Abstract
By massive binaries we mean binaries with initial (ZAMS) mass of the primary beyond 15 M⊙, i.e. massive stars losing mass by stellar wind. Due to this effect layers of the initial convective core may appear at the surface, hence the atmospheric hydrogen abundance decreases. For lower mass stars as well as for massive close binaries, phases of mass exchange can occur during core hydrogen burning, shell hydrogen burning and helium burning. For massive close binaries mass loss by stellar wind already changes the orbital elements (see Chapter 15, eq. 15.34).
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
Literature
Iben, I.(Jr), 1985, The Life of an Intermediate Mass Star in a Close Binary, The Quarterly Journal of the Royal Astronomical Society
Author information
Authors and Affiliations
Rights and permissions
Copyright information
© 1992 Springer Science+Business Media New York
About this chapter
Cite this chapter
De Loore, C.W.H., Doom, C. (1992). The Evolution of Massive Close Binaries. In: Structure and Evolution of Single and Binary Stars. Astrophysics and Space Science Library, vol 179. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-2502-4_17
Download citation
DOI: https://doi.org/10.1007/978-94-011-2502-4_17
Publisher Name: Springer, Dordrecht
Print ISBN: 978-0-7923-1844-6
Online ISBN: 978-94-011-2502-4
eBook Packages: Springer Book Archive