PIA09583: Oudemans Crater Central Uplift: A Sample of Well-Preserved Layering Excavated from Kilometers Below
Target Name: Mars
Is a satellite of: Sol (our sun)
Mission: Mars Reconnaissance Orbiter (MRO)
Spacecraft: Mars Reconnaissance Orbiter (MRO)
Instrument: HiRISE
Product Size: 2048 x 4572 pixels (width x height)
Produced By: University of Arizona/HiRise-LPL
Full-Res TIFF: PIA09583.tif (9.373 MB)
Full-Res JPEG: PIA09583.jpg (582.8 kB)

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This HiRISE image (PSP_001602_1700) covers a portion of the central uplift of the 120-km diameter Oudemans crater.

Oudemans is located at the western end of Valles Marineris and just south of the great canyon system by the Noctis Labyrinthus. Images from the Mars Orbital Camera (MOC) were the first to reveal that this large impact crater exposed layered rock in its central uplift feature.

Such beautifully preserved layered rocks, although rare, are no surprise to planetary scientists. First, layered rocks exposed in the central uplifts are common in terrestrial impact structures. Secondly, there is abundant layering exposed in the nearby Valles Marineris canyon system -- a gash that exposes layering down to 7 km beneath the mean surface. This suggests that layered materials exist to great depths in the subsurface, which is supported by the Oudemans central uplift observation.

Based on estimates of the depth of excavation for a crater the size of Oudemans, these layers originated from just as deep as those exposed in Valles Marineris and possibly deeper. A comparison of the layers in Valles Marineris and in the Oudemans central uplift may prove that they are similar rock types that share the same mode of origin. The fact that these layers are so well intact gives planetary scientists specific clues regarding the subsurface and history of the general area.

Additionly, three other craters, Martin (21.2S, 290.7E), Mazamba (27.3S, 290.2E) and a yet unnamed crater (28.4S, 305E) also possess finely layered materials in their central uplift features and lie within the circum-Tharsis region. The preservation of the layering and geographical occurrence of these four craters suggests that they could be ash layers deposited from numerous episodes from the Tharsis volcanoes. Voluminous volcanic episodes could have produced large volumes of layered rock that could have been rapidly buried and protected from cratering.

Observation Geometry
Acquisition date: 11 November 2006
Local Mars time: 3:34 PM
Degrees latitude (centered): -9.9
Degrees longitude (East): 268.2
Range to target site: 255.7 km (159.8 miles)
Original image scale range: 25.6 cm/pixel(with 1 x 1 binning) so objects ~77 cm across are resolved
Map-projected scale: 25 cm/pixel and north is up
Map-projection: EQUIRECTANGULAR
Emission angle: 2.8
Phase angle: 61.1
Solar incidence angle: 59 , with the Sun about 31 above the horizon
Solar longitude: 142.6 , North

NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, is the prime contractor for the project and built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace and Technology Corp., Boulder, Colo.

Image Credit:
NASA/JPL/Univ. of Arizona

Image Addition Date:
2007-02-01