SCIENTIFIC ABSTRACT MASEVICH, A.G. - MASEVICH, A.G.

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• Collection: Scientific Abstracts
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• Sequence Number: 13
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

KASEVICH, A.G.
Swelu%jonof early-typo stars. Astron. shlir. 32 us.6-498-502
I-D '55. (KIRA 912)
l.GowAarstvonnyy astrosomichaskiy iastitut insai P.I.Shtern-
berga. (stars)

1 .1
--l - - - - - -- I I 1 -1 -f . I - It . , - -
I ~ ~ I ~ .. . I I - . . . I 1 9 1: - L - - . -- . . I.. . . I - I I .

KAMICH,A.G.
On & visit with India's sclent.'sts. Priroda 44 no.6:57-62 Jo '55.
(India--gatentists--Con,gresses) (XIRA 8-7)

BAKULINI P.i., otvat,,tveanyy redaktor; DUBROVSKIY. K.K.. redaktor
[deceased); IMIAGIN. S.G.. redaktor; KASRVIgjI,.AA,.,,,.,.redaktor;
ftRUAGO. P.P.. redaktor; RAKHLIN. KURASHOVA.
N.Ya.. takhatcheakiy redaktor
[Astronomical calendar. Yearbook. Variable section for 19571
Astranoutchookii kelandarl. Bzhagodnik. Perewnnats chant' 1957.
R*d. kollegila P.I.Bakulin i dr. Koskvs. Gos. izd-vo takhniko-
tooret. lit-ry. 1956. 288 p. (Tsasoluzuoa astronano-goodesicha-
skoe obahchostvo. no.60) (KLRA 10:3)
(AstronoxF-Tearbooks)

-PASNICK, A.G. -
Immiaeolty fwwtloa or main ooqtwaco stars and Its Interpretation.
Astron.shur. 33 no.2:216-221 Mr-Ap 156. (MM 9:8)
1. GeoulwetveaW "tronoulobeekly Institut iamnl P.R. Shtorn'borgs.
(Star*--l"latloa)

KASEVICH, A.G.
Subgiants nnd their relation to mRin sequence stRrs. Astrom.znl.,r.'~3
no-3:330-339 MY-Je 156. (KLRA 9:10)
l.GosudAretvennyy -stronomichpskiy institut Iment P.K.Shternbergn.
(Stnrs--Clnsslfl(!ntion)

KI&SVICE, A.G.
- - -IW*IUM of stwv in the lg&4~s claotor. Astrou* sbur, 33 n0-4:576-
576 JI - Ag 156. (KIM 9: 11)
1. GoeudsretweaW wt*owalchoskly Wtltut Uwal F. L Shteraborg&.
(stass-cumters)

MASEVICH, A.G.
----mWpmWWMWMffftU~,
Possible courses Of continuous OvOlutlon of main sequence stare with
constant and varying manses taking into consideration various. Soob.
GAIM no.99:3-32 156. (KLRA 100)
(St&ro--Cono t itut ion)

BAKULIS. ?.L. otvotstvennyy red.; KUIAGIN. S.G.. red.; jJ111Afigambsib, red.
PARNIAGO. IF.P.. red,.. RAKHLIN, I.T*.. red AKHEDIN. S.M., tekhn.rwA.
[Astronomical calendar; a yearbook. Variable section, 19581
Astronoutabaskil kelandarl ; Xzhogodnik. Persuennsia chest' 9 1958e
Red.kolleglia P.I.Bskulin.i dr. Kooky&. Got. Izd-vo tokhniko-teoret.
lit;7n, 1957. 303 p. (Tsesoiuznoe astronoso-geodexicheskoe obeheho-
stv o.61) (KUU 11-2)
(Astrononw-vearboolre)

MASEVICH, A.G., red.
[Nuclear processes in stars; collected reports read at the
Fifth International Colloquium on Astrophysics held in Liege,
on September 10, Up and 12 of 19531 IAdernye protsessy v
zvezdakch; sbornik dokladov, prochitanrqkh na piatom Ilezhdu-
narodnom kollokviume po astrofizike v Llezhe 10, 1-1 1 12 sen-
tiabria 1953 gods. Pod red. A.G.Masevich. Moskva, Izd-vo ino-
str.lit-ry, 1957. 422'p. (MIRA 14:12)
1. Colloque International D'astrophysique. 5th, Liege, 1953.
(Astrophysics-Congresses)

I i,, .11..
. - ~ r'if4- ~-!
"Fre~~ratic-. for Vis--;~:2 , '- - :,:,
a -.- a - ~.- r , i :- c z : - ' e d o t t 1 i(.! :_ I t c, :-:. 0 t , --~ - 3 1 '.s t I. ~--: -. a ": t ; - a I -, : 7S S , 6 - 12
(~rt p -: a .

14AFAVICH. A.q.
Ift MINOMMORM-am'"- -
Ir..)lUtIon of stare '!i open ~Iusters and stellar assoc !at - )~ r w- tn.
mm-mmary in aorman]. Tor. kosm. 5: 56-A-3 15?. i -. -, ,
(Stare-Clusters)
%'I
.0

14ASITICH, &.G.
-'-' *e,-, 1 -,
'~-wlrli-al m-ain. ~*q%An,-e
&ibmutry T,),
oir.4 its thtorstical interpretati,)z 'w,tp~
. kosm. 5 149-180 '57. (KLRA lc.:,,
"Stars)

" -~ - VE"." A - '.
NASITICH A.G. kandidat fisiko-mtemticbesklkh nank.
1
TM physics of plaustery awbulas; conforemaw 9f the Comodmion. el
Cosmogony. Vest.AN SSSR 27 no.4:1:L-)-120 Ap '57. (NLRA 10:5)
(Nebrulas)

/1,1 ! , . " k iA f~
AUTHOR: Masevich, A.G. 30-8-22/37
TITLE: On Outergalaotic Astrono7 and Cosmology (Vnegalakticheakaya
a
"tronamiya i kosmologi a
PERIODICAL: Vestnik Akademli Nauk SSSR, 1957, Vol.27, Nr 8, pp.94-96 ( ussR)
ABSTRACT: The meeting which took place L4 Moscow from June 5th to June 7th
was devoted to the problem of the above mentioned astro. omy
and cosmology. In his report V.A. Ambartsumiyan gave interesting
details on this relatively new branch of science. Observations
proved the assumption that stellar fogs are not evenly dia-
tributed; there are dense parts and accumulations which may be
called "light cloud formations". In spite of this, theoretical
research is based upon the assumption that the distribution of
luminescent cosmic fog is of uniform character. The reviewer
further remarked that already now there is no doubt that an
expansion of the universe exists. Another reviewer contributed.
interesting observation results with respect to spiral fogs.
The assumption hitherto held that the spiral fog t&il3 are
rotating solar system is said to have been disproved.
Card 1/2

30-8-24/37
On Outergalactic AstronomLy and Cosmology
A.L. Zelmanova gave a report on the relativity theory of the
anisotropic heterogeneity of the universe. Some reviewers
dealt with the problems of the thermodynamics of the universe
and a discussion took place on the ao-oalled fluctuation
hypothesis. In omolusion a discussion on general problems
of cosmology took place.
AVAILABLE: Library of Congress
Card 212

AUTHORi Masevioh, A. G. 30-11-23/23
TITLE: The Problem of Cosmic Gaudynamics.
An International Conference in the USA.
(Problemy kosmicheskoy gazodinamikis
Mozhdunarodnaya konferentmiya v SBhA.)
PERIODICALS Vestnik AN SSSR, 1957, Vol. 27, Nr 11, pp. 140-143 (USSR)
LBSTRACTa 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 sistem, 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 (Kembridzho), USA; this was the
third international symposium devoted to problems of cosmic
aerodynamics. The report by the Dut-.hman Van der Kholet (ob-
servations of the radioemission on the 21 oz wave) caused
great interest. G. Vokuler (USA) reported on the observations
made in Australia of the spiral structure of the galactic
system* 0, Vilson (USA) dealt with the now research date rogar-
ding the inner kinetics of the planetary nebulaeg G. Kyunkh
Card 1/5 (USA) with the internal motions in the nebula of Orion,

The Problem of Cosmic Ga~dYnamic~o
30-11-23/23
R. Minkovskiy (USA) reported on the investigation of the
group of fiber-like nebulae in the Swan, A. Devi* (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-
cussions was paid to the problem of the dissipation of energy.
Kh. Petchek (USA), L. Jirman and 1. Shlyuter (German Federal
Republic - FRG) talked on this topic. So&* 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 gao-oorona and of the forma-
tion of the radio-radiation (B.B. Pikellner). V.A. kmbartsumyan
talked an the genetic connection of young stars with the di-
ffuse environment. By means of observations made he rejected
the hitherto existing assumptions with regard to the formation
of the stars from an interastral substance. The members of the
soviet 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.
F,
30-11-23/23
report deals with the details of the optical observations
of the artificail earth satellites in the USA. The delegation
showed gr*at interest for the nr-,~nization and equipment of
t he Masissohnsetts lustitate of Tedmoloff 0
ITAILABLEs Library of Congress
Card 3/3

AUTHOR: Masevich, A. G. 499
TITLE: The evolution of stars in the X and h Per cluster.
(Evolyutjiya zvezd v skopleniy X i h perseya.)
PERIODICAL: "Astronomicheskiy zhurnal" (Journal of Astronomy),
1157,=o _34, Wo.2, pp. 17b-182 (USSR).
ABSTRACT: The H - R diagram for the nucleus and the surrounding
association of the double cluster of 14 and h Per
show marked differences. Fig.1 shows the H-R diagram
for the nucleus of the above double cluster and
Fig.2 the H - R diagram for the association of the
double cluster. (0 - stars uf the main sequence,
0 - weak supergiants, 0 - bright super ants.
From the data of Johnson and Hiltner (1~). The diagram
for the nucleus is similar to the usual diagram for a
cluster of an early spectral ty-pe. The characteristic
difference between this diagram and the diagram for
the association (Fig.2) is the presence in the latter
of stars of the main sequence of the earliest spectral
tY'Pes (05 - BO), which lie on the undeviated (primary)
upper branch of the main sequence. A further
difference is in the interval between the primary
branch and the branches deviated from it. The
disposition of the supergiants in Fig.2 is reminiscent

499
The evolution of stars in the and h Per cluster.
(Cont.)
of the evolutionary curves of gravitauionally
contracting stars (2). This is further emphasized by
the presence in Fig.2 of a few 0 - stars situated
under the main sequence. For massive stars, such as the
supergiants considered here, such an evolution take
place very quickly (in any case a time less than 109
years is required). A comparative study of the H - R
diagram of the double cluster leads to the conclusion
that the age of the nucleus and the association is
roughly the same, but while in the association the
process of star-formation continues, it has ceased
altogether in the nucleus. The deviation of the
brightest stars in clusters from the mean line of the
main sequence is usually taken to be the result of the
evolution of these stars when heterogeneity in the
chemical composition first begins as a result of the
absence of intermixing of matter between the radiant
envelope and convective nucleus (3, 4). The so-called
"primary" main sequence can be found theoretically
in two ways. The first method (evolution of stars
occurs at constant mass with no intermixing) was given
by Johnson and Hiltner (1 and 5). The primary
theoretical main sequence as calculated by them is

