The Golden Era of Neutron Stars: From Hadrons to Quarks
The Golden Era of Neutron Stars: From Hadrons to Quarks
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DOI：
10.7566/jpscp.26.011001
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发表时间：
2019-02
期刊：
影响因子：
--
通讯作者：
G. Baym
中科院分区：
文献类型：
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作者：
G. Baym
中子星最早是在30年代初被提出的，60年代末被发现为中子星;然而，直到最近，我们才开始了解它们所包含的物质。这次谈话描述了一个一致的中子星内部液体的图片，由四个进步驱动的持续发展：两个重中子星与质量$\simeq $2.0太阳质量的观测;质量和半径的推论，同时为越来越多的中子星在低质量X射线双星，并通过NICER天文台未来的决心;通过引力波和电磁波谱观测到的双星合并的中子星星，GW 170817;以及在QCD中对核物质如何在内部转变为非限定夸克物质的新认识。我们描述了现代夸克-强子交叉状态方程，QHC 18，和相应的中子星，这与目前的观测结果吻合得很好。
Neutron stars were first posited in the early thirties, and discovered as pulsars in late sixties; however, only recently are we beginning to understand the matter they contain. This talk describes the continuing development of a consistent picture of the liquid interiors of neutron stars, driven by four advances: observations of two heavy neutron stars with masses $\simeq$ 2.0 solar masses; inferences of masses and radii simultaneously for an increasing number of neutron stars in low mass X-ray binaries, and future determinations via the NICER observatory; the observation of the binary neutron star merger, GW170817, through gravitational waves as well as across the electromagnetic spectrum; and an emerging understanding in QCD of how nuclear matter can turn into deconfined quark matter in the interior. We describe the modern quark-hadron crossover equation of state, QHC18, and the corresponding neutron stars, which agree well with current observations.