Effect of Nucleon Superfluidity and Its Uncertainty on the Neutron Star Cooling  

核子超流动性及其不确定性对中子星冷却的影响

作　　者：WANG Yanping DONG Jianmin BAO Xiaojun WU Puxun 王言平;董建敏;包小军;吴普训(湖南师范大学物理与电子科学学院,长沙410081;中国科学院近代物理研究所,兰州730000)

机构地区：[1]Department of Physics,Collaborative Innovation Center for Quantum Effects,and Key Laboratory of Low Dimensional Quantum Structures and Quantum Control of Ministry of Education,Hunan Normal University,Changsha 410081,China [2]Institute of Modern Physics,Chinese Academy of Sciences,Lanzhou 730000,China

出　　处：《原子核物理评论》2024年第3期910-916,共7页Nuclear Physics Review

基　　金：国家自然科学基金资助项目(12222511,12275080,12175064,U2167203);湖南省杰出青年科学基金(2022JJ10031);中国科学院青年基础研究团队稳定支持项目(YSBR-088)。

摘　　要：We calculate the cooling curves of superfluid neutron stars with the Brueckner-Hartree-Fock(BHF)equation of state(EOS)by employing the AV18 two body force with a microscopic three body force.The gap energy is calculated within the BCS theory,including in the pairing interaction not only two body force but also three body force.The calculated cooling curves show that the nucleon superfluidity strongly reduces the difference between standard and enhanced cooling.This enables one to explain the majority of observational data by the enhanced cooling of the stars with superfluid cores.The possibility of strong direct Urca processes still cannot be excluded from the cooling analysis.采用AV18两体力结合微观三体力作为Brueckner-Hartree-Fock理论的输入量计算了状态方程,进而基于BCS理论计算了对能隙。理论计算的状态方程和对能隙作为冷却理论的输入量计算了冷却曲线。理论计算的冷却曲线表明,核子超流显著地减小了标准冷却理论和增强冷却理论之间的差异。基于考虑超流核心的增强冷却理论可以很大程度上解释天文观测值。因此,中子星冷却包含很强的直接Urca过程的可能性仍旧不能被排除。

关 键 词：BRUECKNER-HARTREE-FOCK nucleon superfluid neutron stars cooling curves 

分 类 号：O571.6[理学—粒子物理与原子核物理]