Quasiequilibrium sequences of black-hole--neutron-star binaries in general relativity

TL;DR

This paper constructs quasiequilibrium models of black hole-neutron star binaries using general relativity, providing initial data for simulations and exploring configurations with specific mass ratios and neutron star properties.

Contribution

It introduces a method to generate initial data for black hole-neutron star binaries with arbitrary mass ratios in general relativity.

Findings

Models satisfy Einstein's constraint equations.

Results applicable as initial data for dynamical simulations.

Focus on irrotational, nonspinning configurations.

Abstract

We construct quasiequilibrium sequences of black hole-neutron star binaries for arbitrary mass ratios by solving the constraint equations of general relativity in the conformal thin-sandwich decomposition. We model the neutron star as a stationary polytrope satisfying the relativistic equations of hydrodynamics, and account for the black hole by imposing equilibrium boundary conditions on the surface of an excised sphere (the apparent horizon). In this paper we focus on irrotational configurations, meaning that both the neutron star and the black hole are approximately nonspinning in an inertial frame. We present results for a binary with polytropic index n=1, mass ratio M_{irr}^{BH}/M_{B}^{NS}=5 and neutron star compaction M_{ADM,0}^{NS}/R_0=0.0879, where M_{irr}^{BH} is the irreducible mass of the black hole, M_{B}^{NS} the neutron star baryon rest-mass, and M_{ADM,0}^{NS} and R_0 the neutron star Arnowitt-Deser-Misner mass and areal radius in isolation, respectively. Our models represent valid solutions to Einstein's constraint equations and may therefore be employed as initial data for dynamical simulations of black hole-neutron star binaries.