A model for short gamma-ray bursts: Heated neutron stars in close binary systems

In this paper we present a model for the short (< second) population of gamma-ray bursts (GRBs). In this model heated neutron stars in a close binary system near their last stable orbit emit neutrinos at large luminosities (similar to 10(53) ergs/sec). A fraction of these neutrinos will annihilate to form an e(+)e(-) pair plasma wind which will, in turn, expand and recombine to photons which make the gamma-ray burst. We study neutrino annihilation and show that a substantial fraction (similar to 1/2) of energy deposited comes from inter-star neutrinos, where each member of the neutrino pair originates from each neutron star. Thus, in addition to the annihilation of neutrinos blowing off of a single star, we have a new source of baryon free energy that is deposited between the stars. To model the e(+)e(-) pair plasma wind between stars, we do three-dimensional relativistic numerical hydrodynamic calculations.