Merger of black hole-neutron star binaries in full general relativity

Abstract

We present our latest results for simulation for merger of black hole (BH)-neutron star (NS) binaries in full general relativity which is performed preparing a quasicircular state as initial condition. The BH is modeled by a moving puncture with no spin and the NS by the $\Gamma$-law equation of state with $\Gamma =2$ and corotating velocity field as a first step. The mass of the BH is chosen to be $\approx 3.2M_{\odot }$ or $4.0M_{\odot }$, and the rest-mass of the NS $\approx 1.4M_{\odot }$ with relatively large radius of the NS $\approx 13$--14 km. The NS is tidally disrupted near the innermost stable orbit but $\sim 80$--90% of the material is swallowed into the BH and resulting disk mass is not very large as $\sim 0.3M_{\odot }$ even for small BH mass $\sim 3.2M_{\odot }$. The result indicates that the system of a BH and a massive disk of $\sim M_{\odot }$ is not formed from nonspinning BH-NS binaries irrespective of BH mass, although a disk of mass $\sim 0.1M_{\odot }$ is a possible outcome for this relatively small BH mass range as $\sim 3$--4$M_{\odot }$. Our results indicate that the merger of low-mass BH and NS may form a central engine of short-gamma-ray bursts.

14 pages. To appear in a special issue of Classical and Quantum Gravity: New Frontiers in Numerical Relativity

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