DOCSLIB.ORG

POSTER SESSION I: CERES: MISSION RESULTS from DAWN 6:00 P.M

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Lunar and Planetary Science XLVIII (2017) sess312.pdf Tuesday, March 21, 2017 [T312] POSTER SESSION I: CERES: MISSION RESULTS FROM DAWN 6: 00 p.m. Town Center Exhibit Area Russell C. T. Raymond C. A. De Sanctis M. C. Nathues A. Prettyman T. H. et al. POSTER LOCATION #171 Dawn at Ceres: What We Have Learned [#1269] A summary of the major discoveries and their implications at the close of the exploration of Ceres by Dawn. Ermakov A. I. Park R. S. Zuber M. T. Smith D. E. Fu R. R. et al. POSTER LOCATION #172 Regional Analysis of Ceres’ Gravity Anomalies [#1374] Put in geological and geomorphological context, the regional gravity anomalies give clues on the structure and evolution of Ceres’ crust. Nathues A. Platz T. Thangjam G. Hoffmann M. Mengel K. et al. POSTER LOCATION #173 Evolution of Occator Crater on (1) Ceres [#1385] We present recent results on the origin and evolution of the bright spots (Cerealia and Vinalia Faculae) at crater Occator on (1) Ceres. Buczkowski D. L. Scully J. E. C. Schenk P. M. Ruesch O. von der Gathen I. et al. POSTER LOCATION #174 Tectonic Analysis of Fracturing Associated with Occator Crater [#1488] The floor, walls, and ejecta of Occator Crater on Ceres are cut by multiple sets of linear and concentric fractures. We explore possible formation mechanisms. Pasckert J. H. Hiesinger H. Raymond C. A. Russell C. POSTER LOCATION #175 Degradation and Ejecta Mobility of Impact Craters on Ceres [#1377] We investigated the degradation and ejecta mobility of craters on Ceres, to investigate latitudinal variations, and to compare it with other planetary bodies. Schmedemann N. Neesemann A. Schulzeck F. Krohn K. von der Gathen I. et al. POSTER LOCATION #176 The Distribution of Impact Ejecta on Ceres [#1233] Ceres is a fast rotating small body. High flying impact ejecta are heavily affected by Coriolis forces, resulting in highly asymmetric distal ejecta patterns. Bland M. T. Raymond C. A. Fu R. R. Ermakov A. Schenk P. M. et al. POSTER LOCATION #177 Ceres’ Largest Impact Crater, Kerwan: Inferring Local Interior Structure from Its Peculiar Morphology [#2040] Ceres’ large crater / Peculiar in form and shape / Something hides below. Schulzeck F. Schmedemann N. Schröder S. Carsenty U. Jaumann R. et al. POSTER LOCATION #178 Ejecta Pattern and Velocities of a Boulder Crater on Ceres [#1387] We model the reimpact pattern of ejected particles of a boulder crater on Ceres and correlate landing sites with the corresponding launch velocities. von der Gathen I. Krohn K. Schulzeck F. Jaumann R. Buczkowski D. L. et al. POSTER LOCATION #179 The Geometry and Possible Origin of Fractures in Floor-Fractured Craters on Ceres [#1390] We determined the length, width, and strike of linear features in FFCs on Ceres to get information about surface, underground, and formation conditions. Lunar and Planetary Science XLVIII (2017) sess312.pdf Toplis M. J. Monnereau M. Prettyman T. H. Castillo-Rogez J. McSween H. Y. Jr et al. POSTER LOCATION #180 Water Within Ceres and the Question of Bulk Composition: Constraints and Implications [#1951] The distribution of water within Ceres is considered using geophysical and chemical constraints of the Dawn mission, and numerical models of thermal evolution. Raponi A. De Sanctis M. C. Ciarniello M. Ammannito E. Frigeri A. et al. POSTER LOCATION #181 Water Ice on Ceres’ Surface as Seen by Dawn-Vir: Properties Retrieval by Means of Spectral Modeling [#2007] Water ice have been derived in localized areas on the surface of Ceres by means of the Dawn/VIR instrument. We derive its properties thank to the Hapke model. Formisano M. Federico C. De Sanctis M. C. Frigeri A. Magni G. et al. POSTER LOCATION #182 Thermal Stability of Water Ice on Ceres’ Surface: The Juling Case [#1976] We study the ice stability on Ceres’ surface, by performing numerical simulations in which we tested the effects of thermal inertia and albedo. Zolotov M. Yu. Mironenko M. V. POSTER LOCATION #183 Bright Salts on Ceres: Aqueous Accumulation and Airborne Emplacement [#1241] Subsurface low-pressure boiling of post-impact water solutions causes accumulation of salts at depth and deposition of salty ice grains from plumes. Ehlmann B. L. Hodyss R. Ammannito E. Rossman G. R. De Sanctis M. C. et al. POSTER LOCATION #184 Ammoniation of Phyllosilicates, Carbonaceous Chondrite Meteorites, and Implications for the Nature of Ammoniated Materials on Ceres [#2088] Comparison of VIR spectra of Ceres with new lab data acquired at Ceres temperatures show ammoniated Mg smectites with Mg-serpentine are the key phases. Bu C. Rodriguez Lope G. Dukes C. A. McFadden L. A. Li J.