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06.01.2012

HRSC Press Release #535 - Tempe Terra (orbit 9622)


'Wrinkle ridges' and grabens in Tempe Terra


Perspective view [1]
Perspective view [1]
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 (also compare press release #265). 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 für 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.


Context Map [2]
Context Map [2]

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' (see image detail 1 in the overview image). 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 twelve kilometres across and its ejecta; inside the crater, the graben is covered by younger sediments (image detail 2).



Color-coded elevation model [3]
Color-coded elevation model [3]



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


Feature Map [4]
Feature Map [4]
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 (image detail 3). 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 (see press release #531).



Nadir Image [5]
Nadir Image [5]
Prominent mesas are visible in the upper left section of the image, to the southwest (image detail 4). 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 (image detail 5) have been almost completely covered with sediment or filled with ejecta.



RGB Colour Image [6]
RGB Colour Image [6]
Tempe Terra was first described by Greek astronomer Eugenios Antoniadis (1870-1944, later known as Eugène 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.



Red-cyan anaglyph [7]
Red-cyan anaglyph [7]
The colour images were created using data from the nadir channel, the field of view of which is which is directed vertically down onto the Martian surface, and the colour channels. The perspective views were computed using data from the HRSC stereo channels. The anaglyph image, which conveys 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 image is based on data from the nadir channel, which has the highest resolution of all the channels. The false-colour view is based on a digital terrain model of the region, from which the topography of the landscape can be derived. The images were produced by the Department of Planetary Sciences and Remote Sensing in the Institute for Geological Sciences of the Freie Universität Berlin.



Perspective view #2 [8]
Perspective view #2 [8]
The High Resolution Stereo Camera (HRSC) experiment on the European Space Agency's Mars Express mission is led by the Principal Investigator (PI) Prof. Dr Gerhard Neukum, who was also responsible for the technical design of the camera. The science team for the experiment consists of 40 co-investigators from 33 institutions and 10 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
Perspective view #3 [9]
Perspective view #3 [9]
and Jena Optronik GmbH. The instrument is operated by the DLR Institute of Planetary Research, through ESA/ESOC. The systematic processing of the HRSC image data is carried out at DLR. The scenes shown here were processed by the PI-group at the Institute for Geological Sciences of the Freie Universität Berlin.








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hochaufgelöste Bilddaten / high resolution image data

Context Map [2]:   TIF
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JPG
(451 KBs)
Color-coded elevation model [3]:   TIF
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JPG
(10 MBs)
Feature Map [4]:   TIF
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Nadir Image [5]:   TIF
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RGB Colour Image [6]:   TIF
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Red-cyan anaglyph [7]:   TIF
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Perspective view [1]:   TIF
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Perspective view #2 [8]:   TIF
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Perspective view #3 [9]:   TIF
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© Copyright: ESA/DLR/FU Berlin (G. Neukum)

 

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07.08.2012

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