Buczkowski, Debra

DeSanctis, Cristina

Elgner, Stephan

Jaumann, Ralf

Kersten, Elke

Krohn, Katrin

Matz, Klaus-Dieter

Nass, Andrea

Otto, Katharina A.

Preusker, Frank

Raymond, Carol A.

Roatsch, Thomas

Russell, Christopher T.

Schenk, Paul

Schröder, Stefan E.

Schulzeck, Franziska

Scully, Jennifer

Stephan, Katrin

von der Gathen, Isabel

Wagner, Roland

Williams, David A.

Institute of Transport Research:Publications

Geophysical Research AbstractsVol. 18, EGU2016-13530, 2016EGU General Assembly 2016© Author(s) 2016. CC Attribution 3.0 License.Ceres’ deformational surface features compared to other planetary bodies.Isabel von der Gathen (1), Ralf Jaumann (1,2), Katrin Krohn (1), Debra L. Buczkowski (3), Stephan Elgner (1),Elke Kersten (1), Klaus-Dieter Matz (1), Andrea Nass (1), Katharina Otto (1), Frank Preusker (1), ThomasRoatsch (1), Stefanus E. Schröder (1), Franziska Schulzeck (1), Katrin Stephan (1), Roland Wagner (1), Maria C.De Sanctis (4), Paul Schenk (5), Jennifer E. C. Scully (6), Dave A. Williams (7), Carol A. Raymond (8), and theDawn Science Team(1) DLR, Planetary Research, Berlin, Germany (isabel.gathen@dlr.de), (2) Freie Universität Berlin, Germany, (3) JohnsHopkins University Applied Physics Laboratory, Laurel, MD, USA, (4) National Institute of Astrophysics, Rome, Italy, (5)Lunar and Planetary Institute, Houston, TX, USA, (6) NASA JPL, California Institute of technology, Pasadena, CA, USA, (7)Arizona State University, Tempe, AZ, USA, (8) Jet Propulsion Laboratory, California Institute of technology, Pasadena, CA,USAOn March 2015, NASA’s Dawn spacecraft arrived at the dwarf planet Ceres and has been providing images of itssurface. Based on High Altitude Mapping Orbiter (HAMO) clear filter images (140 m/px res.), a Survey mosaic(∼400 m/px) and a series of Low Altitude Mapping Orbiter (LAMO) clear filter images (35 m/px) of the Dawnmission [1], deformational features are identified on the surface of Ceres. In order to further our knowledgeabout the nature and origin of these features, we start a comparative analysis of similar features on differentplanetary bodies, like Enceladus, Ganymede and the Moon, based on images provided by the Cassini, Galileo andLunar Orbiter mission. This study focuses on the small scale fractures, mostly located on Ceres’ crater floors, incomparison with crater fractures on the planetary bodies named above. The fractures were analyzed concerningthe morphology and shape, the distribution, orientation and possible building mechanisms. On Ceres, two differentgroups of fractures are distinct. The first one includes fractures, normally arranged in subparallel pattern, whichare usually located on crater floors, but also on crater rims. Their sense of direction is relatively uniform but insome cases they get deformed by shearing. The second group consists of joint systems, which spread out of onesingle location, sometimes arranged concentric to the crater rim. They were likely formed by cooling-meltingprocesses linked to the impact process or up doming material. Fractures located on crater floors are also commonon the icy satellite Enceladus [3]. While Enceladus’ fractures don’t seem to have a lot in common compared tothose on Ceres, we assume that similar fracture patterns and therefore similar building mechanism can be founde.g. on Ganymede and especially on the Moon [2]. Further work will include the comparison of the fractures withadditional planetary bodies and the trial to explain why fracturing e.g. on Enceladus differs from that on Ceres.References:[1] Roatsch T. et al. (2016) PSS, in press. [2] Buczkowski D. L. (2016) LPSC. [3] Stephan, K. et al. (2013), in TheScience of Solar System Ices, p. 279.

Ceres' deformational surface features compared to other planetary bodies

Ceres' deformational surface features compared to other planetary bodies

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Institute of Transport Research:Publications