Lead: Matt Chojnacki  •   Images in this theme   
Aeolian Processes
Aeolian geology is the study of landforms formed by wind (Aeolus is the wind god in Greek mythology). On Mars, where other processes such as fluvial erosion, volcanism, and tectonism are slow, intermittent, or do not occur in the present era, aeolian activity is the most dynamic geologic process in non-polar areas. Numerous depositional and erosional landforms attributable to wind activity are present. On a large scale seen from previous orbiters these include dunes, ripples, yardangs, wind tails, and dust devil tracks. At the small scale seen from landers and rovers, drifts, erosional moats, wind tails, ripples, and ventifacts are found. HiRISE, with its high resolution, color imaging, and ability to produce precise digital elevation models at small scales, should significantly advance our understanding of Martian aeolian processes, providing a link between features seen with older, lower resolution imaging systems and those observed at the landing site scale.

Major science questions for this theme

Relationship to other science themes
By their very nature, aeolian processes modify pre-existing surfaces, either through the redistribution and deposition of fines or the deflation or abrasion of material. In this sense, the aeolian theme crosses over all the other themes, leaving its imprint on all classes of Martian geology. Probably the greatest overlap is with the seasonal processes, climate change, and landscape evolution themes. Seasonal processes outside of the polar caps are predominantly aeolian, with global dust storms, dust devils, and wind streaks occurring on annual and smaller time scales. The wind speeds and sand loading that is possible in the present-day Martian climate seems insufficient to produce many of the observed aeolian landforms, such as dunes, megaripples, and yardangs, implying that past climatic regimes, when wind speeds may have been higher, are required. These aeolian processes integrated over time scales of many seasons and multiple climatic changes (probably driven by quasi-periodic variations in Mars orbital elements) have significantly contributed to landscape evolution through infilling of topographic lows, removal of topographic highs, and redistribution of material.

Features of interest potentially visible at HiRISE scale
The high resolution of HiRISE provides the ability to image and derive topography of features at meter and smaller scales, thereby helping to answer questions that could previously not be pursued with much confidence. We will be able to measure the height and spacing of dunes and ripples and monitor if the bedforms are moved by winds over the life of the MRO mission. Images of landslides on the brinks of dunes will provide information on the stability and lithification (via chemical cementation or ice) of sand. For yardangs, detailed morphometry from high resolution images and stereo DEMs may reveal notches, forms that on Earth are attributable to the height of peak abrasion by saltating sand. Fluting in mantled material seen at small scales should reveal the direction of winds that caused removal. Layering in yardang/mantled material seen by HiRISE will provide evidence on whether the material is of lacustrine (fine layers), volcanic (more massive), or some other origin.