Hirschi 2008 早期宇宙的恒星演化

主要内容:
也就是第一代恒星。
大于60Msun的可能在红巨星支损失足够多的质量而形成伽玛暴。

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Title:		Stellar Evolution in the Early Universe
Authors:		Hirschi, R.; Frischknecht, U.; Thielemann, F. -K.; Pignatari, M.; Chiappini, C.; Ekstroem, S.; Meynet, G.; Maeder, A.
Publication:		eprint arXiv:0808.3723
Publication Date:		08/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		8 pages, 4 figures, proceedings of IAU Symposium 255, "Low-Metallicity Star Formation: From the First stars to Dwarf Galaxies", L.K. Hunt, S. Madden & R. Schneider, eds
Bibliographic Code:		2008arXiv0808.3723H

Abstract

Massive stars played a key role in the early evolution of the Universe. They formed with the first halos and started the re-ionisation. It is therefore very important to understand their evolution. In this paper, we describe the strong impact of rotation induced mixing and mass loss at very low $Z$. The strong mixing leads to a significant production of primary nitrogen 14, carbon 13 and neon 22. Mass loss during the red supergiant stage allows the production of Wolf-Rayet stars, type Ib,c supernovae and possibly gamma-ray bursts (GRBs) down to almost Z=0 for stars more massive than 60 solar masses. Galactic chemical evolution models calculated with models of rotating stars better reproduce the early evolution of N/O, C/O and C12/C13. We calculated the weak s-process production induced by the primary neon 22 and obtain overproduction factors (relative to the initial composition, Z=1.e-6) between 100-1000 in the mass range 60-90.

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