SCIENTIFIC ABSTRACT SAAKYAN, G.S. - SAAKYAN, P.S.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001446610012-6
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: August 23, 2000
• Sequence Number: 12
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

i
i

a Y'd -S'
USSR/Nuclear Elementary Particles C-3
Abst Journal j Itolorat Zhur Fizikaf No 12, 1956t 33922
Mocharyan, N. M Saakyan, G. S., Ayvazyan, M. D.,-
Author 2 ~Kirakosyan Z, A., -ATOM-n-f Mr-,A S
Institution i Institute of Physics,, Academy of Sciences Armenian,SSR,
Title Nuclear Interaction ofii( -Mesons in Copper
Original
Periodical ~Dokl. AN SSSR, 1955P 105, No 6, 1204-1207
Abstract A magnetic spectrometer was used to study the spectra of creation
of it -mesons, generated in copper absorbers at an altitude of 3,250
m. Approximately,400 A -mesons with a total energy exceeding 510
Mev were recorded. ~The*energy spectrum.of the resulting it-mesons
can be approximated by a power law with an index_ T= 2.2 The
magnitude.of theinteraction cross section of it -mesons with copper
nuclei turned.out to be weakly dependent on the energy and.close to
its geometrical value.
Card 1/1

88
7--~ 7.

'e-getectea. -Ina
,cuoi"fiiru4m-rmesons
-which was
60d a, nient'. With

ntY,,
ergy spectrum 0
Ine
so Ir uction th
Phere. G. S
S.S.R. Akad, Nauk Ar;..,o
0. R the basi, Of
t-aell~eirtnesPectm Of A mesons at sea level
and at 3200 m.
calcd. 'thL, en-gy spectra or X-.Meson. Production Ivere
The foliolying as$4UIP80115-I"Te Made., at jn~
as Pe-r=,lt of.detiLy 6
'With depth. -th- e, was ~o gcrvid,
e av- range:Of Idelistle,
nucleons 1 huclearAnt
n tllc.air~-
and
components in the 0 nucleon
attli -iveie.cofts;
Ile k 70 aud~120
g./sq. cin., resp. T
e bit-
the cross sections Of nuaclir. I wien
Fupdons. Calcu
nd ir
and diagra&iiii6 Pfcscnt-i Si
7-
-ZR

SOV56-35-6-35/44
AVORS: Kocharyan, N.M., Saakyan, G. S., Kirakosyan, Z. A.

TITLE: Energy Spectra.ana'lluclear Interactions of Cosmic Ray
Particles fEnergeticheskiye spektry i yadernyye.vzaimodeystv-iya
chastits k~smicheskogo izlucheniya)
PERIODICAL: Zhurnal eksperimentallnoy i teoreticheskoy fiziki, 1958, Vol 351
Nr 6, PP 1335-1349 (USSR)
ABSTRACT: In the present paper the authors published results obtained by
their investigations of cosmic particles carried out in 1955-1956
at the laboratory of the Aragats mountain station (3200 m above
~sea level). The energy spectra of muons and protons were in-
vestigated by means of a magnetic spectrometer (Fig 1). The
accuracy of momentum measurement was great compared with that of~,
previous measurements~(Refsl,2). The energy.distribution of.protons
and muons (nuclear interaction in C-,Cu-) and-.Pb-absorbers) up to
100 Bev was investigated. Experimental results are shown in detail
by tab.Les. Those obtained by the two.series of experiments carried
out for the purpose of determining muon energy distribution are
given by tables land 2. Figure 2 shows the differential and integral
energy spectrIa within the range of 1 100 Bev (diagram). For E> 4 Bev
Card 113 the following applies with respect to muon energy distribution:

