THE GLOBAL LAMO-BASED GEOLOGIC MAP of CERES Abstract #7035 Planetary Data Archiving, Restoration, and Tools Program
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POSTER SESSION I: CERES: MISSION RESULTS from DAWN 6:00 P.M
Lunar and Planetary Science XLVIII (2017) sess312.pdf Tuesday, March 21, 2017 [T312] POSTER SESSION I: CERES: MISSION RESULTS FROM DAWN 6: 00 p.m. Town Center Exhibit Area Russell C. T. Raymond C. A. De Sanctis M. C. Nathues A. Prettyman T. H. et al. POSTER LOCATION #171 Dawn at Ceres: What We Have Learned [#1269] A summary of the major discoveries and their implications at the close of the exploration of Ceres by Dawn. Ermakov A. I. Park R. S. Zuber M. T. Smith D. E. Fu R. R. et al. POSTER LOCATION #172 Regional Analysis of Ceres’ Gravity Anomalies [#1374] Put in geological and geomorphological context, the regional gravity anomalies give clues on the structure and evolution of Ceres’ crust. Nathues A. Platz T. Thangjam G. Hoffmann M. Mengel K. et al. POSTER LOCATION #173 Evolution of Occator Crater on (1) Ceres [#1385] We present recent results on the origin and evolution of the bright spots (Cerealia and Vinalia Faculae) at crater Occator on (1) Ceres. Buczkowski D. L. Scully J. E. C. Schenk P. M. Ruesch O. von der Gathen I. et al. POSTER LOCATION #174 Tectonic Analysis of Fracturing Associated with Occator Crater [#1488] The floor, walls, and ejecta of Occator Crater on Ceres are cut by multiple sets of linear and concentric fractures. We explore possible formation mechanisms. Pasckert J. H. Hiesinger H. Raymond C. A. Russell C. POSTER LOCATION #175 Degradation and Ejecta Mobility of Impact Craters on Ceres [#1377] We investigated the degradation and ejecta mobility of craters on Ceres, to investigate latitudinal variations, and to compare it with other planetary bodies. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
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
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
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
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. -
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). -
Special Crater Types on Vesta and Ceres As Revealed by Dawn Katrin Krohn
Chapter Special Crater Types on Vesta and Ceres as Revealed by Dawn Katrin Krohn Abstract The exploration of two small planetary bodies by the Dawn mission revealed multifaced surfaces showing a diverse geology and surface features. Impact crater are the most distinctive features on these planetary bodies. The surfaces of asteroid Vesta and the dwarf planet Ceres reveal craters with an individual appearance as caused by different formation processes. Special topographic and subsurface conditions on both bodies have led to the development of special crater types. This chapter present the three most characteristic crater forms fund on both bodies. Asymmetric craters are found on both bodies, whereas ring-mold craters and floor-fractured craters are only visible on Ceres. Keywords: asteroids, asymmetric craters, ring mold craters, floor-fractured craters, impact into ice 1. Introduction The Dawn Mission was the first mission exploring two different planetary objects in the asteroid belt between Mars and Jupiter, the asteroid Vesta and the dwarf planet Ceres. Asteroid Vesta is the second most massive asteroid (2.59079 x 1020 kg) with a mean diameter of 525 km and a mean density of 3.456 ± 0.035 g/ cm (e.g., [1, 2]). Vesta is believed to be a dry, differentiated proto-planet with an iron core of about 220 km in diameter, a mantle with diogenite compositions and an igneous crust [1, 3, 4]. Asteroid Vesta is a fully differentiated planetary body with a complex topography [2] and a multifaceted morphology including impact basins, various forms of impact craters, large troughs extending around the equato- rial region, enigmatic dark material, mass wasting features and surface alteration processes [2, 5, 6]. -
Mineralogy of the Occator Quadrangle
Icarus 318 (2019) 205–211 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Mineralogy of the Occator quadrangle ∗ A. Longobardo a, , E. Palomba a,b, F.G. Carrozzo a, A. Galiano a, M.C. De Sanctis a, K. Stephan c, F. Tosi a, A. Raponi a, M. Ciarniello a, F. Zambon a, A. Frigeri a, E. Ammannito d, C.A. Raymond e, C.T. Russell f a INAF-IAPS, via Fosso del Cavaliere 100, I-00133 Rome, Italy b ASI-ASDC, via del Politecnico snc, I-00133 Rome, Italy c Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), D-12489 Berlin, Germany d ASI-URS, via del Politecnico snc, I-00133 Rome, Italy e California Institute of Technology, JPL, 91109 Pasadena, CA, USA f UCLA, Los Angeles, CA 90095, USA a r t i c l e i n f o a b s t r a c t Article history: We present an analysis of the areal distribution of spectral parameters derived from the VIR imaging Received 28 April 2017 spectrometer on board NASA/Dawn spacecraft. Specifically we studied the Occator quadrangle of Ceres, Revised 11 September 2017 which is bounded by latitudes 22 °S to 22 °N and longitudes 214 °E to 288 °E, as part of the overall study Accepted 18 September 2017 of Ceres’ surface composition reported in this special publication. The spectral parameters used are the Available online 22 September 2017 photometrically corrected reflectance at 1.2 μm, the infrared spectral slope (1.1–1.9 μm), and depths of Keywords: the absorption bands at 2.7 μm and 3.1 μm that are ascribed to hydrated and ammoniated materials, Asteroid ceres respectively. -
