Determining the equation of state of neutron stars with Einstein Telescope using tidal effects and r-mode excitations from a population of binary inspirals

TL;DR

This paper predicts how third-generation gravitational wave detectors like Einstein Telescope can accurately determine neutron star equations of state by analyzing tidal effects and r-mode resonances during binary inspirals.

Contribution

It introduces new universal relations for r-mode resonances and assesses their impact on neutron star EOS measurements with ET.

Findings

Resonant r-modes significantly improve EOS constraints.

ET can reconstruct neutron star EOS from tens of binary coalescences.

Inclusion of r-modes enhances the information extracted from inspiral signals.

Abstract

Third-generation gravitational wave (GW) observatories such as Einstein Telescope (ET) and Cosmic Explorer (CE) will be ideal instruments to probe the structure of neutron stars through the GWs they emit when undergoing binary coalescence. In this work we make predictions about how well ET in particular will enable us to reconstruct the neutron star equation of state through observations of tens of binary neutron star coalescences with signal-to-noise ratios in the hundreds. We restrict ourselves to information that can be extracted from the inspiral, which includes tidal effects and possibly r-mode resonances. In treating the latter we go beyond the Newtonian approximation, introducing and utilizing new universal relations. We find that the ability to observe resonant r-modes would have a noticeable impact on neutron star equation of state measurements with ET.