
DATE ACQ: 12Mar64
NO REF SOV: 009
ENCL: 00
OTHER: 008
2/2
Card

PIKELINER, S.B.
Anallsis of possible mechanisms of the formation of magnetic fields
in radio sources. Astron.zhur. 40 no.4:601-611 Jl-Ag '63.
(MIRA 16:8)
1. Gosudarstvennyy astronomicheskiy institut im. P.K.Shternberga.
(Magnetic fields (Cosmic physics)) (Radio astronomy)