利用贝叶斯推断从中子星性质确定状态方程  

Bayesian inference on the equation of state from neutron stars properties

作　　者：单梓扬 杨钧评 焦学胜[1] 袁大庆[1] 夏铖君 张英逊[1,3] SHAN ZiYang;YANG JunPing;JIAO XueSheng;YUAN DaQing;XIA ChengJun;ZHANG YingXun(Department of Nuclear Physics,China Institute of Atomic Energy,Beijing 102413,China;Center for Gravitation and Cosmology,College of Physical Science and Technology,Yangzhou University,Yangzhou 225009,China;Guangxi Key Laboratory Breeding Base of Nuclear Physics and Technology,Guilin 541004,China)

机构地区：[1]中国原子能科学研究院核物理研究所,北京102413 [2]扬州大学物理科学与技术学院引力与宇宙学研究中心,扬州225009 [3]广西核物理与核技术重点实验室,桂林541004

出　　处：《中国科学：物理学、力学、天文学》2024年第11期127-140,共14页Scientia Sinica Physica,Mechanica & Astronomica

基　　金：国家自然科学基金(编号:12275359,11875323,11961141003,12275234,12342027);国家重点基础研究发展计划(编号:2023YFA1606402);稳定基础支持项目(编号:BJ20002501,BJ010261223284);中国原子能科学研究院院长基金(编号:YZ222407001301,YZ232604001601);中核集团领创项目(编号:LC192209000701,LC202309000201);科技部SKA专项项目(编号:2020SKA0120300)资助。

摘　　要：本文讨论了当前天文观测中中子星最大质量、1.4倍太阳质量中子星半径、潮汐形变以及声速限制等对状态方程的约束.如果3倍饱和密度以上状态方程的多方参数取γ=2.9,同时使用上述四种限制约束的Skyrme相互作用下的核物质参数的均值和偏差为:不可压缩模量K_(0)=243.4±22.0 MeV;对称能因子S_(0)=29.3±2.9 MeV;对称能斜率L=74.4±14.8 Me V;同位旋标量有效质量m_(s)^(*)/m=0.79±0.13;有效质量劈裂参数fI=0.08±0.30(中子有效质量小于质子的有效质量).当考虑3倍饱和密度以上状态方程的多方参数取γ=2.45–2.9时,约束出的K_(0)均值增加了11%,S0均值降低了2%,L均值减少了20%,m_(s)^(*)/m均值降低了4%,但是参数f_(I)均值减小了88%.特别是,如果仅利用中子星的质量小于2.05M_(⊙)的数据来进行约束,发现其所需的参数组对应的中子有效质量大于质子有效质量.不同中子星质量区约束出的f_(I)符号的差异表明,未来进一步约束有效的Skyrme相互作用的状态方程的参数还需结合重离子碰撞分析.In this paper,we apply Bayesian inference to constrain the nuclear equation of state parameters by using properties of neutron stars,including the maximum neutron star mass,radius,tidal deformability at 1.4 times the solar mass,and speed of sound.When the polytrope EOS parameterγis fixed at 2.9 and above four astronomical observations are simultaneously used,the mean values and uncertainties of the nuclear matter parameters derived from standard Skyrme interactions are as follows:incompressibility K_(0)=243.4±22.0 MeV,symmetry energy coefficient S 0=29.3±2.9 MeV,the slope of symmetry energy L=74.4±14.8 MeV,the isoscalar effective mass m∗s/m=0.79±0.13,and a quantity related to effective mass splitting fI=0.08±0.30(when fI>0,this implies that the effective mass of neutrons is less than that of protons).When considering the uncertainty ofγin the range of 2.45-2.9,we found that K0 increased by 11%,S 0 decreased by 2%,L decreased by 20%,m^(∗)_(s)/m decreased by 4%,and the averaged value of fI reduced by 88%.Particularly,if constraints are based solely on neutron star masses less than 2.05 M_(⊙),the preferred effective Skyrme interactions exhibit a neutron effective mass greater than the proton effective mass,i.e.,f_(I)<0.The inverse sign of the constrained f_(I)implies that reducing the uncertainties of the effective Skyrme interaction parameters needs combination analysis with heavy-ion collisions in future studies.

关 键 词：核物质状态方程 有效质量劈裂 中子星 贝叶斯推断 

分 类 号：P145.6[天文地球—天体物理]