Mathematics – Logic
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....10484v&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #10484
Mathematics
Logic
Scientific paper
The almost totality of Mars planet surface is recovered by aeolian dust deposit whose thickness varies according to regions. Mariner and Viking imagery highlighted this aeolian dust deposit with the presence of smooth geomorphologic surface characteristic of dust recovering, with the apparition of dust wind streaks to leeward area of numerous relief, and with seasonal changes in surface albedo after dust storms (Greeley, 1992). These observations have been recently confirmed by the high resolution Mars Orbiter Camera (MOC) of Mars Global Surveyor (MGS) orbiter (Malin et al., 1998 ; Edgett and Malin, 2000). At present time no method exists to estimate aeolian dust thickness at global scale. Only the geographic distribution of the first top centimeters have been realized with the help of thermal inertia cartography from Thermal Emission Spectrometer (TES) data (Jakosky et al., 2000). The aeolian dust deposits recover first the small impact craters and consequently disturb their distribution at the planet surface. Variations between distributions curves locally measured and Hartmann's Isochrons (Hartmann and Neukum, 2001) for a Martian lands not affected by surface phenomenon, give the diameter of the biggest crater obliterated by the surface process. This diameter allows us to estimate the minimal aeolian dust thickness using geometrical proprieties of impact crater between diameter (D) and the rim height (H) (Garvin et al., 2002) : H=0.07D0.52 (for D<7km). Indeed the rim height is a good approximation of minimal dust thickness needed to completely erase the impact crater from the surface if one suppose that there's no evidence of aeolian erosion. The first objective of this study is to determine the distribution variations of the small impact craters to estimate locally the different thickness of aeolian dust. The second objective is to realize a global cartography of the aeolian dust thickness. We study the region of Arabia Terra to apply this method because this region is characterized by a thick aeolian mantling which is very documented since Viking missions. So we realize the estimation of minimal aeolian dust thickness on 60 different sites and we interpolate these data, comprised between 20 and 50 m of dust, to make a map. The realization of this map is important for the selection of new landing sites for the next Martian exploration missions. Moreover it will allow to complete actual geological knowledge of Mars surface and Martian aeolian dynamic and climatic changes during its evolution.
Ansan Véronique
Mangold Nicolas
Masson Philippe
Vincendon C.
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