-Y. et al. POSTER LOCATION #185 Instability of Magnesium Sulfate Hexahydrate (MgSO4.6H2O) on Ceres: Laboratory Measurements [#2996] We determine the stability of MgSO4.6H2O on Ceres surface from lab measurements by quantifying the dehydration rate as a function of pressure and temperature. Tosi F. Carrozzo F. G. Zambon F. Ciarniello M. Frigeri A. et al. POSTER LOCATION #186 Mineralogical Analysis of Quadrangle Ac-H-6 Haulani on the Dwarf Planet Ceres [#1857] We report on the mineralogic mapping of quadrangle Ac-H-6 ‘Haulani,’ one of five quadrangles that cover the equatorial region of the dwarf planet Ceres. Longobardo A. Palomba E. De Sanctis M. C. Carrozzo F. G. Galiano A. et al. POSTER LOCATION #187 Mineralogical Mapping of the Occator Quadrangle [#2044] This work describes the mineralogical mapping of the Occator quadrangle of Ceres, extending from latitude 22°S to 22°N and from longitudes 216°E to 288°E. Zambon F. Carrozzo F. G. Tosi F. Ciarniello M. Combe J.-Ph. et al. POSTER LOCATION #188 Spectral Analysis of the Quadrangle Ac-H-10 Rongo on Ceres [#2057] We present the spectral analysis of the quadrangle Ac-H-10 Rongo on Ceres. We describe the principal results obtained by VIR spectrometer onboard Dawn. Lunar and Planetary Science XLVIII (2017) sess312.pdf Palomba E. Longobardo A. De Sanctis M. C. Galiano A. Carrozzo F. G. et al. POSTER LOCATION #189 Mineralogical Mapping of the Kerwan Quadrangle on Ceres [#2066] This work describes the mineralogical mapping of the Kerwan quadrangle of Ceres, extending from latitude 22°S to 22°N and from longitudes 72°E to 144°E. De Sanctis M. C. Ammannito E. Carrozzo F. G. Zambon F. Ciarniello M. et al. POSTER LOCATION #190 Mineralogy of the Sintana-Toharu Region on Ceres [#2093] We present the first mineralogical maps of the Sinatana and Toharu southern quadrangles on Ceres, between latitudes 20°S and 65°S and longitudes 0°E and 180°E. Carrozzo F. G. De Sanctis M. C. Ammannito E. Ciarniello M. Frigeri A. et al. POSTER LOCATION #191 Spectral Analysis of the Qyadrangle Ac-H-08 Nawish on Ceres [#2193] This work describes the mineralogical mapping of the Nawish quadrangle of Ceres, extending from latitude 22°S to 22°N and from longitudes 144°E to 216°E. Stephan K. Jaumann R. Zambon F. Carrozzo F. G. De Sanctis M. C. et al. POSTER LOCATION #192 Spectral Investigation of Quadrangle Ac-H-3 of the Dwarf Planet Ceres – The Region of Impact Crater Dantu [#2446] In this study we explore the surface composition in the Ac-H 3 quadrangle of Ceres’ surface named after its dominating surface feature Dantu. Ammannito E. De Sanctis M. C. Carrozzo F. G. Zambon F. Ciarniello M. et al. POSTER LOCATION #193 Composition of the Urvara-Yalode Region on Ceres [#2659] We present here the first results of the mineralogical mapping of the Urvara and Yalode quadrangles on Ceres. Combe J.-Ph. Singh S. Johnson K. E. McCord T. B. De Sanctis M. C. et al. POSTER LOCATION #194 Surface Composition of Ceres Quadrangle Ac-4 Ezinu by the Dawn Mission [#2849] The surface composition of the quadrangle Ezinu is investigated by near-infrared reflectance spectroscopy and high-resolution imagery. Singh S. Combe J. P. McFadden L. A. Ruesch O. McCord T. et al. POSTER LOCATION #195 Mineralogical Mapping of Ac-05 Fejokoo Quadrangle of Ceres [#2927] Surface mineralogy of the Ac-05 Fejokoo quadrangle. Vu T. H. Hodyss R. Johnson P. V. Choukroun M. POSTER LOCATION #196 Preferential Formation of Sodium Salts from Frozen Sodium-Ammonium-Chloride-Carbonate Brines: Implications for Ceres’ Bright Spots [#2227] Sodium salts form preferentially in frozen Ceres-like brines. Potential presence of NH4Cl on Ceres’ surface may imply an ocean rich in ammonium and/or chloride. Ruesch O. Nathues A. Jaumann R. Quick L. C. Bland M. T. et al. POSTER LOCATION #197 Faculae on Ceres: Possible Formation Mechanisms [#2435] Faculae are bright, carbonate-rich regions on dwarf planet Ceres. Their formation might require extrusion of ice and/or brine in the recent past. Lunar and Planetary Science XLVIII (2017) sess312.pdf Scully J. E. C. Buczkowski D. L. Schenk P. M. Neesemann A. Raymond C. A. et al. POSTER LOCATION #198 The Geologic History and Formation of the Faculae in Occator Crater on Ceres [#1683] Based on a detailed geologic map, we propose a geologic history for Occator Crater and a formation mechanism for the bright regions (faculae) it contains. Mazarico E. Ermakov A. I. Schröder S. E. Carsenty U. Schorghofer N. et al. POSTER LOCATION #199 The History of Ceres’ Obliquity and Its Effect on Permanent Shadow [#1985] We study the periodic variations in Ceres’ obliquity and their effect on permanent shadow. We discuss implications for long-term surface stability. Mao X. McKinnon W. B. POSTER LOCATION #200 Fossil Rotational Bulge from Faster Paleo-Spin and Isostatic Excess Topography Can Explain Ceres’ Present-Day Shape and Gravity [#2744] Whereas a faster spin can reconcile Ceres’ degree-2 gravity from hydrostatic shape prediction, an isostatically-compensated topography fulfills the same purpose.
Recommended publications
  • March 21–25, 2016

