The characterization and distribution of polygonal impact craters on Ceres and their implications for the cerean crust

Polygonal impact craters (PICs) are supposed to form as a result of impacts into structure systems within the target. The an umbrella term which encompass faults, joints, fractures, lithographic boundaries, and other planes weakness. These defined having at least two linear rim segments with recognizable angle between segments. PICs have been reported on both rocky icy bodies including Ceres. Using near-global Cerean crater database, were categorized four different categories: (1) polygonal not related visible (PICNVS), (2) outside (PICVSO), (3) inside (PICVSI), (4) (PICVSIO). Measurements number segments, mean for crater, length each category. Additionally, nearby determined, along crater's cardinal direction relation system. most frequent type PIC is those systems. Hexagonal prominent polygon shape observed, consistent observed throughout solar displayed highest them Junina Samhain Catenae. average Ceres 121.99° ± 0.25° similar Rhea Dione. found in degradation states, indicating influenced formation much Ceres' history. observation greater concentrations northern hemisphere may indicate target strength differences support idea crustal heterogeneity across Ceres; however, lack southern be due younger larger basins (Urvara Yalode) erasing these creating observational bias.