含退禁闭物质中子星g-modes特性及其引力波观测效应研究

双中子星并合引力波信号（GW170817）的首次探测为揭开核饱和密度之上物质状态提供了新的重要途径，天体核物理学从此进入新时代。研究中子星的原因之一就是理解极端密度下强相互作用物质状态。在此密度下，中子星内极有可能出现夸克等新物态相，但到目前为止我们都没有得到确定性的观测证据。根据现有质量、半径观测，含有夸克物质中子星，特别是含有核子-夸克混合相的混杂星，它们可以有着跟普通中子星非常接近的质量-半径关系，从而很难与普通中子星区分。本项目在构造多种中子星结构的基础上，计算分析不同结构下中子星的core g-modes 振荡频谱及特性，深入研究双中子星旋进过程中星体振荡模式与旋进潮汐作用的耦合效应，及其最终对引力波辐射信号的影响。寻找夸克物质出现在双中子星并合引力波信号中留下的观测印迹，为解决含退禁闭物质中子星“伪装”问题找到可靠的观测证据。

With the announcement of the first direct detection of gravitational waves from the late inspiral phase of a double neutron star system, we enter an exciting new era for nuclear astrophysics. These observations are of tremendous importance for nuclear physics as they help unlock the secrets of the equation of state for matter at super-nuclear densities. One of the reasons to study compact stars, comprising the neutron, quark or hybrid class, is to understand the state of strongly interacting matter at extreme density. Novel phases of matter are conjectured to occur inside compact stars, but as yet there is no conclusive observational evidence of any phase that is fundamentally different from hadronic matter. A hybrid star with quark matter in its interior cannot be easily distinguished from an ordinary neutron star based on the current observational status of masses and radii, even more so if quark matter is in a mixed phase. Based on neutron stars with different hadron-quark mixed phase, this work will calculate and analyze core g-mode oscillations frequency spectrum of these stars, and explore dynamical effect of the tidal interaction on the mode oscillations in the spiral phase of neutron binary. If core g-mode oscillations resonantly excited by tidal forces during the inspiral are detected, either directly with third generation detectors or indirectly through gravitational wave phasing, that could finally lift the veil on quark matter inside neutron stars and resolve the masquerade problem.