Ejecta emplacement and modes of formation of Martian fluidized ejecta craters

From an analysis of 1173 craters possessing single (type 1) and double (type 2) concentric ejecta deposits, type 2 craters are found to occur most frequently in areas that have also been described as possessing periglacial features. The frequency of occurrence of central peaks and wall failure (terraces plus scallops) within the craters indicates that, by analogy with previous analyses, type 1 craters form in more fragmental targets than type 2 craters. The maximum range of the outer ejecta deposits of type 2 craters, however, consistently extends about 0.8 crater radii further than ejecta deposits of type 1 craters, suggesting a greater degree of ejecta fluidization for the twin-lobed type 2 craters. Numerous characteristics of Ries Crater, West Germany, show similarities to craters on Mars, indicating that Martian fluidized ejecta craters may be closer analogs to this terrestrial crater than are lunar craters.