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7 - Mineralogy of the Martian surface from Mars Express OMEGA observations

from Part III - Mineralogy and Remote Sensing of Rocks, Soil, Dust, and Ices

Published online by Cambridge University Press:  10 December 2009

By
J.-P. Bibring  and
Y. Langevin
Edited by
Jim Bell
J.-P. Bibring
Affiliation:
Institut d'Astrophysique Spatiale Universite, Paris Sud Bat. 121 Orsay Cedex, F-91405, France
Y. Langevin
Affiliation:
Institut d'Astrophysique Spatiale, 91405 Orsay, France
Jim Bell
Affiliation:
Cornell University, New York
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Summary

ABSTRACT

In orbit on board the European Space Agency's (ESA) Mars Express spacecraft, the Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité (OMEGA) visible to near-infrared spectral imager is acquiring a global compositional surface mapping dataset of Mars in order to reveal its major mineralogical and icy constituents. These data provide insights on the evolution of Mars on timescales ranging from seasonal variations to geological epochs. In particular, the identification and mapping of the spatial distribution of pristine magmatic rocks (including olivine, high-Ca pyroxene, and low-Ca pyroxene) and of three classes of altered minerals (hydrated phyllosilicates, hydrated sulfates, and anhydrous ferric oxides) in distinct areas has enabled the development of a new model for the evolution of the surface. The model includes three major eras spanning Martian history. The first era, during which phyllosilicates appear to have formed, was the most favorable to have hosted habitable conditions, with perennial and neutral to slightly alkaline pH surface liquid water. Mars then underwent a global environmental and climatic change, coupled to the formation of Tharsis and the release of large amounts of SO2 and other volcanic gases, and the likely loss of most of its CO2-rich atmosphere. This second era was characterized by low-pH (acidic) surface and subsurface groundwater, and the creation of large deposits of sulfate minerals. The third and most recent era in this model is dominated by atmospheric processes, leading primarily to the generation of anhydrous weathering products.

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Chapter
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The Martian Surface
Composition, Mineralogy and Physical Properties
 , pp. 151 - 168
Publisher: Cambridge University Press
Print publication year: 2008

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