**5. Conclusions**

Even on small bodies impact craters reveal a multifaced morphology as caused by different formation processes. Impacts into a slope can cause the formation of asymmetric craters. Whereas steep slope angles and bigger slope sizes promote the formation of the asymmetries. However, the formation of ring-mold crater and floor-fractured crater is mainly cause by the subsurface conditions. An impact into a thin layer of regolith on top of a subsurface ice-layer lead to the formation of ring-mold crater. The occurrence of ring-mold craters can be used to detect regolith covered ice layers. Furthermore, the maximum depth of associated bowl-shaped craters can be used to estimate the depth of the ice and the thickness of overlying regolith. Floor-fractured craters is mainly proposed by cryomagmatic intrusion, which are fed by underlaying reservoirs. But also tear-off edges in case of slumping of the crater wall, cooling melting processes that lead to sinkage of the crater floor, degassing, and/or tectonic interactions are supposed to promote the formation of these crater types.

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**Author details**

German Aerospace Center (DLR), Berlin, Germany

\*Address all correspondence to: katrin.krohn@dlr.de

provided the original work is properly cited.

© 2021 The Author(s). Licensee IntechOpen. This chapter is distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/ by/3.0), which permits unrestricted use, distribution, and reproduction in any medium,

Katrin Krohn

*Special Crater Types on Vesta and Ceres as Revealed by Dawn*

*DOI: http://dx.doi.org/10.5772/intechopen.96671*

Antonia crater 58.7° S, 350.78° E Azacca crater 6.66° S, 218.4° E Dantu crater 24.3° N, 138.23° E Ezinu crater 43.24° N, 195.7° E Gaue crater 30.81° N, 86.16° E Haulani crater 5.8° N, 10.77° E Ikapati crater 33.84° N, 45.6° E Kupalo crater 39.44° S, 173.2° E Occator crater 19.82° N, 239.33° E Vinalia Facula 20.2° N, 242° E Yalode crater 42.58° S, 292.48° E
