Abstract
Both morphologic and geometric studies of the “lineated terrains” around Caloris provide evidence of several types of tectonic motions inside the ejecta blanket of the basin. These motions preferentially occurred along a preexisting pattern. In spite of several similarities to mare-filled multiring basins on the Moon, many geometric and chronologic differences suggest that the ridge pattern inside the Caloris basin may not be produced, as observed on the Moon, exclusively by subsidence of the inner basin under volcanic loading. A model of membrane stresses which yield a decrease of the radius of Caloris and the observed tectonics is proposed.
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