Mathematics – Logic
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....7775c&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #7775
Mathematics
Logic
Scientific paper
The Thermal Emission Imaging System (THEMIS) began studying the surface and atmosphere of Mars in February, 2002 using thermal infrared multi-spectral imaging between 6.5 and 15 µm, and visible/near-IR images from 450 to 850 nm. The THEMIS investigation's specific objectives are to: (1) determine the mineralogy of localized deposits associated with hydrothermal or sub-aqueous environments, and to identify future landing sites likely to represent these environments; (2) search for thermal anomalies associated with active sub-surface hydrothermal systems; (3) study small-scale geologic processes and landing site characteristics using morphologic and thermophysical properties; (4) investigate polar cap processes at all seasons; and (5) provide a high spatial resolution link to the global hyperspectral mineral mapping from the TES investigation. THEMIS data collected to date have been used to investigate the nature of geologic units and layers, the distribution of rocks and bedrock, the mobile surface sand and dust, 100-m scale compositional variations, polar processes, and visible color and morphology. Regional-scale infrared mapping shows that Mars has both regional and local geologic units delineated by their thermophysical properties. In Meridiani Planum these units imply a complex history involving changes in the nature of volcanic units, the environment of deposition of sedimentary units, and/or the degree of lithification or cementation of initially unconsolidated units. Mars has km-scale exposures of bedrock, and rocky surfaces are commonly observed on slopes and scarps, demonstrating that the production or exposure rate of rock locally exceeds the rate of rock burial or breakdown. Thermally distinct ejecta deposits with a wide range of thermophysical properties are observed around craters of varying sizes. Most crater ejecta, however, are indistinguishable from the surrounding terrain. Where large fields of sand dune occur, the dunes are typically coarser-grained than the interdune surfaces, suggesting that finer-grained material is accu-mulating where active sand motion may be limited. THEMIS mult-ispectral infrared observations show significant potential for compositional mapping at 100-m scales, as demonstrated by the identification of oli-vine-rich basaltic units on the floor of Ganges Chasma. Polar observations have confirmed the presence of CO2 slab ice and the presence of H2O exposed at the surface of the south polar summer cap. The visible imager also has obtained information on the color properties of the surface and of atmospheric aerosols at the highest spatial resolution yet obtained from Mars orbit.
Christensen Paul
Themis Team
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