Evolution of inspiralling neutron star binaries: effects of tidal interactions and orbital eccentricities

TL;DR

This paper investigates how tidal interactions and orbital eccentricities influence gravitational wave signals from inspiraling neutron star binaries, revealing significant phase shifts that could inform neutron star physics.

Contribution

It introduces a hybrid model combining nonlinear tidal deformation with post-Newtonian orbit evolution to analyze eccentric neutron star inspirals.

Findings

Tidal effects accelerate inspiral and cause phase shifts.

Eccentricity leads to oscillating frequency and phase shifts near pericenter.

GW phase shift can exceed 10 radians at merger.

Abstract

Neutron star (NS) binaries formed dynamically may have significant eccentricities while emitting gravitational waves (GWs) in the LIGO/VIRGO band. We study tidal effects in such eccentric inspiralling NS binaries using a set of hybrid equations. The NS is modelled as a compressible ellipsoid, which can deform nonlinearly due to tidal forces, while the orbit evolution is treated with the post-Newtonian (PN) theory up to 2.5-PN order. We find that in general, the tidal interaction can accelerate the inspiral, and cause orbital frequency and phase shifts. For circular inspirals, our calculations reproduce previous linear result at large binary separations, but incorporate the dynamical response of the NS at small separations. For eccentric inspirals, the frequency and phase shifts oscillate considerably near pericenter passages, and the oscillating amplitudes increase with eccentricities. As a result, the GW phase is also significantly influenced by the tidal effect. At merger, the cumulative GW phase shift can reach more than 10 radians (for typical NS mass $1.4M_\odot$ and radius 11.6 km), much larger than the circular inspiral case. Although the event rate of eccentric NS mergers is likely low, the detection of such mergers could provide a useful constraint on the NS equation of state.