SOV/56-35-6-3/44
Energy Spectra and Nuclear Interactions of CoswJ.c Rzy Particles
nj,(E)dE 6-5(E+5)-3dE (f or, F4 2 Bev -see - reference 2)
The proton energy spectrum was alsoinvestigated, but in four series
of experiments, and,the following was obtained for E>3 Bev;
n (E)dE:= 3.2 jr,-3(2+F.) _2*8
dE
p
There E denotes the kinetic energy of protons in Bev. Details of,
the investigations are given by tables 3 and 4. Figu-e 3 shows the
course of the differential proton energy spectrum (diagram). Furthe3;
the inelastic nuclear interaction cross sections of pions and pro-
tons in copper, graphite, and lead were investigated.'Results are
shown by table 5 (for7r -mesons in copper; with increasing energy
accuracy decreases sharply). Table.6 shows the same for particles
with a positive charge. Table 7 shows+the results of cross section
measurements forlr--mesons in copper, table 8 the total ineiastia
interaction cross sections-for protons in copper. Tables 9 and 10
give the resultslobtained by investigations of inelastic cross
section measurements for'ITI-mesons and protons respectively injead.
Measuring results lead to the following conclusions:
1) The inelastic nuclear interaction cross-sections of pions and
Card 213 protons within the eaergy range of 1 to.several 10 -Bev are equal,
~Z'

14 Is- 0 L) S/022/59/012/05/07/009
AUTHOR: ~Saakzan, G.S.
TITLE: Induced Deceleration Radiationand Absorption
PERIODICAL: Izvestiya Akademii nauk ArmyanskoySSR. Seriya f i ziko-ma.t e-
maticheskikh nauk, 1959, Vol- 12, No. 5, PP- 99-104
TEXT: Besides the usual deceleration radiation the author observes the in-
duced deceleration radiation-and absorption in.presence-of.an, external field.
On behalf'of simplicity the author assumes that the external radiation field
is not polarized and,he calculates the probabilities of the induced processes.
The probability d.'[ of the induced deceleration radiation in the.unit of time,
is obtained as
(Y) dw 1 + 81L 3 dW
t~03 0
where dW is the probability of the usual deceleration radiation, the
0
density of the radiated energy, 0 the frequency, For the probability dW' of
the induced deceleration absorption the, author obtains
(10) dw, a ru3 '? dWo'
3'
Card 1/ 3

Pr'l
Induced Deceleration Radiation and Absorption S/022/59/012/05/07/009
where dW' arises from dW by alternating everywhere the sign of the photon
0 0
impulse. It is stated that for small energies it is always
(15) dW dW
i.e. that the probability of the induced absorption is greaterthan that of the71
induced radiation.-For very intensive radiation*fields (Sun, stars)~the prow-
b,ability of the induced radiation can be greater than the probability_of, the_
usual deceleration radiation. If it is assumedthat in the stars.there is a
black radiation field, then (31) and (10) can be integrated
aT
W( dw dx I e dW dw dx
0
where a is the Bolzmann constant, W E LO)dt,)dx is the-Probability that
~o
an~ electron with the e'nergy F_ after passage through a dx strong medium-layer
radiates a photon, the energy of which lies in the interval 10 j1k) + diO
In.,the case of absorption from (10) it.:follows
Card 2/3

-112 39
I%. V.
Z.
o;i -ol
o A ~-Jj tv
Log a
Aj I'd

88905
S/026/60/000/011/001/009
AUTHOR: Saakyan, Gjj5_
TITLE. Hyperon Stars
PERIODICAL: Priroda, 1960, No. 11, pp. 14 21
TEXT: The authordiscusses V.A.* Ambartsumanis theor on the.formati on of.
~y
star groups and galaxies whereby, in contrast.to previous,opinions,'.the develop-
ment is from the denser prestellar bodies to the lighter states of matter. .,The_~
super-dense prestellar matter "explodes" into,numerous star.groups and masses of
dispersed interstellar matter., The author then turns to a special case of this
theory and advances the hypothesis of the.existeInce of neutron.and hyperon stars,
prefacing the discussion with,a review of current theory on elementary particles.
and antiparticles and the statistical laws which apply to them. The tempera
mass, gravity, density, energy levels-and composition of white dwarfs,.,neutron
and hyperon stars are then compared. The theory.on white dwarfs was developed
by the Soviet physicist,L.D. Landau, while the theory,of neutron stars was de-
by Landau and also by R. Oppengeymer and M Volkov. The author demon-
strates that, with an increase indensity above 0 g/cm3, the percentage of nei-
trons in.the matter will.rise rapidly through a percentage -decrease in electrons
Card 1/3

