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Simulations of black hole—neutron star binary coalescence

We show the results of dynamical simulations of the coalescence of black hole-neutron star binaries. We use a Newtonian Smooth Particle Hydrodynamics code, and include the effects of gravitational radiation back reaction with the quadrupole approximation for point masses, and compute the gravitational radiation waveforms. We assume a polytropic equation of state determines the structure of the neutron star in equilibrium, and use an ideal gas law to follow the dynamical evolution. Three main parameters are explored: (i) The distribution of angular momentum in the system in the initial configuration, namely tidally locked systems vs. irrotational binaries; (ii) The stiffness of the equation of state through the value of the adiabatic index Γ (ranging from Γ=5/3 to Γ=3); (iii) The initial mass ratio q=MNS/MBH. We find that it is the value of Γ that determines how the coalescence takes place, with immediate and complete tidal disruption for Γ⩽2, while the core of the neutron star survives and stays in orbit ...