Wind-Blown Deposits on Mars Revealed by Mars Express

New images from ESA’s Mars Express show the Syrtis Major region on Mars. Once thought to be a sea of water, the region is now known to be a volcanic province dating back billions of years.

Syrtis Major, discovered in 1659 by Christaan Huygens, is a volcanic province on Mars. The image is centred on approximately 16°N/73°E. The High-Resolution Stereo Camera (HRSC) on ESA’s Mars Express collected the data for this image on 8 June 2011 during orbit 9487. The image has a ground resolution of approximately 19 m per pixel. The image size is approximately 90x180 km. Credits: ESA/DLR/FU Berlin (G. Neukum)

Syrtis Major can be spotted from Earth even with relatively small telescopes – the near-circular dark area on the planet stretches over 1300 x 1500 km.

Christiaan Huygens discovered this area in 1659 and by repeated observations he used it to time the length of day on Mars.

Early ideas held that it was a sea with a water level that rose and fell, causing the markings to change.

Now, however, we know that the region is volcanic in origin, devoid of water and that the changes in its shape are due to dust and sand being blown around in the wind.

A wider contextual image of Syrtis Major. The smaller rectangle shows the region covered in this Mars Express HRSC image release. Credits: NASA MGS MOLA Science Team

Newly released images of a part of Syrtis Major seen from ESA’s Mars Express orbiter show lava flows that flooded the older highland material, leaving behind buttes – isolated hills with steep sides that were too high to be affected.

They can be identified by their lighter colours and their eroded state, and some even show ancient valleys on their flanks.

Individual lava flows, filled craters and partly-filled craters can be made out in the images. The prevailing wind direction can be seen from the dispersal of the lighter-toned dust and darker-toned sand in and around the craters and buttes. The smaller craters illustrate this clearly.

The largest crater in the pictures has a small central peak and contains a small dune field of darker-toned dunes to the east of its floor.

The number and size of craters can be used to date surfaces in the Solar System because craters slowly accumulate as impacts occur over time. This information can be used to date the volcanic province and suggests an age of over 3 billion years.

Syrtis Major is a volcanic province on Mars. This image from the High-Resolution Stereo Camera on ESA’s Mars Express orbiter shows lava flows in box 1. Filled craters and partly filled craters can be seen in box 2. The prevailing wind direction can be judged from the dispersal of the lighter-toned material. The smaller craters illustrate this clearly. The largest crater in the picture, highlighted in box 3, has a small central peak and contains a small dune field of darker-toned dunes. ESA’s Mars Express collected the data for this image on 8 June 2011 during orbit 9487. The image has a ground resolution of approximately 19 m per pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

Syrtis Major, discovered in 1659 by Christaan Huygens, is a volcanic province on Mars. The image is centred on approximately 16°N/73°E. The image was created using a Digital Terrain Model (DTM) obtained from the High-Resolution Stereo Camera on ESA’s Mars Express spacecraft. Elevation data from the DTM is colour coded: purple indicates the lowest-lying regions and grey the highest. The scale is in metres. The data for these images were collected on 8 June 2011 during orbit 9487. The images have a ground resolution of approximately 19 m per pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

The image is centred on approximately 16°N/73°E. The High-Resolution Stereo Camera on ESA’s Mars Express collected the data for these images on 8 June 2011 during orbit 9487. The images have a ground resolution of approximately 19 m per pixel. It was derived from the nadir channel, which provides the highest detail of all the channels. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

The High-Resolution Stereo Camera on ESA’s Mars Express collected the data for these images on 8 June 2011 during orbit 9487. The images have a ground resolution of approximately 19 m per pixel. This perspective view has been calculated from the Digital Terrain Model derived from the stereo channels. Some ancient lava flow fronts are seen in the foreground and a lighter-toned butte is emerging on the right. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

This perspective view has been calculated from the Digital Terrain Model derived from the stereo channels. Some ancient lava flow fronts are seen in the foreground and a lighter-toned butte is emerging on the right. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

This perspective view has been calculated from the Digital Terrain Model derived from the stereo channels. Some ancient lava flow fronts are seen in the foreground and a lighter-toned butte is emerging on the right. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

This perspective view has been calculated from the Digital Terrain Model derived from the stereo channels. Some ancient lava flow fronts are seen in the foreground and a lighter-toned butte is emerging on the right. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

The image combines data from the nadir channel and one stereo channel to produce this 3D image. Stereoscopic glasses are required to see the 3D effect. Credits: ESA/DLR/FU Berlin (G. Neukum)
 

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Tagged with: ancient lava flow • Christaan Huygens • Christiaan Huygens • Clea • Craters • Digital Terrain Model • Dispersal •

Filed under: Mars

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