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