Tidal dissipation in rotating fluid bodies: a simplified model
Tidal dissipation in rotating fluid bodies: a simplified model
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DOI：
10.1111/j.1365-2966.2009.14814.x
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发表时间：
2009-03
影响因子：
4.8
通讯作者：
G. Ogilvie
中科院分区：
文献类型：
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作者：
G. Ogilvie
我们研究旋转流体体中线性惯性波的潮汐力、传播和耗散。有意简化的模型涉及一个完全刚性的核心，该核心被由均质不可压缩流体组成的深海包围。忽略离心效应，但充分考虑科里奥利力，并通过粘性力或摩擦力发生耗散。耗散率对潮汐频率表现出复杂的依赖性，并且通常随着核心尺寸的增加而增加。在某些频率间隔内，即使对于非常小的粘度或摩擦系数值，也会发生有效的耗散。我们参考波吸引子、临界纬度和流体内惯性波传播的其他特征来讨论结果，并评论它们与行星和恒星潮汐耗散的相关性。
We study the tidal forcing, propagation and dissipation of linear inertial waves in a rotating fluid body. The intentionally simplified model involves a perfectly rigid core surrounded by a deep ocean consisting of a homogeneous incompressible fluid. Centrifugal effects are neglected, but the Coriolis force is considered in full, and dissipation occurs through viscous or frictional forces. The dissipation rate exhibits a complicated dependence on the tidal frequency and generally increases with the size of the core. In certain intervals of frequency, efficient dissipation is found to occur even for very small values of the coefficient of viscosity or friction. We discuss the results with reference to wave attractors, critical latitudes and other features of the propagation of inertial waves within the fluid, and comment on their relevance for tidal dissipation in planets and stars.