Tidal Dissipation in the Galilean Satellites

Details Tidal Dissipation in the Galilean Satellites Tidal Dissipation in the Galilean Satellites

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001dps....33.1701m&link_type=abstract

American Astronomical Society, DPS Meeting #33, #17.01; Bulletin of the American Astronomical Society, Vol. 33, p.1063

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Numerical simulations of the Galilean satellites' orbits show that the two-dimensional model based on zero inclination gives different results for the evolution of the orbital elements than those obtained with a three-dimensional model. These differences could affect the computation of tidal dissipation and require revisions to previous calculations which were based on the assumption of zero orbital inclination. Starting from Mignard's (1979) expression for the tidal force, based on a first order expansion in the time delay of the body's response, we derive a new expression for the tidal dissipation valid to second order in eccentricity and for arbitrary inclination. Since our previous simulations show that the orbits of the Galilean satellites deviate from perfect Keplerian ellipses (because of Jupiter's large oblateness), eccentricties are not constant. Further work has to be done to take the variation of eccentricity into account in the tidal dissipation computations. Mignard, F. (1979). The evolution of the lunar orbit revisited, I. Moon Planets 20, 301-315

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