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 Γ-law equation of state
with Γ=2 and corotating velocity field as a first step. The mass of the
BH is chosen to be ≈3.2M⊙ or 4.0M⊙, and the rest-mass
of the NS ≈1.4M⊙ 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.Comment: 14 pages. To appear in a special issue of Classical and Quantum
Gravity: New Frontiers in Numerical Relativit