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We report results of numerical relativity simulations for {\it new} 26non-spinning binary neutron star systems with 6 grid resolutions using anadaptive mesh refinement numerical re\ lativity code {\tt SACRA-MPI}. Thefinest grid spacing is $\approx 64$--$85$ m, depending on the systems. First,we derive long-term high-precision inspiral gravitational waveforms and showthat the accumulated gravitational-wave phase error due to the finite gridresolution is less than $0.5$ rad during more than $200$ rad phase evolutionirrespective of the systems. We also find that the gravitational-wave phaseerror for a binary system with a tabulated equation of state (EOS) iscomparable to that for a piecewise polytropic EOS. Then we validate the SACRAinspiral gravitational waveform template, which will be used to extract tidaldeformability from gravitational wave observation, and find that accuracy of \our waveform modeling is $\lesssim 0.1$ rad in the gravitational-wave phase and$\lesssim 20 \%$ in the gravitational-wave amplitude up to thegravitational-wave frequency $1000$ Hz.\  Finally, we calibrate the proposed universal relations between a post-mergergravitational wave signal and tidal deformability/neutron star radius in theliterature and show that th\ ey suffer from systematics and many relationsproposed as universal are not very universal. Improved fitting formulae arealso proposed.

physical review. d/physical review. d.

Sub-radian-accuracy gravitational waves from coalescing binary neutron  stars II: Systematic study on the equation of state, binary mass, and mass  ratio