2005/11/02 by Sylvia Ekström, Ekström, Sylvia, G. Meynet +5
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Pulsars and Gravitational Waves Research #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0511080
4 pages, 3 figures, to appear in Tartu Workshop Proceedings "Stellar Evolution at Low Metallicity: Mass Loss, Explosions, Cosmology" (eds: H. Lamers, N. Langer, T. Nugis), ASP Conf Series in press
arxiv created 2005/11/02 · openalex publication_date 2005/11/02 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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.