EDP Sciences
Free Access
Volume 422, Number 3, August II 2004
Page(s) 981 - 986
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20034041
Published online 16 July 2004

A&A 422, 981-986 (2004)
DOI: 10.1051/0004-6361:20034041

Evolution of rotating binary stars

R. Q. Huang

National Astronomical Observatories/Yunnan Observatory, the Chinese Academy of Sciences, Kunmin 650011, PR China
    e-mail: bislan@public.km.yn.cn

(Received 2 July 2003 / Accepted 16 March 2004 )

A model for the evolution of rotating binary stars is presented. The evolution of a binary system consisting of a 9  $M_{\odot }$ and a 6  $M_{\odot }$ star is studied in the mass transfer phase Case A. Specific attention is focused on the differences between the evolutions with and without the effects of rotation. The results indicate that the effects of rotation prolong the lifetime of the primary, and causes its evolutionary track in the HR diagram to shift towards lower luminosity. The mass and the surface helium composition of the primary become lower and the orbital period of the system becomes significantly longer during the later stage of the evolution.

Key words: stars: rotation -- stars: evolution

© ESO 2004

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