Evolutionary Computations for Intermediate Mass Close Binary Systems
Numerical simulations of the evolution of close binaries with primary mass between 3 and 15 M⊙ and mass ratios of ∼1.5 were carried out. These results show that after mass transfer the system consists of a bright main-sequence star together with a faint He-star in a rather wide orbit (p> 60d) Evolution of this kind predicts isotope anomalies for the CNO-elements with respect to their solar values.
KeywordsMassive Star Convective Zone Close Binary Primary Mass Convective Core
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