低密度物态方程对中子星性质的影响(英文)  

Response of the Neutron Star Properties to the Equation of State at Low Density

作　　者：朱照寰[1] 班淑芳[1] 李俊[1] 孟杰[1] 

机构地区：[1]北京大学物理学院,北京100871

出　　处：《高能物理与核物理》2005年第6期565-569,共5页High Energy Physics and Nuclear Physics

基　　金：国家重点基础研究发展规划项目(G2000077407);国家自然科学基金(10025522,10435010,10221003);教育部博士基金资助~~

摘　　要：利用相对论平均场理论描述中子星的液体区域,Fermi气体模型或者FMT,BPS和BBP模型描述中子星外壳,分别称为Fermigas+RMF和RMF .计算了中子星性质并且和相对论平均场理论给出的结果进行比较.虽然低密度物态方程对中子星最大质量、中心密度、能量密度和压强的影响很小,但是它对中子星的质量半径关系改变很大.对应中子星的最大质量,RMF和RMF 之间的半径差别为0.23—0.33km.Using the RMF theory to describe the neutron liquid region in the neutron star and the Fermi gas model or FMT, BPS, and BBP model to describe the crust of the neutron star (referred as Fermi gas + RMF and RMF* respectively), the properties of the neutron star are calculated and compared with those from the RMF theory. Although the EOS at low density has negligible influence on the maximum mass of the neutron star, and its corresponding central density, energy density, and pressure, it changes the mass-radius relationship of neutron stars considerably. The differences of the neutron star radius corresponding to maximum mass between the RMF theory and RMF* calculations are 0.23-0.33 km.

关 键 词：中子星 低密度物态方程 相对论平均场 外壳半径 

分 类 号：P145.6[天文地球—天体物理] O412[天文地球—天文学]