A Model for the Formation of Paterae on Io

Introduction: Paterae on Io are similar to calderas on the Earth and other planets, yet they have some differences, such as their great sizes (from 2 to 206 km diameter) and lack of high edifices. Tidal heating from Jupiter leads to the production of molten material and the eruption of large amounts of mafic to ultramafic lava within Io’s paterae, as well as across its surface. Formation of paterae is likely also different from our understood models of caldera formation, as the process must lead to the unique morphologies of the features we observe. I describe a possible model for the formation of a typical patera, which uses our collective observations of Io’s paterae and current understanding of Io’s interior as the basis for the steps in the model.