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POSTER SESSION I: CERES: MISSION RESULTS from DAWN 6:00 P.M
Lunar and Planetary Science XLVIII (2017) sess312.pdf Tuesday, March 21, 2017 [T312] POSTER SESSION I: CERES: MISSION RESULTS FROM DAWN 6: 00 p.m. Town Center Exhibit Area Russell C. T. Raymond C. A. De Sanctis M. C. Nathues A. Prettyman T. H. et al. POSTER LOCATION #171 Dawn at Ceres: What We Have Learned [#1269] A summary of the major discoveries and their implications at the close of the exploration of Ceres by Dawn. Ermakov A. I. Park R. S. Zuber M. T. Smith D. E. Fu R. R. et al. POSTER LOCATION #172 Regional Analysis of Ceres’ Gravity Anomalies [#1374] Put in geological and geomorphological context, the regional gravity anomalies give clues on the structure and evolution of Ceres’ crust. Nathues A. Platz T. Thangjam G. Hoffmann M. Mengel K. et al. POSTER LOCATION #173 Evolution of Occator Crater on (1) Ceres [#1385] We present recent results on the origin and evolution of the bright spots (Cerealia and Vinalia Faculae) at crater Occator on (1) Ceres. Buczkowski D. L. Scully J. E. C. Schenk P. M. Ruesch O. von der Gathen I. et al. POSTER LOCATION #174 Tectonic Analysis of Fracturing Associated with Occator Crater [#1488] The floor, walls, and ejecta of Occator Crater on Ceres are cut by multiple sets of linear and concentric fractures. We explore possible formation mechanisms. Pasckert J. H. Hiesinger H. Raymond C. A. Russell C. POSTER LOCATION #175 Degradation and Ejecta Mobility of Impact Craters on Ceres [#1377] We investigated the degradation and ejecta mobility of craters on Ceres, to investigate latitudinal variations, and to compare it with other planetary bodies. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Geologic Mapping of the Ac-H-11 Sintana Quadrangle of Ceres from Nasa’S Dawn Mission
47th Lunar and Planetary Science Conference (2016) 1955.pdf GEOLOGIC MAPPING OF THE AC-H-11 SINTANA QUADRANGLE OF CERES FROM NASA’S DAWN MISSION. F. Schulzeck1, K. Krohn1, R. Jaumann1, D. A. Williams2, D. L. Buczkowski3, S. C. Mest4, J. E. C. Scully5, I. v. d. Gathen1, E. Kersten1, K.-D. Matz1, A. Naß1, K. Otto1, C. M. Pieters6, F. Preusker1, T. Roatsch1, M. C. De Sanctis7, P. Schenk8, S. Schröder1, K. Stephan1, R. Wagner1, C. A. Raymond5, C. T. Russell9, 1DLR, Berlin, Germany; 2School of Earth & Space Exploration, Arizona State University, Tempe, AZ, USA; 3JHU-APL, Laurel, MD, USA; 4Planetary Science Institute, Tucson, AZ, USA; 5Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; 6Department of Earth, Environmental, and Planetary Sciences Brown University, Providence, RI, USA; 7National Institute of Astrophysics, Rome, Italy; 8Lunar and Planetary Institute, Houston, TX, USA; 9UCLA, Los Angeles, CA, USA Introduction: NASA’s Dawn spacecraft arrived at cratering on the primary crater rim. Annona crater Ceres on March 5, 2015, and has been studying the features both characteristics. Whereas collapse dwarf planet through a series of successively lower structures are mostly blocky, Annona’s landslide, orbits, obtaining morphological & topographical triggered by a younger crater on its rim, is image, mineralogical, elemental, and gravity data. The characterized by lobate margins. The occurrence of Dawn Science Team is conducting a geologic mapping mass movements and the type of mass wasting feature campaign for Ceres similar to that done for Vesta [1, might therefore hint to compositional differences. For 2], including production of a Survey- and High complex craters, such as Darzamat and Mondamin, we Altitude Mapping Orbit (HAMO)-based global map, observe many different inner crater structures, like relaxed crater floors, ridges, central peaks, mounds and and a series of 15 Low Altitude Mapping Orbit smooth plains. -
