DOCSLIB.ORG

'A'a Lava 15, 82, 86 Ahsabkab Vallis 80, 81, 82

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
'A'a Lava 15, 82, 86 Ahsabkab Vallis 80, 81, 82 Index Page numbers in italic denote Figures. Page numbers in bold denote Tables. ‘a’a lava 15, 82, 86 Belgica Rupes 272, 275 Ahsabkab Vallis 80, 81, 82, 83 Beta Regio, Bouguer gravity anomaly Aino Planitia 11, 14, 78, 79, 83 332, 333 Akna Montes 12, 14 Bhumidevi Corona 78, 83–87 Alba Mons 31, 111 Birt crater 378, 381 Alba Patera, flank terraces 185, 197 Blossom Rupes fold-and-thrust belt 4, 274 Albalonga Catena 435, 436–437 age dating 294–309 amors 423 crater counting 296, 297–300, 301, 302 ‘Ancient Thebit’ 377, 378, 388–389 lobate scarps 291, 292, 294–295 anemone 98, 99, 100, 101 strike-slip kinematics 275–277, 278, 284 Angkor Vallis 4,5,6 Bouguer gravity anomaly, Venus 331–332, Annefrank asteroid 427, 428, 433 333, 335 anorthosite, lunar 19–20, 129 Bransfield Rift 339 Antarctic plate 111, 117 Bransfield Strait 173, 174, 175 Aphrodite Terra simple shear zone 174, 178 Bouguer gravity anomaly 332, 333, 335 Bransfield Trough 174, 175–176 shear zones 335–336 Breksta Linea 87, 88, 89, 90 Apollinaris Mons 26,30 Brumalia Tholus 434–437 apollos 423 Arabia, mantle plumes 337, 338, 339–340, 342 calderas Arabia Terra 30 elastic reservoir models 260 arachnoids, Venus 13, 15 strike-slip tectonics 173 Aramaiti Corona 78, 79–83 Deception Island 176, 178–182 Arsia Mons 111, 118, 228 Mars 28,33 Artemis Corona 10, 11 Caloris basin 4,5,6,7,9,59 Ascraeus Mons 111, 118, 119, 205 rough ejecta 5, 59, 60,62 age determination 206 canali, Venus 82 annular graben 198, 199, 205–206, 207 Canary Islands flank terraces 185, 187, 189, 190, 197, 198, 205 lithospheric flexure 219, 229–230, 231, 232, 233 pit craters 205–206, 207 magmatism on slow plates 112–114, 115, self-similar clustering 209–210, 212 116, 119 plumbing system 110–111, 210–211, canyons, Mars 34 213–215 Cape Verde Islands, magmatism on slow-moving topography 207, 228 plates 108, 112–114, 115, 116, 119 asperity, Scathach Fluctus 97, 99, 101 Caravaggio peak-ring basin 294, 295–296, 297 asteroids age 303–305, 307 main belt 1, 2, 423, 430, 433 crater-counting 296, 300 composition 142 size–frequency distribution 300–301 as impactors 163, 165 Ceraunius Tholus 28 near-Earth 2, 423–424 Cerro de la Mica double restraining bend 277, 278 density and structure 424 chasmata 12, 330 lineaments 424, 425, 424–433 chondrites 423–424 S-type 423, 424, 427–428, 430 Circum-Hellas volcanic province 26,30 tectonism and magmatism 423–437 climate change atens 423 SPLD deformation 407, 411–419 Atla Regio, wrinkle ridges 358, 359, 360, 365, wrinkle ridges 357 369, 370, 371 companion shield fields 77–78, 83, 86, 90 cones Beagle Rupes system Mars 28, 31, 32 cross-cutting 315 Moon 22 strike-slip kinematics, lateral ramps 270, coronae 277, 279 Venus 13, 14, 15, 77–93 Becuma radiating graben 14 volcanic features 77–78, 82–83 Beethoven basin 4,7 companion shield fields 77–78, 83, 86, 90 Duyfken Rupes thrust 283 lava flow fields 77, 82, 83, 86 Downloaded from http://pubs.geoscienceworld.org/books/book/chapter-pdf/3920420/9781862396777_backmatter.pdf by guest on 01 October 2021 444 INDEX crater-counting fault dip 313–315, 317 Mars 206, 207, 211, 213, 292, 300–301 fault kinematics and geometry 313–315, Mercury 160, 164–169, 296, 297–300, 301, 302 322–324 crater-scaling law 163 estimation 317 craters, faulting 313–324 fault slip 314, 321 Mercury 315, 316, 317–324 measurement 316–317 Crozet Islands, magmatism 108, 112–114, 117, 119 fault strike 314, 317, 322 crustal thickness throw, Rupes Recta 382, 385–388, 390 Lakshmi Planum 332, 334 faulting Venus 332–335 craters 313–324 cryptomaria, Moon 21–22 