Feeding a gamma-ray burster

Statistics – Computation

Scientific paper

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Gamma Ray Bursts, Neutron Stars, Stellar Mass Accretion, Stellar Models, Accretion Disks, Angular Momentum, Computational Astrophysics, Laminar Flow, Position (Location), Viscosity

Scientific paper

The powering of gamma-ray bursters is studied using a model in which the energy source for a gamma ray burster is taken to be the kinetic energy of matter that is orbiting a neutron star. The possibility that a disk with surface density high enough to account for the large energy release of a burst could form from the tidal breakup of a planet is considered and the structure of such a disk is examined. Under the assumption of laminar fluid flow, it is found that the disk must contain highly degenerate electrons and that the magnetic stresses can be neglected if the surface field is less than about 10 to the 11th-12th G. The molecular viscosity of the electrons drives mass inflow and hence causes burst recurrences. The disk radiates steadily due to heat generated by viscous dissipation, and it radiates during bursts by reprocessing the primary burst radiation.

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