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Wolf-Rayet stars from Very Massive Stars

Published online by Cambridge University Press:  23 January 2015

Norhasliza Yusof
Norhasliza Yusof*
Affiliation:
Department of Physics, University of Malaya, 50603 Kuala Lumpur, Malaysia email: [email protected]
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Abstract

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Many studies focused on very massive stars (VMS) within the framework of Pop. III stars, because this is where they were thought to be abundant. In this work, we focus on the evolution of VMS in the local universe following the discovery of VMS in the R136 cluster in the Large Magellanic Cloud (LMC). We computed grids of VMS evolutionary tracks in the range 120–500 M⊙ with solar, LMC and Small Magellanic Cloud metallicities. All models end their lives as Wolf-Rayet (WR) stars of the WC (or WO) type. We discuss the evolution and fate of VMS around solar metallicity with particular focus on the WR phase. For example, we show that a distinctive feature that may be used to disentangle Wolf-Rayet stars originating from VMS from those originating from lower initial masses is the enhanced abundances of Ne and Mg at the surface of WC stars.

Keywords

stars: evolutionrotationWolf-Rayet
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 152 - 153
Copyright
Copyright © International Astronomical Union 2015 

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