Astronomy and Astrophysics – Astrophysics
Scientific paper
2001-04-25
Astronomy and Astrophysics
Astrophysics
12 pages, to appear in proceedings of the 20th Texas Symposium on Relativistic Astrophysics and Cosmology (plenary talk), eds.
Scientific paper
10.1063/1.1419644
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.
Shibata Masaru
Uryu Koji
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