499
The evolution of stars in the % and h Per cluster.
(Cont.)
shown in Fig.3 (dashed line). The second method was
used by the present author and is described in Refs. 3
and 6. The full line of Fig.3 shows the result of
these calculations (absorption law: chemical composition
corresponding to that of the sun; energy source: the
hydrogen-nitrogen cycle). The results of calculation
of evolutionary curves (no intermixing; variable mass)
are given in the table on p.180. (Nucleus: first line
of numbers. Association: last two lines. First column
shows the star under consideration). Further details
are given in Ref.8. As can be seen the age t is
higher by one order for the nucleus. The above
conclusions are in agreement with Oort's theory (11)
on the formation of expanding 0 - associations. It is
argued that Wnch's paper on the age of early type
supergiants leaves out at least one important considera-
tion. A star of the main sequence can only change into
a bright giant of an early spectral type if in it
intermixing does not take place, i.e. hydrogen burns
out only in the convective nucleus which includes about
0.1 of the mass of the star. A sta having the mass 20 M
will reach this stage in , 2 x 109 years. After this, Q

499
The evolution of stars in the )C and h Per cluster.
(cont.)
the "peaceful" evolution of the star ends and it either
undergoes a catastrophe or,if its development continues
with a contracting nucleus,it will become a red giant.
In either case the result will not be a supergiant of
an early type. In order that the stars considered by
Munch (12) should have an age of,-v 2 x 10 years their
mass Ym, t be of the order of 200 Z 300 M .
It is suggested that th9 supergiants coAidered by
11unch have an age -'vlO years, but they were f ormed
not in the galactic plane but at larger latitudes.
3 figures, 1 table, 12 references, 4 of which are
Russian.
State Astronomy Institute
i-meni F. K. 3hternberg. Recd. Oct. 15, 1956.

AUTHOR: Masevich, A. - - 518
TITLE; 1-m6-ettng-of the Committee for Cosmogony devoted to the
development of work on cosmology. (Soveshchaniye
komissii po kosmogonii, posvyashchennoye nerspektivam
razvitiya rabot po kosmologii).
PERIODICAL: "Astronomicheskiy Zhxu.,nal" (Journal of Astronomy),
T757, Vol.34, No.2, pp.-71-1-312.
ABSTRACT: Representatives of astronomical, physical and
philosophical institutions in Moscow and other towns
were present. V. A. Ambartsumyan noted that not
enough attention was given in the U.S.S.R. to the
problems of cosmology while a large number of papers
has appeared in this field in other countries. He
suggested a series of problem that could be tackled.
A, L. El'manov also noted insufficient attention paid
in the U.S.S.R. to non-relativistic cosmology. In the
exposition of a whole series of cosmological aspects,
in particular, those that have ideological implications,
it is necessary to exclude simplifications and dogmatism.
Possible fields of research (origin of chemical elements,
radioastronomy, applications of thermodynamics and
statistical physics etc.) were suggested by other members.
A conference is to be called in 1957 on the problems of
cosmogony. It will be devoted to extragalactic astronomy
and cosmology. An approadh has been made to the "Uspekhi

AL meeting of the Committee for Cosmogony devoted tgAhe
development of work on cosmology. (Cont.)
Fizicheskikh Nauk" and "Voprosy Kosmogonii" to publish
review articles on extragalactic astronomy and
cosmology, Translations of the appropriate foreign
books will be carried out.
Recd. Feb. 23, 195?.

MASCV/C-~~ t-A,C-,
AUTHOR: Nikol!skiy, G.M. and Masevich, A.G. 33-3-27/32
TITLI: Comments by Nikol!skiy on the paper by A.G. N~mvieh
"Iuminosity function for stars of the main sequence" and
author's xWly.
PEMODICALs "Wronomichesuz Zhurnal" (Journal of Astronomy),
IW7# V01*34, No-3v PP. 4.93-494 (U.S.S.R.)
ABSTMOTs A.G., Masevich (1) considers the important problem of the
evolution of stars of the main sequence. The ana3ysis of
this problem is carried out by him in the following ways
Suppose that *Urs are formed continuously and n stars
per second enter the main sequence at the point M 0 (absolute
stellar magnitude). Evolution takes place in the same way far
all stars which move down the main sequence* If t is the
time of evolution of a star frm the point No to the point
N (see formula 7 in (1))- then:
ou'd 1/4 nt = NJ 9 (M)dN
No
where jp(M) is the luminosity function observed at the pres-

33-3-27/32
QLrd 3/4
Comments by Nikol!skiy on the paper by A.G. Masevich
IUAminosity function for stars of the main sequence" and
author's reply. (Cont.)
of the second type ( 9 greater than M dM. ne5ative)
Masevich used the limi?s of the integral in eq (1 incorrectly
and hence his conclusions are invalidated by this mathematical
error. n is always positive. There aiv two Slavic references.
AUTHOR'S REPLY
Nikolskiy's article is based on a mimind rstanding. It is
well known that in all the possible cases of evolution of stars
at constant mass, the luminosity and the radius of the star
increase. Since the mass is constant, it follows that, after a
time, the star ceases to obey the mass-biminosity and tbE; mass-
radius relations characteristic of the main sequence and hence
'leaves' the latter. This was considered in detail in (2) and
(3) and is not, arid cannot be, a consequence of eq. (2) in
NikolskJqts note. It is su:rprising that Nikolskiy should quote
(2) since this work, although printed, has not been issued and
is still being stored by the publishers. Conversely, the
result obtained in a discussion of evolution at constant mass
in U without the transposition of the limits of integration
in (1i is treated (perhaps not very successfully) simply as a

33-3-2T/32
Comments by NikoYskiy on the paper by A.G. Masevich
"Tuminosity function for srars of the main sequence" and
author's reply. (Cont.)
mathematical expression of known facts and could be omitted
without effect on the conclusions t~,at follow.
The choice between the two alternative evolutionary hypo-
theOdS using the luminosity function is based in (1) not on the
of n but on its magnitude ( n is the number of stars
�!e~g formed and is necessarily positive). Nikolskiyls criti-
cism is thus rejected and the conclusions reached in (1)
There are 4 Slavic references.
AVAILABLE: LibrwT of Congmes
Card 4/4

