Mathematics – Logic
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p51c..08m&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P51C-08
Mathematics
Logic
5400 Planetology: Solid Surface Planets, 5410 Composition, 5464 Remote Sensing, 5470 Surface Materials And Properties
Scientific paper
The basic framework of the composition of the red-tinged martian surface was established by the pioneering visible-near infrared (vis-NIR) telescopic observations of Tom McCord and John Adams in 1969. Those observations characterized the planet's surface as a two-component system: unaltered basalt and a heavily altered, mobile component. Telescopic and orbital observations since, coupled with insightful laboratory and theoretical work, have honed this perspective, narrowing the possible options for ferric alteration and mapping the diversity of the basaltic surfaces where exposed. Except for refinement of this broad view, however, Mars has withheld any further insights via vis-NIR reflectance. It has been argued that perhaps the visible-NIR is not sensitive to the important minerals on the surface, or that the globally distributed dust homogenized the surface signal. A new era for understanding the surface emerged with the Thermal Emission Spectrometer which made a surprising discovery of gray hematite, an apparent dichotomy between an andesite crust in the north and basaltic crust in the south, as well as concrete identification of minerals not evident in the previous vis-NIR measurements (e.g. feldspar, olivine). Yet the signals from the surface are subtle and thus some results are subject to debate (e.g. the dichotomy may be due to alteration). Regardless of the wavelength region of the observation, the mineralogic diversity of Mars revealed spectroscopically has not measured up to the expectations based on terrestrial experience and laboratory measurements. Nevertheless, this same situation has been true for all the planetary bodies visited: the Moon, asteroids, and icy bodies. For those bodies, however, detailed observations coupled with theory and laboratory work have resolved the uncertainties leading to new understanding of the their evolution through surface observations. We are on the threshold of a new assault on the martian surface, with high spatial resolution thermal (THEMIS), hyperspectral vis-NIR on global (OMEGA) to local scales (CRISM), and very high spatial resolution lander spectrometers. Will Mars will wither under the assault and finally reveal its inner secrets: the carbonates, the mineralogically rich hydrothermal systems, and the preserved water-rich environments that must be there?
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