Internal Structure of Planetary Icy Bodies

Details Internal Structure of Planetary Icy Bodies Internal Structure of Planetary Icy Bodies

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....7389d&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #7389

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In the case of the icy bodies we could define the differentiation as the separation in two concentric layers, a rocky nucleus, the deepest one, and a superficial layer of water, liquid or solid. I studied the conditions of differentiation of the icy satellites of Jupiter, Saturn, Uranus and Neptune and also Pluto and Charon. Using two criteria, differentiation by accretion and differentiation by radiogenic heating I obtain the same result, the only differentiated bodies are Europa, Ganymede, Callisto, and Titan. All the others icy bodies are no differentiated. I also studied the distribution of ice Ih, exotic ices (III, IV, VI, etc), and liquid water layers in the four planetary bodies.

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