Equation of state of nuclear matter and neutron stars: Quark mean-field model versus relativistic mean-field model

Abstract

The equation of state of neutron-rich nuclear matter is of interest to both nuclear physics and astrophysics. We have demonstrated the consistency between laboratory and astrophysical nuclear matter in neutron stars by considering low-density nuclear physics constraints (from ${}^{208}$Pb neutron-skin thickness) and high-density astrophysical constraints (from neutron star global properties). We have used both quark-level and hadron-level models, taking the quark mean-field (QMF) model and the relativistic mean-field (RMF) model as examples, respectively. We have constrained the equation of states of neutron stars and some key nuclear matter parameters within the Bayesian statistical approach, using the first multi-messenger event GW170817/AT 2017gfo, as well as the mass-radius simultaneous measurements of PSR J0030+0451 and PSR J0740+6620 from NICER, and the neutron-skin thickness of ${}^{208}$Pb from both PREX-II measurement and ab initio calculations. Our results show that, compared with the RMF model, QMF model's direct coupling of quarks with mesons and gluons leads to the evolution of the in-medium nucleon mass with the quark mass correction. This feature enables QMF model a wider range of model applicability, as shown by a slow drop of the nucleon mass with density and a large value at saturation that is jointly constrained by nuclear physics and astronomy.

14 pages, 4 figures, 3 tables, Phys. Rev. C (2023) accepted

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• Neutron Decay Anomaly and Its Effects on Neutron Star Properties
• Modeling matter(s) in SEOBNRv5THM: Generating fast and accurate effective-one-body waveforms for spin-aligned binary neutron stars
• Density-dependent quark mean-field model for nuclear matter and neutron stars
• Exploring nuclear force with pulsar glitch observation
• Effect of isoscalar and isovector scalar fields on baryon semileptonic decays in nuclear matter
• Limitations in constraining neutron star radii and nuclear properties from inspiral gravitational wave detections