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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: S.E.deMink@uu.nl, M.Cantiello@uu.nl, N.Langer@uu.nl
M. Cantiello
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: S.E.deMink@uu.nl, M.Cantiello@uu.nl, N.Langer@uu.nl
N. Langer
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: S.E.deMink@uu.nl, M.Cantiello@uu.nl, N.Langer@uu.nl
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: S.E.deMink@uu.nl, M.Cantiello@uu.nl, N.Langer@uu.nl
E. Glebbeek
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: S.E.deMink@uu.nl, M.Cantiello@uu.nl, N.Langer@uu.nl
M. Verkoulen
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: S.E.deMink@uu.nl, M.Cantiello@uu.nl, N.Langer@uu.nl
O. R. Pols
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: S.E.deMink@uu.nl, M.Cantiello@uu.nl, N.Langer@uu.nl
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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

References

Bonanos, A. Z., Stanek, K. Z., Udalski, A., et al. 2004, Astrophys. J. L., 611, L33CrossRefGoogle Scholar
Cantiello, M., Yoon, S.-C., Langer, N., & Livio, M. 2007, Astron. Astrophys., 465, L29CrossRefGoogle Scholar
de Mink, S. E., Pols, O. R., & Hilditch, R. W. 2007, Astron. Astrophys., 467, 1181CrossRefGoogle Scholar
Evans, C. J., Smartt, S. J., Lee, J.-K., et al. 2005, Astron. Astrophys., 437, 467CrossRefGoogle Scholar
Heger, A. & Langer, N. 2000, Astrophys. J., 544, 1016CrossRefGoogle Scholar
Hilditch, R. W., Howarth, I. D., & Harries, T. J. 2005, Mon. Not. Roy. Astron. Soc., 357, 304CrossRefGoogle Scholar
Hunter, I., Dufton, P. L., Smartt, S. J., et al. 2007, Astron. Astrophys., 466, 277CrossRefGoogle Scholar
Kippenhahn, R. & Weigert, A. 1967, Zeitschrift fur Astrophysik, 65, 251Google Scholar
Lauterborn, D. 1970, Astron. Astrophys., 7, 150Google Scholar
Maeder, A. 1987, Astron. Astrophys., 178, 159Google Scholar
Maeder, A. & Meynet, G. 2000, Astron. Astrophys., 361, 159Google Scholar
Yoon, S.-C. & Langer, N. 2005, Astron. Astrophys., 443, 643Google Scholar
Yoon, S.-C., Langer, N., & Norman, C. 2006, Astron. Astrophys., 460, 199Google Scholar