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Reducing orbital eccentricity in initial data of binary neutron stars

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arxiv 1405.6207 v2 pith:2MHNKUX2 submitted 2014-05-23 gr-qc astro-ph.HE

Koutarou Kyutoku , Masaru Shibata , Keisuke Taniguchi This is my paper · ORCID
classification gr-qcastro-ph.HE
keywords datainitialbinaryorbitalvelocityeccentricityneutronstars
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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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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Celephais: efficient spectral initial data code for precessing compact binaries

    gr-qc 2026-08 conditional novelty 6.0 of 10

    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.

  2. The error budget of binary neutron star merger simulations for configurations with high spin

    gr-qc 2025-06 accept novelty 6.0 of 10

    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.

  3. SACRA-2D: New axisymmetric general relativistic hydrodynamics code with fixed mesh refinement

    astro-ph.HE 2025-02 conditional novelty 6.0 of 10

    SACRA-2D is a new axisymmetric relativistic hydrodynamics code with the HLLC solver and adaptive mesh refinement, validated by benchmarks showing improved accuracy over the TVDLF solver.

  4. Eccentricity reduction of binary neutron star initial data with the entropy based flux limiting scheme

    gr-qc 2024-12 conditional novelty 6.0 of 10

    Using the entropy-based flux limiter in both eccentricity reduction and evolution yields apparent fifth-order convergence in binary neutron star waveform phase.

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