Colourful dunes on wind-swept Mars

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Dunes are distinguished indicators of prevalent winds, as can be seen on this void building on Mars, imaged by ESA’s Mars Express on 16 May.

Dune margin in a crater, viewpoint view

Depressions such as impact craters can act as traps for sediments that have been blown in from elsewhere, accumulating in several patterns churned adult by clever winds.

Dune-filled void in context

The dune margin in this unnamed 48 km-wide impact void in a southern highlands of Mars includes sickle-shaped dunes famous as barchans, and together ridges of dunes called cross dunes.A uniformly distributed silt piece stretches between a dunes and a western wall of a crater.

Barchans are a many common dune form found on Mars, and are also prevalent in Earth’s deserts. The shallower slope faces a wind, with a steeper, winding slope downwind, a ‘horns’ of a particular dunes indicating in a instruction a breeze is blowing. In this example, a southeasterly breeze during a time of dune arrangement can be assumed.Many circuitously craters in this segment also horde dunes, and uncover a northwest change of their dune fields relations to a void centre, arguing for a uniform breeze instruction from a southeast.

Dune-filled void topography

To a south of a dune margin in a immeasurable crater, a singular elongated cross dune extends over a categorical margin for several kilometres. Perhaps a underlying topography total with near-surface winds caused a sediments to raise adult here, or over time a smaller barchan dunes assimilated together.

Dune-filled void in 3D

This stage is situated south of Tharsis, a largest volcanic range on Mars and home to Olympus Mons. Past volcanic activity in Tharsis constructed immeasurable amounts of basalt, excellent pyroclastic deposits and ash, that were expected swept opposite a segment to yield a source for a dim dune element celebrated in these craters today.

Source: ESA

 

 

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