Gullies on Mars look a lot like water-carved channels on Earth, but new evidence supports a hypothesis that they are likely not formed by liquid water. As seen in this view of Hale Crater’s eastern rim (35.7°S, 323.4°E) unaltered mafic material (light blue) from the crater rim is carved and transported downslope along the gully channels. No hydrated minerals are observed within the gullies, indicating limited to no interaction of the mafic material with liquid water. Credit: HiRISE/CRISM NASA/JPL/Univ. of Arizona/JHU APL
Source: Geophysical Research Letters

Networks of narrow channels cut into steep slopes in several regions on Mars. These gullies look much like some water-carved channels that form on Earth, but liquid water would be unstable in the Martian atmosphere, so researchers have proposed alternative gully-forming mechanisms. New research by Núñez et al. shows that seasonal frost-driven processes may serve a primary role in forming the Red Planet’s gullies.

Using data from NASA’s Mars Reconnaissance Orbiter, the researchers analyzed more than 100 gullies in the northern and southern hemispheres of Mars. They examined images captured by the spacecraft’s Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), the High Resolution Imaging Science Experiment (HiRISE), and the Context Camera (CTX).

The images revealed that the mineral composition of sediments deposited in and downhill from the mouth of Martian gullies matched “upstream” rock. This suggests that gully formation processes did transport materials downhill. However, the scientists found no mineral evidence that the deposits had interacted with liquid water. This evidence might include any one of the hydrated minerals that can form in the presence of water—sulfates like gypsum, carbonates like calcite, or clays, for example.

In middle- to high-latitude gullies, the researchers instead observed seasonal accumulation of carbon dioxide and water frost. These findings are consistent with the idea that carbon dioxide sublimation could destabilize rocky materials and cause gas-lubricated debris flows, driving gully formation.

Since scientists first discovered Martian gullies in 2000, some of these channels have undergone visible changes. The team studied the deposits of multiple gullies in detail and found no evidence for long-term interaction with liquid water, such as clays or sulfates. Although the observations do not rule out the possibility that liquid water may have contributed to the formation of some of these features, they favor a frost-driven mechanism for the formation of Martian gullies. (Geophysical Research Letters, doi:10.1002/2016GL068956, 2016)

—Sarah Stanley, Freelance Writer


Stanley, S. (2016), How do gullies form on Mars?, Eos, 97, https://doi.org/10.1029/2016EO058057. Published on 26 August 2016.

Text © 2016. The authors. CC BY-NC-ND 3.0
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