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To detect the gravitational-wave (GW) signal from binary neutron stars andextract information about the equation of state of matter at nuclear density,it is necessary to match the signal with a bank of accurate templates. Wepresent the two longest (to date) general-relativistic simulations ofequal-mass binary neutron stars with different compactnesses, C=0.12 andC=0.14, and compare them with a tidal extension of the effective-one-body(EOB)model. The typical numerical phasing errors over the $\simeq 22$ GW cyclesare $\Delta \phi\simeq \pm 0.24$ rad. By calibrating only one parameter(representing a higher-order amplification of tidal effects), the EOB model canreproduce, within the numerical error, the two numerical waveforms essentiallyup to the merger. By contrast, the third post-Newtonian Taylor-T4 approximantwith leading-order tidal corrections dephases with respect to the numericalwaveforms by several radians.

Analytic modelling of tidal effects in the relativistic inspiral of binary neutron stars