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  • 1
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    Color and albedo heterogeneity of Vesta from Dawn (2012)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2012-05-15
    Description: Multispectral images (0.44 to 0.98 mum) of asteroid (4) Vesta obtained by the Dawn Framing Cameras reveal global color variations that uncover and help understand the north-south hemispherical dichotomy. The signature of deep lithologies excavated during the formation of the Rheasilvia basin on the south pole has been preserved on the surface. Color variations (band depth, spectral slope, and eucrite-diogenite abundance) clearly correlate with distinct compositional units. Vesta displays the greatest variation of geometric albedo (0.10 to 0.67) of any asteroid yet observed. Four distinct color units are recognized that chronicle processes--including impact excavation, mass wasting, and space weathering--that shaped the asteroid's surface. Vesta's color and photometric diversity are indicative of its status as a preserved, differentiated protoplanet.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Reddy, Vishnu -- Nathues, Andreas -- Le Corre, Lucille -- Sierks, Holger -- Li, Jian-Yang -- Gaskell, Robert -- McCoy, Timothy -- Beck, Andrew W -- Schroder, Stefan E -- Pieters, Carle M -- Becker, Kris J -- Buratti, Bonnie J -- Denevi, Brett -- Blewett, David T -- Christensen, Ulrich -- Gaffey, Michael J -- Gutierrez-Marques, Pablo -- Hicks, Michael -- Keller, Horst Uwe -- Maue, Thorsten -- Mottola, Stefano -- McFadden, Lucy A -- McSween, Harry Y -- Mittlefehldt, David -- O'Brien, David P -- Raymond, Carol -- Russell, Christopher -- New York, N.Y. -- Science. 2012 May 11;336(6082):700-4. doi: 10.1126/science.1219088.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max Planck Institute for Solar System Research, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany. reddy@mps.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22582258" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 2
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    Dark material on Vesta from the infall of carbonaceous volatile-rich material (2012)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2012-11-07
    Description: Localized dark and bright materials, often with extremely different albedos, were recently found on Vesta's surface. The range of albedos is among the largest observed on Solar System rocky bodies. These dark materials, often associated with craters, appear in ejecta and crater walls, and their pyroxene absorption strengths are correlated with material brightness. It was tentatively suggested that the dark material on Vesta could be either exogenic, from carbon-rich, low-velocity impactors, or endogenic, from freshly exposed mafic material or impact melt, created or exposed by impacts. Here we report Vesta spectra and images and use them to derive and interpret the properties of the 'pure' dark and bright materials. We argue that the dark material is mainly from infall of hydrated carbonaceous material (like that found in a major class of meteorites and some comet surfaces), whereas the bright material is the uncontaminated indigenous Vesta basaltic soil. Dark material from low-albedo impactors is diffused over time through the Vestan regolith by impact mixing, creating broader, diffuse darker regions and finally Vesta's background surface material. This is consistent with howardite-eucrite-diogenite meteorites coming from Vesta.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉McCord, T B -- Li, J-Y -- Combe, J-P -- McSween, H Y -- Jaumann, R -- Reddy, V -- Tosi, F -- Williams, D A -- Blewett, D T -- Turrini, D -- Palomba, E -- Pieters, C M -- De Sanctis, M C -- Ammannito, E -- Capria, M T -- Le Corre, L -- Longobardo, A -- Nathues, A -- Mittlefehldt, D W -- Schroder, S E -- Hiesinger, H -- Beck, A W -- Capaccioni, F -- Carsenty, U -- Keller, H U -- Denevi, B W -- Sunshine, J M -- Raymond, C A -- Russell, C T -- England -- Nature. 2012 Nov 1;491(7422):83-6. doi: 10.1038/nature11561.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Bear Fight Institute, 22 Fiddler's Road, Box 667, Winthrop, Washington 98862, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23128228" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 3
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    E-type asteroid (2867) Steins as imaged by OSIRIS on board Rosetta (2010)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2010-01-09
    Description: The European Space Agency's Rosetta mission encountered the main-belt asteroid (2867) Steins while on its way to rendezvous with comet 67P/Churyumov-Gerasimenko. Images taken with the OSIRIS (optical, spectroscopic, and infrared remote( )imaging system) cameras on board Rosetta show that Steins is an oblate body with an effective spherical diameter of 5.3 kilometers. Its surface does not show color variations. The morphology of Steins is dominated by linear faults and a large 2.1-kilometer-diameter crater near its south pole. Crater counts reveal a distinct lack of small craters. Steins is not solid rock but a rubble pile and has a conical appearance that is probably the result of reshaping due to Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) spin-up. The OSIRIS images constitute direct evidence for the YORP effect on a main-belt asteroid.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Keller, H U -- Barbieri, C -- Koschny, D -- Lamy, P -- Rickman, H -- Rodrigo, R -- Sierks, H -- A'Hearn, M F -- Angrilli, F -- Barucci, M A -- Bertaux, J-L -- Cremonese, G -- Da Deppo, V -- Davidsson, B -- De Cecco, M -- Debei, S -- Fornasier, S -- Fulle, M -- Groussin, O -- Gutierrez, P J -- Hviid, S F -- Ip, W-H -- Jorda, L -- Knollenberg, J -- Kramm, J R -- Kuhrt, E -- Kuppers, M -- Lara, L-M -- Lazzarin, M -- Lopez Moreno, J -- Marzari, F -- Michalik, H -- Naletto, G -- Sabau, L -- Thomas, N -- Wenzel, K-P -- Bertini, I -- Besse, S -- Ferri, F -- Kaasalainen, M -- Lowry, S -- Marchi, S -- Mottola, S -- Sabolo, W -- Schroder, S E -- Spjuth, S -- Vernazza, P -- New York, N.Y. -- Science. 2010 Jan 8;327(5962):190-3. doi: 10.1126/science.1179559.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany. keller@linmpi.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20056887" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 4
