How Massive Single Stars End their Life

Details How Massive Single Stars End their Life How Massive Single Stars End their Life

2002-12-20

arxiv.org/abs/astro-ph/0212469v1

Astrophys.J. 591 (2003) 288-300

Astronomy and Astrophysics

Astrophysics

24 pages, 9 figues, submitted to ApJ

Scientific paper

10.1086/375341

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 discuss how metallicity, 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. Integrating 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 populations that might produce gamma-ray bursts and jet-driven supernovae.

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