Mineralogy of the Occator Quadrangle
Icarus 318 (2019) 205–211 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Mineralogy of the Occator quadrangle ∗ A. Longobardo a, , E. Palomba a,b, F.G. Carrozzo a, A. Galiano a, M.C. De Sanctis a, K. Stephan c, F. Tosi a, A. Raponi a, M. Ciarniello a, F. Zambon a, A. Frigeri a, E. Ammannito d, C.A. Raymond e, C.T. Russell f a INAF-IAPS, via Fosso del Cavaliere 100, I-00133 Rome, Italy b ASI-ASDC, via del Politecnico snc, I-00133 Rome, Italy c Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), D-12489 Berlin, Germany d ASI-URS, via del Politecnico snc, I-00133 Rome, Italy e California Institute of Technology, JPL, 91109 Pasadena, CA, USA f UCLA, Los Angeles, CA 90095, USA a r t i c l e i n f o a b s t r a c t Article history: We present an analysis of the areal distribution of spectral parameters derived from the VIR imaging Received 28 April 2017 spectrometer on board NASA/Dawn spacecraft. Specifically we studied the Occator quadrangle of Ceres, Revised 11 September 2017 which is bounded by latitudes 22 °S to 22 °N and longitudes 214 °E to 288 °E, as part of the overall study Accepted 18 September 2017 of Ceres’ surface composition reported in this special publication. The spectral parameters used are the Available online 22 September 2017 photometrically corrected reflectance at 1.2 μm, the infrared spectral slope (1.1–1.9 μm), and depths of Keywords: the absorption bands at 2.7 μm and 3.1 μm that are ascribed to hydrated and ammoniated materials, Asteroid ceres respectively. -
Accepted Manuscript
Accepted Manuscript The Mineralogy of Ceres’ Nawish Quadrangle F.G. Carrozzo , F. Zambon , M.C. De Sanctis , A. Longobardo , A. Raponi , K. Stephan , A. Frigeri , Ammannito , M. Ciarniello , J.-Ph. Combe , E. Palomba , F. Tosi , C.A. Raymond , C.T. Russell PII: S0019-1035(17)30330-5 DOI: 10.1016/j.icarus.2018.07.013 Reference: YICAR 12962 To appear in: Icarus Received date: 29 April 2017 Revised date: 19 June 2018 Accepted date: 13 July 2018 Please cite this article as: F.G. Carrozzo , F. Zambon , M.C. De Sanctis , A. Longobardo , A. Raponi , K. Stephan , A. Frigeri , Ammannito , M. Ciarniello , J.-Ph. Combe , E. Palomba , F. Tosi , C.A. Raymond , C.T. Russell , The Mineralogy of Ceres’ Nawish Quadrangle, Icarus (2018), doi: 10.1016/j.icarus.2018.07.013 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. ACCEPTED MANUSCRIPT HIGHLIGHTS Sodium carbonates are found in bright material in ejecta craters Mineralogy of quadrangle Nawish using the band at 2.7, 3.1 and 3.9 µm. Correlation between age of terrains and the mineralogy ACCEPTED MANUSCRIPT 1 ACCEPTED MANUSCRIPT The Mineralogy of Ceres’ Nawish Quadrangle F.G. Carrozzo1, F. Zambon1, M.C. -
Influence of Volatiles on Mass Wasting Processes on Vesta and Ceres”.7Z (
RESEARCH ARTICLE Influence of Volatiles on Mass Wasting Processes on 10.1029/2020JE006573 Vesta and Ceres Key Points: R. Parekh1,2 , K. A. Otto1 , R. Jaumann2 , K. D. Matz1 , T. Roatsch1 , E. Kersten1 , H L • We classified and estimated the / S. Elgner1 , and C. Raymond3 of mass movements to investigate the mechanisms of deposition on 1DLR Institute of Planetary Research, Berlin, Germany, 2Institute of Geological Science Germany, Freie University of Vesta and Ceres 3 • Vesta has dry, granular-like slides Berlin, Berlin, Germany, Jet Propulsion Laboratory, Pasadena, CA, USA as dominant mass wasting feature, whereas Ceres has abundant features of flow-like mass movements Abstract We have analyzed mass wasting features, their