Comparison of Topographic Roughness of Layered Deposits on Mars

Impact craters with layered ejecta deposits are widespread on Mars. Prevailing views suggest that such were formed due to the involvement of target water and/or ice in impact excavation post-deposition movement ejecta. The long-runout landslides and lobate debris aprons likely used as analogs compare roughness at multiple scales, considering these three landforms share some similarities their geomorphology. Analog studies morphological differences different emplacement mechanisms an important approach untangling how might form Mars beyond. Earlier comparisons usually based qualitative descriptions or one-dimensional topographic characteristics given azimuths; however, processes recorded two-dimensional topography scales. In this study, we designed a multiwavelet algorithm characterize multi-scale forms Martian deposits. Our show inner facies exhibited similar characteristics, outer more aprons. This study highlights importance spatial resolution digital terrain models characterizing fine fluctuations deposits, providing additional insights into possible parts