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Glacial, volcanic and fluvial activity on Mars: latest images
Ice and dust at Martian north pole
25 February 2005
These images, taken by the High Resolution Stereo Camera (HRSC) on board ESA’s Mars Express spacecraft, were released at the First Mars Express Science Conference this week. They show the areas of focused research - water, ice, glaciers and volcanism.
 | | | Ice and dust at Martian north pole |
These two images of the Martian north polar ice cap show layers of water ice and dust for the first time in perspective view. The close-up view (right) is the upper right section of the image above.
Here we see cliffs which are almost 2 kilometres high, and the dark material in the caldera-like structures and dune fields could be volcanic ash.
Fields of volcanic cones at Martian north pole
| | Top view of volcanic cone | |
In the image above, also at the north pole, the Mars Express spacecraft saw fields of volcanic cones. Some are up to 600 metres high.
They appear to indicate very recent volcanic activity. The question remains, is it on-going activity?
| | | Top view of volcanic cone |
The two smaller images are close-up top views of two cones: the left one is visible in the lighter top part of the main image, and the right one is just visible half way down the dark side of the slope.
Kasei Valles - the greatest outflow channel on Mars
| | Scouring of the valley floor in Kasei Valles | |
The image above is Kasei Valles, one of the largest outflow channels on Mars, and contains a lot of evidence for glacial and fluvial activity over much of the planet's history.
Kasei Valles has been imaged before by the HRSC during orbit 61 from an altitude of 272 kilometres. These images are located about 29° North and 300° East.
The scour marks in the valley, shown in the image on the left, are most likely due to glacial erosion than by water erosion. This is contrary to what was previously thought.
The glacier that caused this valley was fed by water from the Echus Chasma region, which was driven out from underneath the surface by volcanic activity. Water was released by heating from volcanic activity in the channel floor as relatively recently as 20 million years ago.
Perspective view of Echus Chasma
Echus Chasma is the source region of the Kasei Valles channel. This perspective image was taken by Mars Express during orbit 97. It shows that liquid water was present on the surface of Mars thousands of millions of years ago.
Gigantic waterfalls poured over the 4000-metre high cliffs, and fed a lake in the valley. Later, when the planet became cooler, the lakes froze and glaciers formed, carving the giant Kasei Valles.
Western scarp of Olympus Mons
| | Close-up perspective view of Olympus Mons scarp | |
These perspective views of the western side of the Olympus Mons caldera show evidence of ice/snow and water. The close-up image (right) shows detail in the left side of the scarp above.
On the eastern side of the giant volcano, lava produced between 200 million and 20 million years ago melted a snow and ice layer on the volcanic shield, with the result that liquid water was on the surface as recently as 20 million years ago.
On the western side, lava produced between 200 million and 2.5 million years ago mobilised underground water and formed glaciers as recently as four million years ago.
These findings were presented on 21 February at ESA's Mars Express Science Conference at ESTEC in Noordwijk, the Netherlands, where about 250 scientists from all over the world are discussing the first year of scientific results from Mars Express.
The colour images were processed using the HRSC nadir (vertical view) and three colour channels. The perspective views were calculated from the digital terrain model derived from the stereo channels.
For more information on Mars Express HRSC images, you might like to read our updated 'Frequently Asked Questions'.
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