/-/ " /-) ~, ~ -- I. -* , (I , / .,~ " -
AUTHOR: Ruben, G. and blasevich, A. 33-5-6/12.
TITU: An Investigation of Evolutionary Sequences of Homogeneous
Stellar Models with a Convective 1.,ucleus. (Issledovaniye
Evolyutsionnykh Posledovatellnostey Oclnorod-nykh /,vezdnykh
Modeley s Konvektivnym Yadrom.)
PERIODlCAL: Astronomicheskiy Zhurnal, 1957, Vol.34, Jo.5,
pp. 724-738 (USSR).
ABSTRACT: A detailed calculation using thf, stellar model bi A~5 a_ 3.5
convective nucleus and the absorption law K = K fp , T
has been carried out by one of the present auth8rs in
ReZ. I and 2. PoE;sible ways of developing this model in
the case of homogeneous and inhomogeneous chemical composi-
tion were considemd in application to stars of the main
sequence. In the present work the possibility of an
application of such a model to the problem of structure
and evolution of stars of other sequences in Russell's
dia ram is considered. The authors start with a model
ha:fng the same chemical composition in both the shell
and the convective nucleus. The carbon cyclic reaction n
is taken as the source of enerEj, according to e = F_ XZ IV T
The continuous evolution (as a result of gradual trRnsform-
Card 1/4 ation of hydro6en into helium) of such a model is considered

33-5-6/12.
An Investigation of Evolutional-j ~j-equences of Homogenaous Stellar
Models with a Convective Nucleus.
in the case of constant and variable mass. Using the
notation of References 1 and 2 the relation between the
luminosity I, and the stellar mass Mi is written in the
form My Figure 1 shows the calculated dependence of
lgi,l on lgRl for different values of y where H 1 is the
relative radius. The relation between these two quantities
is linear. An analysis is given of the effect of different
parameters on the form of evolutionary curves. Various
possible law5 of change of mass am considered (different
Y in Ref. 5). In each of the models there is a limiting
value of y which depends on the form of the law of formation
of energy but is almost independent of tile model iteelf.
Within the limits of each possible y there are certain
xia" values of M and R the absolute magnitude of which
depends on the acce?ted moael. It is shown that the
theoretical curve corresponding to y = 3.9 represents the
main sequence quite well. Using other values of y one
obtains evolutionary sequences which do not correspond to
Card 2/4 real stellar sequences for which the mass is a function

33-5-)-6/1'1
An Investigation of Evolutionary Sequences of Homogeneous Stellar
Models with a Convective Nucleus.
of both the luminosity and radius. In the case of Y = 3.9
both Ad and R reach their maximum values at the same
value 8f Z, w8ere Z is the content of elements heavier than
helium. Using results obtained for y # 3.9 it is shown
that the structure and evolution of a sub-dwarfs caz be
explained by the present model if one assumes that the
amount of heavy elements In them is about 20 times less
than in stars of the main sequence. fheoretically possible
masses of such stars are comparable with the masses of
real sub-dwarfs. On the other hand sub-giants can be
explained on this model if one assumes that the amount
of heavy elements in this e;roup is four to five times
higher than in the stars of the main sequence. This is in
agreement with results obtained earlier (Ref. 5). It
is pointx_,A out that although it is possible to explain
the struzture of both sub-dwarfs and sub-giants on the
above mode2 -.,asing certain assumptions as to the heavy
element content -elative to the stars of the main sequence
it =at neverthelei,.: be remembered that the necessary
condition in all t4e cz,Lculations is full inter-mixing
(same chemical composition iL shell and n.1cleus) which in
Card 3/4 gone ral may not be obse rved. The re are 11 f i gure s 0

An Investigation of Evolutionary Sequences of Homogeneous Stellar
Models with a Convective Nucleus.
8 tables, 5 references, all of wnich are Slavic.
SUBMITTED: April, 12, 1957.
ASSOCIATION: State Astronomical Institute, i-:;,eni P.*,~. Shteimberg,
Potsdam Astronomical Observatory, German L)emocratic
Republic. (Gos. Astronomicheskiy In-t im.. 11.1%. '-hternberga,
Potsdamskaya Astronomicheskaya Observatoriya,*.iermanskaya
Demokraticheskaya Res-,publika.)
AVAIIAME: Library of Congres!-..
Card 4/4

I KASZVICH, A.G.
Journey of Soviet astronomers to the Unitod Stntes. Astron.tair.
no.184:24-26 S 157. (MIRA 11:4)
(RuRsts-Relations (G"narml) Vith United States)
(UnIted Stntes-Rolatione (General) With Russift)

GMIN, Te.Z.; IMIN. G.A.; WHOKIT, A.X~; ~Irdwu A -a-; ALIPIM, la.1o.;
CRUJMM~, X.F.; SUP=. B.S.; GAIKM A.X.; GORWY, O.G.; KOIWA,
A.F.; KCWV. LL; =207. A.T.; SEW, A.B.; CHUMV. V.I.;
TAZOnN. V.I.; KMH&TUW, A.A.. etwetstromW red.; WOOKOVA, N.P.d
doktor flue-4at. sank, otvetotvonnl7 red.; S11M. B.1.. red.;
PCWLIMIT. A.B., red.: PSUSAXOWA. ?.A.. t*Mu6 red.
(Prolimiumm7 results of the ociontific research on the first
Soviet artificial earth satellites and rocints; collection of
articles In the 11th section of the IGY prograa (roclats and
matelUses)] Prodwaritoll" Itogi nmchayykh Issledovanii a
powshch I 1u per~j' smotskikh Iskasstrenayft sputnikov z*aU
i rakmt; Aboralk statel (XI rasdol 1:rogrs=W XOG - rakety I
sputulk:1). Plookwa, lsd-vo Ah-4 mak SqqR. No.l. 1958. 148 p.
(xm 11210)
1. Im"a, (1923- U.S.SA) Nesbduvedoust"urn I , 'tot po
pm d*aUuXosw1um&ro4noC* goofizichaskoge god&. 2. Chlon-kor-
respondent AN SSW (for ftkhaylov).
(Atmosphere. Upper-Rockat observations)
Wtificial satellites)

