Other
Scientific paper
Sep 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.2253h&link_type=abstract
American Astronomical Society, DPS meeting #28, #22.53; Bulletin of the American Astronomical Society, Vol. 28, p.1151
Other
Scientific paper
The workings of tidal friction in the Earth-Moon system have been well understood for a century. The Moon raises a tidal bulge on the Earth which is delayed somewhat on average from the time when the Moon is overhead. The phase lag between Moon and bulge results in a tidal torque that accelerates the Moon in its orbit, causing it to spiral outward from the Earth. Of necessity, such orbital evolution can only take place if some of the Earth's rotational energy is dissipated (a process which is thought to take place primarily in shallow seas). A similar interaction between planet and moon is the most likely explanation of many phenomena (like the Laplace resonances) in the giant planet satellite systems. However, a satisfactory source of the required energy dissipation in these largely fluid bodies has not been identified. There are currently three proposed explanations (all with shortcomings) for the tidal dissipation in Jupiter and the other giant planets. One, due to Dermott (Icarus 37, 310, 1979), depends on terrestrial planet-like dissipation in the core (which is however of unknown composition and rheology). The strength of this explanation is that all the giant planets are thought to have similar cores; the weakness is our relative ignorance of the physical properties of those cores. The other two explanations both depend on regions of static stability in the planetary envelopes. Stevenson (J. Geophys. Res. 88, 2445, 1983) would have this stable layer in the region of metallic hydrogen-helium immiscibility (which, depending on Jupiter's atmospheric helium abundance, may only apply to the planet Saturn). Ioannou & Lindzen (Ap. J. 406, 266, 1993) predicted a stable outer envelope for Jupiter. The early report that the Galileo probe entered a region of static stability added interest to the latter prediction and raises the need for further discussion of the tidal dissipation problem. A recalculation of the tidal flow in giant fluid planets is presented. The self-gravity of the planet is treated in a fully self-consistent fashion. The tidal torque and tidal dissipation are calculated from the imaginary part of the gravitational potential. The plausibility of the above explanations can be assessed in terms of this improved model.
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