88905
S,/o26/6o/ooo/on/ooi_/009
Hyperon Stars A166/A026
and protons. Oppengeymer and Volkov have shown that the neutron star can be in
equilibrium with a mass greater than 0.3 and less than 0.7 the mass of the sun.
The immense gravit.ational forces ate here balanced only by the pressure of degx~-
erate neutron gas. During the formation of the neutron from the proton a neu-
trino is liberated, capable of passing freely through the mass of the star., The
neutrinos could carry off themain part of the energy generated during compres-
sion,,thus enabling the neutronstar to develop within thetime interval of our
galaxy. Due to the intense gravitational pull, the neutronstar would diffract
light strongly and would act as an.enormous collecting lens dondensing the ligbt
~from many stars. As matter Iincreases in density beyond 101~ g/cm3, conditions
become-suitable for the formation,of hyperon stars. These stars must have a
mass similar to that of the sun, but a radius ranging from a few kilometers. M-i-,
star consists of 3 regions: 1) an inner hyperon nucleus containing the mainnass
of the star and with a density greater thannormal nuclea rdensity, 2) a spher-
ical neutron layer containing no hyperons but equal parts of protons and elec-
trons; the mass and thickness,are small compared.to the hyperon nucleus;. 3) an
envelope a few.dozen meters thick and consisting.of bare nuclei andelectrons..
or atoms at the surface. Should a hyperon star collide with some other celestial
body, a hyperon star.of unstable mass and size might develop, which would then
-Card 2/3

80825
S/033/60/037/02/001/013
IS-0 0 ~E032/E914
AUTHORS:Ambartsumyan V.A. and 2a S.
I a
,~Zan, G
TITLE: ~Degenerate Superdense Gas of Elementary Particles
PERIODICAL: Astronomicheskiy~zhurnal,1950,tI 37,Nr 21-op 193-209 (USSR)
ABSTRACT: Analysis of available observational material shows that
the evolution of stellap 1~roups and galaxies,takes place
from,dense prestellar bodies to.less dense states. In
-other words, groups of stars and large amounts of-matter
scattered in interstellar space originate from very dense
prestellar bodies. The first,group of facts which may be
used to support this hypothesis relates tolgalaxies~and
groups of galaxies-and was analyzed by Ambartsumyan in
Ref 1. Thereis evidence that the appearance of new galwc-
ies and spiral arms is-associated withmatter in the nuclei
of galaxies. These nuclei.,have small dimensions and high
.density., The second group of facts relates to the format-
ion of-stellar groups making up stellar associations. The,
presence in these associations and, in particular, in their
~Cardl/6 central re-ionsl of large gaseous nebulae tight. stellar

80825
S/033/60/037/02/001/013
E032/E914
Degenerate Superdense Gas of Elementary.Farticles
groups, and systems.of the Trapezium type, is in conflic'c
with the hypothesis-according to which,stellar associations
are formed from.diffuse nebulae. The properties of,systems.
-of the Trapezium type indicate that they have originated
from a massive.and,very dense body. The primary.,superdense
confi-urations should, in general have very complex proper-
ties and it is therefore useful in the firstinstance to
consider configurations whose'temperature is close to
absolute zero, i.e. all the fermions form a degenerate gas;~
An important property of superdense configurations is the
presence of.both neutrons and hyperons. Since at suffic-
iently low temperatures the nucleon gas is stronglydegen-
erate, hyperons having an energy'below a certain limiting
value become stable, since in accordance with the Pauli
principle their decay products cannot be accommodated in
'Card 2/6

U00825
S/033/60/037/02/001/01.~~,
E032/E914
Degenerate superdense Gas of Elementary Particles
the phase space. Mutual transformations of hyperons of
different k:Lnds are:.also forbidden by this principle.
The present authors derive equations giving- the coneIen-
tration of thedifferent1kinds of, baryons~at T =- 0
These equations are derived under the~following'ass-umptionsl.
1) In the equilibrium state the energy of the systems should
be a minimum
2) In all po;sible processes leading to the appearance of
a static equilibrium state between the various components
of matter, the number of baryons must be conserved,
3) Both the star as a whole and its separate macroscopic.
volume elements should be neutral. 7 3 1
It is shown that,for densities below 1.28 x 10 -/CM the.-
degenerate neutral gas at T =~O consists,of protons and:
electrons only.. 'When the density becomes equal to the above
value, neutrons appear for the first.time, As the density
increases above the limiting value,,the number of protons
C;,I,,-d3/6 increases much more slowly than the numberof-neutrons, For
-----------

