论文标题
中子恒星潮汐变形和状态约束的方程
Neutron star tidal deformability and equation of state constraints
论文作者
论文摘要
尽管历史悠久和天体物理的重要性，但中子恒星的某些关键特性仍然不确定。其内部遇到的极端条件，涉及在极密密度和异种不对称的情况下不确定成分的问题，独特地确定了一般相对论中恒星的宏观特性。长期以来，使用了这些宏观特性（例如中子星形质量和半径）的天体物理约束，以了解形成它们的物质的显微镜特性。在本文中，我们讨论了中子星的另一个天体物理可观察到的宏观特性，可用于研究其内部：它们的潮汐变形。与任何其他带有结构的扩展对象一样，中子星在外部潮汐场的影响下潮汐变形。在通过其引力波发射观察到的中子星的结合的背景下，可以测量通过称为\ emph {潮汐变形性}的参数量化的变形。我们讨论了潮汐变形性在与重力波的合并中子恒星观测中的作用，以及如何使用它来探测自然最紧凑的物质物体的内部结构。也许不可避免地，讨论的很大一部分将由GW170817决定，这是最有用的确认检测到截至写作时对引力波的二进制中子恒星合并。
Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars' macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational wave emission, this deformation, quantified through a parameter termed the \emph{tidal deformability}, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature's most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron star coalescence with gravitational waves as of the time of writing.
