  We present the results from new relativistic hydrodynamic simulations of
binary neutron star mergers using realistic non-zero temperature equations of
state. We vary several unknown parameters in the system such as the neutron
star (NS) masses, their spins and the nuclear equation of state. The results
are then investigated with special focus on the post-merger torus-remnant
system. Observational implications on the Gamma-ray burst (GRB) energetics are
discussed and compared with recent observations.
