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On the Distribution of Young Spectroscopic Binary Stars Over the Major Semiaxes of their Orbits

Published online by Cambridge University Press:  12 April 2016

E.I. Popova ,
A.V. Tutukov ,
B.M. Shustov  and
L.R. Yungelson
E.I. Popova
Affiliation:
Astronomical Council, USSR Ac. Sci.
A.V. Tutukov
Affiliation:
Astronomical Council, USSR Ac. Sci.
B.M. Shustov
Affiliation:
Astronomical Council, USSR Ac. Sci.
L.R. Yungelson
Affiliation:
Astronomical Council, USSR Ac. Sci.

Extract

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About 60% of stars of the disc population in our Galaxy are close binary systems (CBS). Half of the known CBS are spectroscopic binary stars (Kraitcheva et al., 1978).

To know the distribution of a correlation between the masses of CBS components and semiaxes of their orbits is necessary for the investigation of the origin and evolution of CBS. For such statistical investigations, a catalogue of CBS was compiled at the Astronomical Council. The catalogue is based on the 6th Batten catalogue (Batten, 1967), its extensions (Pedoussant and Ginestet, 1971; Pedoussant and Carquillat, 1973) and data published up to the end of 1980 (Popova et al., 1981). Now it is recorded on magnetic tape and contains data on 1041 spectroscopic binaries; 333 of them are stars with two visible spectra. The latter are mostly systems prior to mass exchange and the distribution of physical parameters in these systems reflects the distribution and presumably conditions at the time of formation. Using some assumptions, we can obtain for spectroscopic binaries masses of the components M1 and M2 (or the ratio q = M1/M2) and semiaxes of their orbits. Masses of components with the known sin i were obtained by the usual technique; when sin i was not known, masses were estimated from the spectra. We shall discuss here the distribution of CBS in the M-a plane.

Type
Part II: Evolutionary Trends in Wide Binary Systems
Information
International Astronomical Union Colloquium , Volume 69: Binary and Multiple Stars as Tracers of Stellar Evolution , 1982 , pp. 129 - 131
Copyright
Copyright © Reidel 1982

References

Batten, A., 1967, Publ. Dominion Astrophys. Observ. 13, No. 8.Google Scholar
Cohen, M., Kuhi, L.V., 1979, Astrophys. J., 227, L 105.Google Scholar
Kraitcheva, Z.T., Popova, E.I., Tutukov, A.V., Yungelson, L.R., 1978, Astron. Zh. 55, 1176 (English translation in Soviet Astronomy).Google Scholar
Larson, R.B., 1969, Monthly Not. Roy. Astron. Soc., 1969, 145, 271.Google Scholar
Pedoussant, A., Ginestet, N., 1971, Astron. and Astrophys. Suppl. Ser., 4, 253.Google Scholar
Pedoussant, A., Carquillat, J.M., 1973, Astron. and Astrophys. Suppl. Ser., 10, 105.Google Scholar
Popova, E.I., Tutukov, A.V., Yungelson, L.R., 1981, Astron. Zh., in press.Google Scholar
Svechnikov, M.A., 1969, Catalogue of Orbital Elements, Masses and Luminosities of Close Binary Stars, Ural Univ. Press, Sverdlovsk.Google Scholar
Hall, D.S., in: Multiply Periodic Variable Stars, Proceed. IAU Coll. No. 29, Budapest, 1976, p. 287.Google Scholar