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Extending our previous studies, we perform high-resolution simulations ofinspiraling binary neutron stars in numerical relativity. We thoroughly carrythrough a convergence study in our currently available computational resourceswith the smallest grid spacing of $\approx 63$--86~meter for the neutron-starradius 10.9--13.7\,km. The estimated total error in the gravitational-wavephase is of order 0.1~rad for the total phase of $\gtrsim 210$\,rad in the last$\sim 15$--16 inspiral orbits. We then compare the waveforms (withoutresolution extrapolation) with those calculated by the latesteffective-one-body formalism (tidal SEOBv2 model referred to as TEOB model). Wefind that for any of our models of binary neutron stars, the waveformscalculated by the TEOB formalism agree with the numerical-relativity waveformsup to $\approx 3$\,ms before the peak of the gravitational-wave amplitude isreached: For this late inspiral stage, the total phase error is $\lesssim0.1$\,rad. Although the gravitational waveforms have an inspiral-type featurefor the last $\sim 3$\,ms, this stage cannot be well reproduced by the currentTEOB formalism, in particular, for neutron stars with large tidal deformability(i.e., lager radius). The reason for this is described.

Sub-radian-accuracy gravitational waveforms of coalescing binary neutron stars in numerical relativity