Rotational mixing in close binaries

Details Rotational mixing in close binaries Rotational mixing in close binaries

2008-05-16

arxiv.org/abs/0805.2544v1

Astronomy and Astrophysics

Astrophysics

5 pages, 5 figures: to appear in the proceedings of IAU 252 "The Art of Modelling Stars in the 21st Century", April 6-11, 2008

Scientific paper

10.1017/S1743921308023223

Rotational mixing is 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 > 40 solar mass) 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.

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