Abstract Near‐surface wind fields on Mars are profoundly modulated by complex topography, yet fine‐scale wind field characteristics remain poorly resolved for key geomorphological units such as deltas, valleys, and impact craters, due to the spatial constraints of lander‐based wind observations. To address this, we identified three dominant wind directions using measured near‐surface wind data from the Perseverance rover at Jezero Crater and then integrated in situ wind measurements with high‐resolution numerical modeling. We established a high‐resolution three‐dimensional (3D) terrain model encompassing key local geomorphic units, including the delta, valleys, an impact crater, and nearby mesas, and performed Computational Fluid Dynamics simulations under the above‐mentioned three dominant wind directions. The results reveal a robust coupling mechanism between local topography and near‐surface wind field structures. We demonstrate that wind speed is significantly enhanced over windward slopes but evidently attenuated within depressions and crater floors. Crucially, significant wind direction deflection angles were particularly evident in areas characterized by steeper slopes. For instance, wind flow exhibited a symmetrical deflection pattern along the opposing inner walls of the modeled impact crater, but exhibited negligible deflection on the crater floor. Spatial comparisons indicate that wind deflection is most pronounced over steeper slopes, while sector‐based distributions within the impact crater reveal a consistent symmetry between opposing wall and floor regions. These findings offer new and critical insights into the intimate connection between Martian surface aeolian erosion/deposition processes and local topographic evolution, which is vital for interpreting the sedimentary history of Jezero Crater.
Liu et al. (Fri,) studied this question.
Synapse has enriched 5 closely related papers on similar clinical questions. Consider them for comparative context: