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De Sanctis MC, Ammannito E, McSween HY, Raponi A, Marchi S, Capaccioni F, Capria MT, Carrozzo FG, Ciarniello M, Fonte S, Formisano M, Frigeri A, Giardino M, Longobardo A, Magni G, McFadden LA, Palomba E, Pieters CM, Tosi F, Zambon F, Raymond CA, Russell CT. Localized aliphatic organic material on the surface of Ceres. Science 2017; 355:719-722. [PMID: 28209893 DOI: 10.1126/science.aaj2305] [Citation(s) in RCA: 132] [Impact Index Per Article: 18.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/16/2016] [Accepted: 01/17/2017] [Indexed: 11/02/2022]
Abstract
Organic compounds occur in some chondritic meteorites, and their signatures on solar system bodies have been sought for decades. Spectral signatures of organics have not been unambiguously identified on the surfaces of asteroids, whereas they have been detected on cometary nuclei. Data returned by the Visible and InfraRed Mapping Spectrometer on board the Dawn spacecraft show a clear detection of an organic absorption feature at 3.4 micrometers on dwarf planet Ceres. This signature is characteristic of aliphatic organic matter and is mainly localized on a broad region of ~1000 square kilometers close to the ~50-kilometer Ernutet crater. The combined presence on Ceres of ammonia-bearing hydrated minerals, water ice, carbonates, salts, and organic material indicates a very complex chemical environment, suggesting favorable environments to prebiotic chemistry.
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Affiliation(s)
- M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - E Ammannito
- Earth Planetary and Space Sciences, University of California-Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA.,Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - 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
| | - S Marchi
- Southwest Research Institute, Boulder, CO 80302, USA.,Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - 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
| | - F G Carrozzo
- 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
| | - S Fonte
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - M Formisano
- 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
| | - M Giardino
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - A Longobardo
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - G Magni
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - 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
- Brown University, Department of Earth, Environmental, and Planetary Sciences, Providence, RI 02912, USA
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - F Zambon
- Istituto di Astrofisica e Planetologia Spaziali-Istituto Nazionale di Astrofisica, 00133 Roma, Italy
| | - C A Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA
| | - 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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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] [What about the content of this article? (0)] [Affiliation(s)] [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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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] [What about the content of this article? (0)] [Affiliation(s)] [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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Pieters CM, Ammannito E, Blewett DT, Denevi BW, De Sanctis MC, Gaffey MJ, Le Corre L, Li JY, Marchi S, McCord TB, McFadden LA, Mittlefehldt DW, Nathues A, Palmer E, Reddy V, Raymond CA, Russell CT. Distinctive space weathering on Vesta from regolith mixing processes. Nature 2012; 491:79-82. [PMID: 23128227 DOI: 10.1038/nature11534] [Citation(s) in RCA: 105] [Impact Index Per Article: 8.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/17/2012] [Accepted: 08/20/2012] [Indexed: 11/09/2022]
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Denevi BW, Blewett DT, Buczkowski DL, Capaccioni F, Capria MT, De Sanctis MC, Garry WB, Gaskell RW, Le Corre L, Li JY, Marchi S, McCoy TJ, Nathues A, O’Brien DP, Petro NE, Pieters CM, Preusker F, Raymond CA, Reddy V, Russell CT, Schenk P, Scully JEC, Sunshine JM, Tosi F, Williams DA, Wyrick D. Pitted Terrain on Vesta and Implications for the Presence of Volatiles. Science 2012; 338:246-9. [DOI: 10.1126/science.1225374] [Citation(s) in RCA: 86] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- B. W. Denevi
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - D. T. Blewett
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - D. L. Buczkowski
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - F. Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | - M. T. Capria
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | - M. C. De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | - W. B. Garry
- Planetary Science Institute, Tucson, AZ, USA
| | | | - L. Le Corre
- Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
| | - J.-Y. Li
- Planetary Science Institute, Tucson, AZ, USA
- University of Maryland, College Park, MD, USA
| | - S. Marchi
- NASA Lunar Science Institute, Boulder, CO, USA
| | - T. J. McCoy
- National Museum of Natural History, Smithsonian Institution, Washington, DC, USA
| | - A. Nathues
- Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
| | | | - N. E. Petro
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | | | - F. Preusker
- Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Institute of Planetary Research, Berlin, Germany
| | - C. A. Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - V. Reddy
- Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
- University of North Dakota, Grand Forks, ND, USA
| | | | - P. Schenk
- Lunar and Planetary Institute, Houston, TX, USA
| | | | | | - F. Tosi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy
| | | | - D. Wyrick
- Southwest Research Institute, San Antonio, TX, USA
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Mustard JF, Erard S, Bibring JP, Head JW, Hurtrez S, Langevin Y, Pieters CM, Sotin CJ. The surface of Syrtis Major: Composition of the volcanic substrate and mixing with altered dust and soil. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/92je02682] [Citation(s) in RCA: 103] [Impact Index Per Article: 8.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Lucey PG, Hawke BR, Pieters CM, Head JW, McCord TB. A compositional study of the Aristarchus Region of the Moon using near-infrared reflectance spectroscopy. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb091ib04p0d344] [Citation(s) in RCA: 80] [Impact Index Per Article: 6.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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De Sanctis MC, Ammannito E, Capria MT, Tosi F, Capaccioni F, Zambon F, Carraro F, Fonte S, Frigeri A, Jaumann R, Magni G, Marchi S, McCord TB, McFadden LA, McSween HY, Mittlefehldt DW, Nathues A, Palomba E, Pieters CM, Raymond CA, Russell CT, Toplis MJ, Turrini D. Spectroscopic characterization of mineralogy and its diversity across Vesta. Science 2012; 336:697-700. [PMID: 22582257 DOI: 10.1126/science.1219270] [Citation(s) in RCA: 216] [Impact Index Per Article: 18.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The mineralogy of Vesta, based on data obtained by the Dawn spacecraft's visible and infrared spectrometer, is consistent with howardite-eucrite-diogenite meteorites. There are considerable regional and local variations across the asteroid: Spectrally distinct regions include the south-polar Rheasilvia basin, which displays a higher diogenitic component, and equatorial regions, which show a higher eucritic component. The lithologic distribution indicates a deeper diogenitic crust, exposed after excavation by the impact that formed Rheasilvia, and an upper eucritic crust. Evidence for mineralogical stratigraphic layering is observed on crater walls and in ejecta. This is broadly consistent with magma-ocean models, but spectral variability highlights local variations, which suggests that the crust can be a complex assemblage of eucritic basalts and pyroxene cumulates. Overall, Vesta mineralogy indicates a complex magmatic evolution that led to a differentiated crust and mantle.
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Affiliation(s)
- M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy.
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Jaumann R, Williams DA, Buczkowski DL, Yingst RA, Preusker F, Hiesinger H, Schmedemann N, Kneissl T, Vincent JB, Blewett DT, Buratti BJ, Carsenty U, Denevi BW, De Sanctis MC, Garry WB, Keller HU, Kersten E, Krohn K, Li JY, Marchi S, Matz KD, McCord TB, McSween HY, Mest SC, Mittlefehldt DW, Mottola S, Nathues A, Neukum G, O’Brien DP, Pieters CM, Prettyman TH, Raymond CA, Roatsch T, Russell CT, Schenk P, Schmidt BE, Scholten F, Stephan K, Sykes MV, Tricarico P, Wagner R, Zuber MT, Sierks H. Vesta’s Shape and Morphology. Science 2012; 336:687-90. [PMID: 22582254 DOI: 10.1126/science.1219122] [Citation(s) in RCA: 195] [Impact Index Per Article: 16.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- R. Jaumann
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
- Freie Universität Berlin, Planetary Sciences, Germany
| | | | - D. L. Buczkowski
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - R. A. Yingst
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - F. Preusker
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - H. Hiesinger
- Westfälische Wilhelms-Universität Münster, Germany
| | | | - T. Kneissl
- Freie Universität Berlin, Planetary Sciences, Germany
| | - J. B. Vincent
- Max Planck Institute for Solar System Research (MPS), Katlenburg-Lindau, Germany
| | - D. T. Blewett
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - B. J. Buratti
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - U. Carsenty
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - B. W. Denevi
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - M. C. De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Roma, Italy
| | - W. B. Garry
- Planetary Science Institute, Tucson, AZ 85719, USA
| | | | - E. Kersten
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - K. Krohn
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - J.-Y. Li
- University of Maryland, College Park, MD 20742, USA
| | - S. Marchi
- National Aeronautics and Space Administration (NASA) Lunar Science Institute, Boulder, CO 80309, USA
| | - K. D. Matz
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | | | - H. Y. McSween
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA
| | - S. C. Mest
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - D. W. Mittlefehldt
- Astromaterials Research Office, NASA Johnson Space Center, Houston, TX 77058, USA
| | - S. Mottola
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - A. Nathues
- Max Planck Institute for Solar System Research (MPS), Katlenburg-Lindau, Germany
| | - G. Neukum
- Freie Universität Berlin, Planetary Sciences, Germany
| | | | - C. M. Pieters
- Brown University, Planetary Geosciences Department, Providence, RI 02912, USA
| | | | - C. A. Raymond
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - T. Roatsch
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - C. T. Russell
- Institute of Geophysics and Planetary Physics, University of California Los Angeles (UCLA), Los Angeles, CA 90095, USA
| | - P. Schenk
- Lunar and Planetary Institute, Houston, TX 77058, USA
| | - B. E. Schmidt
- Institute for Geophysics, University of Texas, Austin, TX 78712, USA
| | - F. Scholten
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - K. Stephan
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - M. V. Sykes
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - P. Tricarico
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - R. Wagner
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - M. T. Zuber
- Massachusetts Institute of Technology, Cambridge, MA 02139,USA
| | - H. Sierks
- Max Planck Institute for Solar System Research (MPS), Katlenburg-Lindau, Germany
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10
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Hicks MD, Buratti BJ, Nettles J, Staid M, Sunshine J, Pieters CM, Besse S, Boardman J. A photometric function for analysis of lunar images in the visual and infrared based on Moon Mineralogy Mapper observations. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003733] [Citation(s) in RCA: 34] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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11
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Boardman JW, Pieters CM, Green RO, Lundeen SR, Varanasi P, Nettles J, Petro N, Isaacson P, Besse S, Taylor LA. Measuring moonlight: An overview of the spatial properties, lunar coverage, selenolocation, and related Level 1B products of the Moon Mineralogy Mapper. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003730] [Citation(s) in RCA: 84] [Impact Index Per Article: 6.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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12
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McCord TB, Taylor LA, Combe JP, Kramer G, Pieters CM, Sunshine JM, Clark RN. Sources and physical processes responsible for OH/H2O in the lunar soil as revealed by the Moon Mineralogy Mapper (M3). ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003711] [Citation(s) in RCA: 89] [Impact Index Per Article: 6.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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13
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Nozette S, Rustan P, Pleasance LP, Kordas JF, Lewis IT, Park HS, Priest RE, Horan DM, Regeon P, Lichtenberg CL, Shoemaker EM, Eliason EM, McEwen AS, Robinson MS, Spudis PD, Acton CH, Buratti BJ, Duxbury TC, Baker DN, Jakosky BM, Blamont JE, Corson MP, Resnick JH, Rollins CJ, Davies ME, Lucey PG, Malaret E, Massie MA, Pieters CM, Reisse RA, Simpson RA, Smith DE, Sorenson TC, Breugge RW, Zuber MT. The clementine mission to the moon: scientific overview. Science 2010; 266:1835-9. [PMID: 17737076 DOI: 10.1126/science.266.5192.1835] [Citation(s) in RCA: 293] [Impact Index Per Article: 20.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
In the course of 71 days in lunar orbit, from 19 February to 3 May 1994, the Clementine spacecraft acquired just under two million digital images of the moon at visible and infrared wavelengths. These data are enabling the global mapping of the rock types of the lunar crust and the first detailed investigation of the geology of the lunar polar regions and the lunar far side. In addition, laser-ranging measurements provided the first view of the global topographic figure of the moon. The topography of many ancient impact basins has been measured, and a global map of the thickness of the lunar crust has been derived from the topography and gravity.
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14
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Abstract
Reflectance spectra (0.3 to 2.6 micrometers) of 14 C, G, B, and F asteroids and 21 carbonaceous chondrite powders are compared in detail. Only three thermally metamorphosed CM-Cl chondrites that have a weak ultraviolet absorption are shown to have close counterparts among those asteroids. Reflectance spectra of heated Murchison CM2 chondrite are compared with the average C and G type asteroid spectra. Murchison heated at 600 degrees to 1000 degrees C exhibits a similar weak ultraviolet absorption and provides the best analog for those spectra. Comparison of ultraviolet absorption strengths between 160 C, G, B, and F asteroids and carbonaceous chondrites suggests that surface minerals of most of those asteroids are thermally metamorphosed at temperatures around 600 degrees to 1000 degrees C.