    March 21–25, 2016

    FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk,
  • Oxo Crater on (1) Ceres: Geological History and the Role of Water-Ice

    Oxo Crater on (1) Ceres: Geological History and the Role of Water-Ice

    The Astronomical Journal, 154:84 (13pp), 2017 September https://doi.org/10.3847/1538-3881/aa7a04 © 2017. The American Astronomical Society. All rights reserved. Oxo Crater on (1) Ceres: Geological History and the Role of Water-ice A. Nathues1, T. Platz1, M. Hoffmann1, G. Thangjam1, E. A. Cloutis2, D. M. Applin2, L. Le Corre1,3, V. Reddy1,4, K. Mengel5, S. Protopapa6, D. Takir7, F. Preusker8, B. E. Schmidt9, and C. T. Russell10 1 Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, D-37077 Goettingen, Germany; [email protected] 2 University of Winnipeg, Winnipeg, MB R3B 2E9, Canada 3 Planetary Science Institute, 1700 East Fort Lowell Rd, Suite 106, Tucson, AZ 85719-2395, USA 4 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA 5 IELF, TU Clausthal, Adolph-Roemer-Straße 2A, D-38678 Clausthal-Zellerfeld, Germany 6 University of Maryland, Department of Astronomy, College Park, MD 20742, USA 7 SETI Institute, Mountain View, CA 94043, USA 8 German Aerospace Center (DLR), Institute of Planetary Research, D-12489 Berlin, Germany 9 Georgia Institute of Technology, Atlanta, GA, USA 10 Institute of Geophysics and Planetary Physics, Dept. of Earth, Planetary and Space Sciences, University of California Los Angeles, Los Angeles, CA, USA Received 2017 March 1; revised 2017 June 14; accepted 2017 June 14; published 2017 August 4 Abstract Dwarf planet Ceres (∅∼940 km) is the largest object in the main asteroid belt. Investigations suggest that Ceres is a thermally evolved, volatile-rich body with potential geological activity, a body that was never completely molten, but one that possibly partially differentiated into a rocky core and an ice-rich mantle, and may contain remnant internal liquid water.
  • THE PLANETARY REPORT JUNE SOLSTICE 2016 VOLUME 36, NUMBER 2 Planetary.Org

