Measurability of the tidal polarizability of neutron stars in late-inspiral gravitational-wave signals

TL;DR

This paper demonstrates that the tidal polarizability of neutron stars can be measured from late-inspiral gravitational wave signals using advanced detectors, providing insights into the nuclear equation of state.

Contribution

It introduces an analytical model for the gravitational wave phase that enables measurement of neutron star tidal parameters from signals.

Findings

Tidal polarizability can be measured with SNR of 16.

Measurement is feasible for neutron stars with maximum mass > 1.97 solar masses.

Proposes a method to extract nuclear EoS information from multiple events.

Abstract

The gravitational wave signal from a binary neutron star inspiral contains information on the nuclear equation of state. This information is contained in a combination of the tidal polarizability parameters of the two neutron stars and is clearest in the late inspiral, just before merger. We use the recently defined tidal extension of the effective one-body formalism to construct a controlled analytical description of the frequency-domain phasing of neutron star inspirals up to merger. Exploiting this analytical description we find that the tidal polarizability parameters of neutron stars can be measured by the advanced LIGO-Virgo detector network from gravitational wave signals having a reasonable signal-to-noise ratio of $\rho=16$. This measurability result seems to hold for all the nuclear equations of state leading to a maximum mass larger than $1.97M_\odot$. We also propose a promising new way of extracting information on the nuclear equation of state from a coherent analysis of an ensemble of gravitational wave observations of separate binary merger events.