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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 \-law equation of state with \=2 and corotating velocity field as a first step. The mass of the BH is chosen to be \ 3. 2 M\ or 4. 0M\, and the rest-mass of the NS \ 1. 4 M\ with relatively large radius of the NS \ 13--14 km. The NS is tidally disrupted near the innermost stable orbit but \ 80--90% of the material is swallowed into the BH and resulting disk mass is not very large as \ 0. 3M\ even for small BH mass \ 3. 2M\. The result indicates that the system of a BH and a massive disk of \ M\ is not formed from nonspinning BH-NS binaries irrespective of BH mass, although a disk of mass \ 0. 1M\ is a possible outcome for this relatively small BH mass range as \ 3--4M\. Our results indicate that the merger of low-mass BH and NS may form a central engine of short-gamma-ray bursts.
Shibata et al. (Wed,) studied this question.