Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p13b1376h&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P13B-1376
Physics
[5415] Planetary Sciences: Solid Surface Planets / Erosion And Weathering, [8450] Volcanology / Planetary Volcanism, [8486] Volcanology / Field Relationships
Scientific paper
The upper alpine desert on Kilimanjaro is significant as it is an area of low precipitation and little vegetation which provides ample opportunity to further understand the nature of weathering products in a high-altitude volcanic environment. There is also potential for extrapolating these results to orbital studies of Martian volcanic terrain. Rock alteration features were identified and matched with USGS spectra, with likely endmembers including clays, such as montmorillonite and possibly sulfates, such as jarosite. However, an exact spectral match using only one endmember, either jarosite or clay, was not possible. Chemistry data supports spectral data, given abundances of elements such as Al, Fe and S on the rock surface, which can possibly help explain a “mixed” spectrum seen in laboratory analysis. Resampling high resolution lab spectra to Landsat and ASTER resolutions allowed for identification, interpretation and mapping of the weathered unit from orbit. Hydrated mineral phases have been detected with the CRISM instrument in the Valles Marineris region of Mars. An exact spectral match of the material, using terrestrial samples such as jarosite and clay, has not been found, indicating a likely “mixed” spectrum, similar to that found on Kilimanjaro. A jarosite-clay mix on Kilimanjaro makes sense, given the low precipitation environment in the upper alpine desert and access to sulfur-rich fluids near the volcano vents. Though fumarolic activity is minimal in the present-day, it is likely to have affected rock surfaces in the past. It is also important to note the placement of these weathered rocks, down-slope from the active fumaroles, indicating a likelihood of past interaction with acidic fluids. Perhaps finding similar materials in Valles Marineris on Mars is also indicative of past interaction not only with acidic fluids to generate the sulfates, but also with water to create the clays.
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