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Mars Express spots wrinkle ridges and grabens in Tempe Terra
by Staff Writers
Berlin, Germany (SPX) Jan 13, 2012

Topographical map of the north of Tempe Terra.

Tempe Terra is located at the northeastern edge of the Tharsis volcanic region and forms the transition zone between the southern highlands and the northern lowlands. This area is characterised by a large variety of tectonic structures and is one of the most geologically diverse on Mars.

These images from the High Resolution Stereo Camera (HRSC), operated by the German Aerospace Center (Deutsches Zentrum fur Luft- und Raumfahrt; DLR) on board ESA's Mars Express spacecraft, which were acquired on 17 July 2011, show a large number of interesting geological phenomena.

The effects of different forces can be seen adjacent to one another. These have led to both extension of the Martian crust and crustal compression, which has created 'wrinkle ridges'. The most striking result of the crustal extension is a linear graben running across the entire image and only broken by misalignment in a few places.

This graben is up to a kilometre wide and is overlaid by a large impact crater some 12 kilometres across and its ejecta; inside the crater, the graben is covered by younger sediments.

The images show a section of the HRSC image strip located at 42 degrees north and 304 degrees east, obtained during orbit 9622 with a resolution of about 18 metres per pixel.

Landscape shaped by water as well as tectonic forces
To the north of the graben, in the right third of the image, the terrain falls away to the lowlands by over 1000 metres. The landscape here is marked by several extensive valley systems.

Upslope, a number of smaller, dendritic valleys partially covered by impact craters can be made out. Many younger craters in the region south of the graben that still have well-preserved contours exhibit lobate, concentric structures in their interior that have been caused by a slow moving plastic material.

These features, referred to by geologists as concentric crater fill, can be found in a number of places on Mars - including Phlegra Montes, the subject of last month's images.

Prominent mesas are visible in the upper left section of the image, to the southwest. They reveal the original terrain level of the Martian southern highlands. Also conspicuous are the clearly structured ejecta of several impact craters. These partially cover the older flow and graben systems and therefore occurred later. Older, large impact craters have been almost completely covered with sediment or filled with ejecta.

Tempe Terra was first described by Greek astronomer Eugenios Antoniadis (1870-1944, later known as Eugene Michel Antoniadi through his work in France).

His observations of the Tempe Terra region with a powerful new telescope at the Paris Observatory in Meudon during the opposition of Mars in 1909 - described in detail in 1930 - disproved the theory circulating among astronomers that the 'canali' observed by Giovanni Schiaparelli in 1877 were artificial canals; Schiaparelli himself had serious doubts about this interpretation.

As a tribute to both astronomers, who made important contributions to planetary cartography, craters on the Moon, Mars and Mercury bear their names. Tempe Terra was named after a valley to the north of Mount Olympus in Thessaly (Greece), where, according to mythology, Orpheus' wife Eurydice died after being bitten by a snake while fleeing from her tormenter, Aristaios.

The colour images were created from the nadir channel, the field of view of which is aligned perpendicular to the surface of Mars, and the colour channels; the oblique perspective views were generated from HRSC stereo channel data.

The anaglyph, which creates a three-dimensional impression of the landscape when viewed with red/blue or red/green glasses, was derived from the nadir channel and one stereo channel. The black-and-white picture is based on data acquired by the nadir channel, which has the highest resolution of all the channels.

The colour-coded plan view is based on a digital terrain model of the region, from which the topography of the landscape can be derived. The image products shown here were created by the Planetary Sciences and Remote Sensing Department at the Institute of Geological Sciences of the Freie Universitat Berlin.

The HRSC camera experiment on the European Space Agency's Mars Express mission is headed by Principal Investigator (PI) Professor Gerhard Neukum (Freie Universitat Berlin), who was also responsible for the technical design of the camera. The science team consists of 40 co-investigators from 33 institutions in ten nations.

The camera was developed at DLR under the leadership of the PI and it was built in cooperation with industrial partners EADS Astrium, Lewicki Microelectronic GmbH and Jena Optronik GmbH. The instrument is operated by the DLR Institute of Planetary Research in Berlin-Adlershof, through ESA/ESOC.

The systematic processing of the HRSC image data is carried out at DLR. The images shown here were created by PI-group at the Institute of Geological Sciences of the Freie Universitat Berlin.

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