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Helium stars: Towards an understanding of Wolf–Rayet evolution

Published online by Cambridge University Press:  28 July 2017

Liam A. S. McClelland  and
J. J. Eldridge
Liam A. S. McClelland
Affiliation:
Department of Physics, University of Auckland emails:lmcc054@aucklanduni.ac.nz, j.eldridge@auckland.ac.nz
J. J. Eldridge
Affiliation:
Department of Physics, University of Auckland emails:lmcc054@aucklanduni.ac.nz, j.eldridge@auckland.ac.nz
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Abstract

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Recent observational modelling of the atmospheres of hydrogen-free Wolf–Rayet stars have indicated that their stellar surfaces are cooler than those predicted by the latest stellar evolution models. We have created a large grid of pure helium star models to investigate the dependence of the surface temperatures on factors such as the rate of mass loss and the amount of clumping in the outer convection zone. Upon comparing our results with Galactic and LMC WR observations, we find that the outer convection zones should be clumped and that the mass-loss rates need to be slightly reduced. We discuss the implications of these findings in terms of the detectability of Type Ibc supernovae progenitors, and in terms of refining the Conti scenario.

Keywords

stars: evolutionstars: Wolf-Rayetbinaries: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 255 - 259
Copyright
Copyright © International Astronomical Union 2017 

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