1
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Shi X, Castillo-Rogez J, Hsieh H, Hui H, Ip WH, Lei H, Li JY, Tosi F, Zhou L, Agarwal J, Barucci A, Beck P, Bagatin AC, Capaccioni F, Coates AJ, Cremonese G, Duffard R, Grande M, Jaumann R, Jones GH, Kallio E, Lin Y, Mousis O, Nathues A, Oberst J, Sierks H, Ulamec S, Wang M. GAUSS - genesis of asteroids and evolution of the solar system: A sample return mission to Ceres. EXPERIMENTAL ASTRONOMY 2021; 54:713-744. [PMID: 36915624 PMCID: PMC9998589 DOI: 10.1007/s10686-021-09800-1] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 07/30/2020] [Accepted: 09/23/2021] [Indexed: 06/18/2023]
Abstract
The goal of Project GAUSS (Genesis of Asteroids and evolUtion of the Solar System) is to return samples from the dwarf planet Ceres. Ceres is the most accessible candidate of ocean worlds and the largest reservoir of water in the inner Solar System. It shows active volcanism and hydrothermal activities in recent history. Recent evidence for the existence of a subsurface ocean on Ceres and the complex geochemistry suggest past habitability and even the potential for ongoing habitability. GAUSS will return samples from Ceres with the aim of answering the following top-level scientific questions: What is the origin of Ceres and what does this imply for the origin of water and other volatiles in the inner Solar System?What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of dwarf planets?What are the astrobiological implications of Ceres? Is it still habitable today?What are the mineralogical connections between Ceres and our current collections of carbonaceous meteorites?
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Affiliation(s)
- Xian Shi
- Max Planck Institute for Solar System Research, Göttingen, Germany
- Present Address: Shanghai Astronomical Observatory, Shanghai, China
| | | | | | - Hejiu Hui
- School of Earth Sciences and Engineering, Nanjing University, Nanjing, China
| | - Wing-Huen Ip
- Institute of Astronomy and Space Science, National Central University, Chung Li, Taiwan
| | - Hanlun Lei
- School of Astronomy and Space Science, Nanjing University, Nanjing, China
| | | | - Federico Tosi
- Istituto Nazionale di AstroFisica – Istituto di Astrofisica e Planetologia Spaziali (INAF-IAPS), Rome, Italy
| | - Liyong Zhou
- School of Astronomy and Space Science, Nanjing University, Nanjing, China
| | - Jessica Agarwal
- Max Planck Institute for Solar System Research, Göttingen, Germany
- Institute for Geophysics and Extraterrestrial Physics, Technical University Braunschweig, Braunschweig, Germany
| | - Antonella Barucci
- LESIA-Observatoire de Paris, Université PSL, CNRS, Université de Paris, Sorbonne Université, F-92195 Meudon, Principal Cedex, France
| | - Pierre Beck
- CNRS Institut de Planétologie et d’Astrophysique, Univ. Grenoble Alpes, Grenoble, France
| | - Adriano Campo Bagatin
- Universidad de Alicante, Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Alicante, Spain
| | - Fabrizio Capaccioni
- Istituto Nazionale di AstroFisica – Istituto di Astrofisica e Planetologia Spaziali (INAF-IAPS), Rome, Italy
| | - Andrew J. Coates
- Mullard Space Science Laboratory, University College London, Surrey, UK
| | | | - Rene Duffard
- Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain
| | | | - Ralf Jaumann
- Institute of Geological Sciences, Free University of Berlin, Berlin, Germany
| | - Geraint H. Jones
- Mullard Space Science Laboratory, University College London, Surrey, UK
| | - Esa Kallio
- School of Electrical Engineering, Aalto University, Aalto, Finland
| | - Yangting Lin
- Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | | | - Andreas Nathues
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - Jürgen Oberst
- DLR Institute of Planetary Research, Berlin, Germany
| | - Holger Sierks
- Max Planck Institute for Solar System Research, Göttingen, Germany
| | - Stephan Ulamec
- DLR Space Operations and Astronaut Training, Cologne, Germany
| | - Mingyuan Wang
- National Astronomical Observatory, Chinese Academy of Science, Beijing, China
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2