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    COMETARY SCIENCE. The structure of the regolith on 67P/Churyumov-Gerasimenko from ROLIS descent imaging (2015)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2015-08-01
    Description: The structure of the upper layer of a comet is a product of its surface activity. The Rosetta Lander Imaging System (ROLIS) on board Philae acquired close-range images of the Agilkia site during its descent onto comet 67P/Churyumov-Gerasimenko. These images reveal a photometrically uniform surface covered by regolith composed of debris and blocks ranging in size from centimeters to 5 meters. At the highest resolution of 1 centimeter per pixel, the surface appears granular, with no apparent deposits of unresolved sand-sized particles. The thickness of the regolith varies across the imaged field from 0 to 1 to 2 meters. The presence of aeolian-like features resembling wind tails hints at regolith mobilization and erosion processes. Modeling suggests that abrasion driven by airfall-induced particle "splashing" is responsible for the observed formations.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Mottola, S -- Arnold, G -- Grothues, H-G -- Jaumann, R -- Michaelis, H -- Neukum, G -- Bibring, J-P -- Schroder, S E -- Hamm, M -- Otto, K A -- Pelivan, I -- Proffe, G -- Scholten, F -- Tirsch, D -- Kreslavsky, M -- Remetean, E -- Souvannavong, F -- Dolives, B -- New York, N.Y. -- Science. 2015 Jul 31;349(6247):aab0232. doi: 10.1126/science.aab0232.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany. stefano.mottola@dlr.de. ; German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany. ; DLR, Space Management, Space Science. Bonn, Germany. ; German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany. Freie Universitat Berlin, Institute of Geological Sciences, Berlin, Germany. ; Freie Universitat Berlin, Institute of Geological Sciences, Berlin, Germany. ; Institute of Space Astrophysics, Orsay, France. ; German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany. Humboldt University Berlin, Germany. ; Earth and Planetary Sciences, University of California, Santa Cruz, CA, USA. ; Centre National d'Etudes Spatiales, Toulouse, France. ; Magellium, Ramonville Saint-Agne, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26228151" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 5
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    Images from the surface of asteroid Ryugu show rocks similar to carbonaceous chondrite meteorites (2019)
    American Association for the Advancement of Science (AAAS)
    In: Science
    Details
    Publication Date: 2019
    Description: 〈p〉The near-Earth asteroid (162173) Ryugu is a 900-m-diameter dark object expected to contain primordial material from the solar nebula. The Mobile Asteroid Surface Scout (MASCOT) landed on Ryugu’s surface on 3 October 2018. We present images from the MASCOT camera (MASCam) taken during the descent and while on the surface. The surface is covered by decimeter- to meter-sized rocks, with no deposits of fine-grained material. Rocks appear either bright, with smooth faces and sharp edges, or dark, with a cauliflower-like, crumbly surface. Close-up images of a rock of the latter type reveal a dark matrix with small, bright, spectrally different inclusions, implying that it did not experience extensive aqueous alteration. The inclusions appear similar to those in carbonaceous chondrite meteorites.〈/p〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 6
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    Dawn Mission's Search for Satellites of Ceres: Intact Protoplanets Don't Have Satellites (2018)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Upon its approach to orbit the dwarf planet Ceres in early 2015, optical navigation and dedicated satellite search images were acquired with the Dawn mission's framing camera 2. A team of searchers individually processed and examined the images for evidence of objects moving with Ceres. Completeness of search with respect to the space searched was calculated as a function of distance to Ceres and found to be complete down to 15 Ceres radii (Ceres' mean radius is 470 kilometers). Upper limits of detectable magnitude were determined for each observed set of images and an upper limit in size was calculated assuming for the putative objects, Ceres' geometric albedo of 0.11. Nothing was found associated with Ceres down to a radius of 12 meters for the most sensitive search, and down to a radius of 323m for the least sensitive search circumstances. Examination of the physical properties of the 41 largest and most massive main belt asteroids suggests that large asteroids without satellites are intact and their interiors have internal strength. This is consistent with results from the Dawn mission at both Vesta and Ceres. Ceres' volatile-rich composition also is a likely contributor to both the absence of satellites at Ceres and of Ceres meteorites at Earth. These results suggest that collisional disruption creating rubble pile structure is a necessary condition for formation of satellites around main belt asteroids.
