Gamma-Ray Bursts Generated by Hyper-Accreting Kerr Black Hole

Abstract

The observed properties of Gamma-Ray Bursts such as rapid variability of X-ray light curve and large energies strongly signature the compact binary, disk accreting system. Our work particularly highlights the extremely rotating, disk accreting black holes as physical source of the flares variability and X-ray afterglow plateaus of GRBs. We investigate the compact binary mergers (neutron star-neutron star and neutron star onto black hole) and gravitational core collapse of super massive star, where in both cases hyper-accreting Kerr hole is formed. The core collapse in a powerful gravitational wave explained as a potential source for the radiated flux of hard X-rays spectrum. We described the evolution of rapidly rotating, accreting BH in general relativity and the relativistic accretion flow in resistive MHD for viscous radiation. We compute the structure of accretion disk, the accretion luminosity of the dynamical evolution of inner accretion disk and precisely determine their radiation spectra, and compare to observational data of X-ray satellites. Finally, we obtained the resulting disk radiation basically explained as the X-ray luminosity of the central source, such as LMC X-1 and GRO J1655-40. These results are interestingly consistent with observational data of galactic X-ray source binary systems such as X-ray luminosities of Cygnus X-1 and Seyfert galaxies (NGC 3783, NGC 4151, NGC 4486 (Messier 87)) which are powerful emitters in X-ray and gamma-ray wavebands of the observed X-ray variability with typical luminosity.

Distributions of Energy, Luminosity, Duration, and Waiting Times of Gamma-Ray Burst Pulses with Known Redshift Detected by Fermi/GBM

“…The nature of the central engine that powers a GRB is still debated, as either a hyper-accreting stellar-mass black hole (BH; Lei et al 2013;Janiuk et al 2017;Sado 2019) surrounded by a thick accretion disk, or a fast-rotating, highly magnetized neutron star (NS, known as a "millisecond magnetar"; Usov 1992;Wheeler et al 2000;Thompson et al 2004;Metzger et al 2011). In the case of a hyper-accreting BH, the jet can be produced either by a neutrino-dominated accretion flow (NDAF; Liu et al 2017) in which neutrinos tap the thermal energy of the accretion disk via neutrino-antineutrino annihilation, launching a thermally dominated fireball (Popham et al 1999;Di Matteo et al 2002), or through the Blandford-Znajek (BZ) effect (Blandford & Znajek 1977), which converts the BH spinning energy into a Poynting-flux-dominated outflow.…”