  Numerical simulations for the merger of binary neutron stars are performed in
full general relativity incorporating a finite-temperature (Shen's) equation of
state (EOS) and neutrino cooling for the first time. It is found that for this
stiff EOS, a hypermassive neutron star (HMNS) with a long lifetime ($\gg 10$
ms) is the outcome for the total mass $\alt 3.0M_{\odot}$. It is shown that the
typical total neutrino luminosity of the HMNS is $\sim 3$--$8\times 10^{53}$
ergs/s and the effective amplitude of gravitational waves from the HMNS is
4--$6 \times 10^{-22}$ at $f=2.1$--2.5 kHz for a source distance of 100 Mpc. We
also present the neutrino luminosity curve when a black hole is formed for the
first time.
