The issue of secondary craters on Ceres for the example of the Ahuna Mons region

Ceres shows an unusual high fraction of crater clusters and crater chains, unprecedented among other asteroidal bodies. It appears that even relatively small craters on the order of 16 km diameter are able to produce a formidable amount of secondary craters stretching out over at least 300 km or 1/10 the Cerean circumference around the crater. Due to Ceres’ relatively fast rotation and related Coriolis effects as well as the body’s low surface gravity, a significant amount of ejecta is falling back to the surface far from its source crater in a highly asymmetrical distribution. The modelled ejecta distribution pattern predicts certain areas of increased secondary crater density consistent with observations