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Rotational mixing in close binaries

Published online by Cambridge University Press:  01 April 2008

S. E. de Mink ,
M. Cantiello ,
N. Langer ,
S.-Ch. Yoon ,
I. Brott ,
E. Glebbeek ,
M. Verkoulen  and
O. R. Pols
S. E. de Mink
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected], [email protected]
M. Cantiello
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected], [email protected]
N. Langer
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected], [email protected]
S.-Ch. Yoon
Affiliation:
Dep. of Astronomy & Astrophysics, Univ. of California, Santa Cruz, CA95064, USA
I. Brott
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected], [email protected]
E. Glebbeek
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected], [email protected]
M. Verkoulen
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected], [email protected]
O. R. Pols
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected], [email protected]
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Abstract

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Rotational mixing a very important but uncertain process in the evolution of massive stars. We propose to use close binaries to test its efficiency. Based on rotating single stellar models we predict nitrogen surface enhancements for tidally locked binaries. Furthermore we demonstrate the possibility of a new evolutionary scenario for very massive (M > 40M⊙) close (P < 3 days) binaries: Case M, in which mixing is so efficient that the stars evolve quasi-chemically homogeneously, stay compact and avoid any Roche-lobe overflow, leading to very close (double) WR binaries.

Keywords

stars: rotationbinaries: closestars: Wolf-Rayetstars: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 365 - 370
Copyright
Copyright © International Astronomical Union 2008

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