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15
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Pieters CM, Goswami JN, Clark RN, Annadurai M, Boardman J, Buratti B, Combe JP, Dyar MD, Green R, Head JW, Hibbitts C, Hicks M, Isaacson P, Klima R, Kramer G, Kumar S, Livo E, Lundeen S, Malaret E, McCord T, Mustard J, Nettles J, Petro N, Runyon C, Staid M, Sunshine J, Taylor LA, Tompkins S, Varanasi P. Character and Spatial Distribution of OH/H2O on the Surface of the Moon Seen by M3 on Chandrayaan-1. Science 2009; 326:568-72. [DOI: 10.1126/science.1178658] [Citation(s) in RCA: 497] [Impact Index Per Article: 33.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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16
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Pieters CM, Head JW, Gaddis L, Jolliff B, Duke M. Rock types of South Pole-Aitken basin and extent of basaltic volcanism. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001414] [Citation(s) in RCA: 144] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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Abstract
A new type of carbonaceous chondrite, the Tagish Lake meteorite, exhibits a reflectance spectrum similar to spectra observed from the D-type asteroids, which are relatively abundant in the outer solar system beyond the main asteroid belt and have been inferred to be more primitive than any known meteorite. Until the Tagish Lake fall, these asteroids had no analog in the meteorite collections. The Tagish Lake meteorite is a carbon-rich (4 to 5 weight %), aqueously altered carbonaceous chondrite and contains high concentrations of presolar grains and carbonate minerals, which is consistent with the expectation that the D-type asteroids were originally made of primitive materials and did not experience any extensive heating.
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Affiliation(s)
- T Hiroi
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA.
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18
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Clark BC, Baker AL, Cheng AF, Clemett SJ, McKay D, McSween HY, Pieters CM, Thomas P, Zolensky M. Survival of life on asteroids, comets and other small bodies. ORIGINS LIFE EVOL B 1999; 29:521-45. [PMID: 10573692 DOI: 10.1023/a:1006589213075] [Citation(s) in RCA: 24] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Abstract
The ability of living organisms to survive on the smaller bodies in our solar system is examined. The three most significant sterilizing effects include ionizing radiation, prolonged extreme vacuum, and relentless thermal inactivation. Each could be effectively lethal, and even more so in combination, if organisms at some time resided in the surfaces of airless small bodies located near or in the inner solar system. Deep within volatile-rich bodies, certain environments theoretically might provide protection of dormant organisms against these sterilizing factors. Sterility of surface materials to tens or hundreds of centimeters of depth appears inevitable, and to greater depths for bodies which have resided for long periods sunward of about 2 A.U.
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Affiliation(s)
- B C Clark
- Advanced Planetary Studies Group, Lockheed Martin Astronautics, Denver, CO, USA
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19
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Bishop JL, Koeberl C, Kralik C, Fröschl H, Englert PA, Andersen DW, Pieters CM, Wharton RA. Reflectance spectroscopy and geochemical analyses of Lake Hoare sediments, Antarctica: implications for remote sensing of the Earth and Mars. Geochim Cosmochim Acta 1996; 60:765-785. [PMID: 11539146 DOI: 10.1016/0016-7037(95)00432-7] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Visible to infrared reflectance spectroscopic analyses (0.3-25 micromoles) have been performed on sediments from the Dry Valleys region of Antarctica. Sample characterization for these sediments includes extensive geochemical analyses and X-ray diffraction (XRD). The reflectance spectra and XRD indicate major amounts of quartz, feldspar, and pyroxene in these samples and lesser amounts of carbonate, mica, chlorite, amphibole, illite, smectite, and organic matter. Calcite is the primary form of carbonate present in these Lake Hoare sediments based on the elemental abundances and spectroscopic features. The particle size distribution of the major and secondary components influences their detection in mixtures and this sensitivity to particle size is manifested differently in the "volume scattering" and "surface scattering" infrared regions. The Christiansen feature lies between these two spectral regimes and is influenced by the spectral properties of both regions. For these mixtures the Christiansen feature was found to be dependent on physical parameters, such as particle size and sample texture, as well as the mineralogy. Semiquantitative spectroscopic detection of calcite and organic material has been tested in these quartz- and feldspar-rich sediments. The relative spectral band depths due to organics and calcite correlate in general with the wt% C from organic matter and carbonate. The amounts of organic matter and carbonate present correlate with high Br and U abundances and high Ca and Sr abundances, respectively. Variation in the elemental abundances was overall minimal, which is consistent with a common sedimentary origin for the forty-two samples studied here from Lake Hoare.
