Other
Scientific paper
Nov 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006jgre..11111005c&link_type=abstract
Journal of Geophysical Research, Volume 111, Issue E11, CiteID E11005
Other
9
Planetary Sciences: Solar System Objects: Saturnian Satellites, Planetary Sciences: Solid Surface Planets: Interiors (8147), Planetary Sciences: Solid Surface Planets: Composition (1060, 3672), Planetary Sciences: Solar System Objects: Comparative Planetology
Scientific paper
We model the interior of Rhea on the basis of observational constraints and the results from geodynamical models available in the literature. Ten main types of models are defined, depending on the presence or absence of a high-pressure ice layer (ice II), and the extent of separation of the rock component from the volatiles. The degree-two gravity coefficients are computed for each of these models in order to assess which properties of the interior are likely to be inferred from Cassini radio science measurements scheduled on 26 November 2005. C22 greater than 2.5 × 10-4 indicates that the satellite is undifferentiated, except for a slight increase in density with depth resulting from material self-compression. C22 between 1.67 × 10-4 (lower bound) and 1.90 × 10-4 indicates the presence of a rocky core, whose radius can be determined from the satellite's mass and ices densities, for a given temperature profile. For other values, most of the ten models cannot be distinguished from each other. However, assumptions on the density of the rock phase, presence or absence of ice II, and the degree of differentiation could allow a unique model to be determined in many cases. While the calculation presented in this work assumes that Rhea is in hydrostatic equilibrium, it is likely that Rhea' gravity field is partly affected by nonhydrostatic anomalies.
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