distribution and deposit geometry on • The mass wasting deposit mobility the two largest main asteroid belt objects—protoplanet Vesta and dwarf planet Ceres—and compared is influenced by the material composition and volatile content on their geomorphology and mobility. Both asteroids have similar surface accelerations, but different Vesta and Ceres surface compositions. Based on our observations and previous studies, we categorized three distinct morphological mass wasting classes: slumps, slides, and flow-like movements. We conclude that Ceres Supporting Information: has abundant features of flow-like mass movements. Further, sliding and flow-like characteristics are • Supporting Information S1 identified in craters within mid-latitudes which supports the possibility of the presence of water ice in the near subsurface of Ceres. Vesta predominantly shows characteristics of dry granular-like slide features Correspondence to: which are distributed homogenously across the surface. By plotting the ratio between fall height (H) and R. -
Geological Mapping of the Ac-10 Rongo Quadrangle of Ceres
Icarus 316 (2018) 140–153 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Geological mapping of the Ac-10 Rongo Quadrangle of Ceres ∗ T. Platz a,b, , A. Nathues a, H.G. Sizemore b, D.A. Crown b, M. Hoffmann a, M. Schäfer a,c, N. Schmedemann d, T. Kneissl d, A. Neesemann d, S.C. Mest b, D.L. Buczkowski e, O. Ruesch f, K.H.G. Hughson g, A. Naß c, D.A. Williams h, F. Preusker c a Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany b Planetary Science Institute, 1700 E. Fort Lowell Rd., Suite 106, Tucson, AZ 85719-2395, USA c Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, 12489 Berlin, Germany d Planetary Sciences and Remote Sensing, Freie Universität Berlin, Malteserstr. 74-100, 12249 Berlin, Germany e Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA f NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA g University of California Los Angeles, Los Angeles, CA 90024, USA h School of Earth and Space Exploration, Arizona State University, Box 871404, Tempe, AZ 85287-1404, USA a r t i c l e i n f o a b s t r a c t Article history: The Dawn spacecraft arrived at dwarf planet Ceres in spring 2015 and imaged its surface from four suc- Received 18 January 2017 cessively lower polar orbits at ground sampling dimensions between ∼1.3 km/px and ∼35 m/px. To under- Revised 19 July 2017 stand the geological history of Ceres a mapping campaign was initiated to produce a set of 15 quadrangle- Accepted 1 August 2017 based geological maps using the highest-resolution Framing Camera imagery. -
Masterarbeit / Master's Thesis
MASTERARBEIT / MASTER’S THESIS Titel der Masterarbeit / Title of the Master‘s Thesis „Polygonal Impact Craters (PICs) on Rhea, Dione, Tethys, Ceres and Vesta“ verfasst von / submitted by Tanja Neidhart, BSc angestrebter akademischer Grad / in partial fulfilment of the requirements for the degree of Master of Science (MSc) Wien, 2018 / Vienna 2018 Studienkennzahl lt. Studienblatt / A 066 861 degree programme code as it appears on the student record sheet: Studienrichtung lt. Studienblatt / Astronomie degree programme as it appears on the student record sheet: Betreut von / Supervisor: Univ.-Prof. Dr. Maria Gertrude Firneis Contents Acknowledgements I List of Abbreviations IX 1 Introduction 1 1.1 Definition of a Polygonal Impact Crater (PIC) . 1 1.2 Overview ......................................... 2 1.3 Formation of Polygonal Impact Craters (PICs) . 3 2 Previous studies on Polygonal Impact Craters (PICs) 9 2.1 PICsonMercury..................................... 