DOCSLIB.ORG

Ice-Dust Mantles on Mars

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Ice-Dust Mantles on Mars Ice-dust mantles on Mars David Hollibaugh Baker NASA Goddard Space Flight Center SWIM Team Telecon 25 October 2018 Glacial deposits, plains, and mantle units mapped from CTX image mosaic at 1:50,000 scale Study Area: Deuteronilus Mensae SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 2 Three units mapped in study area Plains Mantle Glacial Deposits SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 3 Morphologic evidence of ~100 m thick mantle unit onlapping glacial deposits Mantle Mantle Glacial Deposit Glacial Deposit Mantle Plains HRSC DTM data Baker and Head (2015) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 4 Relatively smooth with: Rimless craters. Small pockmarks or depressions. Fractures <20 m in width; some forming circular patterns. SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 5 Upl LDA CTX image P13_006160_2252 SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 6 Morphologic evidence of ~100 m thick mantle unit onlapping glacial deposits Mangold (2003) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 7 Mantle shows collapse features and fractures, possibly related to sublimation of buried ice Mantle Mantle Glacial Deposits SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 8 Middle Amazonian (~500 Ma) age SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 9 Analyzed SHARAD Radargrams Plains Mantle Glacial Deposits SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 10 279 SHARAD tracks analyzed over mantle SHARAD tracks analyzed SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 11 101 SHARAD tracks showed reflectors SHARAD tracks with reflectors SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 12 101 SHARAD tracks showed reflectors Thick and continuous: Thin and Many reflectors patchy: Few reflectors SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 13 Thick occurrences of mantle unit Glacial Deposits Surrounded by glacial deposits Isolated Patch Plains SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 14 Tw o -way time delays show deep and shallow reflectors shallow deep SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 15 Histogram of two-way time delays 800 shallow 700 600 500 400 deep 300 Frequency 200 100 0 0 0.75 1.75 2.75 3.75 4.75 5.75 6.75 7.75 8.75 9.75 Two-Way Time Delay (µs) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 16 Shallow reflectors in mantle surrounded by plains SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 17 Reflector traces compared with clutter simulations to confirm source radargram 1μs unit boundaries (PDS, US) traced 1μs surface radargram clutter reflection subsurface reflector clutter simulation (UT) Choudhary et al. (2016) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 18 Upper plains mantle likely desiccated from original ice content. Consistent with mAl of Skinner et al. (2012) LDA Mantle on ε ~ 5 LDA Mantle SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 19 Middle Amazonian Lowland Unit (mAl) (Skinner et al., 2012) LPSC 48, 21 March 2017 - Baker and Carter, Mars Radar Reflectors - 20 Skinner et al. (2012): “Our observations are consistent with the widespread emplacement of a loess-like deposit tens of meters thick in the Martian northern lowlands during the Middle Amazonian due to climate-driven erosion of the north polar plateau” SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 21 Pedestal Craters (Kadish et al., 2009) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 22 Utopia Planitia – Scalloped Terrain SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 23 Utopia Planitia Utopia Planitia Deuteronilus Mensae Deuteronilus Mensae Utopia Planitia Continuous Mantle Thickness of several tens of meters. Highly polygonalized. Latitude-dependent degradation dominated by sublimation and differences in insolation. Lower Plains SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 24 Mantle in Arcadia (Ramsdale et al., 2018) pitted smooth SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 25 Arcadia Expanded Secondaries (Viola et al., 2015) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 26 Hellas Region (LeFort et al., 2010) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 27 Southern Mid-Latitude Scarps (Dundas et al., 2018) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 28 Latitude Dependent Mantle e.g., Mustard et al., 2001; Miliken et al., 2003; Head et al., 2003; Kostama et al., 2006; Schon et al., 2009 Mean crater retention age of 0.1 Ma (Kostama et al., 2006); older at southern latitudes. Thickness of several meters to tens of meters. Desiccation via sublimation at mid- latitude regions during low obliquity excursions. LPSC 48, 21 March 2017 - Baker and Carter, Mars Radar Reflectors - 29 Dickson et al. (2015) SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 30 SWIM Telecon, 10/25/2018 - Hollibaugh Baker, Mars Mantle - 31.
Load more