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Affiliation(s)
- J L Bishop
- DLR, Institute for Planetary Exploration, Rudower Chausee, Berlin, Germany
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Bishop JL, Pieters CM, Burns RG, Edwards JO, Mancinelli RL, Fröschl H. Reflectance spectroscopy of ferric sulfate-bearing montmorillonites as Mars soil analog materials. Icarus 1995; 117:101-119. [PMID: 11538594 DOI: 10.1006/icar.1995.1145] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Spectroscopic analyses have shown that smectites enhanced in the laboratory with additional ferric species exhibit important similarities to those of the soils on Mars. Ferrihydrite in these chemically treated smectites has features in the visible to near-infrared region that resemble the energies and band strengths of features in reflectance spectra observed for several bright regions on Mars. New samples have been prepared with sulfate as well, because S was found by Viking to be a major component in the surface material on Mars. A suite of ferrihydrite-bearing and ferric sulfate-bearing montmorillonites, prepared with variable Fe3+ and S concentrations and variable pH conditions, has been analyzed using reflectance spectroscopy in the visible and infrared regions, Mössbauer spectroscopy at room temperature and 4 K, differential thermal analysis, and X-ray diffraction. These analyses support the formation of ferrihydrite of variable crystallinity in the ferrihydrite-bearing montmorillonites and a combination of schwertmannite and ferrihydrite in the ferric sulfate-bearing montmorillonites. Small quantities of poorly crystalline or nanophase forms of other ferric materials may also be present in these samples. The chemical formation conditions of the ferrihydrite-bearing and ferric sulfate-bearing montmorillonites influence the character of the low temperature Mössbauer sextets and the visible reflectance spectra. An absorption minimum is observed at 0.88-0.89 micrometers in spectra of the ferric sulfate-bearing samples, and at 0.89-0.92 micrometers in spectra of the ferrihydrate-bearing montmorillonites. Mössbauer spectra of the ferric sulfate-bearing montmorillonites indicate variable concentrations of ferrihydrite and schwertmannite in the interlaminar spaces and along grain surfaces. Dehydration under reduced atmospheric pressure conditions induces a greater effect on the adsorbed and interlayer water in ferrihydrite-bearing montmorillonite than on the water in ferric sulfate-bearing montmorillonite. Reflectance spectra of ferric sulfate-bearing montmorillonite include a strong 3-micrometers band that is more resistant to dry atmospheric conditions than the 3-micrometers band in spectra of similarly prepared ferrihydrite-bearing montmorillonites.
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Affiliation(s)
- J L Bishop
- Department of Chemistry and Geological Sciences, Brown University, Providence, Rhode Island 02912, USA
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Abstract
The ultraviolet-visible camera on the Clementine spacecraft obtained high-spatial resolution images of the moon in five spectral channels. Impact craters mapped with these multispectral images show a scale of lithologic diversity that varies with crater size and target stratigraphy. Prominent lithologic variations (feldspathic versus basaltic) occur within the south wall of Copernicus (93 kilometers in diameter) on the scale of 1 to 2 kilometers. Lithologic diversity at Tycho (85 kilometers in diameter) is less apparent at this scale, although the impact melt of these two large craters is remarkably similar in this spectral range. The lunar surface within and around the smaller crater Giordano Bruno (22 kilometers in diameter) is largely dominated by the mixing of freshly excavated material with surrounding older soils derived from a generally similar feldspathic lithology.