80825
S/033/60/037/02/001/013:
Degenerate Suprdense Gas of Elementary Particles
8
densities above 2-x 10 the number of.neutrons is.many times
greater than the number of protons.and electrons and the.
gas may be looked upon simply as a neutron gas. The first
hyperons-appear-when the density reaches 1,1 x lo15 g/cm3.
In spite.of the fact that -A. and,
Particles have
rest masses smaller.than the restmass of the latter
particles appear first With furtherinerease of density
up to 2.36 x 1015 g/ci% the number of Z.- hyperons,
increases, but hyperons of other types do not appear, At
2.36 x 1o15 ,,,-/cm3 the first hyperons appear, and
as the density.is increasedfurther other heavier particles
app.ear also. Thus for densities-of the order ~of 1016 3
CM
one has a baryon gas consisting of a mixture of nualeons
Card,4/6

S/033/60/037/02/00'1/0.11
E032/E914
Degenerate Superdense Gas of Elementary Particles
hyperons and nucleon isobars, and the concentration of
the different baryons,is of.the same~ord f iitude
o _3ag
For baryon densities in excess.of 2 x 1C cm 5 X 101~6
g/CM3) the theory meets with the following difficulties:
a) Owing to-thesmall distances between the baryons they
begin to experience very large repulsive f orces whose,
nature is not.well-known at present;
The'distribution of particles.among the dif,ferent.,kinds
of baryons becomes strongly dependent on the presence:of
hyperons.having a mass greater than that of-theC-r; byperon.
For this reason. no definite conclusions can be reached-for
s-Gates of such)~igh density. However,-,the relative number
ti
of these higher hyperons will increase with density un,_l
density is reached at which the existence of 'tr'!- mesons
a
making up a Bose gas, becomes possible. Thus,.superdeense
stars cannot be looked upon as consisting of practically,
pure neutron.configurations. This simple,picture must be
replaced by a more complex configuration conslsting, of a.
Card5/6 hyperon nucleus, a neutron shell surrPunding-the nucleus

83602
S/056/60/038/005/035/050,
B006/BO6.3
~v
AUTHOR; Saakyan, G. S.,
TITLE., Single::~ton~'Annihilation and Electron Pair Production
in a,Medium-
'PERIODICAL: Zhurnal eksperimentallnoy i teoreticheskoy fiziki, ig6o,
Vol. 38, No. 5, pp. 1593-1596
..-TEXT: The present paper.describes.a theoretical investigation of,- the
processes (1): et + e- -,y.in a dispersive medium whose refractive index
n(6o) is smaller than unity. As a, result of the law of conservation of
momentum, the following relation holds for such a medium:-k Pl+P2;
k wn(N) 6J E1+, E2' By,estimating the limit of photon-ener.gy for such
processes,one obtains a value corresponding,.to.a particle density of
N '-k f 1.4-10 32 em-3. Vch dIeInsities do not occur even in the-interior,of the
Sun or other normal'Ostars. Only in the centers of White Dwarfs densities
of the order of ma V
gnitude of nuclear density.or even higher might occur
Card 1/3

83602
Single-photon Annihilation and Electron Pair S/056/60/038/005/035/050
Production' in a Medidm B006/BO63
(cf. Refs.11-3). V. A. Ambartsumyan studied the possible existenceof mat-
ter of superhigh density. As,processes of the type (1) may-occur only.in
disperse media, the photon energy must satisfythe 'condition
1/3
2m CO < N Here,- the temperature of the medium plays a significant
role. At sufficiently~low temperatures, the electron gas is degenerat.e9
and the process y --s- e+ + e- is forbidden according to the Pauli principle..
The author calculates the probability of (1) on the assumption.that the
conditions required for (1) are all satisfied in nature. First, hestudie Is
pair production by a gamma quantum and derives some relations for dW and
W W 1:z* (m/ 13 7(J) ( 12m/6J)X-l:holdsl--approximately; A 1/m is the Compton
C C
wavelength of the electron divided by 2n. The probability of pair produc-.
.tion'by gamma quanta according tothe ordinary mechanism (e.g.~, in the
nuclear field) is given by the relation W = Z24~N, where N denotes the
0
den sity of the nucleus, and _Z 2(b is the total I iIr-p roduGtion cIross section.
p
An estimate-of theseprobabilities and of the W~W ratio shows that in the
energy range 2m < 63. 10m W is much greater than-W In the following,
0
the author investigates single-photon pair annihilation. For the total
Card 2/3

