[摘要]：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 less than or similar to 3.0M(circle dot). It is shown that the typical total neutrino luminosity of the HMNS is similar to 3-8 x 10(53) erg/s and the effective amplitude of gravitational waves from the HMNS is 4-6 x 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.
