Equation of state effects in black hole-neutron star mergers

TL;DR

This study investigates how different neutron star equations of state influence black hole-neutron star merger dynamics, gravitational wave signals, and postmerger structures using full general relativity simulations.

Contribution

It provides a comparative analysis of various EoS models on merger outcomes, including waveform signatures and disk properties, with detailed numerical simulations.

Findings

More compact stars produce stronger gravitational waves.

EoS affects the tail and disk structures post-merger.

Signatures of EoS are observable in waveforms and remnant features.

Abstract

The merger dynamics of a black hole-neutron star (BHNS) binary is influenced by the neutron star equation of state (EoS) through the latter's effect on the neutron star's radius and on the character of the mass transfer onto the black hole. We study these effects by simulating a number of BHNS binaries in full general relativity using a mixed pseudospectral/finite difference code. We consider several models of the neutron star matter EoS, including Gamma=2 and Gamma=2.75 polytropes and the nuclear-theory based Shen EoS. For models using the Shen EoS, we consider two limits for the evolution of the composition: source-free advection and instantaneous beta-equilibrium. To focus on EoS effects, we fix the mass ratio to 3:1 and the initial aligned black hole spin to a/m=0.5 for all models. We confirm earlier studies which found that more compact stars create a stronger gravitational wave signal but a smaller postmerger accretion disk. We also vary the EoS while holding the compaction fixed. All mergers are qualitatively similar, but we find signatures of the EoS in the waveform and in the tail and disk structures.