
%0 Journal Article
%A Pols, Onno R. 
%A Dewi, Jasinta D. M. 
%T Helium-star Mass Loss and Its Implications for Black Hole Formation and Supernova Progenitors
%J Publications of the Astronomical Society of Australia
%D 2002/06/28
%V 19
%N 2
%P 233-237
%K binaries: close &#8212; black hole physics &#8212; stars: evolution &#8212; stars: mass loss &#8212; stars: Wolf-Rayet &#8212; supernovae: general
%R https://doi.org/10.1071/AS01121
%U https://www.publish.csiro.au/paper/AS01121 
%X 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&odot;, 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 (&#126;3 M&odot;) and the minimum observed black hole masses (6 M&odot;). Our calculations also suggest that there are two distinct classes of progenitors for Type Ic supernovae: one with very large initial masses (&gsim;35 M&odot;), which are still massive when they explode and leave black hole remnants, and one with moderate initial masses (&#126;12&#8211;20 M&odot;) undergoing binary interaction, which end up with small pre-explosion masses and leave neutron star remnants. 
