Tidal Dissipation in Stars and Giant Planets

By Gordon I. Ogilvie. 2014

310 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/92ee7fb19ed974ea2a29315a54e274bd510e2c7b

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In Astronomy and Astrophysics

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2. D. Fabrycky
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Citations in the corpus

• The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “( 2008 ) with estimates relying on the timescales of the orbital decay of very hot Jupiters with P (cid:46) 1 d (e.g. Ogilvie 2014).”
• The Occurrence and Architecture of Exoplanetary Systems (2014, background): “The inevitable friction associated with those motions gradually dissipates energy, one consequence of which is the circularization of the orbit (see, e.g., Ogilvie 2014).”
• The Apparently Decaying Orbit of WASP-12b (2017, background): “Theoretically, the quality factor should depend on the orbital period, perturbation strength, and internal structure of the star (Ogilvie 2014).”