We combine remote sensing and geomorphological analyses with landform evolution modeling to investigate whether or not terrestrial impact crater morphologies are comparable with martian impact craters formed in volatile-rich environments. We conduct a detailed remote sensing analysis of the terrestrial Bosumtwi crater in Ghana (10.5 km, 1.07 Ma) investigating its geology and geomorphology. This includes a morphometric analysis of the drainage pattern from digital elevation models and the interpretation of multi-spectral image data. The results are compared with a fresh martian impact crater of similar size for which a hypothetical drainage network and catchment areas are derived. We investigate whether the current morphology of Bosumtwi crater results from erosion of a typical martian-type or lunar-type impact crater morphology using landform evolution modeling. Our results reveal that the morphology of Bosumtwi crater cannot be explained by erosion of a lunar-like impact crater. In contrast, the morphological and spectral characteristics of Bosumtwi crater exhibit striking similarities to those of martian rampart craters, especially double-layered ejecta craters. We therefore suggest that Bosumtwi crater was originally built as a Mars-like rampart crater, and that the current morphology is the result of weakly eroded ejecta ramparts.