X MOSUL ASSUNLY OF THr IMANATIQUI, ASTnOROWWAZ, =I0P
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RVOLUTION OF STARS 0mra"190 IN SAW
A.G. dessevitok
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who" "betas" is met . 4 rallf, leads to a cmtlauow ob~
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PHASE I BOOK EXPLOITATION sov/184o
Vsesoyuznoye astronomo-geodezicheskoye obshchestvo
Astronomicheskiy Kalendar; yezhegodnik. Peremennaya chast'; 1959
(Astronomical Calendar; Yearbook. Variable Part; 191-9) Moscow,
Fizmatgiz, 1958. 370 P. 8,500 copies printed.
Ed.: I.Ye. Rakhlin; Tech. Ed.: S.N. Akhlamov; Editorial Board:
P.I. Bakulin (Reap. ed.), S.G. Kulagin, A.G. Masevich, and
P. P. Parenago.
PURPOSE: This astronomical calendar is intended for specialists in
astronomy, astrophysics, and geophysics.
COVERAGE: The book Is divided into two parts. The first, based on
data taken from the USSR Astronomical Yearbook for 1959, consis%&
of ephemerides and accompanying text, compiled and written by the
following specialists: S.G. Kulagin and L.D. Kovbasyuk of the
GAGO (State Astronomical and Geodetical Soziety) - notes on
ephemerides, the ephemerides of the Sun and Moon; M.M. Dogayev
of the MOVAGO (Moscow Branch of the All-Union Astronomical and
Geodetic Society) - text and maps of the visible trajectories of
the planets, text and maps of eclipses, the physical coordinates
Card 1/1o

. .......... .
Astronomical Calendar; Yearbook. Variable Part; 1959 sov/1840
.1
of the Sun, Moon, Mars, and Jupiter the satellites of Jupiter
and Saturn; N.D. Rozenblyum (MOVAGO~ - emphemerides and hello-
centric longitudes of planets; I.F. Yegorchenko, A.A. Kaverin,
T.G. Konstantinova, V.A. Kuklina, G.V. Kuklin, Z.G. Sazonova,
L.I. Chernykh, and N.S. Chernykh - data on 144 points In t'-le
USSR for the full solar eclipse of October 2, 1959; Ye.G. Demido-
vich (GAGO) - occultation of the stars and planets by the Moon,
observation of the Polar Star, computation of stellar coordinates;
V.A. Bronshteyn (MOVAGO) - comets;N.S. Yakhontova - the lesser
planets; and, N.B. Perova (MOVAGO) - variable stars. The second
part, the Supplement, contains a review of the achievements in
astronomy for the years 1956 and 1957, written by V.A. Bronshteyn,
O.D. Dokuchayeva, L.A. Katasev, M.A. Klyakotko, P.P. Parenago,
and I.S. Shcherb4na-Samoylova under the editorship of A.G,_Mks-y
~& _a _Jc h,
articles on artificial satellites, the danger in astronautics from
meteors, the nature of galaxies, articles on scientific meetings
hold in the Soviet Union and abroad, and articles on the anniver-
saries of events in astronomy. The book is profusely Illustrated
with tables, maps, photographs, and diagrams. The Supplement
includes some 125 Soviet references grouped according to subject
matter and type of publication.
Card 2/10

Astronomical Calendar; Yearbook. Variable Part; 1959 sov/1840
TABLE OF CONTENTS:
From the Editors 5
PART I. EPHEMERIDES
Explanations to the Ephemerides 7
Ephemerides of the Sun and Moon 16
Planets 40
Eclipses 64
Occultation of Stars and Planets by the Moon 79
Physical Coordinates of the Sun, Moon, Marajand Jupiter go
Jupiter's Satellites 98
Card 3/10

Astronomical Calendar; Yearbook. Variable Part; 1959 sov/184o
Saturn's Satellites 110
Comets ill
Lesser Planets ill
Variable Stars 113
Notes on Observations of the Polar Star 121
Notes on the Computation of Stellar Coordinates 130
PART II. SUPPLEMENTS
Advances in Astronomy in the Years 1956 an* 1957 134
This article discusses the observatory studies made on
solar activity, the structure and temperature of the chromo-
spherej the exterior of the solar corona, studies conducted
at the Crimean Astrophysical Observatory, large-scale and
turbulent motions in the Sun's photosphere, studies of the
Sun's general and localized magnetic fields, the stars
Card 4/10

Astronomical Calendar; Yearbook. Variable Parf; 1959 Sov/1840
including the variable ones, the spiral structure of the Galaxy,
the Sun, the planets, comets, the Moon's atmosphere, the nature of
Venus and Mars, and the meteors.
Artificial Satellites of the Earth and the Danger in Astronautics
Fran M&Wors (V.V. Pedynakiy) 197
The author rerorte mainly on studies of cosmic rays, the Sun's
corpuscular :-adiation, micrometeorites (recorded by means of
ammonium-phosphate piezoelectric counters) and the annual dis-
tribution of micrometeorites and their tentativ- quantities.
The Mrkos Comet (1957 d) (F.Yu. Zigell) 208
This article discusses the I os Comet which was discovered
on August 3, 1958. The com-"
et a parabolic orbital elements
are computed and the comet photographed. Observed by several
Soviet astronomers its study provided much now material.
Card 5/10

