During the final stages of a neutron-star binary coalescence, stellar quasi-normal modes can become resonantly excited by tidal fields. If the strain exerted by the excited modes exceeds the extent to which the crust can respond linearly, localized crustal failures may occur. In this work, we re-examine resonant g-mode excitations of relativistic neutron stars in the last ∼10 s of an inspiral. We adopt realistic equations of state that pass constraints from GW170817, include third-order post-Newtonian terms for the conservation orbital motion, and employ a 2.5 post-Newtonian scheme for gravitational back-reaction. Frequency modulations of the modes due to tidal fields, Lorentz forces, and (slow) rotation are also considered to investigate the maximal strain achievable by resonantly excited g modes. Depending on the equation of state, degree of stratification, and stellar magnetic field, we find that certain g-mode excitations may be able to break the crust some seconds prior to coalescence.

中文翻译：

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中子星合并双星中潮汐 g 模式共振的广义相对论处理——I. 理论框架和地壳破裂

在中子星双星合并的最后阶段，恒星准正常模式可以被潮汐场共振激发。如果激发模式施加的应变超过地壳可以线性响应的程度，则可能发生局部地壳破坏。在这项工作中，我们重新检查了在最后 10 秒内相对论中子星的共振 g 模式激发。我们采用通过 GW170817 约束的现实状态方程，包括守恒轨道运动的三阶后牛顿项，并采用 2.5 后牛顿方案进行引力反作用。还考虑了由于潮汐场、洛伦兹力和（慢）旋转引起的模式频率调制，以研究通过共振激发的 g 模式可实现的最大应变。根据状态方程，