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We study the merger of black hole-neutron star binaries by fullygeneral-relativistic neutrino-radiation-hydrodynamics simulations throughoutthe coalescence, particularly focusing on the role of neutrino irradiation indynamical mass ejection. Neutrino transport is incorporated by an approximatetransfer scheme based on the truncated moment formalism. While we fix the massratio of the black hole to the neutron star to be 4 and the dimensionless spinparameter of the black hole to be 0.75, the equations of state forfinite-temperature neutron-star matter are varied. The hot accretion diskformed after tidal disruption of the neutron star emits a copious amount ofneutrinos with the peak total luminosity ~1--3x10^53 erg s^(-1) via thermalpair production and subsequent electron/positron captures on free nucleons.Nevertheless, the neutrino irradiation does not modify significantly theelectron fraction of the dynamical ejecta from the neutrinolessbeta-equilibrium value at zero temperature of initial neutron stars. The massof the wind component driven by neutrinos from the remnant disk is negligiblecompared to the very neutron-rich dynamical component, throughout oursimulations performed until a few tens milliseconds after the onset of merger,for the models considered in this study. These facts suggest that the ejectafrom black hole-neutron star binaries are very neutron rich and are expected toaccommodate strong r-process nucleosynthesis, unless magnetic or viscousprocesses contribute substantially to the mass ejection from the disk. We alsofind that the peak neutrino luminosity does not necessarily increase as thedisk mass increases, because tidal disruption of a compact neutron star canresult in a remnant disk with a small mass but high temperature.

Neutrino transport in black hole-neutron star binaries: neutrino emission and dynamical mass ejection