Thawing "dry ice" drives groovy action on Mars
Transient grooves form on dunes when gas trapped under the ice blanket finds an escape point and whooshes out, carrying sand with it.
January 25, 2013
Researchers using NASA’s Mars Reconnaissance Orbiter (MRO) see seasonal changes on far-northern martian sand dunes caused by warming of a winter blanket of frozen carbon dioxide.
The progression begins at left (Panel A) in early spring, when the ground is covered by a seasonal layer of carbon dioxide ice (dry ice) about two feet thick. As spring progresses, the ice cracks (Panel B), releasing dark sand from the dune below. When pressurized gas trapped below the ice layer is released, it carries along sand and dust to the top of the ice layer, where it is dropped in fan-shaped deposits downhill and downwind (panels C and D). The final panel shows more and more of the dark dunes as the overlying layer of seasonal ice evaporates back into the atmosphere. // Credit: NASA/JPL-Caltech/Univ. of Arizona
Earth has no naturally frozen carbon dioxide, though pieces of manufactured carbon-dioxide ice, called “dry ice,” sublime directly from solid to gas on Earth, just as the vast blankets of dry ice do on Mars. A driving factor in the springtime changes where seasonal coverings of dry ice form on Mars is that thawing occurs at the underside of the ice sheet, where it is in contact with dark ground being warmed by early-spring sunshine through translucent ice. The trapped gas builds up pressure and breaks out in various ways.
Transient grooves form on dunes when gas trapped under the ice blanket finds an escape point and whooshes out, carrying out sand with it. The expelled sand forms dark fans or streaks on top of the ice layer at first, but this evidence disappears with the seasonal ice, and summer winds erase most of the grooves in the dunes before the next winter. The grooves are smaller features than the gullies that earlier research linked to carbon-dioxide sublimation on steeper dune slopes.
Similar activity has been documented and explained previously where seasonal sheets of frozen carbon dioxide form and thaw near Mars’ south pole.
The findings reinforce growing appreciation that Mars today, however different from its former self, is still a dynamic world, and, however similar to Earth in some respects, displays some quite unearthly processes.
“It’s an amazingly dynamic process,” said Candice Hansen of the Planetary Science Institute in Tucson, Arizona. “We had this old paradigm that all the action on Mars was billions of years ago. Thanks to the ability to monitor changes with the Mars Reconnaissance Orbiter, one of the new paradigms is that Mars has many active processes today.”
With three martian years — six Earth years — of data in hand from MRO’s High Resolution Imaging Science Experiment (HiRISE) camera, the researchers report on the sequence and variety of seasonal changes. The spring changes include outbursts of gas carrying sand, polygonal cracking of the winter ice blanketing the dunes, sandfalls down the faces of the dunes, and dark fans of sand propelled out onto the ice.
“It is a challenge to catch when and how those changes happen, they are so fast,” said Ganna Portyankina of the University of Bern in Switzerland. “That’s why only now we start to see the bigger picture that both hemispheres actually tell us similar stories.”
The process of outrushing gas that carves grooves into the northern dunes resembles the process creating spider-shaped features in far southern Mars, but the spiders have not been seen in the north. The seasonal dry-ice sheets overlie different types of terrain in the two hemispheres. In the south, diverse terrains include the flat, erodible ground where the spiders form, but in the north, a broad band of sand dunes encircles the permanent north polar ice cap.
Another difference is in brightening on parts of the ice-covered dunes. This brightening in the north results from the presence of water-ice frost, while in the south similar brightening is caused by fresh carbon dioxide. Antoine Pommerol of the University of Bern reports distribution of the water frost using the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM). The light water frost is blown around by spring winds.