Resonant tides in binary neutron star mergers: analytical-numerical relativity study

Abstract

Resonant excitations of $f$-modes in binary neutron star coalescences influence the gravitational waves (GWs) emission in both quasicircular and highly eccentric mergers and can deliver information on the star interior. Most models of resonant tides are built using approximate, perturbative approaches and thus require to be carefully validated against numerical relativity (NR) simulations in the high-frequency regime. We perform detailed comparisons between a set of high-resolution NR simulations and the state of the art effective one body (EOB) model $\mathtt{TEOBResumS}$ with various tidal potentials and including a model for resonant tides. For circular mergers, we find that $f$-mode resonances can improve the agreement between EOB and NR, but there is no clear evidence that the tidal enhancement after contact is due to a resonant mechanism. Tidal models with $f$-mode resonances do not consistently reproduce, at the same time, the NR waveforms and the energetics within the errors, and their performances is comparable to resummed tidal models without resonances. For highly eccentric mergers, we show for the first time that our EOB model reproduces the bursty NR waveform to a high degree of accuracy. However, the considered resonant model does not capture the $f$-mode oscillations excited during the encounters and present in the NR waveform. Finally, we analyze GW170817 with both adiabatic and dynamical tides models and find that the data shows no evidence in favor of models including dynamical tides. This is in agreement with the fact that resonant tides are measured at very high frequencies, which are not available for GW170817 but might be tested with next generation detectors.

9 pages, 9 figures

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• Effects of Dark Matter on $f$-mode oscillations of Neutron Stars
• Constraining properties of asymmetric dark matter candidates from gravitational-wave observations
• Renormalizing Love: tidal effects at the third post-Newtonian order
• Numerical-Relativity-Informed Effective-One-Body model for Black-Hole-Neutron-Star Mergers with Higher Modes and Spin Precession
• Degeneracy in the inference of phase transitions in the neutron star equation of state from gravitational wave data
• Using Equation of State Constraints to Classify Low-Mass Compact Binary Mergers
• Dynamical tides during the inspiral of rapidly spinning neutron stars: Solutions beyond mode resonance
• Effective one body Hamiltonian in scalar-tensor gravity at third post-Newtonian order
• Tidal Deformability Doppelgangers: Implications of a low-density phase transition in the neutron star equation of state
• Premerger phenomena in neutron-star binary coalescences
• Cost of inferred nuclear parameters towards the f-mode dynamical tide in binary neutron stars
• Real modes and null memory contributions in effective-one-body models
• Modeling matter(s) in SEOBNRv5THM: Generating fast and accurate effective-one-body waveforms for spin-aligned binary neutron stars
• Observability of dynamical tides in merging eccentric neutron star binaries
• Gravitational waves from eccentric binary neutron star mergers: Systematic biases and inadequacy of quasicircular templates
• High-order effective-one-body tidal interactions and gravitational scattering
• Astrophysical constraints on neutron star $f$-modes with a nonparametric equation of state representation
• Early Warning From Eccentric Compact Binaries: Template Initialization And Sub-dominant Mode Effects