Mercury 8, 315, 316, 317–324 Moon, Rupes Recta 377–391 dark material 59, 60, 63, 64,70 Venus 330–331 Deception Island volcanic caldera 173–182, 174, 175 see also strike-slip kinematics; thrust faults collapse 181–182 flank terraces faults and fractures 176 fish-scale pattern 185–186, 187, 197, 198, 205 lithology 176, 177 Martian shield volcanoes 185–200 magma chamber 177, 180, 181–182 formation modelling 186, 188–191 pre-collapse palaeoreconstruction 179, 181 comparison with natural examples Riedel shear 178–180, 181–182 197–200 strike-slip shear zone 176, 178–182 flexural troughs, Mars 199, 205 Discovery Rupes 274, 282 flower structures 270 Divalia Fossa 432, 433 Blossom Rupes 277 domes Enterprise Rupes 274, 275 Moon 18,22–23 folds and thrusts, Venus 14, 331 Venus 14, 15, 77, 80, 81, 82, 89 Fossey crater drift 329, 339, 342–346 impact craters and ejecta 372, 373–374 Duyfken Rupes thrust 283 wrinkle ridge detection 365, 366 dykes fractal analysis, wrinkle ridge analysis 361 elastic reservoir models 259–260 graben formation, Mars 395–402 Gala´pagos Islands magma transport 203–204, 209–210, 214 lithospheric flexure 219, 226, 228 self-similar clustering 206, 208–209, 213 Gaspra, lineaments 426, 427 Vesta 434 ghost craters, Mercury 5, 8, 9 graben Earth annular, Mars 28, 34, 198, 199, 205–206 lithospheric flexure 229–230, 232–233 Ascraeus Mons 198, 199, 205–206 lithospheric thickness 220, 221, 226 dyke-induced, analogue modelling 395–402 magma transport 204 Mercury 8, 9, 67, 72, 160 mantle plumes 107–108, 111–117, 337, 338 Moon 18,25 near-stationary plates 107–108, 111–117 Raditladi basin 67, 72 comparison with Tharsis 118–121 Venus 12, 13, 14, 100, 101, 102 volcanic edifices, lithospheric flexure 219, 220, 226 coronae 79, 81, 85 volcanic rock composition 139–140 GRAIL datasets 130 East Africa, mantle plumes 337, 338, 339 ‘gravity worms’, Venus 331, 332, 333, 335, Eistla Regio 344–345 gravity anomaly 332, 333, 334 grooves, asteroids 424, 425 mantle plume 339, 342 Guinevere Planitia 11, 328 Elysium Mons Bouguer gravity anomaly 332, 333, 335, 339 annular graben 198, 199 flank terraces 185, 187, 189, 197, 198 Hadriacus Montes 26, 27, 30 Elysium Planitia 26,30 Hawaii Elysium volcanic province 26,29–30 hotspots 107–108, 113, 114, 115, 119–120 Eminescu Crater, ejecta 305, 308 volcanoes and lithospheric flexure 219, en echelon folds 13, 270, 283–284, 285 220, 228 Enterprise Rupes Hecates Tholus 185, 187, 197, 198 crater counts 167, 169 Hero Rupes, lateral ramp 283, 284 faulted craters 316, 319 hotspot magmatic activity and Rembrandt basin 160, 161, 162, 169–170 Hawaii 107–108, 113, 114, 115, 119–120 strike-slip kinematics 272–275 swell anomalies 112–113 Eros, lineaments 425, 426, 427, 428–430 hydraulic fracture 242–243 Downloaded from http://pubs.geoscienceworld.org/books/book/chapter-pdf/3920420/9781862396777_backmatter.pdf by guest on 01 October 2021 INDEX 445 Iceland mantle plume 337, 339, 341 reservoir failure 241–242 Ida, lineaments 425, 426, 428 summit eruptions and edifice growth 258 igneous effusive rocks, VNIR spectroscopy surface deformation 250, 251, 253 142–154 Tharsis volcanic province 110–111 impact structures Venusian coronae 91–93 Mercury 4,5,7,9,36 magma transport 110–111, 203–204, 210–211, Moon 17 213–215 Venus, identification 373–375 and lithospheric flexure 224 inner solar system 1, 2 inhibition 226–227 Ishtar Terra 11, 328, 329 magnesian suite rocks, lunar 20 Bouguer gravity anomaly 332, 333, 335 Mahuela Tholus, wrinkle ridge detection Itokawa 426, 427, 430 363, 364 mantle diapir, coronae 77, 92 Kanykey Planitia 83 mantle flow Kerguelen Island, slow-moving plates 112–114, 116 Earth 337, 339, 342–343 Kofi basin 5, 6 Venus 10, 12, 342, 343, 344, 