83602
~Single-photon Annihilation and Electron Pair S/056J60/038/005/035/050
Production in a Medium B006/BO63
positron annihilation probability (positron energy E 2) one obtains:
4 N (E )dE
[n2 2 -n 2 .,,2 1 1 1 - II
W M + --~- 6) where N1(t I)dE1
2E p EI Ej 2
2 21 Elpln
is the number of electrons in the range (E,, E, + dE,),per unit.,v,olume, The
lower limit of theintegralis m, and the upperilimit is equal to cD if-
the electron gas in the medi,um is not degenerate. If the electron gas is
highly degenerate, the upper,limit is.equal-to the Fermi energy limit.
There are 9 references: 7 Soviet and 2 US'.
ASSOCIATION: Yerevanskiy gosudarstvennyy universitet
(Yerevan State University)
SUBMITTED: December 16, 1959*
Card 313

PHASE I BOOK E)(PLOITATION SOV/5723
Saakyan, G. S.
Energeticheskiye spektry i yadernyye vzaimodeystviya chastits
kosmicheskogo izlucheniya (Energy S~ectrum and Nuclear.Inter-
action of Cosmic Radiation Particles) Yerevan,-Izd-vo Yerevan-
skogo univ., 1960, 113 P. Errata slip inserted. -1,000 copies
printed.
Sponsoring Agency:' Yerevanskiy gosudarstvennyy universitet,
Ed-.:. N. Samsonova and G.. Yesayan; Tee.h. Ed.: A.*Ovasapyan.
'PURPOSE This.booklis intended for nuclear and cosmic ray phys-,-
COVERAGE: The book deals with energy spectra md nuclear inter-
actions of cosmic ray particles. Ch. Itconcerns the recording
probability of charged particles by~means of'a magnetic spectro-
meter. General formulas for differential and total recording,,,
Card 1/5

Energy-Spectrum and Nuclear (Cont.) SOV/5723
probability of charged particles required for measuring the
absolute intensities of:charged cosmic radiation particles
are included, Ch. II. treats nuclear interactions.of-pi-mesons
and p Irotons in copper and graphite in which the magnetic sDectro-
meter was:used for measuring the cross sections of inelastic
nuclear interaction of particles. The nuclear interactions of
particles were studied in absorbers placed under themagnetic
gap. Trajectory projections for eac4 particle were plotted on,
a model representIng a drawn-to-scale ima,-,e of two mutually
perpendicular vertical sections of the unit parallel and per-
pendicular tothe lines of.force of the magnetic field. Thc_
cases in which particles passed the absorber system with or
without nuclear interaction were.then determined. Measurement
of effective croas sections was made in the region of energies uD.
IT~
to- 10 Bev for which'no data was available at that time. Ch.
deals with the energy distribution of protons and mu-mesons on
Mount Aragats at 3,200 m,above sea level. The energy distribu-
tion of mu-mesons served as a basisXor calculating the 6nergy.,
spectrum.of pi-meson production in~the atmosphere. The functions
Card 2/5

Energy Spectrum and Nuclear (Cont.) SOV/5723
obtained,of energy distribution of particles are within an
energy range of several hundred,Mev to,100*Bev. Ch. IVtreats
the nature of.nuclear-interactions of:nualeons,,ranging in
energy from several Bev to several hundred BevY with the air
nuclei. The portionof energy, spent during the.nucleon col-
lision with air nuclei on.the formation of-mesons, increases
monotonically with the increasesin energy and at several hun-
dred Bev approaches unity, i.e., the collision is entirely
inelastic. The book is based on research carried,out by the
author in cooperation with the staff of the Laboratorlya
malogo elektromagnita (Small Electromagnet Laboratory).of the
Fizicheskiy institute Akademii nauk (Institute of Physics of
the Academy of Sciences) ofthe Armyanskaya SSR, under the
supervision of Professor N. M. Kocharyan in the years 1955 to
1957. The author thanks M. T. Ayvazyan, Z. A. Kirakosyan, A. S.
"Aleks-anyan,'and Kh B. Pachadzhyan. There are 87 references:
45 English, 37 Soviet, 2 German,.1 Hungarian, 1 Italian-, and.
1 French.
Card 3. 5

