  In this paper we present a model for the short (< 1 second) population of
gamma-ray bursts. In this model heated neutron stars in a close binary system
near its last stable orbit emit a large amount of neutrinos (~10^53 ergs). 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
(~1/2) of energy deposited into e+e- pairs 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,
there is a new source of baryon-free plasma that is deposited between the
stars. To model the e+e- pair plasma wind between stars, we do
three-dimensional relativistic numerical hydrodynamic calculations. We find
that the time scale for these bursts, deriving from the baryon-free plasma, is
less than one second and they will have a hot spectrum ~5 MeV. The energy in
bursts is the order of 10^52 ergs.
