Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p43d1715h&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P43D-1715
Physics
[5704] Planetary Sciences: Fluid Planets / Atmospheres, [5714] Planetary Sciences: Fluid Planets / Gravitational Fields, [5724] Planetary Sciences: Fluid Planets / Interiors
Scientific paper
The physical shape of a giant planet reveals important information about its rotation and internal structure. We investigate how differential rotation on cylinders affects Jupiter's shape. We project Jupiter's measured zonal wind velocities along cylinders to describe its centrifugal potential which is then used to derive Jupiter's shape using an equipotential surface theory. The derived shape for different cylindrical radii is then compared with Jupiter's shape from radio occultation measurements. It is found that both solid-body rotation (System III rotation rate) and differential rotation up to a latitude of ~ 20-30 degrees are consistent with Jupiter's measured shape. We next use a first-order theory that relates the second gravitational coefficient J_2 to the flattening to calculate the corrections to J_2 for the different rotational configurations. We find that the contribution of the flattening to J_2 is significant. We therefore suggest that interior models of the giant planets must account for J_2n corrections caused by both shape (flattening) and internal dynamics.
Anderson John D.
Helled Ravit
Schubert Gerald
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