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How to form a 200 M⊙ star

Published online by Cambridge University Press:  04 August 2017

Hans Zinnecker
Hans Zinnecker*
Affiliation:
Royal Observatory, Edinburgh, Scotland

Abstract

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Stellar coalescence is suggested as a possible mechanism for doubling the upper stellar mass limit from ∼100M⊙ to ∼200M⊙ in a moderately dense cluster of a few hundred young massive stars (∼105 M⊙ pc−3). The merger will be between the two components of the dominant central tight binary formed in the core of the cluster by the N-body evolution. This process may occur in some giant extragalactic HII regions.

Type
Poster Papers 2
Information
Symposium - International Astronomical Union , Volume 116: Luminous Stars and Associations in Galaxies , 1986 , pp. 271 - 273
Copyright
Copyright © Reidel 1986 

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