A. M. Cherepashchuk, V. G. Karetnikov


The statistical study of the mass ratios of the components and eccentricities of close binary systems was made. Relations between these characteristics are obtained. Results of the analysis allows to conclude that at least 70 of all known WR+O binary systems (with orbital period P < 20d) where formed as a result of mass transfer in massive close binary systems. Therefore, mass transfer through Roche lobe overflowing in massive close binary systems is an important mechanism of evolution in these interacting binaries.

Ключові слова

Stars; binary; Wolf-Rayet.

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Antokhina E.A., Cherepashchuk A.M.: 1988, Pis'ma Astron. Zhurn., 14, 252.

Cherepashchuk A.M.: 1981, MNRAS, 194, 761.

Cherepashchuk A.M.: 1991, in: Van der Hucht K.,Hidayat B. (eds.) Wolf-Rayet Stars and Interrelation with other Massive Stars in Galaxies, IAU Symp. No. 143, Dordrecht, Kluwer, 187.

Cherepashchuk A.M., Katysheva N., Khruzina T.S., Shugarov S.Yu.: 1996, Highly Evolved Close Binary Stars: Catalogue, Gordon & Breach, Brussels.

Cherepashchuk A.M., Moat A.F.J.: 1994, Ap.J., 424,L 53.

Karetnikov V.G., Andronov I.L.: 1989, Statistical properties of eclipsing binary stars in the stage of initial mass exchange, Manuscript in Ukr. NIINTI, Kiev, No. 2629-89, 41 pp.

Karetnikov V.G., Cherepashchuk A.M.: 1998, Astronomy Reports, 42, 476.

Massey Ph.: 1981, IAU Symp., 120.

Moffat A.F.J.: 1995, in: Van der Hucht K.A., Williams P.M. (eds). Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution, IAU Symp. No. 163, Dordrecht, Kluwer, 213.

Paczynski B.: 1973, in: Barry M., Sahade J. (eds.) Wolf-Rayet and High Temperature Stars, IAU Symp. No. 40, Dordrecht, Reidel, p.143.

Shore S., Livio M., Van den Heuvel E.P.J.: 1994, Interacting Binaries, Berlin-Budapest, Springer-Verlag.

Tutukov A.V., Yungelson L.R.: 1973, Nauchn. Inform., 27, pp. 58, 70, 86.

Van den Heuvel E.P.J., Heize J.: 1972, Nat. Phys.Sci., 239, 67.

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