TP-02

A Possible Energy Mechanism for Cosmological Gamma-ray Bursts

K.S.Cheng¹, Y. Lu^{1,2,3 1}Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong
²Department of physics, Huang Zhong Normal University, 430079, China
³ Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China

We suggest that an extreme Kerr black hole with a mass $\sim 10^6M_\odot$, a dimensionless angular momentum $A\sim 1$ and a marginal stable orbital radius $r_{ms}\sim 3r_s\sim 10^{12}M_6~cm$ located in a normal galaxy, may produced a GRB by capturing and disrupting a star. During this period, a transient accretion disk is formed and a strong transient magnetic field $\sim 2.4\times 10^9M_6^{-1/2}$ Gauss, lasting for $r_{ms}/c\sim 30 M_6~s$, may be produced in the inner boundary of the accretion disk. A large amount of rotational energy of the black hole is extracted and released in the ultra relativistic jet with a bulk Lorentz factor $\Gamma$ larger than 10³ via Blandford-Znajek process. The relativistic jet energy can be converted into $\gamma$-ray radiation via internal shock mechanism. The gamma-ray burst (GRB) duration should be the same as that of the life time of the strong transient magnetic field. The maximum number of sub-bursts is estimated to be $r_{ms}/h\sim (10 - 10^2)$ because the disk material is likely broken into pieces with the size about the thickness of the disk h at the cusp ( $2r_s\le r \le 3r_s$). The shortest rising time of the burst estimated from this model is $\sim h/\Gamma c\sim 3\times 10^{-4}\Gamma^{-1}_3(h/r)_{-2}M_6$ s. The model gamma-ray burst density rate is also estimated.