Quark-Nova Explosion inside a Collapsar: Application to Gamma Ray Bursts
Shown in this figure are three sequential phases and a fourth possible phase in our model for the case of an SN (i.e., expanding envelope). Phase 1 consists of the interaction between the QN ejecta and the envelope leading to an X-ray precursor (see Section 2.2). An accretion disk forms around the QS leading to Phase 2 where a jet is launched, providing the prompt GRB emission (see Section 3.2). Phase 3 shows the late stages of the QS jet interacting with the QN ejecta leading to an X-ray afterglow. However, if accretion is sufficiently large, the QS may turn into a BH (phase 4 above), causing launch of a second jet extending the prompt GRB phase reminiscent of late time activity observed by Swift (see ).
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