Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p44a..02v&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #P44A-02
Physics
[5430] Planetary Sciences: Solid Surface Planets / Interiors, [5450] Planetary Sciences: Solid Surface Planets / Orbital And Rotational Dynamics
Scientific paper
The rotation of planets and satellites varies periodically as a result of gravitational torques from the central body. In the absence of liquid internal layers, these rotation variations are well approximated by the rotation variations for a rigid body. When a global liquid layer exists, different solid layers, separated by the liquid layer, can rotate differently. As a result, the rotation variations of the surface will be affected by the liquid layer. Observations of the rotation variations provide a unique tool for exploring the deep internal structure of planets and satellites. As examples, we will discuss rotation rate variations of Mercury and icy satellites with a subsurface ocean. For Mercury, the MESSENGER and upcoming BepiColombo missions will measure the librations to estimate the size of its, at least partially, liquid core. Observations of rotation variations of icy satellites may reveal the existence and depth to putative subsurface oceans. A prerequisite for attaining these goals is a good knowledge of the dynamical effect of the liquid layers on the rotation of the object. At present, most models of rotation variations, including those that we will present, assume that the flow in the fluid can be approximated by a solid body rotation. Additional information from numerical and experimental studies is needed to improve these models.
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