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Bayesian modeling of the nuclear equation of state for neutron star tidal deformabilities and GW170817

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arxiv 1902.05502 v2 pith:FADEJVOM submitted 2019-02-14 nucl-th astro-ph.HE

Y. Lim , J. W. Holt This is my paper · ORCID
classification nucl-thastro-ph.HE
keywords neutronstarequationnuclearstatetidalbayesiandeformabilities
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abstract

We present predictions for neutron star tidal deformabilities obtained from a Bayesian analysis of the nuclear equation of state, assuming a minimal model at high-density that neglects the possibility of phase transitions. The Bayesian posterior probability distribution is constructed from priors obtained from microscopic many-body theory based on realistic two- and three-body nuclear forces, while the likelihood functions incorporate empirical information about the equation of state from nuclear experiments. The neutron star crust equation of state is constructed from the liquid drop model, and the core-crust transition density is found by comparing the energy per baryon in inhomogeneous matter and uniform nuclear matter. From the cold $\beta$-equilibrated neutron star equation of state, we then compute neutron star tidal deformabilities as well as the mass-radius relationship. Finally, we investigate correlations between the neutron star tidal deformability and properties of finite nuclei.

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Cited by 3 Pith papers

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

  1. Bayesian inference of neutron star crust properties using an ab initio-benchmarked meta-model

    nucl-th 2025-06 conditional novelty 7.0 of 10

    A blended meta-model with ab initio-based low-density correction reduces neutron star crust uncertainties and shifts crust-core transition density, pressure, and crustal moment of inertia in Bayesian inference.

  2. Building Neutron Stars with the MUSES Calculation Engine

    nucl-th 2025-02 conditional novelty 6.0 of 10

    A new open-source calculation engine produces crust-to-core neutron star equations of state and shows that smooth matching choices change predicted radii and masses by several percent.

  3. Effect of Dark matter and $\sigma$-cut potential on radial and non-radial oscillation modes in neutron stars

    astro-ph.HE 2025-07 conditional novelty 4.0 of 10

    Dark matter-admixed neutron stars oscillate at higher f- and p1-mode frequencies than ordinary or σ-cut models, while quasi-universal oscillation relations still hold.

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