大质量中子星物质内状态方程及复杂相结构的研究

Adjusting coupling constants of relativistic mean field theory (RMFT), possible equations of state (EOS) for massive neutron star are studied. Adopting density-dependent bag parameters in the framework of several important quark models considering strong interaction, thermodynamics of strange quark matter are derived. On this basis, using these models, unpaired quark matter, two-flavor color superconducting phase and color-flavor-locked phase are described, and possible equations of state and phase structures for massive neutron stars as strange star or hybrid star are investigated. Then complex phase structures for massive neutron stars from their high-density core to lower-density crust are given. Mass-radius relations of neutron stars are calculated and contrasting with observational data of pulsars, new physical signals for nuclear matter in extreme conditions are got. Moreover, using these quark models and several nuclear matter parameter sets in the framework of RMFT, we describe quark matter and hadronic matter in hybrid star respectively, and among these EOS, we search non-smooth hybrid star equations of state in which third family of compact star exist in mass-radius relations. Range of parameters in quark model and hadron model are determined simultaneously. Owing to higher density than neutron stars, deconfinement quark matter state, two-flavor color superconducting phase and color-flavor-locked phase may be existed in third family of compact stars.

调节相对论平均场理论中各个耦合常数，研究大质量脉冲星做为超子星可能的状态方程；在考虑夸克间强作用的NJL模型、有效质量口袋模型、质量密度依赖夸克模型和我们最近发展的夸克模型中采用密度依赖口袋常数，描述夸克相及各种色超导相，推导夸克物质新的热力学关系，研究大质量脉冲星做为奇异星或混合星的状态方程及复杂相结构，给出其内高密度核心到低密度表面复杂相结构较全面的图像。计算质量和半径等可观测物理量，与脉冲星观测数据比对，获取极端条件下核物质性质的新物理信号；采用上述几个夸克模型描述两味色超导相、CFL相和夸克相，用相对论平均场框架下的多个参数组描述强子相，研究混合星状态方程，找出存在不光滑状态方程、从而存在致密星第三家族的若干对强子、夸克模型，同时确定与此相应的模型参数范围。由于核心密度比中子星还高，在致密星第三家族内更有可能存在倍受关注的夸克相、色超导相、介子凝聚相等新物态，给出复杂的相结构。

密度依赖口袋常数时，推导了夸克物质新的热力学关系，奇异夸克物质的压强有一个附加项，而能量密度则没有，保证了热力学自洽性。奇异物质和混合星的状态方程变软，质量、半径变小。介子凝聚和考虑引力修正，研究了U玻色子与重子的耦合常数和反介子光学势对中子星质量、半径、自转周期、引力红移及转动惯量的影响。表明，耦合常数使中子星质量变大，中心密度减少，增加转动惯量，减少引力红移。研究了相对论修正对中微子发射率，中微子发光度及中微子冷却率的影响。相对论效应使中微子发射率，中微子发光度及中微子冷却率降低。研究了张量耦合对中子星物质内核子的直接URCA过程的影响。张量耦合略增加中子星的质量，矢量介子和同位旋矢量介子的矢量耦合对直接URCA过程中总中微子发射率明显加强，加速非超流中子星物质内的冷却。研究了色、味封锁色超导相核心的混合星的整体性质。随着CFL能隙的增加，出现强子相到混合相再到纯CFL相的相变。也研究了CFL核心的致密星第三家族，能隙在100 MeV≤Δ<150 MeV内存在第三家族。