Bayesian inference of the crust-core transition density via the neutron-star radius and neutron-skin thickness data
摘要: In this work we perform a Bayesian inference of the crust-core transition density t of neutron stars based upon the neutron-star radius and the neutron-skin thickness data within a thermodynamicalmethod. The uniform and Gaussian distributions for the t prior are adopted in the Bayesianapproach. It has a larger probability to have values higher than 0.1 fm3 for t as the uniform priorand the neutron-star radius data are used. We found that this is controlled by the curvature Ksym ofthe nuclear symmetry energy. This phenomenon will not happen if Ksym is not extremely negative,i.e., Ksym > -200 MeV. The obtained t is 0.075+0.005-0.01fm^3 at 68% confifidence level when both the neutron-star radius and the neutron-skin thickness data are taken into account. The strongly anti-correlations between t and the slope L, curvature of the nuclear symmetry energy are observed.The dependence of the three L-Ksym correlations predicted in the literature on the crust-core densityand pressure is quantitatively investigated. The most probable value of 0.08 fm^3 for t is obtainedfrom the L-Ksym relation raised by Holt et al. and the larger values are preferred by the other tworelations.