A Two-Step Model for Gamma-Ray Bursts Associated with Supernovae

Abstract

We here propose a two-step model for gamma-ray bursts (GRBs) associated with supernovae. In the first step, the core collapse of a star with mass $\ge 19M_\odot$ leads to a massive neutron star and a normal supernova, and subsequently hypercritical accretion of the neutron star from the supernova ejecta may give rise to a jet through neutrino annihilation and/or Poynting flux along the stellar rotation axis. However, because of too much surrounding matter, this jet rapidly enters a nonrelativistic phase and evolves to a large bubble. In the second step, the neutron star promptly implodes to a rapidly rotating black hole surrounded by a torus when the mass of the star increases to the maximum mass and meanwhile its rotation frequency increases to the upper limit due to the accreted angular momentum. The gravitational binding energy of the torus may be dissipated by a magnetized relativistic wind, which may then be absorbed by the supernova ejecta, thus producing an energetic hypernova. The rotational energy of the black hole may be extracted by the Blandford-Znajek's mechanism, leading to another jet. This jet is relatively free of baryons and thus may be accelerated to an ultrarelativistic phase because the first jet has pushed out of its front matter and left a baryon-free exit. We expect that the second jet generates a GRB and its afterglow. Our two-step model may alleviate the baryon-contamination problem suffered possibly from in the hypernova models. Furthermore, this model not only accounts for association of several GRBs with supernovae but also explains well the features of the afterglows of these bursts.