Observability of dynamical tides in merging eccentric neutron star binaries

While dynamical tides only become relevant during the last couple of orbits for circular inspirals, orbital eccentricity can increase their impact during earlier phases of the inspiral by exciting tidal oscillations at each close encounter. We investigate the effect of dynamical tides on the orbital evolution of eccentric neutron star binaries using post-Newtonian numerical simulations and construct an analytic stochastic model that reproduces the numerical results. Our study reveals a strong dependence of dynamical tides on the pericenter distance, with the fractional energy transferred to dynamical tides over that dissipated in gravitational waves (GWs) exceeding similar to 1% at separations rp 50 km for large eccentricities. We demonstrate that the effect of dynamical tides on orbital evolution can manifest as a phase shift in the GW signal. We show that the signal-to-noise ratio of the GW phase shift can reach the detectability threshold of 8 with a single advanced Laser Interferometer Gravitational Wave Observatory detector at design sensitivity for eccentric neutron star binaries at a distance of 40 Mpc. This requires a pericenter distance of rp0 68 km (rp0 76 km) at binary formation with eccentricity close to 1 for a reasonable tidal deformability and f-mode frequency of 500 and 1.73 kHz (700 and 1.61 kHz), respectively. The observation of the phase shift will enable measuring the f-mode frequency of neutron stars independently from their tidal deformability, providing significant insights into neutron star seismology and the properties of the equation of state. We also explore the potential of distinguishing between equal-radius and twin-star binaries, which could provide an opportunity to reveal strong firstorder phase transitions in the nuclear equation of state.