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Bishop JL, Pieters CM, Burns RG. Reflectance and Mossbauer spectroscopy of ferrihydrite-montmorillonite assemblages as Mars soil analog materials. Geochim Cosmochim Acta 1993; 57:4583-4595. [PMID: 11539454 DOI: 10.1016/0016-7037(93)90184-x] [Citation(s) in RCA: 18] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Spectroscopic analyses show that Fe(3+)-doped smectites prepared in the laboratory exhibit important similarities to the soils on Mars. Ferrihydrite has been identified as the interlayer ferric component in Fe(3+)-doped smectites by a low quadrupole splitting and magnetic field strength of approximately 48 tesla in Mossbauer spectra measured at 4.2 K, as well as a crystal field transition at 0.92 micrometer. Ferrihydrite in these smectites explains features in the visible-near infrared region that resemble the energies and band strengths of features in reflectance spectra observed for several bright regions on Mars. Clay silicates have met resistance in the past as Mars soil analogs because terrestrial clay silicates exhibit prominent hydrous spectral features at 1.4, 1.9, and 2.2 micrometers; and these are observed weakly, if at all, in reflectance spectra of Mars. However, several mechanisms can weaken or compress these features, including desiccation under low-humidity conditions. The hydration properties of the interlayer cations also effect band strengths, such that a ferrihydrite-bearing smectite in the Martian environment would exhibit a 1.9 micrometers H2O absorption that is even weaker than the 2.2 micrometers structural OH absorption. Mixing experiments demonstrate that infrared spectral features of clays can be significantly suppressed and that the reflectance can be significantly darkened by mixing with only a few percent of a strongly absorbing opaque material. Therefore, the absolute reflectance of a soil on Mars may be disproportionately sensitive to a minor component. For this reason, the shape and position of spectral features and the chemical composition of potential analogs are of utmost importance in assessing the composition of the soil on Mars. Given the remarkable similarity between visible-infrared reflectance spectra of soils in bright regions on Mars and Fe(3+)-doped montmorillonites, coupled with recent observations of smectites in SNC meteorites and a weak 2.2 micrometers absorption in some Mars soils, ferrihydrite-bearing smectites warrant serious consideration as a Mars soil analog.
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Affiliation(s)
- J L Bishop
- Department of Chemistry, Brown University, Providence, RI 02912, USA
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Belton MJ, Head JW, Pieters CM, Greeley R, McEwen AS, Neukum G, Klaasen KP, Anger CD, Carr MH, Chapman CR, Davies ME, Fanale FP, Gierasch PJ, Greenberg R, Ingersoll AP, Johnson T, Paczkowski B, Pilcher CB, Veverka J. Lunar Impact Basins and Crustal Heterogeneity: New Western Limb and Far Side Data from Galileo. Science 1992; 255:570-6. [PMID: 17792379 DOI: 10.1126/science.255.5044.570] [Citation(s) in RCA: 69] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Multispectral images of the lunar western limb and far side obtained from Galileo reveal the compositional nature of several prominent lunar features and provide new information on lunar evolution. The data reveal that the ejecta from the Orientale impact basin (900 kilometers in diameter) lying outside the Cordillera Mountains was excavated from the crust, not the mantle, and covers pre-Orientale terrain that consisted of both highland materials and relatively large expanses of ancient mare basalts. The inside of the far side South Pole-Aitken basin (>2000 kilometers in diameter) has low albedo, red color, and a relatively high abundance of iron- and magnesium-rich materials. These features suggest that the impact may have penetrated into the deep crust or lunar mantle or that the basin contains ancient mare basalts that were later covered by highlands ejecta.
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Pieters CM, Head JW, Pratt S, Patterson W, Garvin J, Barsukov VL, Basilevsky AT, Khodakovsky IL, Selivanov AS, Panfilov AS, Gektin YM, Narayeva YM. The Color of the Surface of Venus. Science 1986; 234:1379-83. [PMID: 17755059 DOI: 10.1126/science.234.4782.1379] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Multispectral images of the basaltic surface of Venus obtained by Venera 13 were processed to remove the effects of orange-colored incident radiation resulting from interactions with the thick Venusian atmosphere. At visible wavelengths the surface of Venus appears dark and without significant color. High-temperature laboratory reflectance spectra of basaltic materials indicate that these results are consistent with mineral assemblages bearing either ferric or ferrous iron. A high reflectance in the near-infrared region observed at neighboring Venera 9 and 10 sites, however, suggests that the basaltic surface material contains ferric minerals and thus may be relatively oxidized.
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McCord TB, Singer RB, Hawke BR, Adams JB, Evans DL, Head JW, Mouginis-Mark PJ, Pieters CM, Huguenin RL, Zisk SH. Mars: Definition and characterization of global surface units with emphasis on composition. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/jb087ib12p10129] [Citation(s) in RCA: 55] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Abstract
Olivine is identified as the major mafic mineral in a central peak of Copernicus crater. Information on the mineral assemblages of such unsampled lunar surface material is provided by near infrared reflectance spectra (0.7 to 2.5 micrometers) obtained with Earth-based telescopes. The composition of the deep-seated material comprising the Copernicus central peak is unique among measured areas. Other lunar terra areas and the wall of Copernicus exhibit spectral characteristics of mineral assemblages comparable to the feldspathic breccias returned by the Apollo missions, with low-calcium orthopyroxene being the major mafic mineral.
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