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Scully JEC, Schenk PM, Castillo-Rogez JC, Buczkowski DL, Williams DA, Pasckert JH, Duarte KD, Romero VN, Quick LC, Sori MM, Landis ME, Raymond CA, Neesemann A, Schmidt BE, Sizemore HG, Russell CT. The varied sources of faculae-forming brines in Ceres' Occator crater emplaced via hydrothermal brine effusion. Nat Commun 2020; 11:3680. [PMID: 32778642 PMCID: PMC7417532 DOI: 10.1038/s41467-020-15973-8] [Citation(s) in RCA: 30] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/16/2019] [Accepted: 04/06/2020] [Indexed: 11/23/2022] Open
Abstract
Before acquiring highest-resolution data of Ceres, questions remained about the emplacement mechanism and source of Occator crater's bright faculae. Here we report that brine effusion emplaced the faculae in a brine-limited, impact-induced hydrothermal system. Impact-derived fracturing enabled brines to reach the surface. The central faculae, Cerealia and Pasola Facula, postdate the central pit, and were primarily sourced from an impact-induced melt chamber, with some contribution from a deeper, pre-existing brine reservoir. Vinalia Faculae, in the crater floor, were sourced from the laterally extensive deep reservoir only. Vinalia Faculae are comparatively thinner and display greater ballistic emplacement than the central faculae because the deep reservoir brines took a longer path to the surface and contained more gas than the shallower impact-induced melt chamber brines. Impact-derived fractures providing conduits, and mixing of impact-induced melt with deeper endogenic brines, could also allow oceanic material to reach the surfaces of other large icy bodies.
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Affiliation(s)
- J E C Scully
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA.
| | - P M Schenk
- Lunar and Planetary Institute, Houston, TX, USA
| | - J C Castillo-Rogez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - D L Buczkowski
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - D A Williams
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - J H Pasckert
- Institute für Planetologie, University of Münster, Münster, Germany
| | - K D Duarte
- Georgia Institute of Technology, Atlanta, GA, USA
| | - V N Romero
- Georgia Institute of Technology, Atlanta, GA, USA
| | - L C Quick
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - M M Sori
- Lunar and Planetary Laboratory, Tucson, AZ, USA
| | - M E Landis
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, CO, USA
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - A Neesemann
- Free University of Berlin, 14195, Berlin, Germany
| | - B E Schmidt
- Georgia Institute of Technology, Atlanta, GA, USA
| | | | - C T Russell
- University of California, Los Angeles, CA, USA
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3
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Schenk P, Scully J, Buczkowski D, Sizemore H, Schmidt B, Pieters C, Neesemann A, O'Brien D, Marchi S, Williams D, Nathues A, De Sanctis M, Tosi F, Russell CT, Castillo-Rogez J, Raymond C. Impact heat driven volatile redistribution at Occator crater on Ceres as a comparative planetary process. Nat Commun 2020; 11:3679. [PMID: 32778649 PMCID: PMC7417549 DOI: 10.1038/s41467-020-17184-7] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/21/2019] [Accepted: 06/16/2020] [Indexed: 12/02/2022] Open
Abstract
Hydrothermal processes in impact environments on water-rich bodies such as Mars and Earth are relevant to the origins of life. Dawn mapping of dwarf planet (1) Ceres has identified similar deposits within Occator crater. Here we show using Dawn high-resolution stereo imaging and topography that Ceres' unique composition has resulted in widespread mantling by solidified water- and salt-rich mud-like impact melts with scattered endogenic pits, troughs, and bright mounds indicative of outgassing of volatiles and periglacial-style activity during solidification. These features are distinct from and less extensive than on Mars, indicating that Occator melts may be less gas-rich or volatiles partially inhibited from reaching the surface. Bright salts at Vinalia Faculae form thin surficial precipitates sourced from hydrothermal brine effusion at many individual sites, coalescing in several larger centers, but their ages are statistically indistinguishable from floor materials, allowing for but not requiring migration of brines from deep crustal source(s).
