We compare dynamics and waveforms from binary neutron star coalescence as computed by new long-term ($\sim 10$ orbits) numerical relativity simulations and by the tidal effective-one-body (EOB) model including analytical tidal corrections up to second post-Newtonian order. The current analytic knowledge encoded in the tidal EOB model is found to be sufficient to reproduce the numerical data up to contact and within their uncertainties. Remarkably, no calibration of any tidal EOB free parameters is required, beside those already fitted to binary black holes data. The inclusion of second post-Newtonian order tidal corrections minimizes the differences with the numerical data, but it is not possible to significantly distinguish them from the leading-order tidal contribution. The presence of a relevant amplification of tidal effects is likely to be excluded, although it can appear as a consequence of numerical inaccuracies. We conclude that the tidally completed effective-one-body model provides nowadays the most advanced and accurate tool for modeling gravitational waveforms from binary neutron star inspiral up to contact. This work also points out the importance of extensive tests to assess the uncertainties of the numerical data and the potential need of new numerical strategies to perform accurate simulations.

• Received 15 May 2012

DOI:https://doi.org/10.1103/PhysRevD.86.044030