345–346 KREEP basalts 20, 21, 131, 141 mantle plumes Procellarum KREEP Terrane 132, 133–134 coronae 77, 92 Kunapipi Mons 82 Earth 107–108, 111–117, 337, 338, 340, 341 Mars 107, 109–110 La Dauphine Rupes, strike-slip kinematics and and rifting 339–340, 342 lateral ramps 280 Venus 10, 12, 13, 15, 332, 333, 337, 342 Lakshmi Planum 11, 328, 342, 344 mare, Moon 17, 127–136 crustal thickness 332, 334 Mare Fecunditatis 17, 18 fault and shear zones 328, 329, 335–336 Mare Imbrium 17, 18,21 Late Heavy Bombardment 5, 159, 319 Mare Nubium 377, 378, 379, 380, 381 lateral ramps, Mercury 269–287 Mare Serenitatis, wrinkle ridges 25 lava flows Marius Hills domes 22 Mars 28, 30, 31 Marquesas Islands, lithospheric flexure 219, 230, Mercury 5 231, 232, 233 Moon 21 Mars 2,27–34 Venus 15–16 age dating 292 coronae 77, 82, 83, 86, 89 canyons 34 Lebanon transpressional ranges 275, 276 crater counting 292 lithosphere crustal dichotomy 33–34, 109, 110, 118, 141 flexure faulting 34 containment of volcanic material 223 graben 34 edifice shape 224–226, 228 dyke-induced 395–402 large volcanic edifices 219–233, 220 lava flows 28, 30, 31 magma ascent 224 lithospheric thickness 220, 221, 225–226 inhibition 226–227 one-plate/stagnant-lid regime 33, 107, 117 stress state 222, 223–224 pit craters 205–206 thickness 220–221 self-similar clustering 209–210, 212 lobate flows, Venus 98,99 pyroclastic cones 31 lobate scarps rootless cones 32 Mercury 6, 7, 8, 9, 280–282, 286, 287, 291 shield volcanoes 27, 28, 31, 107 see also Blossom Rupes fold-and-thrust belt annular graben 198, 199 Moon 27 flank terraces 185–200 Lutetia, lineaments 430–431 flexural trough 199, 205 model 210–211, 213–215 Madeira, slow-moving plates 113–114, Tharsis volcanic province 108–111, 116, 203 116, 119 SPLD deformational systems 405–419 magma reservoirs 203–204 tectonic structures 33–34 elastic models 239–262 tephra 31–32 applicability and limitations 260–261 upwelling and downwelling 110 caldera formation 260 volcanic edifice shape 225–226, 228 circumferential intrusions 258–259 and lithospheric flexure 219, 220 dyke swarm formation 259–260 volcanic rock composition 140, 141 edifice loading model 252–253 volcanic structures 26, 27, 28, 29, 30–32 failure location 247–250, 252 volcaniclastic deposits 32 hydraulic fracture 242–243 volcanism 29–33 Downloaded from http://pubs.geoscienceworld.org/books/book/chapter-pdf/3920420/9781862396777_backmatter.pdf
Load more

Recommended publications
  • Planetary Geologic Mappers Annual Meeting
    Program Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Planetary Geologic Mappers Annual Meeting June 12–14, 2018 • Knoxville, Tennessee Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Science Organizing Committee David Williams, Chair Arizona State University Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Robert Jacobsen Earth and Planetary Sciences Department, University of Tennessee Knoxville Bradley Thomson Earth and Planetary Sciences Department, University of Tennessee Knoxville Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/pgm2018/ Abstracts can be cited as Author A. B. and Author C. D. (2018) Title of abstract. In Planetary Geologic Mappers Annual Meeting, Abstract #XXXX. LPI Contribution No. 2066, Lunar and Planetary Institute, Houston. Guide to Sessions Tuesday, June 12, 2018 9:00 a.m. Strong Hall Meeting Room Introduction and Mercury and Venus Maps 1:00 p.m. Strong Hall Meeting Room Mars Maps 5:30 p.m. Strong Hall Poster Area Poster Session: 2018 Planetary Geologic Mappers Meeting Wednesday, June 13, 2018 8:30 a.m. Strong Hall Meeting Room GIS and Planetary Mapping Techniques and Lunar Maps 1:15 p.m. Strong Hall Meeting Room Asteroid, Dwarf Planet, and Outer Planet Satellite Maps Thursday, June 14, 2018 8:30 a.m. Strong Hall Optional Field Trip to Appalachian Mountains Program Tuesday, June 12, 2018 INTRODUCTION AND MERCURY AND VENUS MAPS 9:00 a.m. Strong Hall Meeting Room Chairs: David Williams Devon Burr 9:00 a.m.
