  We model the adiabatic inspiral of relativistic binary neutron stars in a
quasi-equilibrium (QE) approximation, and compute the gravitational wavetrain
from the late phase of the inspiral. We compare corotational and irrotational
sequences and find a significant difference in the inspiral rate, which is
almost entirely caused by differences in the binding energy. We also compare
our results with those of a point-mass post-Newtonian calculation. We
illustrate how the late inspiral wavetrain computed with our QE numerical
scheme can be matched to the subsequent plunge and merger waveform calculated
with a fully relativistic hydrodynamics code.