Astronomical Calendar; Yearbook. Variable Part; 1959 sov/184o
Noctilucent Clouds in 1957 (N.I. Grishin) 214
Stersotriangulation methods for determining the height of
clouds are described.
Interaction and Nature of Galaxies (B.A. Vorontsov-Vallyaminov) 231
This article treats galactic bodies, tails, the units
bridging them, and also double and multiple galaxies.
Soviet Astronomers in the United States of America (A.G. Pkeevich) 243
This article describes the June-July 1957 visit cf a Soviet
delegation of astronomers, headed by V.A. Ambartsumyan, to
the United States.
The Eighth International Astronautical Congress (A.G. Masevich) 263
This article describes the Astronautical Congress hold
October 12, 1957 in Barcelona.
Card 6/10

Astronomical Calendar; Yearbook. Variable Part; 1959 SOV/1840
Joint Visiting Session of the Astronomical Council of the AN
SSSR and the Academy of Sciences of the Azerbaydzhan 33R
(M.A . Klyakotko) 271
This article treats the meeting at which M.M. Aliyev,
A.A. Mikhaylov, A.A. YakovkIn, S.K. Vaekhsvyatskiy,
V.V. Sharonov, V.P. Shcheglov, Z.I. Khalilov, V.A. Krat,
and G F. Sultanov participated.
The 350th Anniversary of the Formulation of Keppler's First
Two Laws (Yu.A . Ryabov) 275
This article is a historical account and discussion of
Keppler's first two Laws.
The 85th Anniversary of the Tashkent Astronomical Observatory
(V.P. Sheglov) 286
The article provides a detailed historical account and
description of the Tashkent Astronomical Observatory of
the Academy of Sciences of the Uzbek SSR, the oldest scien-
tific research Institution in Central Asia. The Observatory
Card 7/10

Astronomical Calendar; Yearbook. Variable Part; 1959 sov/184o
maintains Its own meteorological station, a Time Station which
provides 17 time signals In 24 hours, a 3olar Laboratory which
conducts systematic studies of the Sun's chromospheric flares
on the basis of spectroscopic and photometric observations
(Yu.M. Slonim, Chiefj and K.F. Kuleshova, Z.B. Korobova, and
B.N. Tirnshteyn, staff members), and a network of meteoro-
logical and other research staUons. Of particular interest
is the Kitaba International Latitude Station imeni Ulugbek
situated 3 km,from the town of Kitaba in the Kashka-Darlinskaya
oblast'. Administered by the Observatory since 1941, the Statlon
has conducted regular observations since 1930. Its staff members
Include A.M. Kalmykov, Director, D.I. Kravtsev, scientisti and
P.V. Shcheglov and V.S. Obraztsov, laboratory assistants. A
zenith-telescope APM-2 was installed there In June 1958. In 1932
the Observatory came under the jurisdiction of the Committee on
Science of the Central Executive Committee of the Uzbek SSR,
since which time it has engaged in a program of research in exact
time determination, solar activity, and meridian and photographic
astronomy. It had been conducting regular observations of sun
spots and solar protuberances since 1932. The Observatory's staff
includes N.F. Bykov, who completed the work begun in 1945 of
determining the direct ascenalon of weak stars by the absolute
Card 8/10

Astronomical Calendar; Yearbook. Variable Part; 1959 sov/184o
method; Kh.R. Shakirova, B.V. Yasevich, and A. Kadyrovwho made
thorough studies with two passage instruments of personal and
instrument errors: V.P. Shcheglov, V.T. Beds, B.Zh. Ballzhinova,
B.V. Yasevich, N.A. Omelina, L.N. Koshkina, M.G. Llvovajand
G.I. Kazakov
,)who, in cooperation with IGY program, engaged In
daily determinations of time corrections on two passage instru-
ments and In the reception of a large number of rhythui% signals,
V.A. Malltsev and N.N. Sytinskaya - observation of meteors;
A.A. Latypov, I.M. Ishchenko,and G. Kim - regular photographic
observations of the Earth's artificial satellites; F.G. Ustimenko,
Chief Mechanical Engineer, and Ye.P. Kolesnikova, Head Librarian.
Some of the newer equipment possessed by the Observatory include:
a passage instrument APM-10, new printing chromographs, radio
reception and measurement apparatus, two sets of quartz clocks
obtained in 19,1:8, a normal astrograph, a meridian circle, a zenith-
telescope APM-2 set up in 1957, a solar protuberance spectroscope
(obtained 1932), a standard spectrohelioscope (obtained 1935), a
Card 9/10

Astronomical Calendar; Yearbook. Variable Part; 1959 sov/1840
chromo3phere-photosphere telescope, a celostat with a clock
mechanism for spectrohelloscope, and a microphotometer MF-4.
The Tashkent Astronomical Observatory (TAO) published its own
Trudy, a Byulleten', and Circulars,
The TOth Anniversary of the Gorlkiy Division of the All-Union
Astronomical-Geodetical Society (S.G. Kulagin) 315
Anniversary of Soviet and World Astronomy in 1959 (Yu.G. Perell) 325
The article treats briefly the Committee on Solar Research
of the Academy of SciencesUSSR.
The Tenth International Astronomical Meeting In Moscow
(D.Ya. 14artynov) 350
Bibliography (Yu.G. Perell)
AVAILABLE: Library of Congress
362
Card 10/10 MM/ad
6-17-59

8079L
3,7,300 SOV/169-59-6-637'-~
Translation from- Referativnyy zhurnal, Geofizika, 1959, Nr 6, pp 140 - 14-1,
(USSR)
AUTHORSg Gindin, Ye.Z., Leykin, G.A., Lozinskly, A.,M., Masevich, A."
TITLE~ The Optical Observations of Artificial Earth
I
FERIDDICAL, V sb,~ Predvarit. itogi nauchn. issled. s pomosh-hlyu p,~--ykn
sov. Iskustv. sputn1kov Zemll i rakr--*., Mo2ocow, AS USSP,
Pp 5 - 39 (Engl. Res.)
ABSTRAC':., The Astronomicheskly sovet Akademll nauk 33SR (Coun,~;! cf
Astronomy of the USSR Academy of Sciences was put In ha-g--
of organizing the optical observatiorA of artifirlal eirth
satellites. Sixty-sIx visual stations and "menty-four
graphic stations were established for obsqrvIig the satc!'I!.,~s
The visual observation stations begar ~,helr a--.11vII,v a, 'he --r-
when the first Soviet satellite was laun.-hed, whil- -ho,-Dgrar-
observations have been performed systematIcally sln"e the b-
ginning of 1958. The visual observation methcdF wcr~
Card 1/6 by the task,~. +,hey must establish tne posit-Jor- of a

