SCIENTIFIC ABSTRACT FILIN, A.YA. - FEYGIN, N.P.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R000413030013-6
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 19
• Document Creation Date: November 2, 2016
• Document Release Date: June 13, 2000
• Sequence Number: 13
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

FILIN, A. ~~
,~z~-
V499 ScorplozilB. Blul.Stal.astron.obser. no.6:24-27 '53, (MM 7:9)
(St&rp, VRrlable)

FILIN, A.Ta.
- - . - o,1,
I - Xclipsing variable V 687 CYgni. Per.zvezdy 9 no.3:211
J& 153. (MLRA 7:7)
1. Staliattadelm7a astronomicheska7a observatoriya (Stalinabad)
(Stwo, Variable)

FILI _A-Y&-,--
Zero point on the period-luminosity curve for long-period Cepheide.
Biul.Stal.astron.obser. no.10:14-19 154. (KLRA 8:1)
(Stars, Variable)

3 -, - , ~-- F f, I:i~.7_:- -
FILIN, A. Ya,
Bleven stars considered to be probable variables. Astron.tsir.
no.164:20-21 0 '55. (MLRA 9:5)
1. Stalinabadekaya astronomicheakaya observatoriya.
(Stars, Variable)

FILIN, A.Ya.
I-Orie atatintical utudles of otare. fliul. Stal.antron.obser. no.22/23:
13-34 '57.. WIRA 11:7)
(Stars)

AUTHOR: Filin, A. Ya. 33-4-3/19
TITLE: Oxx Kineimttic Properties of B-stars. (0 Kinematicheskikh
oscbenwstyakh B zvezd).
PERIODICAL: Astronomicheakiy Zhurnal, 1957, Vol. 34, No.4
pp-525-538(USSR)'.
ABSTRACT: At 'the present time there is no generally accepted view
as to the causes of kinematic properties of B-stars.
Because of the current views on the origin of stars the
problem of B-stars is particularly topical.
In 1904, Adams and Frost (Ref-5) discovered the so-called
K-effect. Up to now about ten different explanations of
this effoct have been put forwgrd (Refs.?-15)-
Torondzbadze (Ref.16) has critically reviewed all these
hypotheses. The present author suggests that the general
shortcom:Lng of all these attempts to explain the K-effect
consisted in that they all ascribed new pmperties to
B-stars which, in turn, must be explained themselves.
Toroudzhidze's work is the only one where the problem of
the causes of kinematic properties of B-stars is correctly
formulated. These properties are them regarded as
Card 1/4 consequences of initial conditions during the form-ation.

On Kinematic Properties of B-stars. 33-4-3/19
of the st-ars. Assuming that the origin of B-stars
surrounding the sun is connected with the expansion of
stellar associations, Torondzhadze attemptz to explain
the kineinatic propertio-s of B-stars. However, the
hypothesis of expansion of stellar associations is not
well-founded (Of Kholopov, Ref.19 and Vorontsov -
Velyaminov, Ref .2;) -
The problem of the causes of kinematic properties of B-stars
is re-emimined by the present author. Results obtailied
are based on radial velocities. 1270 B-stars having known
radial velocities were used. 'The data of these stars
(radial velocitiest spectra, distances, etc.) were taken
from the card catalogue of the Department of Stellar
Astronom;7 of theShternb3rg State Astronomical Institute.
"Least squares" calculations for these stars lead to the
following results: 1. The constant-s of galactic rotation
A and B ~.Oortls-coeffs.~ are low. 2. The ratio of axes
of the ellipsoid of velocities which lie in the galactic
plane is close to unity (Table 2). At the same time, the
ratio does not differ from that generally accepted for
objects in plane subsystems. 3. The direction of the
Card 2/4 major axes of the ellipsoid of velocities is inclined

On Kinematic Properties of B-stars.
Card 314
33-4-3/19
to the direction through the centre of rotation. 4. In
the relations between other constants characterising the
motion, no differences are found compared with other
objects of the plane component. The number of possible
factors which may have an appreciable effect on the
kinematic constant is considered;
(A) Motion down the spiral arm is estimated to be almost
ne lagible;
(B5 The effect of the spherical component can explain
only a small part of the decrease in -the constant ofl
alactic rotation, "Aft;
The distortion of the values of "All and "B" may be
M
connected with an error in the determination of the mean
distance of B-stars, i.e. it is caused by an inaccuracy
in the :mean absolute magnitude and a determination of the
mean absorption . It is shown that these effects cannot
explain the change in "All either.
BO - B1 stars are found not to have any kinematic
peculiarities. Kamm's function is studied and it is
established that it shows anomalies for these stars in
~he neighbourhood of the sun. The north-sout~ aqymmetry

