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Hadron matter in neutron stars in view of gravitational wave observations
Progress in Particle and Nuclear Physics ( IF 9.6 ) Pub Date : 2019-11-01 , DOI: 10.1016/j.ppnp.2019.103715
Felipe J. Llanes-Estrada , Eva Lope-Oter

Abstract In this review we highlight a few physical properties of neutron stars and their theoretical treatment inasmuch as they can be useful for nuclear and particle physicists concerned with matter at finite density (and newly, temperature). Conversely, we lay out some of the hadron physics necessary to test General Relativity with binary mergers including at least one neutron star, in view of the event GW170817: neutron stars and their mergers reach the highest matter densities known, offering access to the matter side of Einstein’s equations. In addition to minimum introductory material for those interested in starting research in the field of neutron stars, we dedicate quite some effort to a discussion of the Equation of State of hadron matter in view of gravitational wave developments; we address phase transitions and how the new data may help; we show why transport is expected to be dominated by turbulence instead of diffusion through most if not all of the star, in view of the transport coefficients that have been calculated from microscopic hadron physics; and we relate many of the interesting physics topics in neutron stars to the radius and tidal deformability.

中文翻译:

基于引力波观测的中子星中的强子物质

摘要 在这篇综述中,我们重点介绍了中子星的一些物理特性及其理论处理,因为它们对关注有限密度(以及新的温度)物质的核和粒子物理学家很有用。相反,鉴于事件 GW170817:中子星及其合并达到已知的最高物质密度,提供了对物质方面的访问,因此我们列出了一些必要的强子物理学,以通过包括至少一颗中子星的双星合并来测试广义相对论爱因斯坦方程组。除了为那些有兴趣开始中子星领域研究的人提供最少的介绍材料外,我们还致力于从引力波发展的角度讨论强子物质的状态方程;我们解决了相变以及新数据如何提供帮助;考虑到从微观强子物理学计算出的传输系数,我们展示了为什么传输预计会以湍流为主,而不是通过大部分(如果不是全部)恒星进行的扩散;我们将中子星中许多有趣的物理主题与半径和潮汐变形性联系起来。
更新日期:2019-11-01
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