Comprehensive numerical relativity -- effective-one-body comparison to inform improvements in waveform models for binary neutron star systems

Understand

We present a detailed comparison between tidal effective-one-body (EOB) models and new state-of-the-art numerical relativity simulations for non-spinning binary neutron star systems.

• This comparison is the most extensive one to date, covering a wide range in the parameter space and encompassing the energetics of the binary, the periastron advance, the time and frequency evolution of the gravitational wave phase for the dominant mode, and several subdominant modes.
• We consider different EOB models with tidal effects that have been proposed, including the model with dynamical tides of [Phys.Rev.Lett.
• 116 (2016) no.18, 181101] and the gravitational self-force (GSF) inspired tidal EOB model of [Phys.Rev.Lett.