具有稳定分层的高速旋转扁平行星与恒星（如木星）中的动力学潮汐
Dynamical tides in Jupiter and other rotationally flattened planets and stars with stable stratification
AI总结：
开发数值方法计算快速旋转扁球星体和气态行星的耗散动力学潮汐响应，发现混合波共振可解释木星对Io潮汐响应的观测与静力学计算差异。
摘要：
我们开发了一种数值方法，用于直接计算具有真实内部结构的快速旋转、扁球星体和气态行星的耗散动力学潮汐响应。将这些计算应用于中性分层和稳定分层的多方球体，我们在旋转速率接近质量抛射极限的模型中识别出最相关的共振。随后，我们计算了包含稳定分层和对流区域的木星内部模型的动力学潮汐响应。这些计算表明，涉及兼具重力-惯性和纯惯性特征的混合波的共振，能够解释木星对 Io 潮汐强迫响应的观测结果与静力学计算之间的差异。这一结果与近期排除了木星旋转扁平化的研究形成对比，并为涉及比以往考虑的更广泛内部振荡模式的共振开辟了道路。
英文摘要：
We develop a numerical method for directly computing the dissipative dynamical tidal response of rapidly rotating, oblate stars and gaseous planets with realistic internal structures. Applying these calculations to neutrally and stably stratified polytropes, we identify the most relevant resonances in models with rotation rates up to nearly the mass-shedding limit. We then compute the dynamical tidal response for Jupiter interior models including both stably stratified and convective regions. These calculations show that resonances involving mixed waves with both gravito-inertial and purely inertial character are capable of explaining a discrepancy between observations and hydrostatic calculations of Jupiter's response to tidal forcing by Io. This result contrasts with recent work that excluded Jupiter's rotational flattening, and opens the door to resonances involving a wider range of internal oscillation modes than previously considered.
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