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The Evolution of Very Massive Stars

descriptionPublicationkeyboard_double_arrow_right Article , Preprint , Other literature type 20 Apr 2007Embargo end date: 01 Jan 2007 Belgium, Canada English Publisher:American Astronomical SocietyJournal:The Astrophysical Journal, volume 659, pages 1,576-1,581 (issn: 0004-637X, eissn: 1538-4357,

Authors: Dany Vanbeveren; Dany Vanbeveren; J. Van Bever; Houria Belkus;

doi: 10.1086/512181 , 10.48550/arxiv.astro-ph/0701334

arXiv: http://arxiv.org/abs/astro-ph/0701334

handle: 20.500.14017/cb009300-55d0-4e74-a194-9daf02a59254

The Evolution of Very Massive Stars

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Abstract

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

16 pages, 4 figures, 2 tables. Accepted by ApJ

Countries

Belgium, Canada

Related Organizations

Keywords

Astrophysics (astro-ph), Stellar winds, FOS: Physical sciences, Stars -- Evolution, Astrophysics, Supergiant stars, Stellar evolution

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	citations This is an alternative to the "Influence" indicator, which also reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).	53
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	influence This indicator reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).	Top 10%
	impulse This indicator reflects the initial momentum of an article directly after its publication, based on the underlying citation network.	Top 10%