Close binary systems before and after mass transfer. III - Spectroscopic binaries

Details Close binary systems before and after mass transfer. III - Spectroscopic binaries Close binary systems before and after mass transfer. III - Spectroscopic binaries

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ap%26ss..87..377v&link_type=abstract

Astrophysics and Space Science, vol. 87, no. 1-2, Oct. 1982, p. 377-401. Fonds de la Recherche Fondamentale Collective

Astronomy and Astrophysics

Astrophysics

20

Binary Stars, Computer Programs, Mass Transfer, Stellar Evolution, Stellar Models, Stellar Spectra, Bolometers, Roche Limit, Stellar Luminosity, Stellar Mass Ejection, Stellar Temperature

Scientific paper

A method is presented, for the computation of absolute dimensions from spectroscopic data on binary systems, which has been adapted for use with the 7th Catalogue of Batten et al. (1978) and takes into account several results of close binary evolution, with emphasis on the phase of slow mass transfer during a case B mass transfer. Among the unevolved systems, the mass transfer case B is found to be the most abundant type of interaction. In the set of evolving systems, a subset of 18 interacting systems was found with mass ratio near unity, the first star being the mass loser as well as the brightest.

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