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Simultaneously constraining the neutron star equation of state and mass distribution through multimessenger observations and nuclear benchmarks

Bhaskar Biswas and Stephan Rosswog

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Phys. Rev. D 112, 023045 – Published 30 July, 2025

DOI: https://doi.org/10.1103/8lv3-1ywb

Abstract

With ongoing advancements in nuclear theory and experimentation, together with a growing body of neutron star (NS) observations, a wealth of information on the equation of state (EOS) for matter at extreme densities has become accessible. Here, we utilize a hybrid EOS formulation that combines an empirical parametrization centered around the nuclear saturation density with a generic three-segment piecewise polytrope model at higher densities. We incorporate data derived from chiral effective field theory (χEFT), perturbative quantum chromodynamics (pQCD), and experiments such as PREX-II and CREX. Furthermore, we examine the influence of a total of 70 NS mass measurements up to April 2023, as well as simultaneous mass and radius measurements derived from the x-ray emission from surface hot spots on NSs. Additionally, we consider constraints on tidal properties inferred from the gravitational waves emitted by coalescing NS binaries. To integrate this extensive and varied array of constraints, we utilize a hierarchical Bayesian statistical framework to simultaneously deduce the EOS and the distribution of NS masses. We find that incorporating data from χEFT significantly tightens the constraints on the EOS of NSs near or below the nuclear saturation density. However, constraints derived from pQCD computations and nuclear experiments such as PREX-II and CREX have minimal impact. Taking into account all available data, we derive estimates for key parameters characterizing the EOS of dense nuclear matter. Specifically, we determine the slope (L) and curvature (Ksym) of the symmetry energy to be 54−10+10 and −158−63+73  MeV with 90% credibility, respectively. Additionally, we infer the radius and tidal deformability of an NS with a mass of 1.4 solar masses (M⊙) to be 12.34−0.53+0.43  km and 436−117+109, respectively. Furthermore, we estimate the maximum mass of a nonrotating NS to be 2.22−0.19+0.21M⊙ with 90% credibility.

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Phys. Rev. D 112, 023045– Published 30 July, 2025
  • Received 1 February 2025
  • Accepted 15 July 2025
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