9 2.2 PICsonVenus ....................................... 12 2.3 PICsontheMoon ...................................... 15 2.4 PICsonMars......................................... 20 2.5 PICs on other Solar System bodies . 23 3 Data and Methods 29 4 Saturnian Satellites 33 4.1 Rhea............................................. 33 4.2 Dione ............................................. 35 4.3 Tethys........................................... 38 5 Asteroid Belt Objects 43 5.1 Ceres............................................ 43 5.2 Vesta............................................ 46 6 -
The Unique Geomorphology and Structural Geology of the Haulani Crater of Dwarf Planet Ceres As Revealed by Geological Mapping of Equatorial Quadrangle Ac-6 Haulani
ARTICLE IN PRESS JID: YICAR [m5G; October 10, 2017;10:56 ] Icarus 0 0 0 (2017) 1–15 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The unique geomorphology and structural geology of the Haulani crater of dwarf planet Ceres as revealed by geological mapping of equatorial quadrangle Ac-6 Haulani ∗ K. Krohn a, , R. Jaumann a,b, K.A. Otto a, F. Schulzeck a, A. Neesemann b, A. Nass a, K. Stephan a, F. Tosi c, R.J. Wagner a, F. Zambon c, I. von der Gathen a, D.A. Williams d, D.L. Buczkowski e, M.C. De Sanctis c, E. Kersten a, K.-D. Matz a, S.C. Mest f, C.M. Pieters g, F. Preusker a, T. Roatsch a, J.E.C. Scully h, C.T. Russell i, C.A. Raymond h a Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany b Freie Universität Berlin, Inst. of Geosciences, Planetology and Remote Sensing, Berlin, Germany c INAF-IAPS, National Institute for Astrophysics, Rome, Italy d School of Earth & Space Exploration, Arizona State University, Tempe, AZ, USA e JHU-APL, Laurel, MD, USA f Planetary Science Institute, Tucson, AZ, USA g Brown University, Providence, RI, USA h NASA JPL, California Institute of Technology, Pasadena, CA, USA i UCLA, Los Angeles, CA, USA a r t i c l e i n f o a b s t r a c t Article history: The dwarf planet Ceres has been explored by NASA’s Dawn spacecraft with the goal of characterizing its Received 8 August 2016 geology, mineralogy, topography, shape, and internal structure. -
Associated Societies
Associated Societies GSA has a long tradition of collaborating with a wide range of partners in pursuit of our mutual goals to advance the geosciences, enhance the professional growth of society members, and promote the geosciences in the service of humanity. GSA works with other organizations on many programs and services. AASP - The Palynological American Association of American Geophysical Union American Institute of American Quaternary American Rock Mechanics Society Petroleum Geologists (AAPG) (AGU) Professional Geologists (AIPG) Association (AMQUA) Association (ARMA) Association for the Sciences of American Water Resources Asociación Geológica Association for Women Association of American State Association of Earth Science Limnology and Oceanography Association (AWRA) Argentina (AGA) Geoscientists (AWG) Geologists (AASG) Editors (AESE) (ASLO) Association of Environmental Association of Geoscientists Blueprint Earth (BE) The Clay Minerals Society Colorado Scientific Society Council on Undergraduate & Engineering Geologists for International Development (CMS) (CSS) Research Geosciences Division (AEG) (AGID) (CUR) Cushman Foundation (CF) Environmental & Engineering European Association of European Geosciences Union Geochemical Society (GS) Geologica Belgica (GB) Geophysical Society (EEGS) Geoscientists & Engineers (EGU) (EAGE) Geological Association of Geological Society of Africa Geological Society of Australia Geological Society of China Geological Society of London Geological Society