80794
SOV/169-59-6-15375
The optical Observations of Artificial Earth Satellites
the celestial sphere with an accuracy of 0.5 to 1 0 and the time wl-.hin 0 5 to
.1 see, and must report the observation results to the computer center within
the shortest time. Two "optical barriers", each consisting of about 30 tele-
scopes, were established to facilitate the observation of Batellltv3 having
a low brightness and moving on the sky with a velocity of 10 per I sec, if
the orbit Is known only approximately, The barriers are located on the
meridian and along a vertical circle perpendicular to the viss-ible orb!-t. of
the satellite. The sight lines of the telescopes are adjusted in such a
way that each section of the optical barrier is covered twice. For determining
the time of passage of a satellite with an accuracy exceeding I sec, th& time
signals and the signals given by the observer at the time when the sat.elittte
passed, are recorded on tape. After the termination of the observations, th~
tape recording is reproduced at a low speed and the precise moment of passage
is determined by a chronoscope. The coordinates of the satellite ar-9 deter-
mined by the sidereal maps of A.A. Mikhaylov's atlas or of A. Bechvarzh's
atlas, W4en observing satellites of low brightness (15 stellar magnitude)
the AT-ltelescope is used, which is a small wide-angle telescope having a
50 mm objective lens and six-power magnification., The field of view is 110
Card 2/6

80794
SOV/169-59-6-637~)
The Optical observations of Artificial Earth Satellites
The stations observing the satellites are provided with signals of the correct
time-by feeding to them second tone signals. On the basis of observation data.
the computer center informs the stations m the coming passage of a satellite
The station receives a coded telegram containing information on the t1me and
altitude of a satellite's passage in the meridional. plane and In the plane in
which the nearest point of the orbit Is located, Observations of artificial
satellites are also-performed on the territories of the Chinese People's
Republic (KNR), the German Democratic Republic (GDR), Czechoslovakia, Poland
Hungary, Rumania, and Bulgaria, where 45 stations are in operation Further:
observatories in England, Scotland, Ireland, the US and other countries were
included in the visual and photographic observation system of the Sovlel~
satellites. At some stations. besides the visual observations, tha! posl,~ionS
6 0
of the carrier rocket and the se d Soviet satellite are determined pho-~o-
graphically byo*Zorkiy" camerasltiZ~ "Yupiter 8" lensesP At the time of thp
satellites passage across the rield of view of the camera, the shutler Is
opened for a brief time interval (2 - 5 sec) . The begin and the end -.~f *.n~
exposure are marked by a chronograph. Tt is possible to determine tv pho'..-
Card 3/6

80794
sov/169-59-6-637L,
The Optical Observations of Artificial Earth Satellites
graphic observations the position of a satellite with an accuracy of 31 - 5'
of arc. The Council of Astronomy discussed the problem of using light
flashes of short duration on the object for a precise determina-~ion of a
satellite's position. The position of a satellite may be determined with an
acr,uracy of 2 - 3 see of are when using cameras with a long focal length
(F - -1 m) for photographing the satellite, UsIngthe data of Ihese ob-
servations for triangulation%vo-n the earth's surface, the distance between
different points (especially between continents) and also the shape of tine
geold may be determined with an accuracy of 10 m. However, the photography
of satellites is made difficult by the following circumstances, 1) the ob-
servations are possible only at dusk; 2) cameras with a very great. light
power are required; 3) the setting of precise time marks is complicated,
These difficulties can be overcome If the satellite is equipped with a light
source producing brief flashes by which it may be photographed at night. It
is expedient to provide series of flashes and not a continuous feed, taking
into consideration that at least two or three flashes must arrive In the
field of view of the instrument, In this way it is possible to determine
not only the position but also the angular velocity of a satellll~e. otvlou~_ly,
Card 4/6

8079h
30V/i69-59-6-6375
The OpticAl Observations of Artificial Earth Satellites
a pulse gas discharge lamp should be used as a llgh"~ sc r:e, whose Ignt
output reaches 60 lnVvs. The brightness of a satellitel depends or. ~.he
following reasons; 1) changes in the satellite's phases, i e in the
Gonfl,guration sun - satellite - observer; 2) changes in the distance
the observer; 3) light absorption in the section of its path from tlh-
satellite to the observer; 4) rotation and-tumbIlrigQ(f a satellite,
5) changes in the state of the satellite's surface, The determinallon of
the period of rotation (tumbling) of the satellite's body and ohanges of
period in time are of the greatest interest, Another important pr,-.~t-`err
is the investigation of the dependence of the brightness and :o1or of a
satellite on the state of the earth's atmosphere. Finally, the thi-d
problem is the change of the state of the satellite's surface binder *~,,e
influence of the atmosphere and extraterrestrial agents. Fo- srlvlng
the aforementioned problems a precise quantitative determina-,Ion of
brightness changes of a satellite and observations over a possibly great
sect'lon of its trajectory are necessary. Presently, two methods are ased
for measuring a satellite's brightness. The first method consists in a
UK
this
Ca rd 5/6

8079h
SOV-169-59-6-6371c,
The Optical Observations of Artificial Earth Satellites
comparison of the brightness of the satellite's trail with the brightness of
the trails of neighboring stars on a photography obtained by a stationarv
camera. The second method consists In a visual comparison of the UK
brightness with the brightness of stars located along its path. Bo-J,. metnods
are used at Soviet observation stations.
L,V. Terent'yeva
Card 6/6

