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05.07.2012
Mars Express - butterfly ejecta and wrinkle ridges in Melas Dorsa
![Perspective view [1]](javascript:popup('Perspective view [1]','./preleases/558/medres/560-20120613-10532-3D-Solis_MelasDorsa.jpg','Perspective view [1] <br> [#558 Melas Dorsa (Orbit 10532)]')) Perspective view [1] |
On 17 April 2012, 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 acquired images of a region in Melas Dorsa.
![Context Map [2]](javascript:popup('Context Map [2]','./preleases/558/medres/558-20120613-10532-ctxt-Solis_MelasDorsa.jpg','Context Map [2] <br> [#558 Melas Dorsa (Orbit 10532)]')) Context Map [2] |
Melas Dorsa is located in the volcanic highlands of Mars between Sinai and Thaumasia Plana, about 250 kilometres south of Melas Chasma, which is the central part of the large Valles Marineris canyon system. A large, oval crater measuring about 16 kilometres across is immediately apparent in this image, with its ejecta blanket taking the shape of a butterfly. To form such an ejecta blanket, the impact must have occurred at a very shallow angle with respect to the planet's surface; it is thought that subsurface ice was present, and that this liquefied or vaporised on impact.
![Color-coded elevation model [3]](javascript:popup('Color-coded elevation model [3]','./preleases/558/medres/558-20120613-10532-ht-Solis_MelasDorsa.jpg','Color-coded elevation model [3] <br> [#558 Melas Dorsa (Orbit 10532)]')) Color-coded elevation model [3] |
Ridge-like structures resembling twisted rope extend across the image. These terrain features are known as 'wrinkle ridges'. Although volcanic in origin, wrinkle ridges are tectonic terrain forms. They arise in volcanically deposited rock layers that form out of a single hardened lava flow. During the cooling process, the lava contracts and strong compressive forces are generated. The pressure causes areas of rock to shrink - and the corresponding reduction in surface area causes these characteristic wrinkles to form.
![RGB Colour Image [4]](javascript:popup('RGB Colour Image [4]','./preleases/558/medres/559-20120613-10532-co-Solis_MelasDorsa.jpg','RGB Colour Image [4] <br> [#558 Melas Dorsa (Orbit 10532)]')) RGB Colour Image [4] |
Another interesting tectonic phenomenon can be seen in the left half of the full image. After the formation of the wrinkle ridges, further displacements occurred in the crust, which caused several faults to arise. Arranged in a receding sequence, these stress faults run across almost the full height of the image. Formations of this kind are also found on Earth, and are referred to as 'en echelon' displacements or step faults.
![Red-cyan Anaglyph [5]](javascript:popup('Red-cyan Anaglyph [5]','./preleases/558/medres/561-20120613-10532-an-Solis_MelasDorsa.jpg','Red-cyan Anaglyph [5] <br> [#558 Melas Dorsa (Orbit 10532)]')) Red-cyan Anaglyph [5] |
Another striking feature is the filled crater in the upper part of the image. This shows evidence of concentric deposits, which could provide insights into the material properties of the filling.
Image processing and the HRSC experiment on Mars Express
These HRSC images were acquired during Mars Express orbit 10,532. The image resolution is approximately 18 metres per pixel. The data was acquired at approximately 18 degrees south and 288 degrees east.
The plan-view colour image was 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 view was 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 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 HRSC camera experiment on board the European Space Agency's Mars Express mission is headed by Principal Investigator (PI) Professor Gerhard Neukum (Freie Universität Berlin), who was also responsible for the technical design of the camera. The science team consists of 40 co-investigators from 33 institutions in 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 and Jena-Optronik GmbH. The instrument is operated by the DLR Institute of Planetary Research in Berlin-Adlershof. The systematic processing of the HRSC image data is carried out at DLR. The images shown here were created by the Institute of Geological Sciences at Freie Universität Berlin.
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hochaufgelöste Bilddaten / high resolution image data
| Context Map [2]: |
| Color-coded elevation model [3]: |
| RGB Colour Image [4]: |
| Perspective view [1]: |
| Red-cyan Anaglyph [5]: |
© Copyright: ESA/DLR/FU Berlin (G. Neukum)
