Bayesian inference of the parameters involved in the nuclear symmetry energy
This study employs a theoretical framework that combines neutron star models with the Bayesian inference method to infer the parameters of the nuclear symmetry energy based on the currently available observational data regarding the mass,radius,and tidal deformability of neutron stars.Existing observations of neutron star tidal deformability can make only limited contributions to our understanding of nuclear symmetry energy.Results obtained from analyses using the equation of state for neutron star matter obtained from the recent joint studies of heavy-ion collisions and astrophysical observations are consistent with those previously obtained based on observations of neutron stars.Furthermore,we observe that the maximum mass of neutron stars has little sensitivity to the symmetry energy parameters.Comparatively,the experimental data on neutron skin thickness reported by the CREX and PREX-Ⅱ collaborations provide more effective constraints on the parameters of the nuclear symmetry energy.Furthermore,using a theoretical framework that combines the nuclear liquid drop model with the Bayesian inference method,we find that the uncertainty ranges for the symmetry energy parameters obtained from neutron skin thickness data for 208Pb and 48Ca are substantially different and have little overlap.Due to the differences in data error,the parameters of the nuclear symmetry energy constrained by the neutron skin thickness data obtained from the 48Ca data are narrower than those obtained from the 208Pb data.Moreover,the parameter ranges obtained from neutron skin thickness data differ significantly from those obtained from observations of neutron stars,with the former supporting a softer symmetry energy and the latter favoring a stiffer symmetry energy.Finally,we also investigate the effect of prior distributions on the inference of the symmetry energy parameters from neutron star observations.Our calculations demonstrate that the curvature parameter(Ksym)does not depend on the prior distribution,the slope parameter L depends slightly on the prior distribution,and the skewness parameter(Jsym)depends strongly on the prior distribution.
symmetry energy of nuclear matterBayesian inference approachobservational data of neutron starsneutron skin thicknessprior distribution
万方数据
维普
