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Composition, structure and evolution of Uranian and Neptunian satellites

Stevenson, David J. (1984) Composition, structure and evolution of Uranian and Neptunian satellites. In: Uranus and Neptune. NASA conference publication. No.2330. National Aeronautics and Space Administration, Scientific and Technical Information Branch , Washington, D.C., pp. 405-423. ISBN 10861802.

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Large uncertainties in the current estimated densities or 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 or co-clathrate and a small ice/rock ratio. Triton and the four largest satellites or Uranus are massive enough to have undergone significant accretional heating and early differentiation; NH_3-H_2O volcanism; partial outgassing or CO, N_2, CH_4; formation or dark surficial deposits or carbon-rich material obtained by UV irradiation or outgassed material; and, at least in the cases or Ariel and Triton, a possibility or 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 or substantial liquid or solid nitrogen obtained from either primordial NH_3 photolysis or clathrate decomposition.

Item Type:Book Section
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Stevenson, David J.0000-0001-9432-7159
Additional Information:© 1984 NASA. This work is supported by NASA Planetary Geology grant NAGW-450.
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Caltech Division of Geological and Planetary Sciences4042
Series Name:NASA conference publication
Issue or Number:2330
Record Number:CaltechAUTHORS:20130731-102423763
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:39673
Deposited By: Tony Diaz
Deposited On:20 Sep 2013 23:39
Last Modified:03 Oct 2019 05:09

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