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We systematically perform the merger simulation of black hole-neutron star(BH-NS) binaries in full general relativity, focusing on the case that the NSis tidally disrupted. We prepare BH-NS binaries in a quasicircular orbit as theinitial condition in which the BH is modeled by a nonspinning moving puncture.For modeling the NS, we adopt the $\Gamma$-law equation of state with$\Gamma=2$ and the irrotational velocity field. We change the BH mass in therange $M_{\rm BH} \approx 3.3$--$4.6M_{\odot}$, while the rest mass of the NSis fixed to be $M_{*}=1.4 M_{\odot}$ (i.e., the NS mass $M_{\rm NS} \approx1.3M_{\odot}$). The radius of the corresponding spherical NS is set in therange $R_{\rm NS} \approx 12$--15 km (i.e., the compactness $GM_{\rm NS}/R_{\rmNS}c^2 \approx 0.13$--0.16). We find for all the chosen initial conditions thatthe NS is tidally disrupted near the innermost stable circular orbit. For themodel of $R_{\rm NS}=12$ km, more than 97 % of the rest mass is quicklyswallowed into the BH and the resultant torus mass surrounding the BH is lessthan $0.04M_{\odot}$. For the model of $R_{\rm NS} \approx 14.7$ km, bycontrast, the torus mass is about $0.16M_{\odot}$ for the BH mass $\approx4M_{\odot}$. The thermal energy of the material in the torus increases by theshock heating occurred in the collision between the spiral arms, resulting inthe temperature $10^{10}$--$10^{11}$ K. (.. omission ..) We also presentgravitational waveforms during the inspiral, tidal disruption of the NS, andsubsequent evolution of the disrupted material. (.. omission ..)

Merger of black hole and neutron star in general relativity: Tidal disruption, torus mass, and gravitational waves