The evolution of very massive stars

被引：51

作者：

Belkus, H. ^{[1
]}

Van Bever, J.

Vanbeveren, D.

机构：

[1] Vrije Univ Brussel VIB, Astrophys Inst, B-1050 Brussels, Belgium

[2] St Marys Univ, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada

[3] Univ Louvain Associat, Grp T, Dept Math, B-3000 Louvain, Belgium

来源：

ASTROPHYSICAL JOURNAL | 2007年 / 659卷 / 02期

关键词：

stars : evolution; stars; winds; outflows; supergiants;

D O I：

10.1086/512181

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Core collapse of dense massive star clusters is unavoidable, and this leads to the formation of massive objects, with masses of up to 1000 M-circle dot and even larger. When these objects become stars, stellar wind mass loss determines their evolution and final fate, and decides on whether they form black holes (with normal mass or with intermediate mass) or explode as a pair-instability supernova. In this paper we discuss the evolution of very massive stars and present a convenient evolution recipe that can be implemented in a gravitational N-body code to study the dynamics of dense massive clusters.

引用

页码：1576 / 1581

页数：6

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