How do /γ-ray bursts associated with supernovae avoid baryon contamination?

Details How do /γ-ray bursts associated with supernovae avoid baryon contamination? How do /γ-ray bursts associated with supernovae avoid baryon contamination?

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aph....16...67c&link_type=abstract

Astroparticle Physics, Volume 16, Issue 1, p. 67-74.

Physics

3

Scientific paper

Current hypernova models for /γ-ray bursts (GRBs) associated with supernovae suffer from the baryon contamination problem, which prevents formation of relativistic shocks and emission of /γ-rays. Here we present a possible solution to this difficulty. Our model can be divided into two steps. In the first step, the core collapse of a star with mass>=19Msolar leads to a massive neutron star and a supernova (SN), and subsequently, one jet produced via neutrino annihilation during hypercritical accretion of the neutron star will push out of its front matter, resulting in a small cone relatively free of baryons. In the second step, once the mass of the neutron star reaches the maximum value, it will promptly implode to a rapidly rotating black hole surrounded by a torus. The gravitational binding energy of the torus will convert to the expansion energy of the SN ejecta, thus yielding a hypernova, while the rotational energy of the black hole will be extracted via the Blandford-Znajek process to generate another jet responsible for a GRB. We show that the mass of baryons loading with the second jet is smaller than 10-3Msolar and the Lorentz factor of this jet is larger than 100. Thus our model can avoid the baryon contamination problem suffered from in the hypernova models.

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