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Mobilization of cryogenic ice in outer solar system satellitesMechanisms to explain the mobilization of ice on the Uranian satellites Miranda and Ariel at the very low temperatures prevailing on those bodies are considered. A form of pressure solution creep is proposed in which very fine-grained water ice or clathrate hydrate is mobilized by a small amount of intergranular cryogenic fluid (CH4, CO, or N2). Viscosities as low as 10 to the 12th P are possible for a limited time, sufficient to allow flooding of rift valleys and perhaps even substantial lateral flows (glaciers).
Document ID
19870029595
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Stevenson, D. J.
(California Institute of Technology Pasadena, United States)
Lunine, J. I.
(Arizona, University Tucson, United States)
Date Acquired
August 13, 2013
Publication Date
September 4, 1986
Publication Information
Publication: Nature
Volume: 323
ISSN: 0028-0836
Subject Category
Lunar And Planetary Exploration
Accession Number
87A16869
Funding Number(s)
CONTRACT_GRANT: NSF AST-82-06173
CONTRACT_GRANT: NAGW-185
Distribution Limits
Public
Copyright
Other

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