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Affiliation(s)
- P Schenk
- Lunar and Planetary Institute/USRA, Houston, TX, USA.
| | - J Scully
- Jet Propulsion Laboratory/Caltech, Pasadena, CA, USA
| | - D Buczkowski
- Johns Hopkins University-Applied Physics Laboratory, Laurel, MD, USA
| | - H Sizemore
- Planetary Science Institute, Tucson, AZ, USA
| | - B Schmidt
- Georgia Institute of Technology, Atlanta, GA, USA
| | - C Pieters
- Brown University Providence, Providence, RI, USA
| | | | - D O'Brien
- Planetary Science Institute, Tucson, AZ, USA
| | - S Marchi
- Southwest Research Institute, Boulder, CO, USA
| | - D Williams
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - A Nathues
- Max Planck Institute for Solar System Research, Goettingen, Germany
| | - M De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, INAF, Rome, Italy
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali, INAF, Rome, Italy
| | - C T Russell
- University of California, Los Angeles, CA, USA
| | | | - C Raymond
- Jet Propulsion Laboratory/Caltech, Pasadena, CA, USA
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4
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Castillo-Rogez JC, Neveu M, Scully JEC, House CH, Quick LC, Bouquet A, Miller K, Bland M, De Sanctis MC, Ermakov A, Hendrix AR, Prettyman TH, Raymond CA, Russell CT, Sherwood BE, Young E. Ceres: Astrobiological Target and Possible Ocean World. ASTROBIOLOGY 2020; 20:269-291. [PMID: 31904989 DOI: 10.1089/ast.2018.1999] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Ceres, the most water-rich body in the inner solar system after Earth, has recently been recognized to have astrobiological importance. Chemical and physical measurements obtained by the Dawn mission enabled the quantification of key parameters, which helped to constrain the habitability of the inner solar system's only dwarf planet. The surface chemistry and internal structure of Ceres testify to a protracted history of reactions between liquid water, rock, and likely organic compounds. We review the clues on chemical composition, temperature, and prospects for long-term occurrence of liquid and chemical gradients. Comparisons with giant planet satellites indicate similarities both from a chemical evolution standpoint and in the physical mechanisms driving Ceres' internal evolution.
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Affiliation(s)
| | - Marc Neveu
- Sciences and Exploration Directorate, NASA Goddard Space Flight Center, Greenbelt, Maryland
- University of Maryland College Park, Greenbelt, Maryland
| | - Jennifer E C Scully
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Christopher H House
- Department of Geosciences,Penn State Astrobiology Research Center, The Pennsylvania State University, University Park, Pennsylvania
| | - Lynnae C Quick
- Sciences and Exploration Directorate, NASA Goddard Space Flight Center, Greenbelt, Maryland
| | - Alexis Bouquet
- LAM (Laboratoire d'Astrophysique de Marseille), Aix Marseille Université, CNRS, UMR 7326, Marseille, France
| | - Kelly Miller
- Southwest Research Institute, San Antonio, Texas
| | | | | | - Anton Ermakov
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | | | - Carol A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | - Christopher T Russell
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California
| | | | - Edward Young
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California
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5
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Duarte KD, Schmidt BE, Chilton HT, Hughson KHG, Sizemore HG, Ferrier KL, Buffo JJ, Scully JEC, Nathues A, Platz T, Landis M, Byrne S, Bland M, Russell CT, Raymond CA. Landslides on Ceres: Diversity and Geologic Context. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2019; 124:3329-3343. [PMID: 32355585 PMCID: PMC7185231 DOI: 10.1029/2018je005673] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 05/06/2018] [Revised: 08/20/2019] [Accepted: 08/30/2019] [Indexed: 06/11/2023]
Abstract
Landslides are among the most widespread geologic features on Ceres. Using data from Dawn's Framing Camera, landslides were previously classified based upon geomorphologic characteristics into one of three archetypal categories, Type 1(T1), Type 2 (T2), and Type 3 (T3). Due to their geologic context, variation in age, and physical characteristics, most landslides on Ceres are, however, intermediate in their morphology and physical properties between the archetypes of each landslide class. Here we describe the varied morphology of individual intermediate landslides, identify geologic controls that contribute to this variation, and provide first-order quantification of the physical properties of the continuum of Ceres's surface flows. These intermediate flows appear in varied settings and show a range of characteristics, including those found at contacts between craters, those having multiple trunks or lobes; showing characteristics of both T2 and T3 landslides; material slumping on crater rims; very small, ejecta-like flows; and those appearing inside of catenae. We suggest that while their morphologies can vary, the distribution and mechanical properties of intermediate landslides do not differ significantly from that of archetypal landslides, confirming a link between landslides and subsurface ice. We also find that most intermediate landslides are similar to Type 2 landslides and formed by shallow failure. Clusters of these features suggest ice enhancement near Juling, Kupalo and Urvara craters. Since the majority of Ceres's landslides fall in the intermediate landslide category, placing their attributes in context contributes to a better understanding of Ceres's shallow subsurface and the nature of ground ice.
