  We assess two mechanisms to produce a short GRB from a neutron star
coalescence: the annihilation of neutrino and anti-neutrino pairs and magnetic
processes within the remnant. We find that the neutrino-driven wind from the
remnant can collimate the jets produced via neutrino annihilation into a small
solid angle. This mechanism satisfies the observational constraints on the
apparent luminosity and on the merger event rate. Moreover, the supermassive
neutron star that is formed in the center of the remnant is expected to act as
a convective dynamo reaching equipartition field strengths within fractions of
a second. The associated spin-down time scale is similar to the typical
duration of short GRBs.