    [Show full text]
  • Abridged Final Report with Resolutions
    Brussels 18–24 September Regional Association VI (Europe) 2009 Fifteenth session Nassau, 18–24 September 2009 XV-RA VI XV-RA WMO-No. 1046 www.wmo.int WMO-No. 1046 Regional Association VI (Europe) Fifteenth session Brussels 18–24 September 2009 Abridged final report with resolutions WMO-No. 1046 WMO-No. 1046 © World Meteorological Organization, 2009 The right of publication in print, electronic and any other form and in any language is reserved by WMO. Short extracts from WMO publications may be reproduced without authorization, provided that the complete source is clearly indicated. Editorial correspondence and requests to publish, reproduce or translate this publication in part or in whole should be addressed to: Chairperson, Publications Board World Meteorological Organization (WMO) 7 bis, avenue de la Paix Tel.: +41 (0) 22 730 84 03 P.O. Box 2300 Fax: +41 (0) 22 730 80 40 CH-1211 Geneva 2, Switzerland E-mail: [email protected] ISBN 978-92-63-11046-6 NOTE The designations employed in WMO publications and the presentation of material in this publication do not imply the expression of any opinion whatsoever on the part of the Secretariat of WMO concerning the legal status of any country, territory, city or area, or of its authorities, or concerning the delimitation of its frontiers or boundaries. Opinions expressed in WMO publications are those of the authors and do not necessarily reflect those of WMO. The mention of specific companies or products does not imply that they are endorsed or recommended by WMO in preference to others of a similar nature which are not mentioned or advertised.
    [Show full text]
  • Copyrighted Material
    Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED
    [Show full text]
  • Eminescu and the Transition to Peak-Ring Basins on Mercury
    41st Lunar and Planetary Science Conference (2010) 1263.pdf EMINESCU AND THE TRANSITION TO PEAK-RING BASINS ON MERCURY. S. C. Schon,1 J. W. Head,1 L. M. Prockter2, and the MESSENGER Science Team.3 1Dept. of Geological Sciences, Brown University, Providence, RI 02906 USA; 2JHU/APL, Laurel, MD; 3http://messenger.jhuapl.edu/who_we_are/science_team.html. Introduction: The MESSENGER [1] flybys have yielded a range of new scientific findings for Mercury [2] including evidence of embayment relationships indicative of volcanic plains activity [3,4] and an im- proved size estimate for the Caloris basin [5]. These new data reveal a broad continuum of Mercurian crater morphologies [6] in greater detail than prior studies that relied on Mariner 10 or Earth-based radar observa- tions [7]. This study focuses on mapping the interior deposits of Eminescu, a central peak-ring basin, and is part of a larger comparative analysis of transitional crater morphologies observed on Mercury and the Moon in new data sets [8]. Impacts on Mercury occur at much higher veloci- ties than lunar impacts and correspondingly generate more impact melt. Cintala [9] estimated that for a given projectile, the velocity difference will lead to twice as much impact melt on Mercury than on the Moon. Here we examine images at ~150 m/pixel reso- Figure 1: Eminescu Crater, ~125-km in diameter (10.8°N, lution of the fresh impact crater Eminescu to document 114.1°E), imaged during the first MESSENGER flyby. the nature of fresh crater interiors on Mercury at the transition from complex to peak-ring morphology.
