Bayesian inference of the crust–core transition density via the neutron-star radius and neutron-skin thickness data  

作　　者：Wen-Jie Xie Zi-Wei Ma Jun-Hua Guo 

机构地区：[1]Department of Physics,Yuncheng University,Yuncheng,044000,China

出　　处：《Nuclear Science and Techniques》2023年第6期125-133,共9页核技术（英文）

基　　金：supported by the Shanxi Provincial Foundation for Returned Overseas Scholars (No. 20220037);Natural Science Foundation of Shanxi Province (No. 20210302123085);Discipline Construction Project of Yuncheng University

摘　　要：In this work,we perform a Bayesian inference of the crust-core transition density ρ_(t) of neutron stars based on the neutron-star radius and neutron-skin thickness data using a thermodynamical method.Uniform and Gaussian distributions for the ρ_(t) prior were adopted in the Bayesian approach.It has a larger probability of having values higher than 0.1 fm^(−3) for ρ_(t) as the uniform prior and neutron-star radius data were used.This was found to be controlled by the curvature K_(sym) of the nuclear symmetry energy.This phenomenon did not occur if K_(sym) was not extremely negative,namely,K_(sym)>−200 MeV.The value ofρ_(t) obtained was 0.075_(−0.01)^(+0.005) fm^(−3) at a confidence level of 68%when both the neutron-star radius and neutron-skin thickness data were considered.Strong anti-correlations were observed between ρ_(t),slope L,and curvature of the nuclear symmetry energy.The dependence of the three L-K_(sym) correlations predicted in the literature on crust-core density and pressure was quantitatively investigated.The most probable value of 0.08 fm^(−3) for ρ_(t) was obtained from the L-K_(sym) relationship proposed by Holt et al.while larger values were preferred for the other two relationships.

关 键 词：Crust–core transition density of neutron stars Neutron-star radius Neutron-skin thickness Bayesian inference approach L–K_(sym) 

分 类 号：P145.6[天文地球—天体物理]