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We present a first exploration of the results of neutron star-black holemergers using black hole masses in the most likely range of$7M_\odot-10M_\odot$, a neutrino leakage scheme, and a modeling of the neutronstar material through a finite-temperature nuclear-theory based equation ofstate. In the range of black hole spins in which the neutron star is tidallydisrupted ($\chi_{\rm BH}\gtrsim 0.7$), we show that the merger consistentlyproduces large amounts of cool ($T\lesssim 1\,{\rm MeV}$), unbound,neutron-rich material ($M_{\rm ej}\sim 0.05M_\odot-0.20M_\odot$). A comparableamount of bound matter is initially divided between a hot disk ($T_{\rmmax}\sim 15\,{\rm MeV}$) with typical neutrino luminosity $L_\nu\sim10^{53}\,{\rm erg/s}$, and a cooler tidal tail. After a short period of rapidprotonization of the disk lasting $\sim 10\,{\rm ms}$, the accretion disk coolsdown under the combined effects of the fall-back of cool material from thetail, continued accretion of the hottest material onto the black hole, andneutrino emission. As the temperature decreases, the disk progressively becomesmore neutron-rich, with dimmer neutrino emission. This cooling process shouldstop once the viscous heating in the disk (not included in our simulations)balances the cooling. These mergers of neutron star-black hole binaries withblack hole masses $M_{\rm BH}\sim 7M_\odot-10M_\odot$ and black hole spins highenough for the neutron star to disrupt provide promising candidates for theproduction of short gamma-ray bursts, of bright infrared post-merger signalsdue to the radioactive decay of unbound material, and of large amounts ofr-process nuclei.

Neutron star-black hole mergers with a nuclear equation of state and neutrino cooling: Dependence in the binary parameters