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 3.2 M _ { \odot } or 4.0 M _ { \odot } , and the rest-mass of the NS \approx 1.4 M _ { \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 0.3 M _ { \odot } even for small BH mass \sim 3.2 M _ { \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 0.1 M _ { \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 .