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Binary Neutron Stars in Quasi-equilibrium

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arxiv 1005.0958 v1 pith:EBETDXG2 submitted 2010-05-06 astro-ph.SR gr-qc

Keisuke Taniguchi , Masaru Shibata This is my paper · ORCID
classification astro-ph.SRgr-qc
keywords sequencesangularbinaryequationsneutronquasi-equilibriummassorbital
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Quasi-equilibrium sequences of binary neutron stars are constructed for a variety of equations of state in general relativity. Einstein's constraint equations in the Isenberg-Wilson-Mathews approximation are solved together with the relativistic equations of hydrostationary equilibrium under the assumption of irrotational flow. We focus on unequal-mass sequences as well as equal-mass sequences, and compare those results. We investigate the behavior of the binding energy and total angular momentum along a quasi-equilibrium sequence, the endpoint of sequences, and the orbital angular velocity as a function of time, changing the mass ratio, the total mass of the binary system, and the equation of state of a neutron star. It is found that the orbital angular velocity at the mass-shedding limit can be determined by an empirical formula derived from an analytic estimation. We also provide tables for 160 sequences which will be useful as a guideline of numerical simulations for the inspiral and merger performed in the near future.

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Cited by 2 Pith papers

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  1. 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.

  2. Axisymmetric stability of neutron stars as extreme rotators in massive scalar-tensor theory

    gr-qc 2025-02 conditional novelty 6.0 of 10

    Differentially rotating scalarized neutron stars with enormous angular momentum are axisymmetrically stable up to the turning point of their mass sequence, beyond which they collapse to black holes, confirming the tur...

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