Obliquity and non-hydrostaticity: Constraining the interior of Titan
(2012) European Planetary Science Congress — Location: Madrid, Spain (23.September.2012)
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- Abstract
- The orientation of the rotation axis of Titan has been measured on the basis of Cassini radar images [5, 6]. It has been shown that this orientation is more consistent with the presence of an internal global liquid ocean beneath an ice shell than with an entirely solid Titan [1]. The global topography data seem to indicate some departure from the hydrostatic shape expected for a synchronous satellite under the influence of its rota- tion and the static tides raised by the central planet, although the possibility of Titan being in hydrostatic equilibrium cannot be ruled out [7]. We investigate how the non-hydrostaticity may in- fluence the obliquity solution. Then, we derive interior models which are compatible with the observed orien- tation as well as gravity and a non-hydrostatic shape deduced from the solution of [7]
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Baland, R.-M., Tobie, G., & Lefèvre, A. (2012). Obliquity and non-hydrostaticity: Constraining the interior of Titan. European Planetary Science Congress, Madrid, Spain. https://hdl.handle.net/2078.5/186563