Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p22b..02s&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P22B-02
Physics
[5430] Planetary Sciences: Solid Surface Planets / Interiors, [6280] Planetary Sciences: Solar System Objects / Saturnian Satellites, [6281] Planetary Sciences: Solar System Objects / Titan
Scientific paper
A new approach is presented to evaluate the shape, the gravitational coefficients J2 and C22 and the normalized axial moment of inertia C/MR2 for a rotating, axially symmetric satellite in hydrostatic equilibrium and distorted by synchronous rotation and tides. C is the axial moment of inertia and M and R are the mass and radius of the body, respectively. The theory is valid for an arbitrary interior density profile. Application is made to Rhea and Titan assuming that these bodies are in hydrostatic equilibrium. A likely internal structure for Rhea is a uniform mixture of ice and rock, 75% ice and 25% rock, by mass, with an ice I-ice II phase change occurring within Rhea at a fractional radius of about 0.4 to 0.55.
Anderson John D.
Helled Ravit
Schubert Gerald
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