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Exploring tidal effects of coalescing binary neutron stars in numerical relativity II: Longterm simulations
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abstract
We perform new longterm (15-16 orbits) simulations of coalescing binary neutron stars in numerical relativity using an updated Einstein's equation solver, employing low-eccentricity initial data, and modeling the neutron stars by a piecewise polytropic equation of state. A convergence study shows that our new results converge more rapidly than the third order and using the determined convergence order, we construct an extrapolated waveform for which the estimated total phase error should be less than 1 radian. We then compare the extrapolated waveforms with those calculated by the latest effective-one-body (EOB) formalism in which the so-called tidal deformability, higher post-Newtonian corrections, and gravitational self-force effects are taken into account. We show that for a binary of compact neutron stars with their radius 11.1 km, the waveform by the EOB formalism agrees quite well with the numerical waveform so that the total phase error is smaller than 1 radian for the total phase of $\sim 200$ radian up to the merger. By contrast, for a binary of less compact neutron stars with their radius 13.6 km, the EOB and numerical waveforms disagree with each other in the last few wave cycles, resulting in the total phase error of $\sim 3$ radian.
Forward citations
Cited by 4 Pith papers
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Effective-one-body model for coalescing binary neutron stars: Incorporating tidal spin and enhanced radiation from dynamical tides
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Celephais constructs spectrally accurate binary-neutron-star and black-hole-neutron-star initial data with arbitrary spin orientations, using a sparse Jacobian, adaptive hp-refinement, and PN-informed eccentricity reduction.
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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.
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Data-driven approach for extracting tidal information from neutron star binary mergers observed with the Einstein Telescope
A simulation study showing that the tidal phase of neutron-star mergers can be inferred directly from Einstein Telescope data by fitting six free polynomial coefficients and combining posteriors across events.
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