Curious Mars


Changes to Martian Surface Caused by Seasonal CO2 Ice Thaws

©NASA

Seasonal Thaw on Mars

Spring is a dynamic season on the dunes surrounding Mars' north pole. When frozen carbon dioxide, or dry ice, deposited as a winter ice cap on Mars sublimates - changes directly from a solid to a gas - in the spring it causes a variety of geologic changes to the Martian surface, research led by Planetary Science Institute Senior Scientist Candice Hansen has shown.

The HiRISE camera on the Mars Reconnaissance Orbiter snapped this series of pictures of sand dunes in the north polar region of Mars. The progression of false color pictures begins in early spring (panel a) when the ground is covered by a seasonal layer of carbon dioxide ice (dry ice) about 2 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. Image credit: NASA/JPL-Caltech/Univ. of Arizona

The exotic phenomena associated with spring on Mars are described in three associated articles recently published in Icarus. Observations from the High Resolution Imaging Science Experiment (HiRISE) camera and the infrared spectrometer (CRISM) on the Mars Reconnaissance Orbiter have provided a rich data set that now covers three spring seasons in the northern hemisphere, Hansen said.

In the winter Mars' carbon dioxide atmosphere condenses to form a seasonal CO2 - dry ice - polar cap in the northern polar region, blanketing a vast sea of dunes that encircle Mars' permanent water ice polar cap. In the spring the dry ice sublimates, or evaporates, and the gas erodes and destabilizes sand on the dunes.

"It's an amazingly dynamic process," said Hansen. "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."

Hansen is lead author of "Observations of the northern seasonal polar cap on Mars: I. Spring sublimation activity and processes," the first of three related papers published in Icarus. PSI Senior Scientist Mary Bourke is a co-author on the paper.

With three years of data in hand the researchers report on the sequence and variety of changes that take place over the spring, including outbursts of gas carrying sand, polygonal cracking of the ice on the dunes, sandfalls down the slipface of the dunes, and dark fans of sand propelled out onto the ice. Gas escaping from under the seasonal layer of dry ice erodes channels in the dunes, reminiscent of the erosion that carves more permanent "spider" channels in the southern hemisphere polar region.

The second paper describes results from analyses of HiRISE images from a dozen different locations inside the area of northern polar shifting sand dunes. They are at similar latitudes but at various longitudes around the pole, some are inside the polar cap trough but some are not, some close to the polar cap scarp and some are far away. Despite those differences, all the locations follow similar trends during their spring sublimation phase. They all have a brightening phase, they all develop dark streaks, blotches and linear cracks in the ice and wind-modified fan deposits at similar times.

CRISM data shows the variability of the composition of the seasonal polar cap in the spring, described in the third paper. Water ice frost coats the dry ice at some times. The water frost gets blown around on top of the dry ice.

Images are available at http://www.psi.edu/news/press-releases/hansen012413

The study was funded by grants from NASA, the Jet Propulsion Laboratory and the University of Arizona in support of Mars Reconnaissance Orbiter research.

CONTACT:
Candice Hansen
Senior Scientist
626-483-5640
cjhansen@psi.edu

PSI INFORMATION:
Mark V. Sykes
Director
520-622-6300
sykes@psi.edu

References in Icarus:
http://dx.doi.org/10.1016/j.icarus.2012.09.024
http://dx.doi.org/10.1016/j.icarus.2012.10.017
http://dx.doi.org/10.1016/j.icarus.2012.08.039

The Planetary Science Institute is a private, nonprofit 501(c)(3) corporation dedicated to solar system exploration. It is headquartered in Tucson, Arizona, where it was founded in 1972. PSI scientists are involved in numerous NASA and international missions, the study of Mars and other planets, the Moon, asteroids, comets, interplanetary dust, impact physics, the origin of the solar system, extra-solar planet formation, dynamics, the rise of life, and other areas of research. They conduct fieldwork in North America, Australia and Africa. They also are actively involved in science education and public outreach through school programs, children's books, popular science books and art. PSI scientists are based in 18 states and the District of Columbia, Australia, Canada, Ireland, Latvia, Russia, South Africa, Switzerland and the United Kingdom.

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