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

Abstract

We present a first exploration of the results of neutron star-black hole mergers using black hole masses in the most likely range of $7M_{\odot }-10M_{\odot }$, a neutrino leakage scheme, and a modeling of the neutron star material through a finite-temperature nuclear-theory based equation of state. In the range of black hole spins in which the neutron star is tidally disrupted (${\chi }_{\mathrm{BH}}\gtrsim 0.7$), we show that the merger consistently produces large amounts of cool ($T\lesssim 1\mathrm{MeV}$), unbound, neutron-rich material ($M_{\mathrm{ej}}\sim 0.05M_{\odot }-0.20M_{\odot }$). A comparable amount of bound matter is initially divided between a hot disk ($T_{\max }\sim 15\mathrm{MeV}$) with typical neutrino luminosity $L_{\nu }\sim 10^{53}erg/s$, and a cooler tidal tail. After a short period of rapid protonization of the disk lasting $\sim 10\mathrm{ms}$, the accretion disk cools down under the combined effects of the fall-back of cool material from the tail, continued accretion of the hottest material onto the black hole, and neutrino emission. As the temperature decreases, the disk progressively becomes more neutron-rich, with dimmer neutrino emission. This cooling process should stop once the viscous heating in the disk (not included in our simulations) balances the cooling. These mergers of neutron star-black hole binaries with black hole masses $M_{\mathrm{BH}}\sim 7M_{\odot }-10M_{\odot }$ and black hole spins high enough for the neutron star to disrupt provide promising candidates for the production of short gamma-ray bursts, of bright infrared post-merger signals due to the radioactive decay of unbound material, and of large amounts of r-process nuclei.

20 pages, 19 figures

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