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Affiliation(s)
- K. D. Duarte
- School of Earth and Atmospheric SciencesGeorgia Institute of TechnologyAtlantaGAUSA
| | - B. E. Schmidt
- School of Earth and Atmospheric SciencesGeorgia Institute of TechnologyAtlantaGAUSA
| | - H. T. Chilton
- School of Earth and Atmospheric SciencesGeorgia Institute of TechnologyAtlantaGAUSA
| | - K. H. G. Hughson
- School of Earth and Atmospheric SciencesGeorgia Institute of TechnologyAtlantaGAUSA
- Institute of Geophysics and Planetary PhysicsUniversity of CaliforniaLos AngelesCAUSA
| | | | - K. L. Ferrier
- School of Earth and Atmospheric SciencesGeorgia Institute of TechnologyAtlantaGAUSA
| | - J. J. Buffo
- School of Earth and Atmospheric SciencesGeorgia Institute of TechnologyAtlantaGAUSA
| | - J. E. C. Scully
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - A. Nathues
- Max‐Planck Institute for Solar System ResearchKatlenburg‐LindauGermany
| | - T. Platz
- Max‐Planck Institute for Solar System ResearchKatlenburg‐LindauGermany
| | - M. Landis
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
- USGSFlagstaffAZUSA
| | - S. Byrne
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | - M. Bland
- Now at Boulder Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - C. T. Russell
- Institute of Geophysics and Planetary PhysicsUniversity of CaliforniaLos AngelesCAUSA
| | - C. A. Raymond
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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6
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Sizemore HG, Platz T, Schorghofer N, Prettyman TH, De Sanctis MC, Crown DA, Schmedemann N, Neesemann A, Kneissl T, Marchi S, Schenk PM, Bland MT, Schmidt BE, Hughson KHG, Tosi F, Zambon F, Mest SC, Yingst RA, Williams DA, Russell CT, Raymond CA. Pitted terrains on (1) Ceres and implications for shallow subsurface volatile distribution. GEOPHYSICAL RESEARCH LETTERS 2017; 44:6570-6578. [PMID: 28989206 PMCID: PMC5606497 DOI: 10.1002/2017gl073970] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 04/26/2017] [Revised: 06/19/2017] [Accepted: 06/22/2017] [Indexed: 06/07/2023]
Abstract
Prior to the arrival of the Dawn spacecraft at Ceres, the dwarf planet was anticipated to be ice-rich. Searches for morphological features related to ice have been ongoing during Dawn's mission at Ceres. Here we report the identification of pitted terrains associated with fresh Cerean impact craters. The Cerean pitted terrains exhibit strong morphological similarities to pitted materials previously identified on Mars (where ice is implicated in pit development) and Vesta (where the presence of ice is debated). We employ numerical models to investigate the formation of pitted materials on Ceres and discuss the relative importance of water ice and other volatiles in pit development there. We conclude that water ice likely plays an important role in pit development on Ceres. Similar pitted terrains may be common in the asteroid belt and may be of interest to future missions motivated by both astrobiology and in situ resource utilization.
