The shape of large landslides and fluidized ejecta on Mars

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6225 Mars

Scientific paper

Several kinds of large mass movements have been identified on Mars. Among the most spectacular are the long runout landslides of Vallis Marineris and the fluidized ejecta of many fresh Martian craters. In both cases, it has long been thought that volatiles play some role in their emplacement. This interpretation has relied primarily on the fluid appearance of both these landslides and ejecta, the apparent corroborating regional and global geology, evidence in the case of ejecta for fluidized ejecta on volatile-rich icy satellites, and indications in the case of landslides that water frequently initiates and influences emplacement of terrestrial analogues. In the case of both fluidized ejecta and extremely large landslides, contrasting viewpoint relaxes the assumption that subsurface volatiles are required to generate their flow-like morphologies. A large body of evidence for Earth, Venus and Mars has suggested that the presence of an atmosphere is the critical factor in the formation of fluidized ejecta. Similarly, authors have suggested among others thermal lubrication and acoustic fluidization as alternative factors controlling the emplacement of large landslides. Regardless of which factors dominate, it is generally agreed that these fluidized ejecta and landslides must have flowed across the surface. In this work, we use data from the Mars Global Surveyor laser altimeter (MOLA) and camera (MOC) along with Viking images to characterize, compare and contrast the shape of fluidized ejecta of fresh craters in Lunae Planum and the landslides of Vallis Marineris in order to improve our understanding of the physical processes that may have influenced their emplacement. The data compiled is compared to the shape of known terrestrial mass movements, and several possible models describing flowing ejecta and landslides.

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