Composition, structure and evolution of Uranian and Neptunian satellites

Details Composition, structure and evolution of Uranian and Neptunian satellites Composition, structure and evolution of Uranian and Neptunian satellites

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984nascp2330..405s&link_type=abstract

In JPL Uranus and Neptune p 405-423 (SEE N85-11927 02-91)

Computer Science

4

Evolution (Development), Natural Satellites, Neptune (Planet), Oberon, Satellite Atmospheres, Uranus (Planet), Ariel, Atmospheric Composition, Ice, Liquid Nitrogen, Outgassing, Titania, Volcanoes

Scientific paper

Large uncertainties in the current estimated densities of all of these satellites prevent detailed modeling or predictions. Nevertheless, current evidence suggests that at least Titania and Oberon might have "anomalously" high densities (2 - 3 g cm-3), possibly requiring almost ice-free hydrated silicates or formation in a CO-rich environment, implying presence of CO-clathrate and a small ice/rock ratio. Triton and the four largest satellites of Uranus are massive enough to have undergone significant accretional heating and early differentiation; NH3-H2O volcanism; partial outgassing of CO, N2, CH4; formation of dark surficial deposits of carbon-rich material obtained by UV irradiation of outgassed material; and, at least in the cases of Ariel and Triton, a possibility of weak ongoing icy volcanic activity. Triton may be the largest captured body in the solar system, with an unusual history and composition, including the possibility of substantial liquid or solid nitrogen obtained from either primordial NH3 photolysis or clathrate decomposition.

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