论文标题
相对论$ ab〜InitiO $模型描述的中子星的属性
Properties of neutron star described by a relativistic $ab~ initio$ model
论文作者
论文摘要
Properties of neutron star are investigated by an available relativistic $ab~ initio$ method, i.e., the relativistic Brueckner-Hartree-Fock (RBHF) model, with the latest high-precision relativistic charge-dependent potentials, pvCD-Bonn A, B, C. The neutron star matter is solved within the beta equilibrium and charge neutrality conditions in the framework of RBHF model.与常规处理相比，Lepton的化学潜力近似于核物质的对称能量，在当前的自搭配计算中Neutron Star Matters的状态（EOS）方程与PVCD-BONN B具有显着的差异，其差异超过了Baryon数量密度$ n_b = 0.55 $ n_b = 0.55 $ fm $ fm $^$^$^3} $。但是，这些差异仅影响中子星的全球性能，仅$ 1 \％\ sim2 \％$。然后，在RBHF模型中系统地应用了三个具有不同张量分量的两体势PVCD-BONN A，B，C，以计算中子星的性质。发现中子星的最大质量约为$ 2.21 \ sim2.30m_ \ odot $，相应的半径为$ r = 11.18 \ sim11.72 $ km。 1400万美元的半径$ r_ {1.4} = 12.34 \ sim12.91 $ km且它们的无尺寸潮汐变形能力为$λ_{1.4} = 485 \ sim 626 $。此外，中子星冷却中的直接URCA过程将从$ n_b = 0.414 \ sim0.530 $ fm $^{ - 3} $带有质子分数，$ y_p = 0.136 \ sim0.138 $。仅具有两体PVCD-BONN电位的RBHF模型获得的所有结果完全满足了最近对大型中子星的天文观测，重力波检测（GW 170817）和质量 - 拉迪乌斯同时测量（NECER）。
Properties of neutron star are investigated by an available relativistic $ab~ initio$ method, i.e., the relativistic Brueckner-Hartree-Fock (RBHF) model, with the latest high-precision relativistic charge-dependent potentials, pvCD-Bonn A, B, C. The neutron star matter is solved within the beta equilibrium and charge neutrality conditions in the framework of RBHF model. Comparing to the conventional treatment, where the chemical potential of lepton was approximately represented by the symmetry energy of nuclear matter, the equation of state (EOS) of neutron star matter in the present self-consistent calculation with pvCD-Bonn B has striking difference above the baryon number density $n_b=0.55$ fm$^{-3}$. However, these differences influence the global properties of neutron star only about $1\%\sim2\%$. Then, three two-body potentials pvCD-Bonn A, B, C, with different tensor components, are systematically applied in RBHF model to calculate the properties of neutron star. It is found that the maximum masses of neutron star are around $2.21\sim2.30M_\odot$ and the corresponding radii are $R =11.18\sim11.72$ km. The radii of $1.4M_\odot$ neutron star are predicated as $R_{1.4} = 12.34\sim12.91$ km and their dimensionless tidal deformabilities are $Λ_{1.4} = 485\sim 626$. Furthermore, the direct URCA process in neutron star cooling will happen from $n_b=0.414\sim0.530$ fm$^{-3}$ with the proton fractions, $Y_p=0.136\sim0.138$. All of the results obtained from RBHF model only with two-body pvCD-Bonn potentials completely satisfy various constraints from recent astronomical observations of massive neutron stars, gravitational wave detection (GW 170817), and mass-radius simultaneous measurement (NICER).
