Abstract
We present grids of massive star evolution models at four different metallicities (Z = 0.004, 0.002, 0.001, 0.00001). The effects of
rotation on the stellar structure and the transport of angular momentum and chemical elements through the Spruit-Tayler dynamo and
rotationally induced instabilities are considered. After discussing uncertainties involved with the adopted physics, we elaborate the
final fate of massive stars as a function of initial mass and spin rate, at each considered metallicity. In particular, we investigate for
which initial conditions long gamma-ray bursts (GRBs) are expected to be produced in the frame of the collapsar model. Then, using
an empirical spin distribution of young massive metal-poor stars and a specified metallicity-dependent history of star-formation, we
compute the expected GRB rate as function of metallicity and redshift based on our stellar evolution models. The GRB production
in our models is limited to metallicities of Z
Original language | Undefined/Unknown |
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Pages (from-to) | 199-208 |
Number of pages | 10 |
Journal | Astronomy and Astrophysics |
Volume | 460 |
Issue number | 1 |
Publication status | Published - 2006 |