Investigating Aeolian Features at Gale Crater, Mars Using Geospatial Approach

Gale Crater, located in Mars’ southern hemisphere, is a key site for studying Martian aeolian processes. This study employs Remote Sensing and GIS techniques to analyze the influence of local topography and seasonal variations on dune morphology within the crater. High-resolution imagery from the Context Camera (CTX) and HiRISE onboard the Mars Reconnaissance Orbiter (MRO) reveals distinct dune patterns shaped by wind flows influenced by the crater’s topography. The northern region is characterized by unidirectional and bidirectional dunes, formed by corresponding wind patterns, while the southern region features complex star dunes due to multidirectional winds. Martian seasonal cycles, particularly during dust storm seasons (Ls $180^{\circ}-360^{\circ}$), further sculpt the dune fields into three primary types: Migrating, Elongating, and Accumulating dunes, located at elevations between -4500 m and -3500 m. This research enhances our understanding of Martian surface-atmosphere interactions and provides valuable insights into the planet’s atmospheric dynamics.