CERES: TECTONIC FEATURES JUXTAPOSED WITH ANALOGIES ON OTHER PLANETARY BODIES

VON DER GATHEN, Isabel¹, JAUMANN, Ralf², KROHN, Katrin², WILLIAMS, David A.³, BUCZKOWSKI, Debra L.⁴, RAYMOND, Carol A.⁵, RUSSELL, Christopher.T.⁶, PREUSKER, Frank¹, ROATSCH, Thomas¹ and SCHENK, Paul M.⁷, (1)German Aerospace Center (DLR), Institute of Planetary Research, Rutherfordstr. 2, Berlin, 12489, Germany, (2)Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, Berlin, 12489, Germany, (3)School of Earth & Space Exploration, Arizona State University, Box 871404, Tempe, AZ 85287, (4)Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, (5)Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, (6)Institute of Geophysics, University of California, Los Angeles, Los Angeles, CA 90095, (7)Lunar and Planetary Institute, Universities Space Research Association, 3600 Bay Area Boulevard, Houston, TX 77058, Isabel.Gathen@dlr.de

Analyzation and interpretation of tectonic features on Ceres’ surface, plays an important role in understanding and reconstructing the history and surface formation. The most common tectonic structures on Ceres are troughs, ridges, scarps, fractures, depressions and domes. Analogues can be found on other planetary bodies like Enceladus, Ganymede, Europa or Mercury.

Current investigations of the surface reveal that some tectonic structures seem to be caused by interaction of extensional tectonics and impact cratering. An example is the Urvara crater (46°S and 249°E), which shows radial depressions out of the craters interior. Analogue structures can be found on Mercury. We assume that tectonic deformations influence the appearance of craters and crater walls. Many of frequently subparallel fissures seem to appear in combination with smooth material. Patterns similar to fractures, cracks and scarps on Ceres can also be found on Enceladus, Europa and Mercury. On Enceladus e.g. in form of the “tiger stripes” or on smaller scale as structures intersecting cratered terrain. Analogies to ridges on Ceres’ surface are existent on Enceladus, Europa and Ganymede, but they are more dominant, complex and more regular shaped. Troughs are relatively rare on Ceres’ surface. However, similarities are evident on Enceladus and Mercury, and could also be related to those on Europa and Ganymede.

The determination of Ceres’ tectonic features caused by deformation processes and the comparison with structures on other planetary bodies will allow us to reconstruct formation processes, the surface morphology, and the topographic signature.

We thank F. Schulzeck, K. Otto, M.C. De Sanctis¸ S. Elgner, E. Kersten, K.D. Matz, A. Nass, S. Schröder, K. Stephan,and R. Wagner for their support.

Session No. 282

T172. Geology of Dwarf Planets: First Results from NASA's Dawn Mission to Ceres

Wednesday, 4 November 2015: 8:00 AM-12:00 PM

Room 344 (Baltimore Convention Center)

Geological Society of America Abstracts with Programs. Vol. 47, No. 7, p.710

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2015 GSA Annual Meeting in Baltimore, Maryland, USA (1-4 November 2015)

CERES: TECTONIC FEATURES JUXTAPOSED WITH ANALOGIES ON OTHER PLANETARY BODIES