The post-RLOF structure of the secondary components in close binary systems, with an application to masses of Wolf-Rayet stars

Details The post-RLOF structure of the secondary components in close binary systems, with an application to masses of Wolf-Rayet stars The post-RLOF structure of the secondary components in close binary systems, with an application to masses of Wolf-Rayet stars

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.104...83h&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 104, no. 1, Sept. 1984, p. 83-109. Research supported by the Fonds Nationa

Astronomy and Astrophysics

Astrophysics

20

Binary Stars, Roche Limit, Stellar Evolution, Stellar Mass Accretion, Stellar Mass Ejection, Wolf-Rayet Stars, B Stars, Hertzsprung-Russell Diagram, Line Spectra, O Stars, Stellar Structure, Tables (Data), Thermal Stability, Two Body Problem

Scientific paper

The structure of the secondary components of a close group of model binary systems (with initial primary masses 15-30 solar mass and initial mass ratios 0.3-0.9) after Roche-lobe overflow (RLOF) and relaxation toward thermal equilibrium is calculated, assuming the primaries are evolving through the early B phase of mass transfer and allowing for the possibility of mass loss from the system during RLOF. The results are presented in graphs and tables showing the final evolutionary status, mass and mass ratio, chemical profile, and core-H burning lifetime of the secondary. The primary is found to evolve to a sueprnova before the exhaustion of the H core in all cases, and no WR + WR binaries are identified. These findings are then used to estimate the masses of 10 double-lined spectroscopic WR + OB binaries from observational data; most of the WR masses are in the range 8-14 solar mass and are smaller by factors as large as two than those compiled by Massey (1982).

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