Tidal deformations of neutron stars with elastic crusts
Tidal deformations of neutron stars with elastic crusts
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DOI：
10.1103/physrevd.101.103025
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发表时间：
2020-03
影响因子：
5
通讯作者：
F. Gittins;N. Andersson;J. P. Pereira
中科院分区：
文献类型：
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作者：
F. Gittins;N. Andersson;J. P. Pereira
随着引力波探测器首次探测到中子星星并合双星，人们及时地考虑了中子星的内部结构如何影响它们的不对称变形方式。这种变形可能会在引力波信号上留下可测量的印记，并且可以通过潮汐相互作用或山脉的形成来获得。我们详细的形式主义，描述完全相对论中子星星模型与弹性地壳进行静态扰动。这种形式主义为研究各种能使中子星星变形的机制提供了基础。我们提出的正压状态方程和弹性地壳，这使我们能够计算相关的量，如潮汐变形参数的现实模型的结果。我们发现，包含弹性地壳提供了一个非常小的修正潮汐变形。这些结果使我们能够证明在双星螺旋上升期间地壳何时何地开始破裂，我们发现大部分地壳将保持完整，直到合并。
With the first detections of binary neutron star mergers by gravitational-wave detectors, it proves timely to consider how the internal structure of neutron stars affects the way in which they can be asymmetrically deformed. Such deformations may leave measurable imprints on gravitational-wave signals and can be sourced through tidal interactions or the formation of mountains. We detail the formalism that describes fully-relativistic neutron star models with elastic crusts undergoing static perturbations. This formalism primes the problem for studies into a variety of mechanisms that can deform a neutron star. We present results for a barotropic equation of state and a realistic model for the elastic crust, which enables us to compute relevant quantities such as the tidal deformability parameter. We find that the inclusion of an elastic crust provides a very small correction to the tidal deformability. The results allow us to demonstrate when and where the crust starts to fail during a binary inspiral and we find that the majority of the crust will remain intact up until merger.