    Keywords: Lunar and Planetary Science and Exploration
    Type: GSFC-E-DAA-TN68836 , Icarus (ISSN 0019-1035) (e-ISSN 1090-2643); 316; 191-204
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  • 7
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    Investigating the Origin of Bright Materials on Vesta: Synthesis, Conclusions, and Implications (2012)
    In:  CASI
    Details
    Publication Date: 2019-08-26
    Description: The Dawn spacecraft started orbiting the second largest asteroid (4) Vesta in August 2011, revealing the details of its surface at an unprecedented pixel scale as small as approx.70 m in Framing Camera (FC) clear and color filter images and approx.180 m in the Visible and Infrared Spectrometer (VIR) data in its first two science orbits, the Survey Orbit and the High Altitude Mapping Orbit (HAMO) [1]. The surface of Vesta displays the greatest diversity in terms of geology and mineralogy of all asteroids studied in detail [2, 3]. While the albedo of Vesta of approx.0.38 in the visible wavelengths [4, 5] is one of the highest among all asteroids, the surface of Vesta shows the largest variation of albedos found on a single asteroid, with geometric albedos ranging at least from approx.0.10 to approx.0.67 in HAMO images [5]. There are many distinctively bright and dark areas observed on Vesta, associated with various geological features and showing remarkably different forms. Here we report our initial attempt to understand the origin of the areas that are distinctively brighter than their surroundings. The dark materials on Vesta clearly are different in origin from bright materials and are reported in a companion paper [6].
    Keywords: Astronomy
    Type: JSC-CN-25701 , 43rd Lunar and Planetary Science Conference; Mar 19, 2012 - Mar 23, 2012; The Woodlands, TX; United States
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  • 8
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    Visible Color and Photometry of Bright Materials on Vesta (2012)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: The Dawn Framing Camera (FC) collected images of the surface of Vesta at a pixel scale of ~70 m in the High Altitude Mapping Orbit (HAMO) phase through its clear and seven color filters spanning from 430 nm to 980 nm. The surface of Vesta displays a large diversity in its brightness and colors, evidently related to the diverse geology [1] and mineralogy [2]. Here we report a detailed investigation of the visible colors and photometric properties of the apparently bright materials on Vesta in order to study their origin. The global distribution and the spectroscopy of bright materials are discussed in companion papers [3, 4], and the synthesis results about the origin of Vestan bright materials are reported in [5].
    Keywords: Astronomy
    Type: JSC-CN-25715 , 43rd Lunar and Planetary Science Conference; Mar 19, 2012 - Mar 23, 2012; The Woodlands, TX; United States
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  • 9
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    Types and Distribution of Bright Materials in 4 Vesta (2012)
    In:  CASI
    Details
    Publication Date: 2019-07-13
    Description: A strong case can be made that Vesta is the parent asteroid of the howardite, eucrite and diogenite (HED) meteorites [1]. As such, we have over a century of detailed sample analysis experience to call upon when formulating hypotheses regarding plausible lithologic diversity on Vesta. It thus came as a surprise when Dawn s Framing Camera (FC) first revealed distinctly localized materials of exceptionally low and high albedos, often closely associated. To understand the nature and origin of these materials, and how they inform us of the geological evolution of Vesta, task forces began their study. An initial step of the scientific endeavor is to develop a descriptive, non-genetic classification of objects to use as a basis for developing hypotheses and observational campaigns. Here we present a catalog of the types of light-toned deposits and their distribution across Vesta. A companion abstract [2] discusses possible origins of bright materials and the constraints they suggest for vestan geology.
    Keywords: Astronomy
    Type: JSC-CN-25711 , 43rd Lunar and Planetary Science Conference; Mar 19, 2012 - Mar 23, 2012; The Woodlands, TX; United States
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  • 10
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    Boulders on Ceres (2017)
    In:  CASI
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    Publication Date: 2019-07-13
    Description: Introduction: In December 2015 the Dawn spacecraft moved into the Low Altitude Mapping Orbit (LAMO) around Ceres, encircling the dwarf planet at a distance of 400 km to the surface below. At this altitude, images of the on-board framing camera have a resolution of 36 meters per pixel, high enough to distinguish large boulders on the surface. Indeed, LAMO images show a multitude of boulders around what seem to be fresh craters. The average life-time of boulders on Dawn's previous target, Vesta, was estimated to be similar to that of Lunar boulders, as may be expected from the basaltic surface composition. The bulk composition of Ceres may be carbonaceous chondrite-like with significant contributions of clays, salt, and water ice. As such, the abundance and distribution of boulders on Ceres may be different from that on Vesta. We mapped, counted, and measured the diameter of boulders over the entire surface of Ceres. Our analysis of the data in combination with crater age estimates may provide clues to the physical nature and composition of the surface.
    Keywords: Lunar and Planetary Science and Exploration
    Type: GSFC-E-DAA-TN38242 , Asteroids, Comets, Meteors (ACM) 2017; Apr 10, 2017 - Apr 14, 2017; Montevideo, UY; Uruguay
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