On Kinematic Properties of B-stars. 33-4-3/19
in proper motion8 and radial velocities is explained by
the rotation of the 1qcV system.
There are 5 figures, 11 tables and 36 references, 22 of
which are Slavic.
SUBMITTED: December 7,1956.
ASSOCIATION: Stalinabad Astronomical Observatory of the Academy,
of Sciencas of the Tadzhik S.S.R. (Stalinabadskays
Astronomicheskaya Observatoriya Alcademii Nouk Tadzhikskoy
SSR) .
AVAILABLE: Libi:eary of Congress
Card 4/4

;-+ I
FILINP A.7a.
dandow M I OWSBUMINAMAW,
Kinematic characteristics of B stars and the rotation of the local
system (with sumnaries in Gomm]. Antron. zhur. 34 no.6-838-S47
W-D 157. imm lito
1. Stalinabadskaya astronomichealmys. observatoriya AN Tad%hSSR.
(Stars--Proper motion)

FILIK, A.Ta.
Brief comments on chnnges in the brightness of 15 uninvestigated
variable stare. Astron. teir. no.191:19-21 MY '58- OGRA 11:9)
1. Stalinabadskaya astronomicheakaya observatoriya.
(Stare, Variable) -

FILIN, A. Ya.: Mas~cr Phys-Ilath Sci (cliss) -- of the movaiient of'
B-stars". Stalitiabad, 1958. 10 pp (Acad Sci Tadzhik SSR, T-nst of kitro-physics),
150 copics (K1,, No U, 1959, 100)

FILIN. A. Ya.
quarVI in a poselble long-peziod Cepheid. Astron.tair.
no.198:14 D 158- (MM 12:7)
1. Institut antrofiziki AU TadzhSSR.
(Cephaids)

RS Ophiuchi. Astron.tvirs n0.200:12-13 Mr 159. (MIRA 13:2)
1. Institut astrofisl3d AN Tadshikokoy SSR-
(Star@, Variable)

FILTN, A.Yao
n- - , ~
Phritcgrap"olic observations of six v&riable stars. Biu-1. inst. astro-
fiz. All Tadzh. S3R no.31:33-44 162.
Peteridning stellar comparison magnitudes for 15 variable stars.
Ibid. s 49-1,1 (MLRA 17:11)

L 19331-63 DIT (d)/EWII- W/FCC (.w)/BDS/FS (v) AFFTG/FSff-3/iJP(C) Fe-4,. OW
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ZSSION AIR300ZA4 S/0269/63/000/003/0039/0039
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00,113: RZh. Astionomiy~i. OtdolInyy vypusk. Abe. 5.51.364
AMOR: Filin, A. Ya.
TIMUP: Use oil the Xamn method
CITED SOURCE: Byulleti)nt Instituta astrofizW.iAN TadzhSSR, no. 32, 1962, 3-16
,;ioh,, -a btronomical observatlo~
TOPIC M S: Kai= func:,,
jT?,JVSLkTION: To study the influence of random errors of radial velocities and IIP
vanca3 and of the disporsion.of velocities on deterainatio,
'dist n of Kammfs functi2n,
the author coilst-ructs a kinematic model of a plane star system. For each of 1,380
points un-4fo*.-;:,-Iy distributed in a circle with a radius of 3 kps, centered on the
sun, for t1he law of radial velocitieu
(a + bR2)-l
(where is the 'distance f r:bm '12he galactic center and aand b are constants), he
determines the radial volocities, distances, Ve values of Kamm's function and
Card

L 19.331-63
ACCESSIOIN AR300201A.
ot"hor quzntL ties. These data are plotted on a card. The influence upon Kam% I s
fwnctaon of x-andom errors of distances and rad-Ul velocities and the role of the
dis-xrsion of radial velocities are studied by'adding to the card the values of the;
procica. distances and radial velocities and the corresponding random magnitudes,
~-it:i z-Wb-.cquont Plotting of graphs of Kam's function. '7he author concludes that
in t1ho prosence,of iando'M errors alone, Kamm's method yields entirely reliable
results. B. Fesonko i
nm- jwQ: 3omay63
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