IA)ZINSKIT. A.k: WEVICH. A.G.
- ------
Optical observations of artificial earth satellitea in the U.S.S.R.
Meshdunar. geofts. god no.5:23-28 '58. (KIRA 11:10)
(Artificial satellites)

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e re q re r - c -: o n 9 r 77
-a r

AUTHOR: Masevich, A. C.) De-,"It Cl;uirm,:". of tile
J~_,qtronomic.rll Co .:.ci'- .,S 1~'~SR
TIfLE: A New Ef fi, I! a Ci O-J 3 ln.3 f- r t.1-it
Knowledge of the 'Universe eKtivno5~e oru.__i,-_-
ani'a
PERIODICAL: Vestnik I'LE SSSR, -,5Fj, Vol. 26, ~'r 1, _p. e-12 (T,'s:;R)
ABSTRACT: The first earth Was Of 3,-'herical ~_I.d ".-tal
diameter of 5'~ cin ,-,rd a of 67,6 kL. It -sas la":nc-,ed --n
Oct:-.ber 4, 1957 --aid 'isa~peared or. Januar-, Jj, 19'~5. TKe
Createst lieig-ht ef its nrbit was ?00 km. Tl.t~ Z:_rth
ratellite forms t`.f~ last rocket ste- and --eithts acre than
-he i-ree-test heirht 1
112 ton. of -its orbit is 7C,%~ ki.. 'h e
orbits of the earti: satellite h..ve a proximat-_-I~ the form,
of un ellinsc, Ori, of th,~ foci of vhich is in the center
of the ~-,rth. Phu !-1ane of both orbits is inclined to'caris tif,e
equatorial :)!dine an in:.le of 650. Because, of the
rotation of the th,-. earth satellite in e-ch
succesnive revolution passes a domain -%hich is located
al-proximately by 1000 to 17000 km more 'hest thLn the
Card 1/3 preceding one, in de-endence of the deEree of latitude.

A N ew Ef f i c a c i ou s I i. !. ru;., -- r; t fKnowledge of
the Universe
2he period Gf' :t r,)t;:itiori of the first earth satelliti:
firr,t amouiited to 96,2 minut"-s and that of the second to
10397 minutes. Tht-- earth satellites are visible only
at dusk without thf-: help -)f it telescope etc. For th,; ~ur--ose
of optical ob~;erv,j~ion ----f artificial earth
th~, Astroro%Acril C,-,~i,-.cii 0 USSR or,anized 66
3tation3 at the Ph,sic;tl-.'Aat1.ematical Faculties cf
univ~rsit:e!; and iediij-0,,ic iflStitutt!s. A ~3pecial small-
sized tele3co;-~- AT-' --'(~-velop-d bind producud, of .-I.ic"'.
titation 20-2.,; ',irthe-rmore, star char's, f-,t.);?
watc'-,t--s, atid a ril~--vic,; for r~cordii16 ob.,3t:rvi--d' ti~.ies
and thL- of --act tim.- sii-Tih1s -iiere providel. 1'1e
or LLniz:ttion fc.- i.- lescribed in -letail, it. thich
conn,:ctic).,, lalso t:,,- :-1,6toj 1-~%- I.,.atl-.od is [.'Ienli it'. ~. Oil the
busis k-~f j.-.cA'Lfic.!tions cf the
or'-,i'. co.,.171--isiori:3 ;r:t-r- c-cncerr,in.-, the co-2~fic; tion
thp force c-f , r;-.vit~ at v ., ious pointq of the -Lrth.
ri--- r t li-~ i i :,, t r! 'iti L i on of e mans of 01--, -irth r:tri
1:3 nut posgible in it thorout:1-1
Card 2/~ 1) , 'To :irt if icial etirth sate lite:i tire

A New Efficacious Instrument f-.r th Krawlefts of
the Universe
flying I&-boratories and make direct observations of the
ionos7,here of the u,-per atm-odheric strata, of shortwave-
solar radiation, ~o-jsible, %,hich is impossible to be carried
out from tht-- earth. In this way also the primarj cosmic rays
can be investJ~.-ated. By taking -ith it a living beinL (dok:)
the second artificial earth sate'-lite mado it ~osaible
to carry out medical and bioloLical invustiLationsq the
results of which will contribute Lreatly towards makinU the
flight of human beinLs into cosmic s ace .-.-ithout dant.ter
possible. In this way the most important problems of tstro-
and t:eoph.(sico can be investiL;ated and studied, whicl. J.3
impossible on -3arth.
ASSMATION: Astronomical Council AN USSR (A3tronomicheskiy sovet
Akademii nauk 533R).
1.,VAI I AB LE Library of CoriCresa
1. -Ratellites-Nomenclature 2. S&ts311t"-*OtiOn 3. Satellites-
Card 3/3 Observation

30)
AUTHOR: Wj Sh A S 3V/'z'z- 3 z - 2-14,121
TITLE: On Some Peculiar Stars Below th, Main Sequence of the
H-R Diagram (0 nekotorykh pekuliarnykh zvezdakh, nakhodyashchikh-
sya pod glarnoy posledovatellnostlyu diagrammy Ressella)
PERIODICAL: Astronomicheskiy zhurnal, 1958, Vol 35, Nr 2,pp 292-294 (USSR)
ABSTRACT: According to the proposal of P.P.Parenago the author cons-'ders
four stars ( XBoo, 29 Cyg, )Aqr, 2 And) with peculiar spectra
which lie below the main sequence of the 2-R diagram. There
seems to be no reaaon for taking these stars as representatives
of population II. Their present position on the H-R diagram
can be explained if they are considered as initially main
sequence stars (1 0 -e.M4 20 , 0.84X40.9, 0.01