How Massive Single Stars End Their Life

Authors

A. Heger, Department of Astronomy and Astrophysics, Enrico Fermi Institute,The University of ChicagoFollow
C. L. Fryer, Theoretical Astrophysics - Los Alamos National LaboratoriesFollow
S. E. Woosley, Department of Astronomy and Astrophysics, University of CaliforniaFollow
N. Langer, Astronomical Institute,NL-3508 TA Utrecht, The NetherlandsFollow
Dieter H. Hartmann, Clemson University - Department of Physics and AstronomyFollow

Document Type

Article

Publication Date

Winter 12-20-2002

Publication Title

The Astrophysical Journal

Publisher

The American Astronomical Society

Abstract

How massive stars die - what sort of explosion and remnant each produces - depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are the only means of mass loss, and these are chiefly a function of the metallicity of the star. We dicuss how meallicity, and a simplified prescription for its effect on mass loss, affects the evolution and final fate of massive stars. We map, as a function of mass and metallicity, where black holes and neutron stars are likely to form and where different types of supernovae are produced. Intergrating over an initial mass function, we derive the relative populations as a function of metallicity. Provided single stars rotate rapidly enough at death, we speculate upon stellar population that might produce gamma-ray bursts and jet-driven supernovae.

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