Pulsational characteristics of mass accreting stars in close binary systems
Abstract
Eclipsing binaries with pulsating components are a distinct subclass of binaries, merging orbital and pulsational analyses. In recent years, that subclass led to the definition of a newly formed branch of tidal asteroseismology. While single-star pulsators are well understood, the effects of binarity and possible mass transfer on pulsational characteristics, particularly in mass-gaining stars, remain to be systematically explored. Here, I present preliminary results on the asteroseismic properties of a mass-accreting model for a 10 M β Cephei-type star
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