    THE PLANETARY REPORT JUNE SOLSTICE 2016 VOLUME 36, NUMBER 2 Planetary.Org

    THE PLANETARY REPORT JUNE SOLSTICE 2016 VOLUME 36, NUMBER 2 planetary.org ILLUMINATING CERES DAWN SHEDS NEW LIGHT ON AN ENIGMATIC WORLD BREAKTHROUGH STARSHOT C LIGHTSAIL 2 TEST C MEMBERSHIP UPGRADES SNAPSHOTS FROM SPACE EMILY STEWART LAKDAWALLA blogs at planetary.org/blog. Black Sands of Mars ON SOL 1192 (December 13, 2015), Curiosity approached the side of Namib, a Faccin and Marco Bonora Image: NASA/JPL/MSSS/Elisabetta massive barchan sand dune. Namib belongs to a field of currently active dark basaltic sand dunes that form a long barrier between the rover and the tantalizing rocks of Mount Sharp. This view, processed by Elisabetta Bonora and Marco Faccin, features wind-carved yardangs (crests or ridges ) of Mount Sharp in the background. After taking this set of photos, Curiosity went on to sample sand from the dune, and it is now working its way through a gap in the dune field on the way to the mountain. —Emily Stewart Lakdawalla SEE MORE AMATEUR-PROCESSED SPACE IMAGES planetary.org/amateur SEE MORE EVERY DAY! planetary.org/blogs 2 THE PLANETARY REPORT C JUNE SOLSTICE 2016 CONTENTS JUNE SOLSTICE 2016 COVER STORY Unveiling Ceres 6 Simone Marchi on why Ceres is a scientific treasure chest for Dawn. Pathway to the Stars Looking back at years of Society-led solar sail 10 development as Breakthrough Starshot is announced. Life, the Universe, and Everything 13 Planetary Radio in Death Valley. ADVOCATING FOR SPACE Partisan Peril 18 Casey Dreier looks at the U.S. President’s impact on space policy and legislation. DEVELOPMENTS IN SPACE SCIENCE Update on LightSail 2 20 Bruce Betts details the progress we’ve made in the year since LightSail 1 launched.
  • Jjmonl 1802.Pmd

    Jjmonl 1802.Pmd

    alactic Observer John J. McCarthy Observatory G Volume 11, No. 2 February 2018 A porpoise or a penguin or a puppet on a string? — Find out on page 19 The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue OUT THE WINDOW ON YOUR LEFT .................................... 4 REFERENCES ON DISTANCES ............................................ 18 VALENTINE DOME .......................................................... 4 INTERNATIONAL SPACE STATION/IRIDIUM SATELLITES .......... 18 PASSING OF ASTRONAUT JOHN YOUNG ............................... 5 SOLAR ACTIVITY ........................................................... 19 FALCON HEAVY DEBUT ..................................................
  • 1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992

    1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992

    Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H.
  • Mineralogical Mapping of the Kerwan Quadrangle on Ceres

