Tidal Dissipation in Stars and Giant Planets
Tidal Dissipation in Stars and Giant Planets
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DOI：
10.1146/annurev-astro-081913-035941
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发表时间：
2014-06
影响因子：
33.3
通讯作者：
G. Ogilvie
中科院分区：
文献类型：
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作者：
G. Ogilvie
天体物理学中的流体体彼此靠近，会引起潮汐扭曲和流动，这些都是耗散过程。自旋和轨道运动在天文时间尺度上经历耦合演化，这与太阳系中许多类型的双星星星、短周期太阳系外行星系统和巨行星的卫星有关。我回顾的主要机制，已讨论的潮汐耗散在恒星和巨行星的线性和非线性制度。我还比较了基于理论模型的预期与最近的观察结果。
Astrophysical fluid bodies that orbit close to one another induce tidal distortions and flows that are subject to dissipative processes. The spin and orbital motions undergo a coupled evolution over astronomical timescales, which is relevant for many types of binary star, short-period extrasolar planetary systems, and the satellites of the giant planets in the Solar System. I review the principal mechanisms that have been discussed for tidal dissipation in stars and giant planets in both linear and nonlinear regimes. I also compare the expectations based on theoretical models with recent observational findings.