Mathematics – Logic
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p13a1263j&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #P13A-1263
Mathematics
Logic
[6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
Previous studies (Osterloo et al., 2008) have located and characterized spectrally unique units on the surface of Mars based on their spectral signatures in mid-IR data collected by the Thermal Emission Imaging System (THEMIS) instrument aboard the 2001 Mars Odyssey spacecraft. The unique spectral slopes associated with these deposits in THEMIS data can be best explained by the admixture of spectrally neutral chloride salts and basaltic materials. These deposits can be recognized in THEMIS daytime infrared images by a distinct aqua-blue color in 9/6/4 (RGB) decorrelation stretch images and a relatively featureless emissivity spectrum that slopes toward lower wavenumbers. Identification of these units has been constrained to the ancient cratered southern highlands of Mars suggesting that water was persistent and widespread, either on the surface or in the near subsurface of Mars early in its history. The objective of this study is to determine the geologic context of these deposits over the Martian landscape as well as to define any spectral variation between defined units, if any. On Earth, chloride salt deposits have three possible origins: (1) precipitation from evaporating surface water (e.g. saline lakes), (2) volcanic outgassing, or (3) direct crystallization (forming crusts). Using MOLA elevation data, the local topography around these spectrally distinct units can be derived and compared. In localities where CRISM FRT data overlaps the deposit positions, the detection of clays indicate a persistent aqueous environment, while their absence may indicate a short lived presence of liquid water at the locality. Variations of spectral slope as well as other spectral characteristics derived from atmospherically corrected daytime THEMIS IR data may indicate variations in the thickness, concentration, and geologic context of the deposits. Through a greater understanding of the geologic environment around these units, we can glean a greater understanding of the conditions under which liquid water was introduced and subsequently removed from the ancient Martian surface.
Glotch Timothy D.
Jensen Heidi B.
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