    Mineralogical Mapping of the Kerwan Quadrangle on Ceres

    Icarus 318 (2019) 188–194 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Mineralogical mapping of the Kerwan quadrangle on Ceres ∗ E. Palomba a,e, , A. Longobardo a, M.C. De Sanctis a, F.G. Carrozzo a, A. Galiano a,b, F. Zambon a, A. Raponi a, M. Ciarniello a, K. Stephan c, D.A. Williams d, E. Ammannito a,g, M.T. Capria a,e, S. Fonte a, M. Giardino a, F. Tosi a, C.A. Raymond f, C.T. Russell g a Istituto di Astrofisica e Planetologia Spaziali, INAF, via del fosso del Cavaliere, 100, 00133, Rome, Italy b Università di Roma Tor Vergata, Department of Physics, via della ricerca scientifica, 1, 00133 Rome, Italy c Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstrasse 2, d-12489 Berlin, Germany d School of Earth & Space Exploration, Arizona State University, Tempe, AZ 85287-1404, USA e Space Science Data Center (SSDC) - Agenzia Spaziale Italiana (ASI), Via del Politecnico snc, Edificio D, 00133 Roma, Italy f Jet Propulsion Laboratory, Pasadena, CA 91109, USA g Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095-1567, USA a r t i c l e i n f o a b s t r a c t Article history: The Ceres surface is globally composed of Mg-phyllosilicates, ammoniated clays, carbonates and dark Received 28 April 2017 components. To obtain a more detailed mineralogical and geological investigation, the dwarf planet sur- Revised 11 July 2017 face has been divided into fifteen quadrangles. The aim of this work is to investigate the abundance of Accepted 25 July 2017 phyllosilicates and ammoniated clays in the Kerwan quadrangle, classified as Ac-H-7 and spanning from Available online 25 July 2017 22 °S to 22 °N in latitude and from 72 °E to 144 °E in longitude.
  • Surface Processes and Space Weathering on Ceres

    Surface Processes and Space Weathering on Ceres

    47th Lunar and Planetary Science Conference (2016) 1383.pdf SURFACE PROCESSES AND SPACE WEATHERING AT CERES. C. M. Pieters1, E. Ammannito2,3, M. Ciarniello3, M. C. De Sanctis3, M. Hoffman4, R. Jaumann5, T. B. McCord6, L. A. McFadden7, S. Mest8, A. Nathues4, A. Raponi3, C. A. Raymond9, C. T. Russell3, M. Schaefer4, P. Schenk10 , 1Dept. Earth, Environmental, and Planetary Science, Brown Univ., Providence, RI 02912 ([email protected]); 2UCLA CA; 3IAPS, INAF Italy; 4MPS Germany; 5DLR Germany; 6Bear Fight Inst. WA; 7Goddard MD; 8PSI AZ; 9JPL CA; 10LPI TX Introduction: When Dawn arrived at Ceres in 2015 it found a unique and perplexing ice-rock dwarf planet [1]. As anticipated, the overall surface is very dark, but small local areas exhibit unexpectedly bright materials that are likely indigenous in origin [2]. Near-infrared spectroscopic analyses identified the presence of am- moniated phyllosilicates (which are typically associated with the outer solar system) [3], and these were shown to be present everywhere across the surface although their relative abundance varies regionally [4]. The sur- face is heavily cratered, except for the largest craters [5], allowing relative ages to be derived [6]. The most recent craters often exhibit rays as well as local spectral properties that are relatively blue (440-960 nm) com- pared to their surroundings [2, 7]. Fresh craters that ex- hibit regular but distinct optical properties compared to similar but older areas is a characteristic indication that some form of alteration, or space weathering, occurs with time across the surface that transforms freshly ex- posed material into background soils. Fresh craters at Ceres.
  • Ceres from Geologic and Topographic Mapping and Crater Counts Using Images of the Dawn Fc2 Camera

    Ceres from Geologic and Topographic Mapping and Crater Counts Using Images of the Dawn Fc2 Camera

    47th Lunar and Planetary Science Conference (2016) 2156.pdf STRATIGRAPHY OF (1) CERES FROM GEOLOGIC AND TOPOGRAPHIC MAPPING AND CRATER COUNTS USING IMAGES OF THE DAWN FC2 CAMERA. R. J. Wagner1, N. Schmedemann2, K. Stephan1, R. Jaumann1, T. Kneissl2, A. Neesemann2, K. Krohn1, K. Otto1, F. Preusker1, E. Kersten1, T. Roatsch1, H. Hiesing- er3, D. A. Williams4, R. A. Yingst5, D. A. Crown5, S. C. Mest5, C. A. Raymond6, and C. T. Russell7; 1Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany (Email: [email protected]); 2Institute for Geological Sciences, Free University Berlin, Germany; 3Institute of Planetology, Westphalian Wilhelm Universi- ty, Münster, Germany; 4School of Earth & Space Exploration, Arizona State University, Tempe/Az., USA; 5Planetary Science Institute, Tucson/Az., USA; 6Jet Propulsion Laboratory, Pasadena/Ca., USA; 7Institute of Geo- physics & Planetary Physics, UCLA, Los Angeles/Ca., USA. Introduction: The Dawn spacecraft has been in Previous results from RC2 images. Investigating orbit around dwarf planet (1) Ceres since its capture on data from the RC2 sequence in the first mapping cam- March 6, 2015. Since then, the FC2 Framing Camera paign has been finished [9][10]. Densely cratered [1][2] has been acquiring imaging data at increasing plains are the spatially most abundant units and occur spatial resolution from continuously lower altitudes. In at all three topographic levels. Their cratering model this paper we use image and topographic data to map ages range from ~ 3.7 to ~ 3.3 Ga. Sparsely cratered geologic units and to carry out crater counts in order to plains show frequencies a factor ~ 3 to 5 lower than the derive the global, regional and local stratigraphy of densely cratered plains.
  • Results from the NASA Dawn Mission to Vesta and Ceres

