Abstract
The Collapsar model, in which a massive star (≳20M⊙) fails to produce a supernova (SN) and forms a black hole (BH), provides the main framework for understanding long Gamma‐Ray Bursts (GRBs) and the accompanying hypernovae (HNe). However, single massive‐star models that explain the population of pulsars, predict cores that rotate too slowly to produce GRBs/HNe. We present a model of binary evolution that allows the formation of Kerr BHs where the spin of the BH can be estimated from the pre‐collapse orbit, and use the Blandford‐Znajek (BZ) mechanism to estimate the available energy for a GRB/HN. A population synthesis study shows that this model can account for both, the long GRB and the subluminous GRB populations.
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