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Subsidence of Topography on Io

Webb, Erik K. and Stevenson, David J. (1987) Subsidence of Topography on Io. Icarus, 70 (2). pp. 348-353. ISSN 0019-1035. doi:10.1016/0019-1035(87)90140-0.

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Topographic features on Io tend to subside because their underlying roots are softened and eroded by contact with hot mantle. This can be offset by crustal thickening, due primarily to ongoing volcanism, but observations suggest that this is ≲1 cm year^(−1) at current topographic highs. Since crustal thinning occurs at ∼50 cm year^(−1) if the underlying material is a pure magma ocean, we conclude that Io has no global magma ocean. Viscosities in excess of ∼10^(10) P are implied for Io's interior.

Item Type:Article
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Stevenson, David J.0000-0001-9432-7159
Additional Information:© 1987 Academic Press, Inc. Received October 29, 1986; revised January 28, 1987. We are grateful to Torrence Johnson for his review and helpful comments on resurfacing. The first author acknowledges support of NASA's Planetary Geology Undergraduate Research Program. Partial support was also supplied by NASA Grant NAGW-185.
Group:UNSPECIFIED, UNSPECIFIED, Division of Geological and Planetary Sciences
Funding AgencyGrant Number
NASA Undergraduate Student Research ProgramUNSPECIFIED
Issue or Number:2
Record Number:CaltechAUTHORS:20131113-152707499
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Official Citation:Erik K. Webb, David J. Stevenson, Subsidence of topography on Io, Icarus, Volume 70, Issue 2, May 1987, Pages 348-353, ISSN 0019-1035, (
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42439
Deposited By: Ruth Sustaita
Deposited On:13 Nov 2013 23:40
Last Modified:10 Nov 2021 16:23

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