    Results from the NASA Dawn Mission to Vesta and Ceres

    EPSC Abstracts Vol. 13, EPSC-DPS2019-5-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. The Geologic Mapping of Small Bodies: Results from the NASA Dawn Mission to Vesta and Ceres Williams, David A. and the Dawn Science Team School of Earth and Space Exploration, Arizona State University, Tempe, Arizona, USA, ([email protected]) Abstract 2. Ceres mapping & chronostratigraphy NASA’s Dawn mission was a Discovery-class robotic mission to send an orbiter to the two most massive The geologic mapping of Ceres was described in [5] objects in the Main Asteroid Belt, asteroid (4) Vesta and its chronostratigraphy is still being finalized at the and dwarf planet (1) Ceres [1]. Dawn orbited Vesta time of this writing. Ceres has a globally distributed from July 2011 to September 2012, and it remains in cratered terrain, with three large, ill-defined orbit of Ceres since it arrived in March 2015. As part topographic depressions that could be ancient basins. of the spacecraft’s nominal mission, the Dawn Science Kerwan crater (285 km diameter) is the largest Team requested geologic mapping campaigns of both identifiable impact crater, infilled and surrounded by Vesta and Ceres, which included global mapping a unique smooth material that marks this oldest crater. using High Altitude Mapping Orbit (HAMO) images In the southeastern hemisphere Yalode and Urvara (Vesta: 70 m/px; Ceres: 140 m/px) and quadrangle craters mark the next two youngest basins, with mapping using Low Altitude Mapping Orbit (LAMO) complex ejecta units. Intermediate and younger aged images (Vesta: 25/m/px; Ceres: 35 m/px).
  • Geologic Mapping of the Ac-H-11 Sintana Quadrangle of Ceres from Nasa’S Dawn Mission

    Geologic Mapping of the Ac-H-11 Sintana Quadrangle of Ceres from Nasa’S Dawn Mission

    47th Lunar and Planetary Science Conference (2016) 1955.pdf GEOLOGIC MAPPING OF THE AC-H-11 SINTANA QUADRANGLE OF CERES FROM NASA’S DAWN MISSION. F. Schulzeck1, K. Krohn1, R. Jaumann1, D. A. Williams2, D. L. Buczkowski3, S. C. Mest4, J. E. C. Scully5, I. v. d. Gathen1, E. Kersten1, K.-D. Matz1, A. Naß1, K. Otto1, C. M. Pieters6, F. Preusker1, T. Roatsch1, M. C. De Sanctis7, P. Schenk8, S. Schröder1, K. Stephan1, R. Wagner1, C. A. Raymond5, C. T. Russell9, 1DLR, Berlin, Germany; 2School of Earth & Space Exploration, Arizona State University, Tempe, AZ, USA; 3JHU-APL, Laurel, MD, USA; 4Planetary Science Institute, Tucson, AZ, USA; 5Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA; 6Department of Earth, Environmental, and Planetary Sciences Brown University, Providence, RI, USA; 7National Institute of Astrophysics, Rome, Italy; 8Lunar and Planetary Institute, Houston, TX, USA; 9UCLA, Los Angeles, CA, USA Introduction: NASA’s Dawn spacecraft arrived at cratering on the primary crater rim. Annona crater Ceres on March 5, 2015, and has been studying the features both characteristics. Whereas collapse dwarf planet through a series of successively lower structures are mostly blocky, Annona’s landslide, orbits, obtaining morphological & topographical triggered by a younger crater on its rim, is image, mineralogical, elemental, and gravity data. The characterized by lobate margins. The occurrence of Dawn Science Team is conducting a geologic mapping mass movements and the type of mass wasting feature campaign for Ceres similar to that done for Vesta [1, might therefore hint to compositional differences. For 2], including production of a Survey- and High complex craters, such as Darzamat and Mondamin, we Altitude Mapping Orbit (HAMO)-based global map, observe many different inner crater structures, like relaxed crater floors, ridges, central peaks, mounds and and a series of 15 Low Altitude Mapping Orbit smooth plains.
  • Channels and Cryogenic Flow Features on Ceres K

