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

2017/08/29 by Kenta Kiuchi, Kyohei Kawaguchi, Koutarou Kyutoku +3 · 5 citations
Earth and Planetary Sciences · Physics and Astronomy · #Amplitude #Astrophysics #Binary number #Computational physics #Formalism (music) #General relativity #Geophysics and Gravity Measurements #Gravitational redshift #Gravitational wave #Mathematical physics #Neutron star #Numerical relativity #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #RADIUS #Seismic Imaging and Inversion Techniques #astro-ph.CO #astro-ph.HE #gr-qc

paper · pdf · doi:10.1103/physrevd.96.084060

published as Phys. Rev. D 96, 084060 (2017) · 13 pages, 11 figures, submitted to PRD

arxiv created 2017/08/29 · openalex publication_date 2017/10/27 · arxiv updated 2017/11/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06

Abstract

Extending our previous studies, we perform high-resolution simulations of inspiraling binary neutron stars in numerical relativity. We thoroughly carry through a convergence study in our currently available computational resources with the smallest grid spacing of \ensuremath≈63--86 meter for the neutron-star radius 10.9--13.7 km. The estimated total error in the gravitational-wave phase is of order 0.1 rad for the total phase of \ensuremath\gtrsim210 rad in the last \ensuremath∼15--16 inspiral orbits. We then compare the waveforms (without resolution extrapolation) with those calculated by the latest effective-one-body formalism (tidal SEOBv2 model referred to as TEOB model). We find that for any of our models of binary neutron stars, the waveforms calculated by the TEOB formalism agree with the numerical-relativity waveforms up to \ensuremath≈3 ms before the peak of the gravitational-wave amplitude is reached: For this late inspiral stage, the total phase error is \ensuremath\lesssim0.1 rad. Although the gravitational waveforms have an inspiral-type feature for the last \ensuremath∼3 ms, this stage cannot be well reproduced by the current TEOB formalism, in particular, for neutron stars with large tidal deformability (i.e., lager radius). The reason for this is described.

Citations

• Gravitational-Wave Extraction from an Inspiraling Configuration of Merging Black Holes
• Gravitational self-force corrections to two-body tidal interactions and the effective one-body formalism
• Constraining neutron-star tidal Love numbers with gravitational-wave detectors
• A two-solar-mass neutron star measured using Shapiro delay
• Effective one-body approach to general relativistic two-body dynamics
• A Massive Pulsar in a Compact Relativistic Binary
• Observation of Gravitational Waves from a Binary Black Hole Merger
• Effects of Neutron-Star Dynamic Tides on Gravitational Waveforms within the Effective-One-Body Approach
• Measurability of the tidal deformability by gravitational waves from coalescing binary neutron stars
• GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2
• Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries

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• Black holes, gravitational waves and fundamental physics: a roadmap
• Evolution of bare quark stars in full general relativity: Single star case
• Diversity of Kilonova Light Curves