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Title:
The Progenitor Stars of Gamma-Ray Bursts
Authors:
Woosley, S. E.; Heger, A.
Affiliation:
AA(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064; .), AB(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064; .; Theoretical Astrophysics Group, MS B227, Los Alamos National Laboratory, Los Alamos, NM 87545; .)
Publication:
The Astrophysical Journal, Volume 637, Issue 2, pp. 914-921. (ApJ Homepage)
Publication Date:
02/2006
Origin:
UCP
ApJ Keywords:
Gamma Rays: Bursts, Stars: Rotation, Stars: Supernovae: General
DOI:
10.1086/498500
Bibliographic Code:
2006ApJ...637..914W

Abstract

Those massive stars that give rise to gamma-ray bursts (GRBs) during their deaths must be endowed with an unusually large amount of angular momentum in their inner regions, 1-2 orders of magnitude greater than the ones that make common pulsars. Yet the inclusion of mass loss and angular momentum transport by magnetic torques during the precollapse evolution is known to sap the core of the necessary rotation. Here we explore the evolution of very rapidly rotating massive stars, including stripped-down helium cores that might result from mergers or mass transfer in a binary, and single stars that rotate unusually rapidly on the main sequence. For the highest possible rotation rates (about 400 km s-1), a novel sort of evolution is encountered in which single stars mix completely on the main sequence, never becoming red giants. Such stars, essentially massive ``blue stragglers,'' produce helium-oxygen cores that rotate unusually rapidly. Such stars might comprise roughly 1% of all stars above 10 Msolar and can, under certain circumstances, retain enough angular momentum to make GRBs. Because this possibility is very sensitive to mass loss, GRBs are much more probable in regions of low metallicity.
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