of South Canada (GAC) (GSAF) (GSAus) (GSC) (GSL) Africa (GSSA) Geologische Vereinigung (GV) Geoscience Information Society Geoscience Society of New Groundwater Resources History of Earth Sciences International Association for (GSIS) Zealand (GSNZ) Association of California Society (HESS) Geoscience Diversity (IAGD) (GRA) 100 2016 GSA Annual Meeting & Exposition As the Society looks to the future, it aims to build strong, meaningful partnerships with societies and organizations across the country and around the world in service to members and the larger geoscience community. -
Crater Morphologies and the Distribution of Ejecta Deposits on the Dwarf Planet Ceres
Dissertation zur Erlangung des akademischen Grades „doctor rerum naturalium“ (Dr. rer. nat.) Crater Morphologies and the Distribution of Ejecta Deposits on the Dwarf Planet Ceres vorgelegt von Dipl.-Geophysikerin Franziska Schulzeck im Fachbereich Geowissenschaften der Freien Universität Berlin Berlin, 2018 Erstgutachter: Prof. Dr. Ralf Jaumann Freie Universität Berlin Institut für Geologische Wissenschaften Fachrichtung Planetologie und Fernerkundung sowie Deutsches Zentrum für Luft- und Raumfahrt Institut für Planetenforschung, Abt. Planetengeologie Zweitgutachter: Prof. Dr. Lena Noack Freie Universität Berlin Institut für Geologische Wissenschaften Fachrichtung Geochemie, Hydrogeologie, Mineralogie Tag der Disputation: 19. November 2018 V EIDESSTATTLICHE ERKLÄRUNG Hiermit erkläre ich, dass ich die beigefügte Dissertation selbstständig verfasst und keine anderen als die angegebenen Hilfsmittel genutzt habe. Alle wörtlich oder inhaltlich übernommenen Stellen habe ich als solche gekennzeichnet. Ich versichere außerdem, dass ich die beigefügte Dissertation nur in diesem und keinem anderen Promotionsverfahren eingereicht habe und, dass diesem Promotionsverfahren keine endgültig gescheiterten Promotionsverfahren vorausgegangen sind. Berlin, 07. Dezember 2018 Franziska Schulzeck VII DANKSAGUNG Ich danke Herrn Prof. Dr. Ralf Jaumann und Frau Dr. Katrin Stephan für die Betreuung meiner Doktorarbeit und Frau Prof. Dr. Lena Noack für die Übernahme des Zweitgutachtens. Darüber hinaus danke ich allen Mitarbeitern der Abteilung Planetengeologie -
Accepted Manuscript
Accepted Manuscript Compositional differences among Bright Spots on the Ceres surface E. Palomba , A. Longobardo , M.C. De Sanctis , N.T. Stein , B. Ehlmann , A. Galiano , A. Raponi , M. Ciarniello , E. Ammannito , E. Cloutis , F.G. Carrozzo , M.T. Capria , K. Stephan , F. Zambon , F. Tosi , C.A. Raymond , C.T. Russell PII: S0019-1035(17)30313-5 DOI: 10.1016/j.icarus.2017.09.020 Reference: YICAR 12616 To appear in: Icarus Received date: 26 April 2017 Revised date: 8 September 2017 Accepted date: 18 September 2017 Please cite this article as: E. Palomba , A. Longobardo , M.C. De Sanctis , N.T. Stein , B. Ehlmann , A. Galiano , A. Raponi , M. Ciarniello , E. Ammannito , E. Cloutis , F.G. Carrozzo , M.T. Capria , K. Stephan , F. Zambon , F. Tosi , C.A. Raymond , C.T. Russell , Compositional differences among Bright Spots on the Ceres surface, Icarus (2017), doi: 10.1016/j.icarus.2017.09.020 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. ACCEPTED MANUSCRIPT Highlights A catalogue of bright spots on Ceres is presented Scatterplot analysis of 2.7,3.1, 3.4, 4 m band depth for each bright spot is presented Compositional difference between bright spots is discussed Some Peculiar Bright spots are discussed in detail A path for formation and evolution of Bright Spots on Ceres is proposed ACCEPTED MANUSCRIPT ACCEPTED MANUSCRIPT Compositional differences among Bright Spots on the Ceres surface E.