For highly spinning (chi=0.5) binary neutron stars, evolution code choice is the largest numerical waveform error, and current analytical models disagree with numerical relativity beyond that error after the stars touch.
Reducing orbital eccentricity in initial data of binary neutron stars
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We develop a method to compute low-eccentricity initial data of binary neutron stars required to perform realistic simulations in numerical relativity. The orbital eccentricity is controlled by adjusting the orbital angular velocity of a binary and incorporating an approaching relative velocity of the neutron stars. These modifications improve the solution primarily through the hydrostatic equilibrium equation for the binary initial data. The orbital angular velocity and approaching velocity of initial data are updated iteratively by performing time evolutions over ~3 orbits. We find that the eccentricity can be reduced by an order of magnitude compared to standard quasicircular initial data, specifically from ~0.01 to <~0.001, by three successive iterations for equal-mass binaries leaving ~10 orbits before the merger.
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The error budget of binary neutron star merger simulations for configurations with high spin
For highly spinning (chi=0.5) binary neutron stars, evolution code choice is the largest numerical waveform error, and current analytical models disagree with numerical relativity beyond that error after the stars touch.