用相对论性的$ab~ initio$方法研究了中子星的性质，相对论Brueckner-Hartree-Fock（RBHF）模型，最新的高精度相对论电荷依赖势，pvCD-Bonn A，B，C。中子星物质在RBHF模型框架下，在β平衡和电中性条件下求解。与用核物质的对称能近似表示轻子化学势的传统处理方法相比，在重子数密度$n_b=0.55$ fm $^{-3}$以上，本文用pvCD-Bonn B自洽计算的中子星物质的物态方程有显著的差异。然而，这些差异对中子星整体性质的影响仅限于$1\%\sim2\%$。然后，系统地将三种不同张量分量的两体势pvCD-Bonn A，B，C应用到RBHF模型中，计算了中子星的性质。发现中子星的最大质量在$2.21\sim2.30M_\odot$附近，对应的半径为$R =11.18\sim11.72$ km。计算了$1.4M_\odot$中子星的半径为$R_{1.4} = 12.34\sim12.91$ km，无因次潮汐形变率为$Λ_{1.4} = 485\sim 626$。此外，中子星冷却中的直接URCA过程将从具有质子分数$Y_p=0.136\sim0.138$的$n_b=0.414\sim0.530$ fm $^{-3}$发生。从RBHF模型得到的所有结果完全满足最近的大质量中子星天文观测、引力波探测（GW 170817）和质量-半径同时测量（NICER）的各种约束条件。
英文摘要：
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. 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).
Impact of ab initio E1 strength on neutron capture rates along the nickel isotopic chain
Facility for Rare Isotope Beams, Michigan State University（稀有同位素束设施，密歇根州立大学）；Physics Division, Oak Ridge National Laboratory（橡树岭国家实验室物理部）；Department of Physics, Chalmers University of Technology（查尔姆斯理工大学物理系）
Ab initio calculations of beta-decay half-lives for $N=50$ neutron-rich nuclei
Technische Universität Darmstadt（达姆施塔特工业大学）；ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH（极端物质研究所（EMMI），GSI亥姆霍兹重离子研究中心有限公司）；Max-Planck-Institut für Kernphysik（马克斯·普朗克核物理研究所）；Center for Computational Sciences, University of Tsukuba（筑波大学计算科学中心）
New ab initio constrained extended Skyrme equations of state for simulations of neutron stars, supernovae and binary mergers: II. Thermal response in the suprasaturation density domain
National Institute for Physics and Nuclear Engineering (IFIN-HH)（核物理与核工程国家研究所）
New {\em ab initio} constrained extended Skyrme equations of state for simulations of neutron stars, supernovae and binary mergers: I. Subsaturation density domain
Ab initio Green's function theory of superfluid neutron matter
Johannes Gutenberg-Universität Mainz（美因茨约翰内斯·古腾堡大学）；Institut für Kernphysik（核物理研究所）；PRISMA++ Cluster of Excellence（PRISMA++卓越集群）；Università degli Studi di Milano（米兰大学）；Dipartimento di Fisica “Aldo Pontremoli”（阿尔多·蓬特莫利物理系）；INFN, Sezione di Milano（意大利国家核物理研究所米兰分部）
Ab Initio Calculations of the Carbon and Oxygen Isotopes: Energies, Correlations, and Superfluid Pairing
Institute for Basic Science（韩国基础科学研究所）；Korea Institute of Science and Technology Information（韩国科学技术信息研究所）；Gaziantep Islam Science and Technology University（加济安泰普伊斯兰科学与技术大学）；King Fahd University of Petroleum and Minerals (KFUPM)（法赫德国王石油与矿产大学）；Michigan State University（密歇根州立大学）；Universitat Bonn（波恩大学）；Institute for Advanced Simulation (IAS-4)（先进模拟研究所 (IAS-4)）；Beihang University（北京航空航天大学）
Ab initio study of the halo structure in $^{11}$Be
Beihang University（北京航空航天大学）；King Fahd University of Petroleum and Minerals (KFUPM)（法赫德国王石油与矿产大学）；Gaziantep Islam Science and Technology University（加济安特普伊斯兰科学与技术大学）；Universität Bonn（波恩大学）；Michigan State University（密歇根州立大学）；Forschungszentrum Jülich（于利希研究中心）；Nankai University（南开大学）
