Volume 477, Number 1, January I 2008
|Page(s)||223 - 237|
|Section||Stellar structure and evolution|
|Published online||26 October 2007|
On the evolution and fate of super-massive stars
Astronomical Institute “Anton Pannekoek”, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands e-mail: firstname.lastname@example.org
2 Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya Str., 119017 Moscow, Russia
3 Isaac Newton Institute, Moscow branch, 13 Universitetskii pr., Moscow, Russia
4 Armagh Observatory, College Hill, BT61 9DG, Northern Ireland, UK
5 Section Computational Science, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
Accepted: 4 October 2007
Context.We study the evolution and fate of solar composition super-massive stars in the mass range 60–1000 . Our study is relevant for very massive objects observed in young stellar complexes as well as for super-massive stars that could potentially form through runaway stellar collisions.
Aims.We predict the outcomes of stellar evolution by employing a mass-loss prescription that is consistent with the observed Hertzsprung-Russell Diagram location of the most massive stars.
Methods.We compute a series of stellar models with an appropriately modified version of the Eggleton evolutionary code.
Results.We find that super-massive stars with initial masses up to 1000 end their lives as objects less massive than 150 . These objects are expected to collapse into black holes (with ) or explode as pair-instability supernovae.
Conclusions.We argue that if ultraluminous X-ray sources (ULXs) contain intermediate-mass black holes, these are unlikely to be the result of runaway stellar collisions in the cores of young clusters.
Key words: stars: evolution / stars: mass-loss / galaxies: clustere: general
© ESO, 2007
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