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Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily on the properties of the material ejected from the system. We find that a fraction of the material is ejected as a mildly relativistic and mildly anisotropic outflow with the typical and maximum velocities 0. 15--0. 25c and 0. 5--0. 8c (where c is the speed of light), respectively, and that the total ejected rest mass is in a wide range 10^-4--10^-2M_, which depends strongly on the EOS, the total mass, and the mass ratio. The total kinetic energy ejected is also in a wide range between 10^49 and 10^51 ergs. The numerical results suggest that for a binary of canonical total mass 2. 7M_, the outflow could generate an electromagnetic signal observable by the planned telescopes through the production of heavy-element unstable nuclei via the r-process 6, 20, 21 or through the formation of blast waves during the interaction with the interstellar matter 7, if the EOS and mass of the binary are favorable ones.
Hotokezaka et al. (Wed,) studied this question.