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Affiliation(s)
| | - T. Platz
- Max Planck Institute for Solar System ResearchGöttingenGermany
| | | | | | | | | | - N. Schmedemann
- Department of Earth SciencesFreie Universität BerlinBerlinGermany
| | - A. Neesemann
- Department of Earth SciencesFreie Universität BerlinBerlinGermany
| | - T. Kneissl
- Department of Earth SciencesFreie Universität BerlinBerlinGermany
| | - S. Marchi
- Southwest Research InstituteBoulderColoradoUSA
| | | | - M. T. Bland
- USGS Astrogeology Science CenterFlagstaffArizonaUSA
| | - B. E. Schmidt
- Department of Planetary and Space PhysicsGeorgia Institute of TechnologyAtlantaGeorgiaUSA
| | - K. H. G. Hughson
- Department of Earth, Planetary, and Space SciencesUniversity of California Los AngelesLos AngelesCaliforniaUSA
| | - F. Tosi
- Istituto di Astrofisica e Planetologia Spaziali, INAFRomeItaly
| | - F. Zambon
- Istituto di Astrofisica e Planetologia Spaziali, INAFRomeItaly
| | - S. C. Mest
- Planetary Science InstituteTucsonArizonaUSA
| | | | - D. A. Williams
- School of Earth and Space SciencesArizona State UniversityTempeArizonaUSA
| | - C. T. Russell
- Department of Earth, Planetary, and Space SciencesUniversity of California Los AngelesLos AngelesCaliforniaUSA
| | - C. A. Raymond
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCaliforniaUSA
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7
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Russell CT, Raymond CA, Ammannito E, Buczkowski DL, De Sanctis MC, Hiesinger H, Jaumann R, Konopliv AS, McSween HY, Nathues A, Park RS, Pieters CM, Prettyman TH, McCord TB, McFadden LA, Mottola S, Zuber MT, Joy SP, Polanskey C, Rayman MD, Castillo-Rogez JC, Chi PJ, Combe JP, Ermakov A, Fu RR, Hoffmann M, Jia YD, King SD, Lawrence DJ, Li JY, Marchi S, Preusker F, Roatsch T, Ruesch O, Schenk P, Villarreal MN, Yamashita N. Dawn arrives at Ceres: Exploration of a small, volatile-rich world. Science 2017; 353:1008-1010. [PMID: 27701107 DOI: 10.1126/science.aaf4219] [Citation(s) in RCA: 161] [Impact Index Per Article: 23.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/04/2016] [Accepted: 07/13/2016] [Indexed: 11/02/2022]
Abstract
On 6 March 2015, Dawn arrived at Ceres to find a dark, desiccated surface punctuated by small, bright areas. Parts of Ceres' surface are heavily cratered, but the largest expected craters are absent. Ceres appears gravitationally relaxed at only the longest wavelengths, implying a mechanically strong lithosphere with a weaker deep interior. Ceres' dry exterior displays hydroxylated silicates, including ammoniated clays of endogenous origin. The possibility of abundant volatiles at depth is supported by geomorphologic features such as flat crater floors with pits, lobate flows of materials, and a singular mountain that appears to be an extrusive cryovolcanic dome. On one occasion, Ceres temporarily interacted with the solar wind, producing a bow shock accelerating electrons to energies of tens of kilovolts.
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Affiliation(s)
- C T Russell
- Earth Planetary and Space Sciences, University of California, Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA.
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - E Ammannito
- Earth Planetary and Space Sciences, University of California, Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - D L Buczkowski
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723-6099, USA
| | - M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - H Hiesinger
- Institut für Planetologie, 48149 Münster, Germany
| | - R Jaumann
- Deutsches Zentrum fur Luft-und Raumfahrt, Institute of Planetary Research, 12489 Berlin, Germany
| | - A S Konopliv
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - H Y McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA
| | - A Nathues
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - R S Park
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - C M Pieters
- Brown University, Department of Earth, Environmental, and Planetary Sciences, Providence, RI 02912, USA
| | | | - T B McCord
- The Bear Fight Institute, Winthrop, WA 98862, USA
| | - L A McFadden
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - S Mottola
- Deutsches Zentrum fur Luft-und Raumfahrt, Institute of Planetary Research, 12489 Berlin, Germany
| | - M T Zuber
- Massachussetts Institute of Technology, Cambridge, MA 02139, USA
| | - S P Joy
- Earth Planetary and Space Sciences, University of California, Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - C Polanskey
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - M D Rayman
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - J C Castillo-Rogez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - P J Chi
- Earth Planetary and Space Sciences, University of California, Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - J P Combe
- The Bear Fight Institute, Winthrop, WA 98862, USA
| | - A Ermakov
- Massachussetts Institute of Technology, Cambridge, MA 02139, USA
| | - R R Fu
- Lamont-Doherty Earth Observatory, Columbia University, Palisades, NY 10968, USA
| | - M Hoffmann
- Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
| | - Y D Jia
- Earth Planetary and Space Sciences, University of California, Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - S D King
- Virginia Tech, Geosciences, Blacksburg, VA 24061, USA
| | - D J Lawrence
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723-6099, USA
| | - J-Y Li
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - S Marchi
- Southwest Research Institute, Boulder, CO 80302, USA
| | - F Preusker
- Deutsches Zentrum fur Luft-und Raumfahrt, Institute of Planetary Research, 12489 Berlin, Germany
| | - T Roatsch