    [Show full text]
  • Clara E. Sipprell Papers
    Clara E. Sipprell Papers An inventory of her papers at Syracuse University Finding aid created by: - Date: unknown Revision history: Jan 1984 additions, revised (ASD) 14 Oct 2006 converted to EAD (AMCon) Feb 2009 updated, reorganized (BMG) May 2009 updated 87-101 (MRC) 21 Sep 2017 updated after negative integration (SM) 9 May 2019 added unidentified and "House in Thetford, Vermont" (KD) extensively updated following NEDCC rehousing; Christensen 14 May 2021 correspondence added (MRC) Overview of the Collection Creator: Sipprell, Clara E. (Clara Estelle), 1885-1975. Title: Clara E. Sipprell Papers Dates: 1915-1970 Quantity: 93 linear ft. Abstract: Papers of the American photographer. Original photographs, arranged as character studies, landscapes, portraits, and still life studies. Correspondence (1929-1970), clippings, interviews, photographs of her. Portraits of Louis Adamic, Svetlana Allilueva, Van Wyck Brooks, Pearl S. Buck, Rudolf Bultmann, Charles E. Burchfield, Fyodor Chaliapin, Ralph Adams Cram, W.E.B. Du Bois, Albert Einstein, Dorothy Canfield Fisher, Ralph E. Flanders, Michel Fokine, Robert Frost, Eva Hansl, Roy Harris, Granville Hicks, Malvina Hoffman, Langston Hughes, Robinson Jeffers, Louis Krasner, Serge Koussevitzky, Luigi Lucioni, Emil Ludwig, Edwin Markham, Isamu Noguchi, Maxfield Parrish, Sergei Rachmaninoff, Eleanor Roosevelt, Dane Rudhyar, Ruth St. Denis, Otis Skinner, Ida Tarbell, Howard Thurman, Ridgely Torrence, Hendrik Van Loon, and others Language: English Repository: Special Collections Research Center, Syracuse University Libraries 222 Waverly Avenue Syracuse, NY 13244-2010 http://scrc.syr.edu Biographical History Clara E. Sipprell (1885-1975) was a Canadian-American photographer known for her landscapes and portraits of famous actors, artists, writers and scientists. Sipprell was born in Ontario, Canada, a posthumous child with five brothers.
    [Show full text]
  • Glossary Glossary
    Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts.
    [Show full text]
  • Extraordinary Rocks from the Peak Ring of the Chicxulub Impact Crater: P-Wave Velocity, Density, and Porosity Measurements from IODP/ICDP Expedition 364 ∗ G.L
    Earth and Planetary Science Letters 495 (2018) 1–11 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Extraordinary rocks from the peak ring of the Chicxulub impact crater: P-wave velocity, density, and porosity measurements from IODP/ICDP Expedition 364 ∗ G.L. Christeson a, , S.P.S. Gulick a,b, J.V. Morgan c, C. Gebhardt d, D.A. Kring e, E. Le Ber f, J. Lofi g, C. Nixon h, M. Poelchau i, A.S.P. Rae c, M. Rebolledo-Vieyra j, U. Riller k, D.R. Schmitt h,1, A. Wittmann l, T.J. Bralower m, E. Chenot n, P. Claeys o, C.S. Cockell p, M.J.L. Coolen q, L. Ferrière r, S. Green s, K. Goto t, H. Jones m, C.M. Lowery a, C. Mellett u, R. Ocampo-Torres v, L. Perez-Cruz w, A.E. Pickersgill x,y, C. Rasmussen z,2, H. Sato aa,3, J. Smit ab, S.M. Tikoo ac, N. Tomioka ad, J. Urrutia-Fucugauchi w, M.T. Whalen ae, L. Xiao af, K.E. Yamaguchi ag,ah a University of Texas Institute for Geophysics, Jackson School of Geosciences, Austin, USA b Department of Geological Sciences, Jackson School of Geosciences, Austin, USA c Department of Earth Science and Engineering, Imperial College, London, UK d Alfred Wegener Institute Helmholtz Centre of Polar and Marine Research, Bremerhaven, Germany e Lunar and Planetary Institute, Houston, USA f Department of Geology, University of Leicester, UK g Géosciences Montpellier, Université de Montpellier, France h Department of Physics, University of Alberta, Canada i Department of Geology, University of Freiburg, Germany j SM 312, Mza 7, Chipre 5, Resid.
