Binary neutron star mergers in fully general relativistic simulations

We perform 3D numerical simulations for merger of equal mass binary neutron stars in full general relativity preparing irrotational binary neutron stars in a quasiequilibrium state as initial conditions. Simulations have been carried out for a wide range of stiffness of equations of state and compactness of neutron stars, paying particular attention to the final products and gravitational waves. We take a fixed uniform grid in Cartesian coordinates with typical grid size (293, 293, 147) in (x, y, z) assuming a plane symmetry with respect to the equatorial plane. A result of one new large-scale simulation performed with grid size (505, 505, 253) is also presented. We find that the final product depends sensitively on the initial compactness of the neutron stars: In a merger between sufficiently compact neutron stars, a black hole is formed in a dynamical timescale. As the compactness is decreased, the formation timescale becomes longer and longer. For less compact cases, a differentially rotating massive neutron star is formed instead of a black hole. In the case of black hole formation, the disk mass around the black hole appears to be smaller than 1% of the total rest mass. It is also indicated that waveforms of high-frequency gravitational waves after merger depend strongly on the compactness of neutron stars.