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Helium-star Mass Loss and Its Implications for Black Hole Formation and Supernova Progenitors

Published online by Cambridge University Press:  05 March 2013

Onno R. Pols  and
Jasinta D. M. Dewi
Onno R. Pols
Affiliation:
Department of Mathematics, PO Box 28M, Monash University, Vic 3800, Australia Astronomical Institute, Postbus 80000, 3508 TA Utrecht, The Netherlands; o.r.pols@astro.uu.nl
Jasinta D. M. Dewi
Affiliation:
Astronomical Institute, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands; jasinta@astro.uva.nl Bosscha Observatory and Department of Astronomy, Lembang 40391, Bandung, Indonesia
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Abstract

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Recently the observationally derived stellar-wind mass-loss rates for Wolf-Rayet stars, or massive naked helium stars, have been revised downwards by a substantial amount. We present evolutionary calculations of helium stars incorporating such revised mass-loss rates, as well as mass transfer to a close compact binary companion. Our models reach final masses well in excess of 10 M⊙, consistent with the observed masses of black holes in X-ray binaries. This resolves the discrepancy found with previously assumed high mass-loss rates between the final masses of stars which spend most of their helium-burning lifetime as Wolf-Rayet stars (˜3 M⊙) and the minimum observed black hole masses (6 M⊙). Our calculations also suggest that there are two distinct classes of progenitors for Type Ic supernovae: one with very large initial masses (35 M⊙), which are still massive when they explode and leave black hole remnants, and one with moderate initial masses (˜12–20 M⊙) undergoing binary interaction, which end up with small pre-explosion masses and leave neutron star remnants.

Keywords

binaries: closeblack hole physicsstars: evolutionstars: mass lossstars: Wolf-Rayetsupernovae: general
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 19 , Issue 2 , 2002 , pp. 233 - 237
Copyright
Copyright © Astronomical Society of Australia 2002

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