  The data analysis of the gravitational wave signals emitted by coalescing
neutron star binaries requires the availability of an accurate analytical
representation of the dynamics and waveforms of these systems. We propose an
effective-one-body (EOB) model that describes the general relativistic dynamics
of neutron star binaries from the early inspiral up to merger. Our EOB model
incorporates an enhanced attractive tidal potential motivated by recent
analytical advances in the post-Newtonian and gravitational self-force
description of relativistic tidal interactions. No fitting parameters are
introduced for the description of tidal interaction in the late, strong-field
dynamics. We compare the model energetics and the gravitational wave phasing
with new high-resolution multi-orbit numerical relativity simulations of
equal-mass configurations with different equations of state. We find agreement
within the uncertainty of the numerical data for all configurations. Our model
is the first semi-analytical model which captures the tidal amplification
effects close to merger. It thereby provides the most accurate analytical
representation of binary neutron star dynamics and waveforms currently
available.
