Other
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p13d..05r&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #P13D-05
Other
5220 Hydrothermal Systems And Weathering On Other Planets, 5400 Planetary Sciences: Solid Surface Planets, 5415 Erosion And Weathering, 5419 Hydrology And Fluvial Processes, 5470 Surface Materials And Properties
Scientific paper
Layered, massive or mound-shaped light-toned deposits are present at several locations on Mars. They include crater bulges (e.g. Gale), Interior Layered Deposits in Valles Marineris canyon system (e.g. Candor Chasma), bright deposits in chaotic terrains (e.g. Aram Chaos). Despite the differences among these various kinds of deposits and morphologies, they all share some features, such as layering, and a similar topographic setting, i.e. they form bulges in wide topographic depressions (Valles, craters, chaos). Moreover several of these deposits are located in areas where hydrated minerals have been detected (Bibring et al., 2006). The internal architecture of these deposits is often complex, with inclined layering and even angular unconformities. Their size range from few kilometers up to few hundreds generally, with thicknesses from a few hundred meters up to several km (ILD). So far the origin of these deposits has remained enigmatic, although they have been proposed to represent fluvial, lacustrine or volcanic deposits. We suggest chemical precipitation of spring deposits as a possible formation mechanism for several massive, mound-like or layered deposits on Mars. This working hypothesis could explain the co-occurrence of different characteristics in a wide range of deposits: - massive, dome-shaped or well-stratified stacking pattern - horizontal stacking and clinostratification - hiatus in deposition and subsequent erosion of older portion of deposits (e.g. in Gale Crater, of several ILD) - strong lateral facies variations - presence of hydrated minerals - presence of fluvial features closely connected with deposits - location in low areas, where lithostatic pressure could help the fluid expulsion and subsequent buildup - possibility of large buildups due to low gravity - no need for earth-like surface conditions (P, T, precipitation) given groundwater availability On Earth, spring deposits show a wide variety of internal architectures (e.g. Martin-Algarra et al., 2003). Spring deposits have been proposed for small-scale landforms and deposits on Mars (e.g. Crumpler, 2003). We are testing our hypothesis using morphological and spectral information. References: Bibring, J.-P., et al. (2006) Science 312(5772): 400-404. Crumpler, L. S. (2003) Sixth International Conference on Mars. Martin-Algarra, A., M. Martin-Martin, et al. (2003) Sedimentary Geology 161(3-4): 217-228.
Chicarro Agustin
Gerhard Neukum
Hauber Ernst
Mason Paolo
Ori Gian Gabriele
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