- Deutsches Zentrum fur Luft-und Raumfahrt, Institute of Planetary Research, 12489 Berlin, Germany
| | - O Ruesch
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - P Schenk
- Lunar and Planetary Institute, Houston, TX 77058, USA
| | - M N Villarreal
- Earth Planetary and Space Sciences, University of California, Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - N Yamashita
- Planetary Science Institute, Tucson, AZ 85719, USA
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8
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Hiesinger H, Marchi S, Schmedemann N, Schenk P, Pasckert JH, Neesemann A, O'Brien DP, Kneissl T, Ermakov AI, Fu RR, Bland MT, Nathues A, Platz T, Williams DA, Jaumann R, Castillo-Rogez JC, Ruesch O, Schmidt B, Park RS, Preusker F, Buczkowski DL, Russell CT, Raymond CA. Cratering on Ceres: Implications for its crust and evolution. Science 2016; 353:353/6303/aaf4759. [PMID: 27701089 DOI: 10.1126/science.aaf4759] [Citation(s) in RCA: 125] [Impact Index Per Article: 15.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/14/2016] [Accepted: 07/29/2016] [Indexed: 11/02/2022]
Abstract
Thermochemical models have predicted that Ceres, is to some extent, differentiated and should have an icy crust with few or no impact craters. We present observations by the Dawn spacecraft that reveal a heavily cratered surface, a heterogeneous crater distribution, and an apparent absence of large craters. The morphology of some impact craters is consistent with ice in the subsurface, which might have favored relaxation, yet large unrelaxed craters are also present. Numerous craters exhibit polygonal shapes, terraces, flowlike features, slumping, smooth deposits, and bright spots. Crater morphology and simple-to-complex crater transition diameters indicate that the crust of Ceres is neither purely icy nor rocky. By dating a smooth region associated with the Kerwan crater, we determined absolute model ages (AMAs) of 550 million and 720 million years, depending on the applied chronology model.
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Affiliation(s)
- H Hiesinger
- Institut für Planetologie, Westfälische Wilhelms-Universität, Münster, Germany.
| | - S Marchi
- Southwest Research Institute, Boulder, CO 80302, USA
| | - N Schmedemann
- Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany
| | - P Schenk
- Lunar and Planetary Institute, Houston, TX 77058, USA
| | - J H Pasckert
- Institut für Planetologie, Westfälische Wilhelms-Universität, Münster, Germany
| | - A Neesemann
- Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany
| | - D P O'Brien
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - T Kneissl
- Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany
| | - A I Ermakov
- Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - R R Fu
- Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - M T Bland
- U.S. Geological Survey, Astrogeology Science Center, Flagstaff, AZ 86001, USA
| | - A Nathues
- Max-Planck Institute for Solar System Research, Göttingen, Germany
| | - T Platz
- Max-Planck Institute for Solar System Research, Göttingen, Germany
| | | | - R Jaumann
- German Aerospace Center (DLR), Berlin, Germany. Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany
| | - J C Castillo-Rogez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - O Ruesch
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - B Schmidt
- Georgia Institute of Technology, Atlanta, GA 30332, USA
| | - R S Park
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - F Preusker
- German Aerospace Center (DLR), Berlin, Germany
| | - D L Buczkowski
- John Hopkins Applied Physics Laboratory, Laurel, MD 20723, USA
| | - C T Russell
- Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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9
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Ruesch O, Platz T, Schenk P, McFadden LA, Castillo-Rogez JC, Quick LC, Byrne S, Preusker F, O’Brien DP, Schmedemann N, Williams DA, Li JY, Bland MT, Hiesinger H, Kneissl T, Neesemann A, Schaefer M, Pasckert JH, Schmidt BE, Buczkowski DL, Sykes MV, Nathues A, Roatsch T, Hoffmann M, Raymond CA, Russell CT. Cryovolcanism on Ceres. Science 2016; 353:353/6303/aaf4286. [DOI: 10.1126/science.aaf4286] [Citation(s) in RCA: 145] [Impact Index Per Article: 18.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/05/2016] [Accepted: 07/20/2016] [Indexed: 11/02/2022]
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10
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Combe JP, McCord TB, Tosi F, Ammannito E, Carrozzo FG, De Sanctis MC, Raponi A, Byrne S, Landis ME, Hughson KHG, Raymond CA, Russell CT. Detection of local H2O exposed at the surface of Ceres. Science 2016; 353:353/6303/aaf3010. [PMID: 27701085 DOI: 10.1126/science.aaf3010] [Citation(s) in RCA: 116] [Impact Index Per Article: 14.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/05/2016] [Accepted: 06/22/2016] [Indexed: 01/10/2023]
Abstract
The surface of dwarf planet Ceres contains hydroxyl-rich materials. Theories predict a water ice-rich mantle, and water vapor emissions have been observed, yet no water (H2O) has been previously identified. The Visible and InfraRed (VIR) mapping spectrometer onboard the Dawn spacecraft has now detected water absorption features within a low-illumination, highly reflective zone in Oxo, a 10-kilometer, geologically fresh crater, on five occasions over a period of 1 month. Candidate materials are H2O ice and mineral hydrates. Exposed H2O ice would become optically undetectable within tens of years under current Ceres temperatures; consequently, only a relatively recent exposure or formation of H2O would explain Dawn's findings. Some mineral hydrates are stable on geological time scales, but their formation would imply extended contact with ice or liquid H2O.
