Constraining the density dependence of the symmetry energy with nuclear data and astronomical observations in the KIDS framework

Abstract

The KIDS framework for the nuclear equation of state (EoS) and energy density functional (EDF) offers the possibility to explore symmetry-energy (SE) parameters such as J (value at saturation density), L (slope), Ksym (curvature) and so on independently of each other and of assumptions about the effective mass. Here we examine the performance of EoSs with different SE parameters in reproducing nuclear properties and astronomical observations in an effort to constrain especially L and Ksym or the droplet-model counterpart Ktau. Assuming a standard EoS for symmetric matter, we explore several points on the hyperplane of (J,L,Ksym or Ktau) values. For each point, the corresponding EDF parameters and a pairing parameter are obtained for applications in spherical even-even nuclei. This is the first application of KIDS EDFs with pairing correlations. The EoSs are tested successively on properties of closed-shell nuclei, along the Sn isotopic chain, and on astronomical observations, in a step-by-step process of elimination and correction. A small regime of best-performing parameters is determined. The results strongly suggest that Ksym is negative and no lower than -200MeV, that Ktau lies between roughly -400 and -300MeV and that L lies between 40 and 65MeV with L<55MeV more likely. Correlations between symmetry-energy parameters are critically discussed. Predictions for the position of the neutron drip line and the neutron skin thickness of selected nuclei are reported. They are only weakly affected by the choice of effective mass values. Parts of the drip line can be sensitive to the SE parameters. The results underscore the role of Ktau and of precise astronomical input. Better constraints are possible with precise fits to nuclear energies and, in the future, more-precise input from astronomy.

15 pages incl. 7 figures, 4 tables; this version of the preprint (v2) corresponds to the published version (some comments added, a few typos corrected)

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• Bayesian inference of neutron-star observables based on effective nuclear interactions
• Bayesian inference of finite-nuclei observables based on the KIDS model
• Quasi-elastic electron scattering with KIDS nuclear energy density functional
• Quasielastic Charged-Current Neutrino-Nucleus Scattering with Nonrelativistic Nuclear Energy Density Functionals
• Bayesian inference of neutron-skin thickness and neutron-star observables based on effective nuclear interactions
• Inclusive electron scattering in the quasielastic region with Korea-IBS-Daegu-SKKU density functional
• Incompressibility and Symmetry Energy of Neutron Star
• Realizing the potential of deep neural network for analyzing neutron star observables and dense matter equation of state
• KIDS density functional for deformed nuclei: Examples of the even-even Nd isotopes
• Non-radial oscillations of hadronic neutron stars, quark stars, and hybrid stars : Calculation of $f$, $p$, and $g$ mode frequencies
• Influence of the effective mass on the properties of nuclear matter at finite density and temperature
• Calculations for nuclear matter and finite nuclei within and beyond energy--density--functional theories through interactions guided by effective field theory
• Nuclear mass table in density functional approach inspired by neutron-star observations
• Hadron-quark phase transition in the neutron star with vector MIT bag model and Korea-IBS-Daegu-SKKU functional
• Renormalization-Group Invariant Parity-Doublet Model for Nuclear and Neutron-Star Matter
• Systematic study for the surface properties of neutron star