Merger of black hole-neutron star binaries: nonspinning black hole case

We perform a simulation for merger of a black hole (BH)-neutron star (NS) binary in full general relativity preparing a quasicircular state as initial condition. The BH is modeled by a moving puncture with no spin and the NS by the $\mathrm{\Gamma }$-law equation of state with $\mathrm{\Gamma }=2$. Corotating velocity field is assumed for the NS. The mass of the BH and the rest-mass of the NS are chosen to be $\approx 3.2M_{\odot }$ and $\approx 1.4M_{\odot }$ with relatively large radius of the NS $\approx 14$ km. The NS is tidally disrupted near the innermost stable orbit but $\sim 80$ of the material is swallowed into the BH with small disk mass $\sim 0.3M_{\odot }$ even for such small BH mass $\sim 3M_{\odot }$. 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, although a disk of mass $\sim 0.1M_{\odot }$ is a possible outcome.