Energy Spectrum and Nuclear (Cont.)
TABLE, OF CONTENTS:
Introduction
Ch. I.. Probability of.Charged,Particle~Recording
1. Differential recording probability
2. Total recording probability of particles 17
3. Solid angle of a beam otparticles accessible to
recording 2-1
Ch. II. Cross Sections,of Interaction of Pi-Meaon6 and'
Protons in.Copper and Graphite
4. Cross section's of inelastic nuclear interaction of pi-
mesons and protons in copper
5. Cross sections of inelastic nuclear interaction of pi-
mesons and protons in,graphite 39
Ch.,III. Energy Spectra of Cosmic.Radiation Particles at
an Altitude of 3,200 mAbove Sea Level
Energy spectrum of mu-mesons 4-7
Card 4/ 5

S/022/61/014/005/005,/007
D218/D301
~kUTHORS: Saakyan, G. S. and Sedrakyan, D.
TITLE: On thetheory of hyperon configurations'of.,stellar
masses
PERIODICAL: Akademiya naukArmyanskoy SSR. Izvestiya. Seriya fizi-
ko-matematicheskikh na Iuk, v. 14, no. 5, 1961, 109-113
TEXT: Ambartsumyan and Saakyan-(Ref. 1: Astron. Zh., 37,193,
~1~60) have shown that if the density of matter in ultr4-dense stel-
lar configurationsis 'greater by a factor of 3-than the density of
nuclear matter, then its "chemical" composition becomes radically
altered. In particular, it contains hyperons and negative muons,
Such configurations ofstellar masses are known as hyperon stars.
It was also shown that a hyperon star consists of a hyperon nucleus
,a neutron layer.and an outer shell which is roughly in the same
state as in the case of white dwarfs, i.e. it contains bare nuclei
and free electronst and neutral atoms at the surface. The dimensions
and the%mass of the outer shell of hyperon starswere not investi-
Card 1/2

S/022/61/014/006/004/004
D299/D301
AUTHOR: Saakyan G. S.
TITLE: On the equation of state at superhigh densities of
matter
PERIODICAL: Akademiya nauk Armyanskoy SSR. Izvestiya. v. 14, no.
6. 1961, 117-1,23
TEXT: The article has two objects: 1) to show that for,any type
of interaction, in which the energy of interaction of the partic-
les exceeds their kinetic energy, the well-known law P/o/_1/3
is invalidated; 2.) to show that the equation..
P(n)~~p(n)_-/n2
(n particle density, P pressure, p,- energy density) is not
related to a.particular type of interaction.through a neutral me-
sonic field, but follows from general physical principles (such.
as the principle of indeterminacy and the fact that the velocity
Card 1/ 7

On the equation of state ... D299/D301
of sound cannot exceed that of light). Eq. (1.1) was obtained by
Ya. B. Zelldovich (Ref. 5: Uravneniye,sostoyanlya pri sverkhvyso-
~koy plotnosti i relyativistkiya.ogranicheniya, ZhETF (in print)).
First the indeterminacy relation is considered. For the total means
energy of particles one obtains
2 4 2 2 2/3
m C + C h n 1/2 + u(n) (1.3)
k
where u(n) has the meaning of potential energy which is assumed as
similar for-all types of particles. For the mean energy density
one obtains
P(n)~:vcn (m2c2 h 2n2/3 1/2 + nu(n)
where m is the average mass of barionB (nucleons and hyperons).
Tor the pressure-to-density ratio Pne obtains
Card 2/7.

S/622/61/014/ob6/004/004
On the equation-of state-.-.-.~ D299/D301
whose solution is
u(n)--an + b
n (1.12)
where a. and b are integration constants Hence one obtains, for
sufficiently high densities of matter, Zel.1dovich's result
2
P-;:~p~z~a n
The relation between this.result and the cosmological problem is
considered. Sound propagation in very dense media: In the forego-
ing, the velocity of sound was expressed by the formula v
.=_cV7P7ap_. This formula was derived on the assumption of a Eucli-
dean space. It is shown that this formula remains valideven in the
case of very dense media, with a metric considerably differing from
Euclidean. Thereby the author proceeds from the hydrodynamics
Card 4/7