Ceres: Astrobiological Target and Possible Ocean World
ASTROBIOLOGY Volume 20 Number 2, 2020 Research Article ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2018.1999 Ceres: Astrobiological Target and Possible Ocean World Julie C. Castillo-Rogez,1 Marc Neveu,2,3 Jennifer E.C. Scully,1 Christopher H. House,4 Lynnae C. Quick,2 Alexis Bouquet,5 Kelly Miller,6 Michael Bland,7 Maria Cristina De Sanctis,8 Anton Ermakov,1 Amanda R. Hendrix,9 Thomas H. Prettyman,9 Carol A. Raymond,1 Christopher T. Russell,10 Brent E. Sherwood,11 and Edward Young10 Abstract Ceres, the most water-rich body in the inner solar system after Earth, has recently been recognized to have astrobiological importance. Chemical and physical measurements obtained by the Dawn mission enabled the quantification of key parameters, which helped to constrain the habitability of the inner solar system’s only dwarf planet. The surface chemistry and internal structure of Ceres testify to a protracted history of reactions between liquid water, rock, and likely organic compounds. We review the clues on chemical composition, temperature, and prospects for long-term occurrence of liquid and chemical gradients. Comparisons with giant planet satellites indicate similarities both from a chemical evolution standpoint and in the physical mechanisms driving Ceres’ internal evolution. Key Words: Ceres—Ocean world—Astrobiology—Dawn mission. Astro- biology 20, xxx–xxx. 1. Introduction these bodies, that is, their potential to produce and maintain an environment favorable to life. The purpose of this article arge water-rich bodies, such as the icy moons, are is to assess Ceres’ habitability potential along the same lines Lbelieved to have hosted deep oceans for at least part of and use observational constraints returned by the Dawn their histories and possibly until present (e.g., Consolmagno mission and theoretical considerations. -
Features Named After 07/15/2015) and the 2018 IAU GA (Features Named Before 01/24/2018)
The following is a list of names of features that were approved between the 2015 Report to the IAU GA (features named after 07/15/2015) and the 2018 IAU GA (features named before 01/24/2018). Mercury (31) Craters (20) Akutagawa Ryunosuke; Japanese writer (1892-1927). Anguissola SofonisBa; Italian painter (1532-1625) Anyte Anyte of Tegea, Greek poet (early 3rd centrury BC). Bagryana Elisaveta; Bulgarian poet (1893-1991). Baranauskas Antanas; Lithuanian poet (1835-1902). Boznańska Olga; Polish painter (1865-1940). Brooks Gwendolyn; American poet and novelist (1917-2000). Burke Mary William EthelBert Appleton “Billieâ€; American performing artist (1884- 1970). Castiglione Giuseppe; Italian painter in the court of the Emperor of China (1688-1766). Driscoll Clara; American stained glass artist (1861-1944). Du Fu Tu Fu; Chinese poet (712-770). Heaney Seamus Justin; Irish poet and playwright (1939 - 2013). JoBim Antonio Carlos; Brazilian composer and musician (1927-1994). Kerouac Jack, American poet and author (1922-1969). Namatjira Albert; Australian Aboriginal artist, pioneer of contemporary Indigenous Australian art (1902-1959). Plath Sylvia; American poet (1932-1963). Sapkota Mahananda; Nepalese poet (1896-1977). Villa-LoBos Heitor; Brazilian composer (1887-1959). Vonnegut Kurt; American writer (1922-2007). Yamada Kosaku; Japanese composer and conductor (1886-1965). Planitiae (9) Apārangi Planitia Māori word for the planet Mercury. Lugus Planitia Gaulish equivalent of the Roman god Mercury. Mearcair Planitia Irish word for the planet Mercury. Otaared Planitia Arabic word for the planet Mercury. Papsukkal Planitia Akkadian messenger god. Sihtu Planitia Babylonian word for the planet Mercury. StilBon Planitia Ancient Greek word for the planet Mercury. -
Ceres Observed at Low Phase Angles by VIR-Dawn M
A&A 634, A39 (2020) https://doi.org/10.1051/0004-6361/201936492 Astronomy & © ESO 2020 Astrophysics Ceres observed at low phase angles by VIR-Dawn M. Ciarniello1, M. C. De Sanctis1, A. Raponi1, B. Rousseau1, A. Longobardo1, J.-Y. Li2, S. E. Schröder3, F. Tosi1, F. Zambon1, E. Ammannito4, F. G. Carrozzo1, A. Frigeri1, E. Rognini5, C. A. Raymond6, and C. T. Russell7 1 IAPS-INAF, Via Fosso del Cavaliere, 100, 00133 Rome, Italy e-mail: [email protected] 2 Planetary Science Institute, Tucson, AZ, USA 3 German Aerospace Center DLR, Institute of Planetary Research, Berlin, Germany 4 ASI, Rome, Italy 5 ASI-SSDC, Rome, Italy 6 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA 7 University of California Los Angeles, Earth Planetary and Space Sciences, Los Angeles, CA, USA Received 9 August 2019 / Accepted 11 December 2019 ABSTRACT Context. Particulate surfaces exhibit a surge of reflectance at low phase angles, a phenomenon referred to as the opposition effect (OE). Two mechanisms are recognized as responsible for the OE: shadow hiding (SH) and coherent backscattering. The latter is typically characterized by a small angular width of a few degrees at most and according to the theoretical prediction should exhibit wavelength and albedo dependence. Aims. We characterize the OE on the surface of Ceres using Dawn Visible InfraRed mapping spectrometer hyperspectral images at low phase angles. Furthermore, this dataset, coupled with previous observations, allows us to perform a complete spectrophotometric modeling at visual-to-infrared (VIS-IR) wavelengths (0.465–4.05 µm) in the broad phase angle range ≈0◦−132◦.