Abstract

We systematically performed numerical-relativity simulations for black hole-neutron star (BH-NS) binary mergers with a variety of the BH spin orientation and nuclear-theory-based equations of state (EOS) of the NS. The initial misalignment angles of the BH spin measured from the direction of the orbital angular momentum are chosen in the range of i tilt,0 ≈30°−90° . We employed four models of nuclear-theory-based zero-temperature EOS for the NS in which the compactness of the NS is in the range of C=M NS /R NS =0.138−0.180 , where M NS and R NS are the mass and the radius of the NS, respectively. The mass ratio of the BH to the NS, Q=M BH /M NS , and the dimensionless spin parameter of the BH, χ , are chosen to be Q=5 and χ=0.75 , together with M NS =1.35M ⊙ so that the BH spin misalignment has a significant effect on tidal disruption of the NS. We obtain the following results: (i) The inclination angles of i tilt,0