Eccentric black hole-neutron star mergers: effects of black hole spin and equation of state

TL;DR

This study uses general relativistic simulations to explore high-eccentricity black hole-neutron star mergers, revealing diverse gravitational wave signals, matter dynamics, and electromagnetic emission potential influenced by black hole spin and neutron star equation of state.

Contribution

It provides the first detailed analysis of eccentric BH-NS mergers across various spins and equations of state, including a simple model for orbital changes during close encounters.

Findings

Gravitational wave emission exceeds perturbative predictions near innermost stable separations.

Mass transfer varies from negligible to significant during non-merging encounters.

Large neutron star oscillations consistent with f-modes are excited during close encounters.

Abstract

There is a high level of interest in black hole-neutron star binaries, not only because their mergers may be detected by gravitational wave observatories in the coming years, but also because of the possibility that they could explain a class of short duration gamma-ray bursts. We study black hole-neutron star mergers that occur with high eccentricity as may arise from dynamical capture in dense stellar regions such as nuclear or globular clusters. We perform general relativistic simulations of binaries with a range of impact parameters, three different initial black hole spins (zero, aligned and anti-aligned with the orbital angular momentum), and neutron stars with three different equations of state. We find a rich diversity across these parameters in the resulting gravitational wave signals and matter dynamics, which should also be reflected in the consequent electromagnetic emission. Before tidal disruption, the gravitational wave emission is significantly larger than perturbative predictions suggest for periapsis distances close to effective innermost stable separations, exhibiting features reflecting the zoom-whirl dynamics of the orbit there. Guided by the simulations, we develop a simple model for the change in orbital parameters of the binary during close encounters. Depending upon the initial parameters of the system, we find that mass transfer during non-merging close encounters can range from essentially zero to a sizable fraction of the initial neutron star mass. The same holds for the amount of material outside the black hole post-merger, and in some cases roughly half of this material is estimated to be unbound. We also see that non-merging close encounters generically excite large oscillations in the neutron star that are qualitatively consistent with f-modes.