Can the PREX-2 and CREX results be understood by relativistic mean-field models with the astrophysical constraints?

Abstract

We construct new effective interactions using the relativistic mean-field models with the isoscalar- and isovector-meson mixing, ${\sigma }^2{\mathbf{\delta }}^2$ and ${\omega }_{\mu }{\omega }^{\mu }{\mathbf{\rho }}_{\nu }{\mathbf{\rho }}^{\nu }$. Taking into account the particle flow data in heavy-ion collisions, the observed mass of PSR J0740$+$6620, and the tidal deformability of a neutron star from binary merger events, GW170817 and GW190814, we study the ground-state properties of finite, closed-shell nuclei, and try to explain the recent results from the PREX-2 and CREX experiments. It is found that the $\sigma$--$\delta$ mixing is very powerful to understand the terrestrial experiments and astrophysical observations of neutron stars self-consistently. We can predict the large neutron skin thickness of ${}^{208}$Pb, $R_{\mathrm{skin}}^{208}=0.243$~fm, using the slope parameter of nuclear symmetry energy, $L=70$~MeV, which is consistent with the PREX-2 result. However, to explain the CREX data, it is preferable to adopt the small value of $L=20$~MeV. It is very difficult to understand the PREX-2 and CREX results simultaneously within relativistic mean-field models.

7 pages, 6 figures, 4 tables

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• Neutron stars and the dense matter equation of state: from microscopic theory to macroscopic observations
• Compiled Properties of Nucleonic Matter and Nuclear and Neutron Star Models from Non-Relativistic and Relativistic Interactions
• Hybrid stars in light of the HESS J1731-347 remnant and the PREX-II experiment
• Equation of state of nuclear matter and neutron stars: Quark mean-field model versus relativistic mean-field model
• New quantification of symmetry energy from neutron skin thicknesses of ${}^{48}$Ca and ${}^{208}$Pb
• Estimation of the slope of nuclear symmetry energy via charge radii of mirror nuclei
• Probe and Prejudice: Classification of compact objects and model comparison using EOS knowledge
• Ab initio computations of the fourth-order charge density moments of ${}^{48}$Ca and ${}^{208}$Pb
• Influence of the effective mass on the properties of nuclear matter at finite density and temperature
• Constraining neutron star properties through parity-violating electron scattering experiments and relativistic point coupling interactions
• I-C-Q relations for rapidly rotating stable hybrid stars
• Confronting recent light compact star observations with color-flavor locked quark matter
• Effect of isoscalar and isovector scalar fields on baryon semileptonic decays in nuclear matter
• Novel features of asymmetric nuclear matter from terrestrial experiments and astrophysical observations of neutron stars
• Equation of state for hyperonic neutron-star matter in SU(3) flavor symmetry
• Effects of isovector spin-orbit interaction on the charge-weak form factor difference in ${}^{48}$Ca, ${}^{208}$Pb, ${}^{90}$Zr and ${}^{62}$Ni
• Examining the possibility of a thick crust in the compact stellar object HESS J1731-347
• Accuracy and Applicability of the Hartle-Thorne and Komatsu-Eriguchi-Hachisu Methods for Modeling Rotating Neutron Stars
• Equation-of-State Independent Relations in Rapidly Rotating Hybrid Stars