Sub-radian-accuracy gravitational waves from coalescing binary neutron stars in numerical relativity. II. Systematic study on the equation of state, binary mass, and mass ratio
Kenta Kiuchi, Kyohei Kawaguchi, Koutarou Kyutoku, Yuichiro Sekiguchi, Masaru Shibata
Abstract
We report results of numerical relativity simulations for 26 new nonspinning binary neutron star systems with 6 grid resolutions using an adaptive mesh refinement numerical relativity code SACRA-MPI. The finest grid spacing is 64-85 m, depending on the systems. First, we derive long-term high-precision inspiral gravitational waveforms and show that the accumulated gravitational-wave phase error due to the finite grid resolution is less than 0.5 rad during more than 200 rad phase evolution irrespective of the systems. We also find that the gravitational-wave phase error for a binary system with a tabulated equation of state (EOS) is comparable to that for a piecewise polytropic EOS. Then we validate the SACRA inspiral gravitational waveform template, which will be used to extract tidal deformability from gravitational wave observation, and find that accuracy of our waveform modeling is 0.1 rad in the gravitational-wave phase and 20% in the gravitational-wave amplitude up to the gravitational-wave frequency 1000 Hz. Finally, we calibrate the proposed universal relations between a postmerger gravitational wave signal and tidal deformability/ neutron star radius in the literature and show that they suffer from systematics and many relations proposed as universal are not very universal. Improved fitting formulas are also proposed.