One of the first topics we covered in astrogeology is impact craters. They are characterized by circular or ellipitical depressions in a planetary body and sometimes contain central peaks. The shape is a function of the angle at which the impactor hits the body and the central peak is a product of isostatic rebound. The more shallow the angle at which the impactor hits, the more oblique the crater. The central peak forms as the crust in the center “springs” to a higher elevation after the impact. The debris that gets kicked up during this process surrounds the crater and becomes the ejecta blanket.
What’s interesting is that impact craters follow nearly the same pattern throughout the solar system. From Venus to the Moon, and Mercury, they all look fairly similar.