Neighbouring volcanoes on Mars

Neighbouring volcanoes on Mars

1 April 2011

ESA’s Mars Express has returned images of mist-capped volcanoes located in the northern hemisphere of the red planet. Long after volcanic activity ceased, the area was transformed by meteor impacts that deposited ejected material over the lower flanks of the volcanoes.

Permanent and transient features are on display in this newly released image of Mars. The image is derived from data acquired during three orbits of ESA’s Mars Express between 25 November 2004 and 22 June 2006. In that time, these dead volcanoes were not expected to change but, during the middle orbit, Mars Express captured icy clouds drifting past the summit of Ceraunius Tholus.

Ceraunius Tholus and Uranius Tholus in context

By the time Mars Express crossed again and took the final strip of data needed for this image, the clouds had long since dispersed and so there is a sharp line across them in the finished mosaic.

The Latin word “tholus” means a conical dome and the base of Ceraunius Tholus is 130 km across, while the peak rises 5.5 km above the surrounding plains. At its summit is a large caldera 25 km across. With similar morphology to its neighbour and lying 60 km to the north, Uranius Tholus is a smaller volcano, with a base diameter of 62 km and a height of 4.5 km.

Features around Ceraunius Tholus and Uranius Tholus

The flanks of Ceraunius Tholus are relatively steep, at about 8° inclination, and are etched with valleys. They are deeply cut in many places, suggesting that soft and easily eroded material, such as layers of ash, were deposited during the volcano’s eruptions.

The largest and deepest of these valleys is about 3.5 km wide and 300 m deep. It terminates inside an otherwise unrelated elongated impact crater that happens to lie between the two volcanoes, and has created a fascinating fan shape of deposits.

Elevation of Ceraunius Tholus and Uranius Tholus

Although the source of the fan is still being debated in scientific circles, it may have been formed when material from a lava channel or tube was washed downwards by a melting ice cap on the volcano.

Certainly, the summit crater – the caldera – is flat and smooth, so it may have contained a lake early in Mars’ history when the atmosphere was denser. It is also possible that the water was produced when volcanic activity melted buried ice lenses. An ice lens forms when moisture seeps below the surface and forms a frozen layer between the top ‘soil’ and the rocky layer below.

Ceraunius Tholus and Uranius Tholus in high resolution

The elongated crater between the two volcanoes is called Rahe. It measures 35 km by 18 km and is the result of an oblique impact by a meteorite.

A smaller impact crater 13 km across can be seen to the west of Uranius Tholus. This one also formed after all the volcanic activity ended and served to cover the lower flanks of the volcanoes with ejected material, with the result that only the upper regions of the original structures are now visible.

Ceraunius Tholus in perspective
Ceraunius Tholus and Uranius Tholus in perspective
Ceraunius Tholus and Uranius Tholus in perspective
Ceraunius Tholus and Uranius Tholus in 3D
Ceraunius Tholus and Uranius Tholus in 3D
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