Origin of mountains of Io by trust faulting and large-scale mass movements

Science

Volumn 279, Issue 5356, 1998, Pages 1514-1417

  Schenk, Paul M ^a   Bulmer, Mark H ^b  

^a LUNAR AND PLANETARY INSTITUTE   (United States)

^b SMITHSONIAN INSTITUTION   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

DEBRIS FLOW; MOUNTAIN BUILDING; SLOPE FAILURE; THRUST FAULT; UPLIFT;

ARTICLE; GEOLOGY; METEOROLOGY; MOON; PRIORITY JOURNAL; SPACE FLIGHT; TOPOGRAPHY; VOLCANO;

I0, EUBOEA MONTES;

EID: 0032489636     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.279.5356.1514     Document Type: Article

References (42)

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29. The average friction coefficient is given by the tangent of the slope connecting the pre- and postevent centers of gravity of a failed mass (30). Because it is not possible to determine the pre- and postevent centers of gravity for masses on lo or most other planets, we use the tangent of the slope angle of the line connecting the top of the scarp to the toe of the apron (13) to derive the ratio H:L. The value derived using this method approximates the center of gravity gradient for those slope failures whose center of gravity lies near the toe (10), which may be the case for Euboea. Taking these caveats into consideration, we use H:L as an estimate of the coefficient of friction.
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31. At 16 km height, Boosaule Montes (10°S, 270°W) is the highest mountain identified to date on lo. The automated stereogrammetry (5) measurement we report has been confirmed by manual measurement of parallax in the Voyager images.
32. Previous estimates that the crust of Io is ∼30 km thick (31) assumed that mountain heights are due to isostatic buoyancy of material that is lower in density than the surrounding crust. Our interpretation of the formation of Euboea Montes suggests that mountains may have the same density as the surrounding crust, indicating that these crustal thickness estimates are not generally relevant to lo.
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42. This report is Lunar and Planetary Contribution No. 940. This work was done while M.H.B. was a Garber Fellow at the National Air and Space Museum. We are grateful to J. Moore, W. McKinnon, and an anonymous reviewer for comments.