Observation of cycloidal features on Enceladus

We observe geologically young cycloidal segments in different places on the surface of Saturn’s moon Enceladus. These features likely have formed as tension cracks with their form being con-trolled by diurnal variation of tides, as suggested for Europa. For this model to work the ice must be weak and, to allow for sufficient tidal amplitude, there must be a fluid layer below the icy surface. Thus, rather than being confined to just southern latitudes, our observations hint at the presence of fluid layers in also other areas on Enceladus, potentially at a global sub-suface ocean in recent times