The structural control of venusian polygonal impact craters

Pre-impact inhomogeneities of the target material sometimes cause the rim of an impact crater to be composed of several straight segments, instead of being circular. The venusian surface hosts 121 such polygonal impact craters (PICs)>12 km in diameter. Their straight rim segments are often parallel to the orientations of the surrounding tectonic structures, particularly those in tessera terrain and young rift zones, as well as the concentric components of coronae. This match is notably more distinct in distances less than two crater diameters between the PICs and the tectonic structures than further away. Surrounding wrinkle ridges, lineaments or radial components of volcano-tectonic features seem to have very little influence on the orientations of PIC rims. These results imply that the formation of straight segments of venusian PIC rims is controlled by pre-existing tectonic structures of the crust, but not by the apparently most surficial ones. Thus, PICs could be used to provide further constraints on the distribution and orientations of zones of weakness in the venusian crust.