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The number of B-type binary mass gainers in general, binary Be stars in particular, predicted by close binary evolution
J. Van Bever and
Received 18 December 1995 / Accepted 27 June 1996
Compared to earlier studies on the subject, we use results of intermediate mass case B close binary evolution computed with updated data, to predict the population of B-type accretion stars for different regions of star formation, in the Galaxy and in the Magellanic Clouds. We will make a distinction between accretion stars with a (helium burning) subdwarf, respectively white dwarf and neutron star companion. Our population model incorporates recent ideas on asymmetric supernova explosions. Establishing a link between the formation of B-type accretion stars (mass gainers) and the formation of Be stars enables us to get an idea about the importance of close binary evolution on the Be star phenomenon. A comparison between the obtained results and the observations, related to regions of continuous star formation and starburst regions, reveals that only a minority of the Be stars (less than 20 and possibly as low as 5 ) is due to close binary evolution.
Key words: binaries: close stars: evolution Galaxy: stellar content galaxies: stellar content Magellanic Clouds
© European Southern Observatory (ESO) 1997
Online publication: June 30, 1998