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 $\mathcal{M}$, symmetric ratio $\eta$, and the mutual tidal deformability $\tilde{\mathrm{\Lambda }}$), while this universality is gradually lost for increasing spin. For binaries with fast rotating members ($\gtrsim 800\mathrm{Hz}$) the phase shift due to the $f$-mode will exceed the uncertainty in the waveform phase at reasonable signal-to-noise ratio ($\rho =25$) and cutoff frequency of $\gtrsim 400\mathrm{Hz}$. Assuming a high cutoff frequency of ${10}^3\mathrm{Hz}$ and fast ($\gtrsim 800\mathrm{Hz}$) members, a significant phase shift of $\gtrsim 100$ 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 $\sim 5$, 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：

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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$\mathcal{米}$, 对称比$\eta$, 以及相互潮汐变形性$\stackrel{～}{\mathrm{\Lambda }}$)，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 ($\gtrsim 800\mathrm{赫兹}$) 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（$\rho =25$) 和截止频率$\gtrsim 400\mathrm{赫兹}$. 假设高截止频率${10}^3\mathrm{赫兹}$并且快速（$\gtrsim 800\mathrm{赫兹}$) 成员，显着相移$\gtrsim 100$ 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。