Multiple configurations of neutron stars containing quark matter
Multiple configurations of neutron stars containing quark matter
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含有夸克物质的中子星的多种配置
DOI：
10.1088/1674-1137/44/9/094104
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发表时间：
2020
期刊：
影响因子：
--
通讯作者：
Fan Weiru
中科院分区：
文献类型：
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作者：
Wei Wei;Yang Shuhua;Bao Zehan;Zhang Chong;Gao Chang;Fan Weiru
本研究的主要目的是解释不同相变路径下混合星构型的可能性，并提供不同构型的条件和特征的一般描述。我们假设有两种可能的相变路径，即从核相直接到2f /3f夸克相，或者先从核相到2f夸克相，然后依次从2f夸克相到3f夸克相。此外，我们考虑了基于一阶跃迁假设的麦克斯韦和吉布斯结构，得到了混合星的多种构型：麦克斯韦结构为N-2f、N-3f和N-2f-3f，吉布斯结构为N-2fmix-2f、N-3fmix-3f、N-2f3fmix和N-2fmix-3f。从相同质量为1.95M⊙的不同混合星构型的半径分析来看，夸克物质（从核夸克到2f夸克或3f夸克物质）的出现导致了0.5km~2km的半径差异，为未来NICER探测提供了可能。然而，从2f夸克物质到3f夸克物质的顺序跃迁很难探测，因为这种跃迁不会导致太大的半径变化（远小于0.5 km）。仅仅依靠测量恒星半径来探测中子星中致密物质的状态方程是有困难的。多信使观测可以帮助我们在未来推断中子星的内部。
The main purpose of this study is to interpret the possibilities of hybrid star configurations under different phase transition paths and provide a general description of the conditions and features of the different configurations. We assume that there are two possible phase transition paths, i.e., from a nuclear phase to a 2flavor(2f)/3flavor(3f) quark phase directly, or first from a nuclear phase to a 2f quark phase, and then from that phase to a 3f quark phase sequentially. In addition, we consider Maxwell and Gibbs constructions based on the assumption of a first-order transition, which yields multiple configurations of hybrid stars: N-2f, N-3f, and N-2f-3f for a Maxwell construction, and N-2fmix-2f, N-3fmix-3f, N-2f3fmix, and N-2fmix-3f for a Gibbs construction. From the radii analysis of different hybrid star configurations with the same mass of 1.95M⊙, the appearance of the quark matter (from nuclear to 2f or 3f quark matter) causes a radius difference of 0.5km~2km and provides the possibility of detection by NICER in the future. However, the sequential transition from 2f to 3f quark matter is difficult to detect because the transition does not lead to too high of a change in radius (far smaller than 0.5 km). The dependence solely on the measurements of the stellar radii to probe the equation of state of dense matter in neutron stars causes difficulties. Multi-messenger observations can help us to infer the interior of a neutron star in the future.