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Ceres’ Ezinu quadrangle: a heavily cratered region with evidence for localized subsurface water ice and the context of Occator crater

Scully, J.E.C. and Buczkowski, D.L. and Neesemann, Adrian and Williams, D.A. and Mest, S. and Raymond, C.A. and Nass, Andrea and Hughson, K. and Kneissl, T. and Paschkert, J.H. and Ruesch, O. and Frigeri, A. and Marchi, S and Combe, J.-P. and Schmedemann, N. and Schmidt, B. and Chilton, H. and Russell, C.T. and Jaumann, Ralf and Preusker, Frank and Roatsch, Thomas and Hoffmann, M. and Nathues, A. and Schaefer, Martin and Ermakov, A. (2018) Ceres’ Ezinu quadrangle: a heavily cratered region with evidence for localized subsurface water ice and the context of Occator crater. Icarus, 316, pp. 46-62. Elsevier. DOI: 10.1016/j.icarus.2017.10.038 ISSN 0019-1035

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Official URL: https://www.sciencedirect.com/science/article/abs/pii/S0019103516305139


Dawn is the first spacecraft to visit and orbit Ceres, the largest object in the asteroid belt and the only dwarf planet in the inner Solar System. The Dawn science team undertook a systematic geologic mapping campaign of Ceres’ entire surface. Here we present our contribution to this mapping campaign, a geologic map and geologic history of the Ezinu quadrangle, located in the northern mid latitudes from 21–66° N and 180–270° E. From our map, we reconstruct the geologic history of Ezinu quadrangle, which is dominated by impact cratering. Large impact craters that formed a few hundreds to tens of millions of years ago, such as Datan, Messor, Ninsar and Occator, are surrounded by ejecta and contain the products of mass wasting (hummocky crater floor material and talus material) and crater-wall collapse (terrace material). Two of these large impact craters are the sources of lobate flows, which we interpret as melt flows emplaced after the ballistically deposited ejecta. Morphological evidence suggests these lobate flows are rich in water–ice-bearing material that was excavated during the formation of the impact craters. There are only a few localized occurrences of lobate flows, suggesting that the water–ice-bearing source materials have restricted extents and/or are deeply buried within Ceres’ subsurface. The quadrangle also contains a variety of linear features: secondary crater chains are formed by the impact of locally and globally sourced material and pit chains and grooves are formed by the collapse of surficial materials into sub-surface fractures. The Ezinu quadrangle contains the northern portion of Occator crater, which is the host crater of prominent bright regions called faculae. Our geologic analysis therefore also provides context for the future investigation of Occator and its intriguing faculae.

Item URL in elib:https://elib.dlr.de/125184/
Document Type:Article
Title:Ceres’ Ezinu quadrangle: a heavily cratered region with evidence for localized subsurface water ice and the context of Occator crater
AuthorsInstitution or Email of AuthorsAuthors ORCID iD
Scully, J.E.C.NASA JPL, California Institute of Technology, Pasadena, CaliforniaUNSPECIFIED
Buczkowski, D.L.Johns Hopkins University Applied Physics Laboratory 11100 Johns Hopkins Rd. Laurel, MD 20723-6099, USAUNSPECIFIED
Neesemann, AdrianFU BerlinUNSPECIFIED
Williams, D.A.Arizona State UniversityUNSPECIFIED
Mest, S.Planetary Science Institute, 1700 E. Ft. Lowell, Suite 106, Tucson, AZ, 85719, USAUNSPECIFIED
Raymond, C.A.Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USAUNSPECIFIED
Nass, Andreaandrea.nass (at) dlr.deUNSPECIFIED
Hughson, K.University of California Los AngelesUNSPECIFIED
Kneissl, T.Freie Universität Berlin, Inst. of Geosciences, Planetology and Remote SensingUNSPECIFIED
Paschkert, J.H.Westfälische Wilhelms-Universität MünsterUNSPECIFIED
Ruesch, O.NASA Goddard Space Flight CenterUNSPECIFIED
Frigeri, A.National Institute of Astrophysics, Rome, ItalyUNSPECIFIED
Combe, J.-P.Bear Fight Center, A Columbus Technologies and Services Inc. Affiliate, P.O. Box 667, 22 Fiddler's Road, Winthrop, WA 98862, USAUNSPECIFIED
Schmedemann, N.Freie Universitaet Berlin, Inst. of Geosciences, Planetology and Remote Sensing, Malteserstr. 74, 12249 Berlin, GermanyUNSPECIFIED
Schmidt, B.Georgia Institute of TechnologyUNSPECIFIED
Chilton, H.Georgia Institute of TechnologyUNSPECIFIED
Russell, C.T.Institute of Geophysics, University of California, Los Angeles, Los Angeles, CA 90095UNSPECIFIED
Jaumann, Ralfralf.jaumann (at) dlr.dehttps://orcid.org/0000-0002-9759-6597
Preusker, Frankfrank.preusker (at) dlr.deUNSPECIFIED
Roatsch, ThomasThomas.Roatsch (at) dlr.deUNSPECIFIED
Hoffmann, M.Max Planck Institute for Solar System Research , Katlenburg-Lindau, GermanyUNSPECIFIED
Nathues, A.Max-Planck Institute for Solar System Research, Katlenburg-Lindau, GermanyUNSPECIFIED
Schaefer, Martinmartin.schaefer (at) dlr.deUNSPECIFIED
Ermakov, A.California Institute of Technology Jet Propulsion Laboratory Pasadena California USAUNSPECIFIED
Journal or Publication Title:Icarus
Refereed publication:Yes
Open Access:Yes
Gold Open Access:No
In ISI Web of Science:Yes
DOI :10.1016/j.icarus.2017.10.038
Page Range:pp. 46-62
Keywords:Asteroid Ceres Asteroids, surfaces Geological processes Ices Impact processes
HGF - Research field:Aeronautics, Space and Transport
HGF - Program:Space
HGF - Program Themes:Space Science and Exploration
DLR - Research area:Raumfahrt
DLR - Program:R EW - Erforschung des Weltraums
DLR - Research theme (Project):R - Projekt DAWN
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Planetary Geology
Institute of Planetary Research > Planetary Geodesy
Deposited By: Eckart, Lisa Maria
Deposited On:17 Dec 2018 08:57
Last Modified:06 Sep 2019 15:26

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