Mathematics – Logic
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusm.p32a..02b&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #P32A-02
Mathematics
Logic
5410 Composition, 5464 Remote Sensing, 5470 Surface Materials And Properties, 5494 Instruments And Techniques
Scientific paper
Most rock-forming minerals have distinctive absorptions in the thermal infrared portion of the spectrum (roughly 5-50 microns). This useful property is the primary motivation for sending a series of thermal infrared instruments to Mars: The Thermal Emission Spectrometer (TES) on the Mars Global Surveyor, the Thermal Emission Imaging System (THEMIS) on the Mars Odyssey, and the Miniature Thermal Emission Spectrometers on the two Mars Exploration Rover spacecraft. The massive volume of data returned from these instruments has provided the means to determine the global and local scale mineralogical compositions of the Martian surface. A broad question that the Martian surface mineralogy addresses is: What is the timing and extent of igneous processes on a planet that does not have plate tectonics? TES data has revealed that the Martian surface displays a striking hemispheric dichotomy in surface composition. Basalts or basaltic andesites similar in bulk composition to those commonly found on Earth dominate the southern highlands. A more silica rich surface that closely matches typical terrestrial basaltic andesites or andesites is present everywhere on the planet, though the highest concentrations are found within the younger northern lowlands. Though this dichotomy may be explained by two different igneous compositions, the high-silica glass in the more silicic composition could instead be a secondary mineral related to an alteration process rather than volcanism. Regardless of the source of the glass, Martian meteorite compositions are not typical of much of Martian igneous compositions. Mars Odyssey THEMIS data has exposed local scale compositional variability and provided an enhanced spatial context for the TES results. Layered olivine rich units appear in Valles Marineris, Ares Valles, and Nili Fossae. A quartz and feldspar lithology appears near the central peaks of two craters in Syrtis Major. In addition, a spectrally distinct unit is associated with surface units near Apollinaris Patera. The combined mineralogical information provided by TES with the geologic context provided by THEMIS have provided a picture that is emerging that Mars is perhaps more interesting than expected from an igneous perspective. A variety of processes and mechanisms must be present to produce the range of compositions seen from orbit.
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