Other
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..143r&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Other
Scientific paper
Light-toned deposits Light-toned deposits (LTDs) occur extensively on Mars [e.g. 1,2,3]. Several of them have been imaged by the Mars Express (MEX) High Resolution Stereo Camera (HRSC) [4], adding valuable 3-D information [5,6] to the available large extent of datasets from several missions. (e.g. MGS, Odyssey, MRO) HRSC & SHARAD Although LTDs are often located in steep and rough areas (e.g. Valles Marineris, chaotic terrains), the use of HRSC high-resolution Digital Elevation Models (DEMs) [6] greatly helps the analysis of ground penetrating radars such as Mars Reconnaissance Orbiter (MRO) Shallow Radar (SHARAD) [7]. We are concentrating on Crommelin crater and its neighbour as a starting point. Those 2 large structures host extensive LTDs. We are building a Digital Elevation Model covering the entire area (preliminary DEM in Fig. 1) in order to better simulate the surface clutter: the resolution would be roughly 5 to 10 times better than MOLA, at these latitudes. Crommelin crater LTDs LTDs in Crommelin crater have a thickness ranging from 1.5 to 2 km, and the crater just south of Crommelin shows comparable thickness. The deposits are finely stratified and they are affected by a variable amount of erosion. The morphology and structure of the deposits cropping out within the craters show a complex interplay between primary deposition, possible deformation and erosion, increasing the spatial variability of LTDs surface expression. Therefore the surface geology of Crommelin is rather complex, which suggests, up to a certain extent, that its subsurface could be comparably complex as well. The relatively close distance between these LTDs and Meridiani Planum [3], which is characterized by the presence of LTDs that share several features with those in Crommelin offers the possibility of a comparison, not only on the surface geology and geomorphology of the two areas, but also on their subsurface radar expression, possibly useful to draw comparisons and distinctions between them. Further areas We plan to extend the synergic observation campaign to further areas where extensive (and relatively rough/steep) LTDs are present: this include other crater bulges, such as Gale, close to the dichotomy boundary, and few case studies of LTDs in the Valles Marineris canyon system. Although the choice of targets is challenging, the use of high resolution DEMs will hopefully provide better chances to detect subsurface echoes. References [1] Lucchitta, B. K., et al. (1992), in Mars, edited, pp. 453-492. [2] Malin, M. C., and K. S. Edgett (2000) Science, 290(5498), 1927-1937. [3] Arvidson, R. E., et al. (2003) JGR (Planets), 108, 8073. [4] Neukum, G., et al.. (2004), ESA SP-1240. [5] Jaumann, R., et al. (2007), PSS, 55, 928-952. [6] Gwinner, K., et al. (2005), Photogrammetrie - Fernerkundung - Geoinformation, 5, 387-394. [7] Seu, R., et al. (2007) JGR (Planets), 112, E05S05, doi: 10.1029/ 2006JE002745.
Cutugni M.
Dumke Alexander
Gerhard Neukum
Hauber Ernst
Orosei Roberto
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