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Affiliation(s)
- Jean-Philippe Combe
- Bear Fight Institute, 22 Fiddler's Road, P.O. Box 667, Winthrop, WA 98862, USA.
| | - Thomas B McCord
- Bear Fight Institute, 22 Fiddler's Road, P.O. Box 667, Winthrop, WA 98862, USA
| | - Federico Tosi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Rome, Italy
| | - Eleonora Ammannito
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Rome, Italy. Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA, USA
| | | | | | - Andrea Raponi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, Rome, Italy
| | - Shane Byrne
- Lunar and Planetary Laboratory, Tucson, AZ, USA
| | | | - Kynan H G Hughson
- Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA, USA
| | | | - Christopher T Russell
- Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA, USA
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11
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Ammannito E, DeSanctis MC, Ciarniello M, Frigeri A, Carrozzo FG, Combe JP, Ehlmann BL, Marchi S, McSween HY, Raponi A, Toplis MJ, Tosi F, Castillo-Rogez JC, Capaccioni F, Capria MT, Fonte S, Giardino M, Jaumann R, Longobardo A, Joy SP, Magni G, McCord TB, McFadden LA, Palomba E, Pieters CM, Polanskey CA, Rayman MD, Raymond CA, Schenk PM, Zambon F, Russell CT. Distribution of phyllosilicates on the surface of Ceres. Science 2016; 353:353/6303/aaf4279. [PMID: 27701086 DOI: 10.1126/science.aaf4279] [Citation(s) in RCA: 146] [Impact Index Per Article: 18.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/05/2016] [Accepted: 07/29/2016] [Indexed: 11/02/2022]
Abstract
The dwarf planet Ceres is known to host phyllosilicate minerals at its surface, but their distribution and origin have not previously been determined. We used the spectrometer onboard the Dawn spacecraft to map their spatial distribution on the basis of diagnostic absorption features in the visible and near-infrared spectral range (0.25 to 5.0 micrometers). We found that magnesium- and ammonium-bearing minerals are ubiquitous across the surface. Variations in the strength of the absorption features are spatially correlated and indicate considerable variability in the relative abundance of the phyllosilicates, although their composition is fairly uniform. These data, along with the distinctive spectral properties of Ceres relative to other asteroids and carbonaceous meteorites, indicate that the phyllosilicates were formed endogenously by a globally widespread and extensive alteration process.
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Affiliation(s)
- E Ammannito
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA.
| | - M C DeSanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Ciarniello
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - A Frigeri
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F G Carrozzo
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - J-Ph Combe
- The Bear Fight Institute, Winthrop, WA 98862, USA
| | - B L Ehlmann
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - S Marchi
- Southwest Research Institute, Boulder, CO 80302, USA
| | - H Y McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA
| | - A Raponi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M J Toplis
- Institut de Recherche en Astrophysique et Planétologie (UMR 5277), Université de Toulouse, F-31400 Toulouse, France
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - J C Castillo-Rogez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - F Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M T Capria
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S Fonte
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Giardino
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - R Jaumann
- Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt, 12489 Berlin, Germany
| | - A Longobardo
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - S P Joy
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - G Magni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - T B McCord
- The Bear Fight Institute, Winthrop, WA 98862, USA
| | - L A McFadden
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C M Pieters
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - C A Polanskey
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - M D Rayman
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - P M Schenk
- Lunar and Planetary Institute, Houston, TX 77058, USA
| | - F Zambon
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C T Russell
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
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12
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Skibba R. Giant ice volcano spotted on dwarf planet Ceres. Nature 2016. [DOI: 10.1038/nature.2016.20526] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/21/2022]
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