Effects of Rotation on Mass Loss for Population III stars

Details Effects of Rotation on Mass Loss for Population III stars Effects of Rotation on Mass Loss for Population III stars

2005-11-02

arxiv.org/abs/astro-ph/0511080v1

Astronomy and Astrophysics

Astrophysics

4 pages, 3 figures, to appear in Tartu Workshop Proceedings "Stellar Evolution at Low Metallicity: Mass Loss, Explosions, Cosm

Scientific paper

The effects of rotation on low-metallicity stellar models are twofold: first, the models reach break-up during main sequence and may lose mass by mechanical process; second, strong internal mixing brings freshly synthesized elements towards the surface and raises the effective metallicity to higher values, so that the initially very low radiative winds are enhanced. Those two effects are also found in Z=0 models, but to a lesser degree because of structural differences. This weak mass loss becomes interesting though in the case of the black hole-doomed stars (25-140 M_\sun and > 260 M_\sun) because it allows these stars to contribute to the enrichment of the medium by stellar winds.

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