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Neutron star-black hole binaries are among the strongest sources ofgravitational waves detectable by current observatories. They can also powerbright electromagnetic signals (gamma-ray bursts, kilonovae), and may be asignificant source of production of r-process nuclei. A misalignment of theblack hole spin with respect to the orbital angular momentum leads toprecession of that spin and of the orbital plane, and has a significant effecton the properties of the post-merger remnant and of the material ejected by themerger. We present a first set of simulations of precessing neutron star-blackhole mergers using a hot, composition dependent, nuclear-theory based equationof state (DD2). We show that the mass of the remnant and of the dynamicalejecta are broadly consistent with the result of simulations using simplerequations of state, while differences arise when considering the dynamics ofthe merger and the velocity of the ejecta. We show that the latter can easilybe understood from assumptions about the composition of low-density, coldmaterial in the different equations of state, and propose an updated estimatefor the ejecta velocity which takes those effects into account. We also presentan updated mesh-refinement algorithm which allows us to improve the numericalresolution used to evolve neutron star-black hole mergers.

Dynamical ejecta from precessing neutron star-black hole mergers with a hot, nuclear-theory based equation of state