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The Orbital Search for Altered Materials on Mars

¹ Department of Geological Sciences
Arizona State University
Tempe, AZ 85287-6305, USA
E-mail: michael.wyatt{at}asu.edu
² Department of Earth and Planetary Sciences
University of Tennessee
Knoxville, TN 37996-1410, USA
E-mail: mcsween{at}utk.edu

The Martian surface is dominated by primary igneous minerals common in basaltic rocks. Limited chemical alteration exists in fine-grained dust, and is likely in sands and rocks at high latitudes and in the northern lowland plains where materials have interacted with ice and snow. Evidence for extensive production of secondary phases is revealed at higher spatial resolutions, where alteration effects of unique, and perhaps time-limited, aqueous environments are observed. The distribution of ice on Mars thus appears to have a global influence on the production of alteration materials, whereas the effects of water are discovered in unique and locally diverse geological settings.

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Elements 2006 2: 138. [PDF]