    Channels and Cryogenic Flow Features on Ceres K

    47th Lunar and Planetary Science Conference (2016) 2001.pdf CHANNELS AND CRYOGENIC FLOW FEATURES ON CERES K. Krohn1, R. Jaumann1, K.A. Otto1, I. von der Gathen1, K.-D. Matz1, F. Schulzeck1, D.L. Buczkowski2, D.A. Williams3, K. Stephan1, R. J. Wagner1, C.M. Pieters4, F. Preusker1, T. Roatsch1, C.T. Russell5, C.A. Raymond6. 1Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany ([email protected]), 2JHU-APL, Laurel, Maryland, USA; 3School of Earth & Space Exploration, Arizona State University, Tempe, USA; 4Brown University, Providence, RI, USA, 5UCLA, Los Angeles, California, USA, 6NASA JPL, California Institute of Technology, Pasadena, California, USA. Introduction: After studying the asteroid Vesta between 2011 and 2012 [1], NASA’s Dawn spacecraft entered its orbit around the dwarf planet (1) Ceres in April 2015 [2]. The mission goal is to characterize the geology, elemental and mineralogical composition, topography, shape, and internal structure of Ceres [3]. Ceres´ surface is affected by numerous impact cra- ters and some of them show features such as channels or multiple flow events forming a smooth, less cratered surface, indicating possible post-impact resurfacing [4,5]. Data: For the analysis of channels and flow fea- tures Dawn Framing Camera (FC) data (monochrome and color ratio images) [6] from the High Altitude Mapping Orbit (HAMO) with a spatial resolution of 140 m/px as well as a Digital Terrain Model (DTM) [7] derived from HAMO orbit data have enabled an initial characterization of the surface. At the time of this writing LAMO images (35 m/pixel) are just be- coming available.
  • Nasa Planetary Mission Concept Study: Assessing Dwarf Planet Ceres’ Past and Present Habitability Potential

    Nasa Planetary Mission Concept Study: Assessing Dwarf Planet Ceres’ Past and Present Habitability Potential

    NASA PLANETARY MISSION CONCEPT STUDY: ASSESSING DWARF PLANET CERES’ PAST AND PRESENT HABITABILITY POTENTIAL. J. C. Castillo-Rogez1, M. T. Bland2, D. L. Buczkowski3, A. R. Hen- drix4, K. E. Miller5, T. H. Prettyman4, L.C. Quick6, J. E. C. Scully1, Y. Sekine7, M. M. Sori8,9, T. Titus2, D. A. Wil- liams10, H. Yano11, M. Zolensky12, C. A. Raymond1, J. Brophy1, W. Frazier1, G. Lantoine1, B. G. Lee1, M. S. Kelley13, 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA. 2United States Geological Sur- vey, Flagstaff, AZ. 3John Hopkins University, Applied Physics Laboratory, Laurel, MD. 4Planetary Science Institute. 5Southwest Research Institute, San Antonio, TX. 6NASA Goddard Space Flight Center, Greenbelt, MD. 7Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo, Japan. 8Lunar and Planetary Laboratory, University of Ari- zona, Tucson, AZ. 9Purdue University, West Lafayette, IN. 10School of Earth and Space Exploration, Arizona State University, Phoenix, AZ. 11Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kana- gawa, Japan. 12Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX. 13NASA Headquarters, Washington, DC. Email: [email protected]. Introduction: The Dawn mission revolutionized ical evolution. While the latter goal does not directly re- our understanding of Ceres during the same decade that late to ROW, it addresses the place of Ceres in the early has also witnessed the rise of ocean worlds as a research solar system and its potential connection to other large and exploration focus. We will report progress on the dwarf planets. Planetary Mission Concept Study (PMCS) on the future Future exploration of Ceres would reveal the de- exploration of Ceres under the New Frontiers or Flag- gree to which liquid water and other environmental fac- ship program that was selected for NASA funding in tors may have combined to make this dwarf planet a October 2019.