The number of B-type binary mass gainers in general, binary Be stars in particular, predicted by close binary evolution.

Details The number of B-type binary mass gainers in general, binary Be stars in particular, predicted by close binary evolution. The number of B-type binary mass gainers in general, binary Be stars in particular, predicted by close binary evolution.

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...322..116v&link_type=abstract

Astronomy and Astrophysics, v.322, p.116-126

Astronomy and Astrophysics

Astrophysics

45

Binaries: Close, Stars: Evolution, Galaxy: Stellar Content, Galaxies: Stellar Content, Magellanic Clouds

Scientific paper

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.

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