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_⊙ –10M_⊙, 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 (χ BH ≳0.7), we show that the merger consistently produces large amounts of cool (T≲1  MeV), unbound, neutron-rich material (M_(ej) ∼ 0.05M_⊙ –0.20M_⊙). A comparable amount of bound matter is initially divided between a hot disk (T_(max) ∼15  MeV) with typical neutrino luminosity of L_ ν ∼10^(53)   erg/s, and a cooler tidal tail. After a short period of rapid protonization of the disk lasting ∼10  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 of M_(BH) ∼7M_⊙ –10M_⊙, 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 postmerger signals due to the radioactive decay of unbound material, and of large amounts of r-process nuclei.

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