    [Show full text]
  • Mercury's Low-Reflectance Material: Constraints from Hollows
    Mercury’s low-reflectance material: Constraints from hollows Rebecca Thomas, Brian Hynek, David Rothery, Susan Conway To cite this version: Rebecca Thomas, Brian Hynek, David Rothery, Susan Conway. Mercury’s low-reflectance material: Constraints from hollows. Icarus, Elsevier, 2016, 277, pp.455-465. 10.1016/j.icarus.2016.05.036. hal-02271739 HAL Id: hal-02271739 https://hal.archives-ouvertes.fr/hal-02271739 Submitted on 27 Aug 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Accepted Manuscript Mercury’s Low-Reflectance Material: Constraints from Hollows Rebecca J. Thomas , Brian M. Hynek , David A. Rothery , Susan J. Conway PII: S0019-1035(16)30246-9 DOI: 10.1016/j.icarus.2016.05.036 Reference: YICAR 12084 To appear in: Icarus Received date: 23 February 2016 Revised date: 9 May 2016 Accepted date: 24 May 2016 Please cite this article as: Rebecca J. Thomas , Brian M. Hynek , David A. Rothery , Susan J. Conway , Mercury’s Low-Reflectance Material: Constraints from Hollows, Icarus (2016), doi: 10.1016/j.icarus.2016.05.036 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript.
    [Show full text]
  • Feature of the Month – January 2016 Galilaei
    A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: Wayne Bailey [email protected] 17 Autumn Lane, Sewell, NJ 08080 RECENT BACK ISSUES: http://moon.scopesandscapes.com/tlo_back.html FEATURE OF THE MONTH – JANUARY 2016 GALILAEI Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA October 26, 2015 03:32-03:58 UT, 15 cm refl, 170x, seeing 8-9/10 I sketched this crater and vicinity on the evening of Oct. 25/26, 2015 after the moon hid ZC 109. This was about 32 hours before full. Galilaei is a modest but very crisp crater in far western Oceanus Procellarum. It appears very symmetrical, but there is a faint strip of shadow protruding from its southern end. Galilaei A is the very similar but smaller crater north of Galilaei. The bright spot to the south is labeled Galilaei D on the Lunar Quadrant map. A tiny bit of shadow was glimpsed in this spot indicating a craterlet. Two more moderately bright spots are east of Galilaei. The western one of this pair showed a bit of shadow, much like Galilaei D, but the other one did not. Galilaei B is the shadow-filled crater to the west. This shadowing gave this crater a ring shape. This ring was thicker on its west side. Galilaei H is the small pit just west of B. A wide, low ridge extends to the southwest from Galilaei B, and a crisper peak is south of H. Galilaei B must be more recent than its attendant ridge since the crater's exterior shadow falls upon the ridge.
    [Show full text]
  • Shallow Crustal Composition of Mercury As Revealed by Spectral Properties and Geological Units of Two Impact Craters
    Planetary and Space Science 119 (2015) 250–263 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Shallow crustal composition of Mercury as revealed by spectral properties and geological units of two impact craters Piero D’Incecco a,n, Jörn Helbert a, Mario D’Amore a, Alessandro Maturilli a, James W. Head b, Rachel L. Klima c, Noam R. Izenberg c, William E. McClintock d, Harald Hiesinger e, Sabrina Ferrari a a Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, D-12489 Berlin, Germany b Department of Geological Sciences, Brown University, Providence, RI 02912, USA c The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA d Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA e Westfälische Wilhelms-Universität Münster, Institut für Planetologie, Wilhelm-Klemm Str. 10, D-48149 Münster, Germany article info abstract Article history: We have performed a combined geological and spectral analysis of two impact craters on Mercury: the Received 5 March 2015 15 km diameter Waters crater (106°W; 9°S) and the 62.3 km diameter Kuiper crater (30°W; 11°S). Using Received in revised form the Mercury Dual Imaging System (MDIS) Narrow Angle Camera (NAC) dataset we defined and mapped 9 October 2015 several units for each crater and for an external reference area far from any impact related deposits. For Accepted 12 October 2015 each of these units we extracted all spectra from the MESSENGER Atmosphere and Surface Composition Available online 24 October 2015 Spectrometer (MASCS) Visible-InfraRed Spectrograph (VIRS) applying a first order photometric correc- Keywords: tion.
