Evolution of Gamma-Ray Burst Progenitors at Low Metallicity

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dc.creatorYoon, Sung-Chul
dc.creatorLanger, Norbert
dc.date2005-11-08
dc.date.accessioned2026-07-07T06:44:56Z
dc.date.available2026-07-07T06:44:56Z
dc.descriptionDespite the growing evidence that long Gamma-Ray Bursts (GRBs) are associated with deaths of Wolf-Rayet stars, the evolutionary path of massive stars to GRBs and the exact nature of GRB progenitors remained poorly known. However, recent massive star evolutionary models indicate that -- for sufficiently low metallicity -- initially very rapidly rotating stars can satisfy the conditions for collapsar formation. Even though magnetic torques are included in these models, a strong core spin-down is avoided through quasi-chemically homogeneous evolution induced by rotational mixing. Here, we explore for which initial mass and spin-range single stars of Z=Zsun/20 are expected to produce GRBs. We further find a dichotomy in the chemical structure of GRB progenitors, where lower initial masses end their lives with a massive helium envelope which still contains some amounts of hydrogen, while higher initial masses explode with C/O-dominated hydrogen-free atmospheres.
dc.description6 pages, 4 figures, to appear in Proc "Stellar Evolution at Low Metallicity: Mass-Loss, Explosions, Cosmology" (eds: H. Lamers, N. Langer, T. Nugis), ASP Conf Series in press)
dc.identifierhttps://arxiv.org/abs/astro-ph/0511222
dc.identifierhttp://arxiv.org/abs/astro-ph/0511222
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/102918
dc.subjectAstrophysics
dc.titleEvolution of Gamma-Ray Burst Progenitors at Low Metallicity
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