色香味锁夸克物质核旋转混合致密星的结构性质及其潮汐形变
Structural Properties of Rotating Hybrid Compact Stars with Color-Flavour-Locked Quarks Matter core and its Tidal Deformability
摘要：
在整体中性和化学平衡条件下，我们研究了由核子、超子和三味色味锁夸克组成的混合致密星的可能结果。在相对论平均场论的能量密度泛函框架内，采用两种不同的模型参数化方法计算了强子状态方程。用非相对论性能量密度泛函方法导出的夸克准粒子模型计算了夸克物态方程的物质相位。利用GW 170817双星中子星（BNS）并合的频率和最大引力质量2 $M_\odot$的观测数据及其提取的半径、开普勒极限、长期轴对称不稳定性和潮汐形变极限，得到了一组合理的超密强子-夸克混合状态方程。我们得到了非旋转和旋转致密星的结构性质，等重子质量恒星在电磁辐射和引力辐射作用下自旋下降的演化序列，讨论了强子到夸克物质相的相变问题。在重子质量不变的情况下，讨论了具有观测到的自旋下降频率的旋转星的内部结构，表明致密星的软夸克核收缩。本文给出了与最近观测到的毫秒双星相对应的混合星自旋下降构型的半径极限的理论计算值。给出了非自旋混合星的潮汐变形能力、$Λ$和潮汐参数$Λ_1$、$Λ_2$的计算结果，并进行了讨论，其结果与GW 170817 BNS的波形模型分析一致。
英文摘要：
We investigate the possible sequels, for the hybrid compact stars consisting of nucleons, hyperons and three flavour color-flavor-locked quarks phase under global neutrality and chemical equilibrium conditions. The hadron equations of state are computed within the framework of energy density functionals based on the relativistic mean field theory by employing two different model parameterizations. The quarks matter phase of equation of state is computed by using Quarks Quasiparticle model derived from a non-relativistic energy density-functional approach. A plausible set of hybrid equations of state for superdense hadron-quarks matter is obtained and, which satisfies the constraints provided by bulk nuclear matter, the observational data of frequencies and maximum Gravitational mass 2$M_\odot$ with their extracted radii, Keplerian limits, secular axisymmetric instability and limits of tidal deformabilities from GW170817 binary neutron stars (BNS) merger. We obtained structural properties of nonrotating and rotating compact stars, the evolutionary sequences with constant baryonic mass star spinning down by electromagnetic and gravitational radiations and, discuss the issues relating to phase transition from hadrons to quarks matter phase. The internal structure of rotating star with observed spin down frequencies, exhibiting shrinkage of soft quarks core of compact stars are discussed for constant baryonic mass. We present the theoretically computed limits of radii for the spin down configurations of hybrid stars corresponding to the recently observed millisecond pulsars. We also present and discuss the calculated results for tidal deformability, $Λ$ and tidal parameters $Λ_1$, $Λ_2$ of non spining hybrid star which are consistent with the waveform model analysis of GW170817 BNS.
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