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Hybrid equation of state approach in binary neutron-star merger simulations

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arxiv 2005.08691 v2 pith:ESJTVWKD submitted 2020-05-18 gr-qc

A. Figura , J.-J. Lu , G.F. Burgio , Z.H. Li , H. -J. Schulze This is my paper · ORCID
classification gr-qc
keywords stateequationhybridbinarygammaneutron-starsimulationsadiabatic
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abstract

We investigate the use of hybrid equations of state in binary neutron-star simulations in full general relativity, where thermal effects are included in an approximate way through the adiabatic index $\Gamma_{\rm{th}}$. We employ a newly developed finite-temperature equation of state derived in the Brueckner-Hartree-Fock approach and carry out comparisons with the corresponding hybrid versions of the same equation of state, investigating how different choices of $\Gamma_{\rm{th}}$ affect the gravitational-wave signal and the hydrodynamical properties of the remnant. We also perform comparisons with the widely used SFHo equation of state, detailing the differences between the two cases. Overall, we determine that when using a hybrid equation of state in binary neutron-star simulations, the value of thermal adiabatic index $\Gamma_{\rm{th}} \approx 1.7$ best approximates the dynamical and thermodynamical behaviour of matter computed using complete, finite-temperature equations of state.

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Cited by 2 Pith papers

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

  1. From Multimessenger Inference to Simulations: A Ranked Ensemble of Finite-Temperature Equations of State

    astro-ph.HE 2026-08 conditional novelty 7.0 of 10

    The paper constructs a 12-member ensemble of finite-temperature neutron star equations of state that spans the posterior from multimessenger and nuclear-physics constraints and releases simulation-ready tables.

  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.

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