S/022/61/014/006/004/004
On the equation of state ... D299/D301-
I ik )w
g.9 T, = 0 (2 9
k
f g x
-where x 0 vt. The quantity v = c0p/ap) 1/2 can be interpreted as.
the velocity of sound. Thus the formula remains valid for strong
gravitational fields, too. As bP/6p is (in general) a.function.of
r9 the velocity of sound v is also a function of the coordinate ro
The author expresses his thanks to V. A. Ambartsumyan, Ya. B. Zel'
dovich, V. L. Ginzburg and Ye. L. Feynberg. There are 7 referen-
ces. 5 Soviet-bloc and 2 non-Soviet-bloc. The references to the
English-language publications readas follows: A. G. W. Cameron,
Neutron Models, Astrophys. J., 1507 884t 1959; & E Salpeter,
Matter at High Densities. Ann. of Phys., 11, 393, 1660.
ASSOCIATION: Yerevanskiy gosudarstvenny universitet (Yerevan State
University); Fizicheskiy institut Ali Armyanskoy SSR
Card 6/7

I . ! . -~j - --.. :~- - -;. ~ -
. . I " - ~! -- , , ; ~-
. : : ~ ~- - ~ , . 1
- : '. , k ~ .: ~ - ~; c,,. - f- ~!~ , .1 -, - , !~-

.~ " -;i4. '4. , -, 7 - - , "r ~. ~ -- -,
- - " z-,~': -~ . ~ t. ! z.: - -, ~~4 j-
.. ~- :.- _,~ , ; ~ ~ . , ~4-, I -, ~ o, - -- ~,~ ~ I -- - ~; ~ I ~ ~ -~W.

35307
0 Od S"7, 1,53 S/02Y6 21011 5 /001 /007/007
D2_57 1~301
12 t1. If/ 0 0
AUTHOR Saakyan, G. S~
T I ThE On the superdense state of matter in the universe
PERIODICAL: Akademiya nauk Armyanskoy SSR. Izvestiya. Fiziko-mate-
maticheskiye nauki, v. 15, no. 1,,1962, 123-134
TEXT,, The author investigates some physical properties of matter
on -the assumption that at the beginning of the expansion of the
universe, density of energy in it was.of the order of the density
occu--r-ing within the nucleus, or higher. The problem stated is to
investigate the properties of the gas-of elementary particles in a
closed system. Only the whole universe can be such a system, and
the author bases his deductions on the general.principles of the
thermodynamics of systems in equilibrium. It is assumed that.the
~change of state of matter caused by contraction or expansion of
:space is slow enough to permit-the occurrence of quasi-equilibrium
state in at least some regions of space. Barions, leptons and bo-
sons are assumed to be present in, the gas and statistical formulas
Card 1/4

3/022/62/015/001/007/007
,.On the superdense state D237/D301
are given.for their thermodynamic potentials, entropies and ener-
gies, 'Erue for both particles and anti-partuicles and for photonso,
Assuming the laws of: conservation of the number of barions, con-
servation of leptons, conservation of.charge and conservation of
the sum of the energy of matter'and gravitational field,' and as-
suming also that the noimal entropy is maximum, the author derives..
I me-
the conditions of'thermodynamic equilibrium by variational
thods and shows that the conditions obtained are not only necegs-
ary, but also sufficient for the entropy to be maximum. Considera_
tion of the equilibrium relations leads,to the conclusion that
knowledge of the volume or radius of curvature (in the case of a
.aomogeneous isotropic model) alone is sufficient for detailed des-
of the state of matter in the universe if is at any
instant in the state of thermodynamic equilibrium, I.e. if the
Change of state is adiabatic and reversible. The author discusses
next the problem of concentration.of the particles and ends the
paper with the following conclusions: If it- is assumed that the
distribution of matter in the universe is homogeneous and isot-ropic
'Card 2/4

S/022/62/015/001/001/007
On thesuperdense state ... ~D237/D3011
then its physical properties arecharacterized by four basic para-
meters; Electrical, lepton and barion charges and the -total energy
of matter and that of the.gravitational field (mass of the uni-
verse). These parameters:are time independent and if their m agni-
tudes are known (the to Ital electrical charge is known to be equal
to zero), then the volume or the radius of curvature of space de-
termines the state of matter in the universe, assuming.that the
change of.state of the universe is adiabatic. The.above conclusion
is stated to be true also for other (rarified)-systems..The author..
expresses his gratitude to:Academician V.. A6 Ambartsumyan, I. Ia
Goldman and A. Ts Amatuni for theinterest shown by them towards v~4
his work. There-a;e 11 references: 9.Soviet-bloc and 2 non-Soviet-
bloc. The references to the English-language publications read as
follows; R-C. Tolman. Relativity thermodynamics and cosmology-
Glava X. Oxford, 1949; S. Sakata,. Progess'. theor. Phys., 167 6867
1956.
A.SSOCIATION: Yerevanskiy gosudarstvennyy universitet (Yerevan
Ca rd 3/4

s/02 62/015/006/005/006
D218 308
AUTHORS. Saakyan, G.S., dnd Vartanyan, Yu. L.

