A New Computation of Tidal Dissipation in Tethys

Details A New Computation of Tidal Dissipation in Tethys A New Computation of Tidal Dissipation in Tethys

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.4501l&link_type=abstract

American Astronomical Society, DPS meeting #40, #45.01; Bulletin of the American Astronomical Society, Vol. 40, p.479

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Scientific paper

Orbital study of Saturn's main satellites suggests a peculiar behaviour for one of them: Tethys. Its motion is characterized by a rapid circulation of the periapsis, while the mean anomaly oscillates around this latter. Such behaviour is caused by Saturn's strong oblateness. In this kind of configuration, neither the osculating eccentricity nor the mean eccentricity do reflect directly the distance variation of the satellite to its primary. Considering Tethys, we found that the distance variation and geometrical libration angle are about 3-4 times less than the ones derived from its mean eccentricity. Hence, as a Keplerian orbit is assumed in the usual expressions for tidal dissipation, they provide an erroneous and excessive value. This work presents a much more accurate value by considering the dynamical feature of Tethys.
Tethys is no isolated case, other satellites found in the same dynamical configuration are Telesto, Helene, Metis and Adrastea.

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