Key points are not available for this paper at this time.
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 (10 ms) is the outcome for the total mass 3. 0M_. It is shown that the typical total neutrino luminosity of the HMNS is 3--810^53 erg/s and the effective amplitude of gravitational waves from the HMNS is 4--610^-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.
Sekiguchi et al. (2011) studied this question.