Abstract
For the evolution of the secondary component of a massive close binary system, it is generally assumed that the mass accretion during core H-burning simply leads to its rejuvenation, i.e. that it evolves like a normal main sequence star with a mass corresponding to its mass after the accretion ceased. We reinvestigate this problem in the framework of a time-dependent semiconvection theory. We find that the process of adaptation of the convective core size to the new (larger) stellar mass may not be completed until core hydrogen depletion, i.e. no rejuvenation occurs. The resulting secondaries show strong differences compared to single stars of same mass.
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© 1994 Springer Science+Business Media Dordrecht
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Braun, H., Langer, N. (1994). On the Evolution of Secondary Components in Massive Close Binary Systems. In: Vanbeveren, D., van Rensbergen, W., de Loore, C. (eds) Evolution of Massive Stars. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1080-8_49
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DOI: https://doi.org/10.1007/978-94-011-1080-8_49
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-4471-4
Online ISBN: 978-94-011-1080-8
eBook Packages: Springer Book Archive