Dependence of the tidal deformability of neutron stars on the nuclear equation of state  

作　　者：谢文杰 陈建玲 马紫微 郭俊华 祝龙 Wen-Jie Xie;Jian-Ling Chen;Zi-Wei Ma;Jun-Hua Guo;Long Zhu(Department of Physics,Yuncheng University,Yuncheng 044000,China;Sino-French Institute of Nuclear Engineering and Technology,Sun Yat-sen University,Zhuhai 519082,China)

机构地区：[1]Department of Physics,Yuncheng University,Yuncheng 044000,China [2]Sino-French Institute of Nuclear Engineering and Technology,Sun Yat-sen University,Zhuhai 519082,China

出　　处：《Chinese Physics C》2023年第1期160-167,共8页中国物理C（英文版）

基　　金：Supported by the Shanxi Provincial Foundation for Returned Overseas Scholars(20220037);the Natural Science Foundation of Shanxi Province(20210302123085);the discipline construction project of Yuncheng university;the National Natural Science Foundation of China(12075327)。

摘　　要：Within the Bayesian framework,using an explicitly isospin-dependent parametric equation of state(EOS)for the core of neutron stars(NSs),we studied how the NS EOS behaves when we confront it with the tidal deformabilitiesΛ1.4abilities of massive NSs.We found that it does not significantly improve the constraints on the NS EOS but has a weak effect on narrowing down the slope parameter of the symmetry energy by decreasing the measurement errors ofΛ1.4.Both the isospin-dependent and isospin-independent parts of the NS EOS were significantly constrained and raised as the tidal deformabilities of massive NSs were adopted in the calculations,especially in high-density regions.We also found thatΛ1.4symmetry energy,whereas the opposite occurs for the radius of canonical NSs R1.4.The tidal deformability of an NS with two times the solar massΛ2.0ergy,andΛ1.4and R1.4have no correlation with the former.

关 键 词：symmetry energy equation of state tidal deformability Bayesian inference approach neutron stars 

分 类 号：P145.6[天文地球—天体物理]