TITLE-
On the solutions of Einstein's equations
,
for axially symmetric fields
PERIODICAL :
Akademiya nauk Armyanskoy SSR. Izvestiya
1%
v- 157 no. 6, 1962, 83 87
TEXT: Olijnychenko (Nuovo Cimento, 21 389v
1961) has' considered Wey-l's solution andIhas shown that in the
case of a static field with an arbitrary.metri
10

ds 2 2
Xdx + 2 2 2'
Ydy + Zdz + fdu

there are no solutiona,with non-zero distribution of matter.'i
It is now shown that this paradox could,be.sliminated by. the,
use of the following expression
.~T ik (P U uk pg ik
Card 1/2

ACCESSION URI: AT4019687 S/2555/63/009/000/0091/0131
AUTHOR: Ambartsumyan, V. A.; Saakyan, G. S.~
TITLE: Ile present status of the theory of superdense celestial bodies
SOURCE: AN SSSR. Astronomicheskly sovet. Voprosy*, kosmogonii (Problems of cosmogoa~'
V. 9, 1963, 91-131
TOPICTAGS- astrophysics, astronomy, elementary particle, elementary particle physics,
electron, neutron, barion, barion star, neturon star, star formation, lepton, star
ABSTRACT: The paper deals w ith the'theory of superdense celestial bodies (barioa configura-
tions). In the bibliography of 26 items, 22 of the articles listed are in English oravailable'
in English translation. An investigation of the gas of elementary particles at a temperature
of OC led to the following results: (a) at densities p < pn, where p. 1. 28 - 107 g- cm-3,
the gas consists of,protons andneutrons. (b) When p = p,,,neutrons appear. With a
further Increase in density the number of protons increases far more slowly than the number
ofneutrons. At, densities greaier than 2-108g.cm-3 the number of neutrons already greatly
exceeds the numberof protons and electrons. At these densities matter virtually, consists----
eard 1/3

ACCESSION NR: AT4019687
only of neutrons. (c) When p =pp- 1.1-1015g.cryr3 the first h erons appear. Despite
yp
the fact that A, -!"and possess rest masses small
er than Q-, the latter are the first
to appear. With'a further increase in density, to p 2.36- 1015g. cm-3 the number.
of F_7hyperons increases, but hyperons of other Idnds still do not appear. (d) Af ter
the appearance of L hyperons in matter, the proton 'concentration increases rapidly
and soon becomes on the order of the neutron coqcentration. (e) V&mp = P-A-% -r'\
hyperons appear, and with a further increase of tensity, other heavier particles appear.
e 1. 44,
(f) When 1017g- cm-3, tr-mesons will appear. Thus, at sufficiently high
densities there& will be a gas consisting of a mixture of nucleons hyperons, resonance
barions, /T-mesons, and leptons. The concentration of all the particles in this gas is
of the same order of magnitude, except, in the case. of leptons (electrons and p- mesons)
whose concentration is three or four ordersof magnitude less than the concentration of
each ldnd of barion. In a general. case, when the 6entral densities of energy are sufficiently
.great, the hypothetical superdense celestial body (ba-rion star) consists of four principal
re.Pons: first, a central sphere, consisting for the most part of barions, barion resonances,
and -A-niesons. This regiorf is followed by a spherical layer in which matter coijists for
the most part of definite ldnds bf.barions, specifically, hyperons. The next layer for the
2/3
Cardd

TR: AT4019687
ACCESSION IN
most part consists of neutrons. The last, outer layer, consists of protons, nuclei, and
electrons. Tlie dimensions of all the regions are about the same, but the thickness of the
outer layer is very small. In configurations consisti f I eal barion gas, the thickness
of the outer layer is several hundreds of motors (6 < 150 m), while1n. configurations-
consisting of a real gas it Is several tens of meter ( 6