Hebes Chasma, a trough in the Grand Canyon of Mars
28 March 2008
Hebes Chasma, colour-coded elevation model
Hebes Chasma, perspective view
Hebes Chasma is an enclosed trough, almost 8000 m deep, in Valles Marineris, the Grand Canyon of Mars, where water is believed to have flown. The DLR-operated High Resolution Stereo Camera (HRSC) on ESA’s Mars Express studied the area providing new pictorial clues to its history.
Annotated nadir view of Hebes Chasma.
The steep flanks of the trough (1) show branched incisions and small veins of rock. Below the flanks, run-off and material from larger landslides is visible (2).
A flat-topped mountain is located in the centre of Hebes Chasma (3). It reaches 8000 metres above the graben floor and rises to almost the same height as the plain surrounding the trough.
The mountain is made up of numerous rock layers stacked on top of each other, perhaps constituted from remnants of an older plateau, sediments from a lake, wind-blown sediments or volcanic rocks. The rock layers were exposed by erosion.
Hebes Chasma, perspective view
Hebes Chasma is located at approximately 1° south and 282° east. Image data was obtained on 16 September 2005 with a ground resolution of approximately 15 m/pixel.
Hebes Chasma, false-colour nadir view
Hebes Chasma is an enclosed, almost 8000 m-deep trough in the northern-most part of Valles Marineris, the 3000-km long "Grand Canyon of Mars".
The latest data acquired by the OMEGA spectrometer on-board Mars Express has revealed water-bearing minerals such as gypsum in some areas of Hebes Chasma. This is proof that at least significant quantities of water once existed in Hebes Chasma.
The origin of Hebes Chasma is thought to be connected to the near-by Tharsis Region, which was uplifted in the course of intense volcanism. The uplift created tremendous amounts of stress in the crust forming a series of faults oriented radially
The colour scenes have been derived from the three HRSC-colour channels and the nadir channel. The perspective views have been calculated from the digital terrain model derived from the stereo channels.
The anaglyph image was calculated from the nadir and one stereo channel, stereoscopic glasses are required to view it. The black and white high resolution images were derived from the nadir channel which provides the highest detail of all channels.
3D view of Hebes Chasma
Hebes Chasma context map
The High Resolution Stereo Camera (HRSC) experiment on the ESA Mars Express Mission is led by the Principal Investigator (PI) Prof. Dr Gerhard Neukum who also designed the camera technically.
The science team for the experiment consists of 45 Co-Investigators from 32 institutions and 10 nations. The camera was developed at the German Aerospace Center (DLR) under the leadership of the PI G. Neukum and built in cooperation with industrial partners (EADS Astrium, Lewicki Microelectronic GmbH and Jena-Optronik GmbH). The experiment on Mars Express 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 Geosciences of the Freie Universitaet Berlin in cooperation with the German Aerospace Center (DLR), Institute of Planetary Research, Berlin.