Constraining the development of the upper martian crust using orbital and in-situ thermophysical, mineralogical, and geochemical observations

Details Constraining the development of the upper martian crust using orbital and in-situ thermophysical, mineralogical, and geochemical observations Constraining the development of the upper martian crust using orbital and in-situ thermophysical, mineralogical, and geochemical observations

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p53a1439b&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P53A-1439

Other

5410 Composition (1060, 3672), 5460 Physical Properties Of Materials, 5464 Remote Sensing, 5470 Surface Materials And Properties, 6225 Mars

Scientific paper

Measurements from the Mars Exploration Rovers (MER) indicate distinct compositional differences between rock interiors, rock surfaces, and soil that may indicate a close relationship between mechanical and chemical weathering [Hurowitz et al., 2006, Ming et al., 2006, Morris et al., 2006]. This is most clearly indicated by olivine-rich Adirondack Class basalts and relatively olivine-poor dark soils in the plains of Gusev crater, consistent with aqueous alteration in an water-limited acidic environment [e.g. Tosca et al., 2004; Hurowitz et al., 2006]. Similar spectral and thermophysical relationships can be observed from orbit with the Thermal Emission Spectrometer (TES) and the Thermal Emission Imaging System (THEMIS) [ Bandfield and Rogers, 2008]. The detailed rover observations combined with the large spatial coverage of the orbital observations are highly complimentary, allowing for global inferences to be made from more detailed local observations. The combined set of observations may give an indication of the extent of chemical and mechanical weathering of the martian crust. Mafic, olivine-rich compositions are highly correlated with high inertia rocky surfaces and are rare elsewhere. Because olivine is highly sensitive to dissolution with limited amounts of liquid water, its presence or absence may be a proxy for the amount of chemical weathering that has occurred. This is the case even where spectroscopic measurements do not otherwise show clear evidence for significant alteration throughout martian dark regions. High thermal inertia surfaces, consistent with relatively unprocessed rocky materials, are not common on Mars [Edwards et al., 2005]. Even where several kilometers of canyon or crater wall are exposed, high inertia materials are commonly absent except in isolated layers. This is also the case for materials exposed at the MER landing sites [Fergason et al., 2006]. The high inertia materials that are present are relatively unaltered blocks. Materials that appear to be altered (including in-place units) have relatively low thermal inertia values. Mechanical and chemical weathering are highly correlated on Mars as on Earth and unweathered materials are not commonly exposed. The martian near surface may have experienced significantly more alteration than previously assumed and our understanding of martian igneous processes and aqueous history based on orbital remote sensing may need to be revised. Bandfield, J.L. and A.D. Rogers (2008) Geology, 10.1130/G24724A. Edwards, C.S., et al. (2005) Eos Trans. AGU, 86, P21C-0158. Fergason, R.L., et al. (2006) J. Geophys. Res., 10.1029/2005JE002583. Hurowitz, J.A., et al. (2006) J. Geophys. Res., 10.1029/2005JE002515. Ming, D.W., et al. (2006) J. Geophys. Res., 10.1029/2005JE002560. Morris, R.V., et al. (2006) J. Geophys. Res., 10.1029/2005JE002584. Tosca, N.J., et al. (2004) J. Geophys. Res., 10.1029/2003JE002218.

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