A new geologic map of part of the ancient Martian highlands produced by Scott C. Mest and David A. Crown of the Planetary Science Institute provides new insights into the planet’s history of water modifying the planet’s surface.
“This map depicts the complicated sequence of geologic processes that have served to modify ancient, rugged highland terrains surrounding the Hellas impact basin and shows evidence for the persistent effects of water and ice in degrading the Martian surface,” Crown said.
The most prominent examples for the presence of water in this area are the canyon systems of Waikato Vallis in the north part of the map and Reull Vallis in the central part of the map. These canyons are believed to have formed when underground water was released from plains materials to the surface, causing the ground to collapse. The water could have been stored within the plains in localized aquifers or as ice, which could have melted due to the heat from nearby volcanoes.
“The canyon systems of Waikato Vallis and Reull Vallis, are unlike anything we see here on Earth so trying to understand how they formed requires us to be detectives,” Mest said. “We use images and topographic data from spacecrafts to map the locations of these features, evaluate their relationships to each other, and estimate their ages from superposed impact craters, then we can begin to get a better understanding of the geologic processes that modified the surface and the sequences of events that present us with the surface we see today.”