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8 - Planetary structural mapping

Published online by Cambridge University Press:  30 March 2010

By
Kenneth L. Tanaka ,
Robert Anderson ,
James M. Dohm ,
Vicki L. Hansen ,
George E. McGill ,
Robert T. Pappalardo ,
Richard A. Schultz  and
Thomas R. Watters
Edited by
Thomas R. Watters  and
Richard A. Schultz
Kenneth L. Tanaka
Affiliation:
U.S. Geological Survey, Flagstaff
Robert Anderson
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena
James M. Dohm
Affiliation:
Department of Hydrology and Water Resources, University of Arizona, Tucson
Vicki L. Hansen
Affiliation:
Department of Geological Sciences, University of Minnesota Duluth
George E. McGill
Affiliation:
University of Massachusetts, Amherst
Robert T. Pappalardo
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena
Richard A. Schultz
Affiliation:
Geomechanics – Rock Fracture Group, Department of Geological Sciences and Engineering, University of Nevada, Reno
Thomas R. Watters
Affiliation:
Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC
Thomas R. Watters
Affiliation:
Smithsonian Institution, Washington DC
Richard A. Schultz
Affiliation:
University of Nevada, Reno
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Summary

Summary

As on Earth, other solid-surfaced planetary bodies in the solar system display landforms produced by tectonic activity, such as faults, folds, and fractures. These features are resolved in spacecraft observations directly or with techniques that extract topographic information from a diverse suite of data types, including radar backscatter and altimetry, visible and near-infrared images, and laser altimetry. Each dataset and technique has its strengths and limitations that govern how to optimally utilize and properly interpret the data and what sizes and aspects of features can be recognized. The ability to identify, discriminate, and map tectonic features also depends on the uniqueness of their form, on the morphologic complexity of the terrain in which the structures occur, and on obscuration of the features by erosion and burial processes. Geologic mapping of tectonic structures is valuable for interpretation of the surface strains and of the geologic histories associated with their formation, leading to possible clues about: (1) the types or sources of stress related to their formation, (2) the mechanical properties of the materials in which they formed, and (3) the evolution of the body's surface and interior where timing relationships can be determined. Formal mapping of tectonic structures has been performed and/or is in progress for Earth's Moon, the planets Mars, Mercury, and Venus, and the satellites of Jupiter (Callisto, Ganymede, Europa, and Io).

Type
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Information
Planetary Tectonics , pp. 351 - 396
Publisher: Cambridge University Press
Print publication year: 2009

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