Models of the Internal Structure of Callisto

Details Models of the Internal Structure of Callisto Models of the Internal Structure of Callisto

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sosyr..39..283k&link_type=abstract

Solar System Research, Volume 39, Issue 4, pp.283-301

Physics

Scientific paper

Models of the internal structure of Callisto were constructed and the extent of its differentiation was determined based on geophysical information from the Galileo spacecraft (the mass, the radius, the mean density, and the moment of inertia), geochemical data (the chemical composition of meteorites), and the equations of state of water, ices, and meteoritic material. The thickness and the phase state of the water-ice shell were defined as well as the ice concentrations in the rock-ice mantle and the bulk concentration of H2O. The constraints on the density distribution in the mantle and the size of the rock-iron core were derived. We considered models of the internal structure of Callisto in which the presence of a continuous ice shell was assumed (models without ocean) and models with an internal ocean. We demonstrated that it is possible to apply three-layer models with an icy shell up to 320 km in thickness and a rock-iron core in different combinations with a rock-ice mantle. These models do not reject a two-layer structure of Callisto (an ice lithosphere plus a rock-ice mantle or a rock-ice mantle plus a rock-iron core) and a one-layer model of the satellite composed only of a rock-ice mantle with an ice concentration that is variable in depth. Taking into account the chemically bound water, the bulk content of H2O in the satellite is found to be 49 55 wt %. For the model with an internal ocean, the geophysically allowed thickness of the water-ice shell of Callisto was estimated to be 270 315 km with thicknesses of the icy crust and the underlying water layer of 135 150 and 120 180 km, respectively. The results of reconstruction of the composition and structure of the regular satellites of Jupiter allow us to conclude that they were possibly formed from material whose composition was close to ordinary L/LL chondrites at relatively low temperatures, lower than the temperature of evaporation of iron and Fe-Mg silicates.

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