  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 $4.0M_{\odot}$, 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 $\sim 0.3M_{\odot}$ 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.
