The formation of Be stars through close binary evolution

Details The formation of Be stars through close binary evolution The formation of Be stars through close binary evolution

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...241..419p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 241, no. 2, Jan. 1991, p. 419-438.

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105

B Stars, Computational Astrophysics, Star Formation, X Ray Binaries, Neutron Stars, Star Distribution, Stellar Luminosity, Stellar Models, White Dwarf Stars

Scientific paper

The possibility that Be stars are the remnants of case B mass transfer in intermediate-mass close binaries is investigated. It is shown that only progenitors with mass ratios greater than a certain minimum value q-min are capable of producing a Be star after the mass transfer. The value of q-min lies between 0.3 and 0.5, depending on the evolution parameters as well as on the observationally determined lower mass limit of Be/X-ray binaries. In more than 80 percent of the predicted systems, the evolved companion is an He star, particularly among the late-type B stars; these systems may be detectable as XUV sources.

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