The evolution of very massive stars

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dc.creator Bever, J. Van
dc.creator Belkus, H.
dc.creator Vanbeveren, D.
dc.date.accessioned 2014-11-14T15:17:01Z
dc.date.available 2014-11-14T15:17:01Z
dc.date.issued 2007-04
dc.identifier.issn 0004-637X
dc.identifier.issn 1538-4357
dc.identifier.uri http://library2.smu.ca/xmlui/handle/01/25907
dc.description Publisher's version/PDF en_CA
dc.description.abstract 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[circled 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. en_CA
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dc.language.iso en en_CA
dc.publisher American Astronomical Society en_CA
dc.relation.uri http://dx.doi.org/10.1086/512181
dc.rights Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
dc.subject.lcsh Stars -- Evolution
dc.subject.lcsh Supergiant stars
dc.subject.lcsh Stellar winds
dc.title The evolution of very massive stars en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Astrophysical Journal 659(2), 1576-1581. (2007) en_CA
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Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
 
Published Version: http://dx.doi.org/10.1086/512181
 
 

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