Mars and Earth can have many things in common, but processes that release their sand on sand are not among them. Exactly how moving the sand of Martian around crevasses and impact crater has become a mystery – but we can have a better idea.
Planet scientists have thoroughly announced how wild winds, thin environments, temperatures, and terrain work together in shaping the alien landscape – and how it differs from the Earth's sand movement.
This research can help our plans for humanity End trip to Mars.
Despite the occasional planet of the huge RIP Opportunity, the Martian winds generally do not tend to move as much sand as you expect. That is because the atmosphere of the planet is thin and weak; In fact, the average atmospheric surface pressure is only 0.6 percent of atmospheric pressure at the Earth's marine level.
As such, this is why the Red Planet's air is also weak.
"On Mars, there is not enough wind energy to move a large amount of material around the surface," said planetary scientist Matthew Chojnacki of the University of Arizona Lunar and Planetary Lab.
"It may take two years to Mars to see the same movement that you would normally see at a time on Earth."
Scientists of the planet are unsure if Martian sandscapes are still active. Major features are the best places to look for changes, so the team took some sand to study.
They chose 54 dune fields, covering 495 individual sand sized between 2 to 1
"We want to know: The movement of sand uniforms across the planet, or is it enhanced in some regions of the other?" Chojnacki said. "We measured the rate and the volume of sand on Mars."
They found the speed of moving for crescent-shaped sand is an average of only half a meter per year – almost 50 times slower than some of the faster sand dunes on Earth.
While researchers are exploring sand in different locations, including craters, crevasses, canyons, craters, plains and polar basins, they find that, in all regions of the sand, the movement is strongest in three locations.  These are the Syrtis Major Planum, a large dark area between the northern lowlands and the mountains in the south, west of the Isidis impact basin; Hellespontus Montes, a mountain range that reaches 711 kilometers between Noachis Terra and the Hellas Planitia impact basin; and the circumpolar ergs of Olympia and Abalos Undae, sand dunes circling the north pole.
These three locations are quite different from each other, except two basic things: they have changes in topography and surface temperatures.
"These are not factors you can see in terrestrial geology," Chojnacki says. "On Earth, things work differently than Mars. For example, groundwater near the ground or plants growing in the area deny the movement of sand in the sand."
There is another area with a higher rate of sand transfer – although not as high as the first three. They are bases full of bright dust, which strongly reflects sunlight and warms the air, creating localized convection interchanges that move to the sand.
The research was published in Geology .