The Physics of Bodily Tides in Terrestrial Planets, and the Appropriate Scales of Dynamical Evolution

Details The Physics of Bodily Tides in Terrestrial Planets, and the Appropriate Scales of Dynamical Evolution The Physics of Bodily Tides in Terrestrial Planets, and the Appropriate Scales of Dynamical Evolution

2007-09-13

arxiv.org/abs/0709.1995v3

Astronomy and Astrophysics

Astrophysics

arXiv admin note: substantial text overlap with arXiv:astro-ph/0605521

Scientific paper

10.1029/2007JE002908

Any model of tides is based on a specific hypothesis of how lagging depends on the tidal-flexure frequency. For example, Gerstenkorn (1955), MacDonald (1964), and Kaula (1964) assumed constancy of the geometric lag angle, while Singer (1968) and Mignard (1979, 1980) asserted constancy of the time lag. Thus, each of these two models was based on a certain law of scaling of the geometric lag. The actual dependence of the geometric lag on the frequency is more complicated and is determined by the rheology of the planet. Besides, each particular functional form of this dependence will unambiguously fix the appropriate form of the frequency dependence of the tidal quality factor, Q. Since at present we know the shape of the dependence of Q upon the frequency, we can reverse our line of reasoning and single out the appropriate actual frequency-dependence of the angular lag. This dependence turns out to be different from those employed hitherto, and it entails considerable alterations in the time scales of the tide-generated dynamical evolution. Phobos' fall on Mars is an example we consider.

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