Black-hole–neutron-star mergers at realistic mass ratios: Equation of state and spin orientation effects

Black-hole-neutron-star mergers resulting in the disruption of the neutron star and the formation of an accretion disk and/or the ejection of unbound material are prime candidates for the joint detection of gravitational-wave and electromagnetic signals when the next generation of gravitational-wave detectors comes online. In this paper, we study the impact of the radius of the neutron star and the alignment of the black-hole spin on black-hole-neutron-star mergers within the range of mass ratio currently deemed most likely for field binaries (M[subBH] ~ 7M[subNS]) and for black-hole spins large enough for the neutron star to disrupt (J[subBH]/M[[sup 2] [subBH]] = 0.9).