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f-mode imprints on gravitational waves from coalescing binaries involving aligned spinning neutron stars
Physical Review D ( IF 4.6 ) Pub Date : 2022-09-29 , DOI: 10.1103/physrevd.106.064052
Hao-Jui Kuan , Kostas D. Kokkotas

The excitation of f-mode in a neutron star member of coalescing binaries accelerates the merger course, and thereby introduces a phase shift in the gravitational waveform. Emphasizing the tidal phase shift by aligned, rotating stars, we provide an accurate, yet economical, method to generate f-mode-involved, premerger waveforms using realistic spin-modulated f-mode frequencies for some viable equations of state. We find for slow-rotating stars that the dephasing effects of the dynamical tides can be uniquely, equation-of-state-independently determined by the direct observables (chirp mass M, symmetric ratio η, and the mutual tidal deformability Λ˜), while this universality is gradually lost for increasing spin. For binaries with fast rotating members (800Hz) the phase shift due to the f-mode will exceed the uncertainty in the waveform phase at reasonable signal-to-noise ratio (ρ=25) and cutoff frequency of 400Hz. Assuming a high cutoff frequency of 103Hz and fast (800Hz) members, a significant phase shift of 100 rads has been found. For systems involving a rapidly spinning star (potentially the secondary of GW190814), neglecting the f-mode effect in the waveform templates can therefore lead to considerable systemic errors in the relevant analysis. In particular, the dephasing due to f-mode is larger than that caused by equilibrium tides by a factor of 5, which may lead to a considerably overestimated tidal deformability if dynamical tidal contribution is not accounted. The possibility of accompanying precursors flares due to f-mode excitation is also discussed.

中文翻译:

f 模式印记在来自合并双星的引力波上,这些双星涉及对齐的自旋中子星

的激发F合并双星的中子星成员中的 - 模式加速了合并过程,从而在引力波形中引入了相移。通过对齐的旋转恒星强调潮汐相移,我们提供了一种准确且经济的方法来生成F- 使用逼真的自旋调制的涉及模式的合并前波形F一些可行的状态方程的模态频率。我们发现对于慢速旋转的恒星,动力潮汐的移相效应可以是唯一的,状态方程独立地由直接可观测的(啁啾质量)确定, 对称比η, 以及相互潮汐变形性Λ),而随着自旋的增加,这种普遍性逐渐消失。对于具有快速旋转成员的二进制文件 (800赫兹) 相移由于F-模式将在合理的信噪比下超过波形相位的不确定性(ρ=25) 和截止频率400赫兹. 假设高截止频率103赫兹并且快速(800赫兹) 成员,显着相移100 rads 已被发现。对于涉及快速旋转的恒星(可能是 GW190814 的次级)的系统,忽略F因此,波形模板中的模式效应会导致相关分析中出现相当大的系统性错误。特别是,由于相位差F- 模式比平衡潮汐引起的模式大一倍5,如果不考虑动态潮汐贡献,这可能导致相当高估的潮汐变形能力。伴随前体耀斑的可能性是由于F还讨论了模激励。
更新日期:2022-09-29
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