Tidal dissipation in the solid cores of the major planets

Details Tidal dissipation in the solid cores of the major planets Tidal dissipation in the solid cores of the major planets

Jan 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979icar...37..310d&link_type=abstract

Icarus, vol. 37, Jan. 1979, p. 310-321.

Physics

13

Energy Dissipation, Gas Giant Planets, Planetary Cores, Tides, Internal Friction, Jupiter (Planet), Orbital Resonances (Celestial Mechanics), Planetary Evolution, Saturn (Planet), Solar Orbits, Uranus (Planet), Jupiter, Saturn, Orbits, Tidal Dissipation, Core, Planets, Resonance, Mantle, Uranus, Evolution, Mass, Energy, Interior

Scientific paper

If the orbital resonances in the Jovian and Saturnian satellite systems are the result of orbital evolution due to tidal dissipation, then the present rates of energy dissipation (EDRs) are in excess of 2 x 10 to the 20th erg/s (Jupiter) and at least about 2 x 10 to the 16th erg/s (Saturn). These values of EDR can be accounted for if the planets have rocky cores with volumes equal to those suggested by current models of the interiors and if the material of these cores is both solid and imperfectly elastic (elastic tidal dissipation function, Qe, of about 34). The calculated values of Qe are not strongly dependent on either the rigidity of the core or the densities of the core and the mantle. Thus, these quantities need not be known precisely. It may be significant that approximately the same value of Qe is needed for all the major planets (Jupiter, Saturn, and Uranus) even though the values of EDR for these planets differ by a factor greater than 10,000.

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