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• W2336173620 abstract "Introduction and Background: Dark aeolian sediments can be observed almost all over Mars. They are preferably deposited as aeolian dunes on the floor of impact craters and in the north polar erg, but also as thin sand sheets and wind streaks in topographically unconfined places. The sediments are enriched in pyroxene and olivine pointing to a basaltic origin of the dune sands [1, 6]. Hypotheses of material origin include volcaniclastic sediments and volcanic ash [e.g. 1, 2], impact melts [3], and local geologic units, e.g. the Planum Boreum cavi unit [4] or the Medusae Fossae Formation [5]. In previous works [e.g. 6, 7] we have shown that the material seems to have its local source inside the depressions in the form of dark sedimentary layers exposed at crater walls or beneath crater floors – it is not blown into the craters as widely assumed. Similar intracrater sources have also been described in Noachis Terra [8] and Amazonis Planitia [9]. In this work we present further examples of dark material emerging from local intra-crater sources and provide further spectral evidence for a mineralogical correlation between emerging material and the dune sands. The results will help to refine our view of these aeolian deposits on Mars. Data and Methods: For feature identification HRSC nadir (12.5 m/px), CTX (6 m/px), and HiRISE (up to 0.25 m/px) image data were examined and provide a database from regional to local scale. Topographical information was gained from HRSC DTMs (up to 50 m/px). CRISM datasets with a spatial resolution of up to 18 m/px were used for the mineralogical analysis of the dark sediments. Results and Discussion: We found numerous locations (e.g. western Arabia Terra, Noachis Terra, Terra Sirenum) where dark aeolian material emerges from distinct dark layers and is deposited as basaltic dunes nearby. The layers can be exposed at impact crater walls (Fig. 1, 2), along the scarps of channels and plateaus or are located beneath the floors of larger craters, which are blotched by smaller impacts. In the latter case the dark material emerges from these small impact craters, cutting the subsurface dark layer (Fig. 3). It is unlikely that the aeolian material has been blown into these small craters earlier because there are numerous similar craters nearby comprising no dark sand at all. These “clean” craters did not cut the subsurface layer because it is heavily degraded and fragmented. Hence it can take place that craters comprising dark sand and Fig. 1: A 7.8 km crater near Meridiani Planum showing layered structures and dark aeolian sediments emerging from a dark layer exposed in the crater wall. White box indicates location of inset (color and red image of HiRISE observation ESP_011277_1825 superimposed onto CTX P12_005647_1814_XI_01N002W, image center is at 2.5°S; 2.2°E)." @default.
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• W2336173620 date "2012-06-01" @default.
• W2336173620 modified "2023-09-27" @default.
• W2336173620 title "On the Sources of Dark Dune Sands on Mars" @default.
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