Elysium volcanic province – perspective color-coded topography
This perspective image shows a view of the Elysium volcanic province from the northeast. The picture is based on an image mosaic computed from 12 HRSC nadir images (a channel in the camera system directed vertically onto the surface of Mars and yielding the highest resolution), with a resolution of 25 metres per pixel, and the associated stereo image data for deriving a digital terrain model. The picture is a colour-coded perspective view. Different colours are used for the elevation information; the lowest lying areas are shown in blue and the highest points of the volcano in light beige.
Elysium is the second largest volcanic province on Mars. It consists of three volcanic complexes - Elysium Mons (on the right in the background), Albor Tholus (on the left at the back) and Hecates Tholus (in the foreground).
Credit: ESA/DLR/FU Berlin (G. Neukum).
This perspective image shows a view of the central part of the Elysium volcanic province from the southeast. The picture is based on an image mosaic computed from 12 HRSC nadir images (a channel in the camera system directed vertically onto the surface of Mars and yielding the highest resolution), with a resolution of 25 metres per pixel, and the associated stereo image data for deriving a digital terrain model. The picture is a colour-coded perspective view. Different colours are used for the elevation information: the lowest lying areas are shown in blue and the highest points of the volcano in light beige.
Tiu Vallis – perspective view from south to north
Over the course of 10 separate orbits, the High Resolution Stereo Camera (HRSC) on Mars Express captured image data from the central region of Tiu Vallis, which has been compiled into a mosaic with a resolution of 12.5 metres per pixel. The mosaic extends over 379 kilometres from north to south and 298 kilometres from east to west. It covers a total area of around 113,000 square kilometres, larger than that of the five new German Federal states.
Tiu Vallis is one of a number of valley systems known in Martian geology as 'outflow channels', which extend from the central Martian highlands for hundreds of kilometres to the plains of the northern lowland. These valley systems are characterised by flow structures and streamlined buttes and craters such as those in the centre, around which the highly energetic masses of water that carved out these valleys once flowed.
For more highlights of the Mars Express visit: http://www.dlr.de/dlr/en/desktopdefault.aspx/tabid-10571/
Elysium is the second largest volcanic province on Mars. It consists of three volcanic complexes - Elysium Mons (on the right in the background), Albor Tholus (on the left at the back) and Hecates Tholus (in the foreground).
The section of the volcanic region shown here extends for about 10 degrees ofvolcanic region shown here extends for about 10 degrees of longitude in an east-west direction and 20 degrees of latitude in a north-south direction. Overall, the volcanic deposits cover an area of around 3.4 million square kilometres - almost 10 times the size of Germany. Elysium Mons is the highest volcano in this region, standing 17.7 kilometres above the western plain. The Elysium volcanic province has been active for over four billion years; elevation in this perspective oblique view is exaggerated by a factor of three.
Credit: ESA/DLR/FU Berlin (G. Neukum).
Over the course of 10 separate orbits, the High Resolution Stereo Camera (HRSC) on Mars Express captured image data from the central region of Tiu Vallis, which has been compiled into a mosaic with a resolution of 12.5 metres per pixel. The mosaic extends over 379 kilometres from north to south and 298 kilometres from east to west. It covers a total area of around 113,000 square kilometres, larger than that of the five new German Federal states.
Tiu Vallis is one of a number of valley systems known in Martian geology as 'outflow channels', which extend from the central Martian highlands for hundreds of kilometres to the plains of the northern lowland. These valley systems are characterised by flow structures and streamlined buttes and craters such as those in the centre, around which the highly energetic masses of water that carved out these valleys once flowed.
Credit: ESA/DLR/FU Berlin (G. Neukum).
Digital terrain models have been generated using image data from the HRSC camera system’s nadir and stereo channels, from which the topography of the surface can be derived. In this image, colours have been allocated to the different elevations in the landscape. It is clear that the Tiu Vallis and the masses of water flowing within it have dug to a depth of between 1500 and 2000 metres into the northern runouts of the Martian highlands. Individual impact craters in the valley floor form striking
depressions. They occurred at a time when water no longer flowed here – otherwise they would have been filled with the sediment load being carried along with it.
The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
The images shown in this gallery were generated at the Institute for Geological Sciences at the Freie Universität Berlin and published there as 'Highlights of the Month' in 2011. They present special Mars products obtained using the HRSC camera on board Mars Express and comprise image mosaics, video-sequences or anaglyphs.
For more highlights of the Mars Express visit: http://www.dlr.de/dlr/en/desktopdefault.aspx/tabid-10571/
Source: DLR
Really interesting posting!!! Elysium Mons is the highest volcano in this region, standing 17.7 kilometers above the western plain. Thanks for sharing this post.
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