    [Show full text]
  • Triton: Topography and Geology of a Probable Ocean World with Comparison to Pluto and Charon
    remote sensing Article Triton: Topography and Geology of a Probable Ocean World with Comparison to Pluto and Charon Paul M. Schenk 1,* , Chloe B. Beddingfield 2,3, Tanguy Bertrand 3, Carver Bierson 4 , Ross Beyer 2,3, Veronica J. Bray 5, Dale Cruikshank 3 , William M. Grundy 6, Candice Hansen 7, Jason Hofgartner 8 , Emily Martin 9, William B. McKinnon 10, Jeffrey M. Moore 3, Stuart Robbins 11 , Kirby D. Runyon 12 , Kelsi N. Singer 11 , John Spencer 11, S. Alan Stern 11 and Ted Stryk 13 1 Lunar and Planetary Institute, Houston, TX 77058, USA 2 SETI Institute, Palo Alto, CA 94020, USA; chloe.b.beddingfi[email protected] (C.B.B.); [email protected] (R.B.) 3 NASA Ames Research Center, Moffett Field, CA 94035, USA; [email protected] (T.B.); [email protected] (D.C.); [email protected] (J.M.M.) 4 School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85202, USA; [email protected] 5 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85641, USA; [email protected] 6 Lowell Observatory, Flagstaff, AZ 86001, USA; [email protected] 7 Planetary Science Institute, Tucson, AZ 85704, USA; [email protected] 8 Jet Propulsion Laboratory, Pasadena, CA 91001, USA; [email protected] 9 National Air & Space Museum, Washington, DC 20001, USA; [email protected] 10 Department of Earth and Planetary Sciences, Washington University in Saint Louis, Saint Louis, MO 63101, USA; [email protected] 11 Southwest Research Institute, Boulder, CO 80301, USA; [email protected] (S.R.); [email protected] (K.N.S.); [email protected] (J.S.); [email protected] (S.A.S.) Citation: Schenk, P.M.; Beddingfield, 12 Johns Hopkins Applied Physics Laboratory, Laurel, MD 20707, USA; [email protected] 13 C.B.; Bertrand, T.; Bierson, C.; Beyer, Humanities Division, Roane State Community College, Harriman, TN 37748, USA; [email protected] R.; Bray, V.J.; Cruikshank, D.; Grundy, * Correspondence: [email protected] W.M.; Hansen, C.; Hofgartner, J.; et al.
    [Show full text]
  • Impact Cratering
    6 Impact cratering The dominant surface features of the Moon are approximately circular depressions, which may be designated by the general term craters … Solution of the origin of the lunar craters is fundamental to the unravel- ing of the history of the Moon and may shed much light on the history of the terrestrial planets as well. E. M. Shoemaker (1962) Impact craters are the dominant landform on the surface of the Moon, Mercury, and many satellites of the giant planets in the outer Solar System. The southern hemisphere of Mars is heavily affected by impact cratering. From a planetary perspective, the rarity or absence of impact craters on a planet’s surface is the exceptional state, one that needs further explanation, such as on the Earth, Io, or Europa. The process of impact cratering has touched every aspect of planetary evolution, from planetary accretion out of dust or planetesimals, to the course of biological evolution. The importance of impact cratering has been recognized only recently. E. M. Shoemaker (1928–1997), a geologist, was one of the irst to recognize the importance of this process and a major contributor to its elucidation. A few older geologists still resist the notion that important changes in the Earth’s structure and history are the consequences of extraterres- trial impact events. The decades of lunar and planetary exploration since 1970 have, how- ever, brought a new perspective into view, one in which it is clear that high-velocity impacts have, at one time or another, affected nearly every atom that is part of our planetary system.
    [Show full text]