Recommended publications
  • North Polar Region of Mars: Advances in Stratigraphy, Structure, and Erosional Modification
    Icarus 196 (2008) 318–358 www.elsevier.com/locate/icarus North polar region of Mars: Advances in stratigraphy, structure, and erosional modification Kenneth L. Tanaka a,∗, J. Alexis P. Rodriguez b, James A. Skinner Jr. a,MaryC.Bourkeb, Corey M. Fortezzo a,c, Kenneth E. Herkenhoff a, Eric J. Kolb d, Chris H. Okubo e a US Geological Survey, Flagstaff, AZ 86001, USA b Planetary Science Institute, Tucson, AZ 85719, USA c Northern Arizona University, Flagstaff, AZ 86011, USA d Google, Inc., Mountain View, CA 94043, USA e Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA Received 5 June 2007; revised 24 January 2008 Available online 29 February 2008 Abstract We have remapped the geology of the north polar plateau on Mars, Planum Boreum, and the surrounding plains of Vastitas Borealis using altimetry and image data along with thematic maps resulting from observations made by the Mars Global Surveyor, Mars Odyssey, Mars Express, and Mars Reconnaissance Orbiter spacecraft. New and revised geographic and geologic terminologies assist with effectively discussing the various features of this region. We identify 7 geologic units making up Planum Boreum and at least 3 for the circumpolar plains, which collectively span the entire Amazonian Period. The Planum Boreum units resolve at least 6 distinct depositional and 5 erosional episodes. The first major stage of activity includes the Early Amazonian (∼3 to 1 Ga) deposition (and subsequent erosion) of the thick (locally exceeding 1000 m) and evenly- layered Rupes Tenuis unit (ABrt), which ultimately formed approximately half of the base of Planum Boreum. As previously suggested, this unit may be sourced by materials derived from the nearby Scandia region, and we interpret that it may correlate with the deposits that regionally underlie pedestal craters in the surrounding lowland plains.
    [Show full text]
  • Thursday, October 29, 2015 HIGH-LATITUDE I 10:00 A.M. Lecture Hall
    First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars (2015) sess302.pdf Thursday, October 29, 2015 HIGH-LATITUDE I 10:00 a.m. Lecture Hall 10:00 a.m. Head J. W. III * Dickson J. Milliken R. Scott D. Johnson B. Marchant D. Levy J. Kinch K. Hvidberg C. Forget F. Boucher D. Mikucki J. Fastook J. Klaus K. Mars Human Science Exploration and Resource Utilization: The Dichotomy Boundary Deuteronilus Mensae Exploration Zone [#1033] Deuteronilus Mensae EZ combines: 1) Fundamental MEPAG scientific objectives; 2) Samples from the Noachian, Hesperian and Amazonian); 3) ISRU access to abundant water ice mapped by SHARAD; 4) Civil engineering to reduce reliance on Earth supplies. 10:15 a.m. Rice J. W. Jr. * Crown D. A. Feldman W. C. Pathare A. V. Feustel A. J. Gertsch L. S. Manned Mars Mission Exploration Zone: Eastern Rim of Hellas Impact Basin [#1038] Our proposed 200 km diameter Exploration Zone centered near 40°S; 104°E is located along the eastern rim of the Hellas basin which will allow astronauts to study and collect very ancient deep seated materials which were excavated in the impact event. 10:30 a.m. Levy J. S. * Holt J. W. A Human Landing Site on the Hellas Rim: Ancient Craters, Flowing Water, and Abundant Ice [#1037] Hellas basin rim/Ancient highlands and lavas/Lots of ice to drink. 10:45 a.m. Plaut J. J. * A Resource-Rich, Scientifically Compelling Exploration Zone for Human Missions at Deuteronilus Mensae, Mars [#1044] The Deuteronilus Mensae region of Mars is promising as a potential landing site for human exploration because it contains vast, readily accessible deposits of water ice in a setting of key scientific importance.
    [Show full text]
  • De Jóvenes Investigadores
    Actas 30º Certamen Jóvenes Investigadores Directora General del Instituto de la Juventud Ruth Carrasco Ruiz Secretario General de Universidades José Manuel Pingarrón Carrazón Director Científico del Certamen Dr. Jesús F. Jordá Pardo Coordinadoras de la publicación Marta Jurado Marta Leyra Diseño gráfico y maquetación Elsa Paricio Textos Autores de los proyectos seleccionados © de los textos e imágenes, sus autores Edita INJUVE (Instituto de la Juventud) C/ Marqués del Riscal, 16, Madrid www.INJUVE.es Catálogo General de Publicaciones Oficiales https://publicacionesoficiales.boe.es NIPO: 684-18-029-9 Madrid, 2018 ÍNDICE - 06 - Directora General - 08 - Secretario General de Universidades - 11 - Presentación del Certamen - 15 - CIENCIAS SOCIALES Y JURÍDICAS - 17 - Economía colaborativa en suspensión: legalidad o no de Uber y Blablacar - 27 - ¿Qué horas son estas? Estudio sobre la racionalización de los horarios españoles - 35 - La otra cara de Molina. Radiografía socioeconómica de la pobreza, la mendicidad, los rebuscadores en los contenedores de basura y el “sinhogarismo” en el municipio de Molina de Segura (Murcia) - 47 - La sanidad no es un gasto, es una inversión - 57 - “Llevarse a la novia”. Usos matrimoniales en una comunidad rural. Lorquí (1934 - 1983) - 67 - Enseñar a enseñar - 77 - ¿Tradición o imposición? Evolución del papel de la mujer en Granollers (Barcelona). Una visión interdisciplinaria - 87 - La industria de la cultura: Evolución Humana, Revolución Económica - 95 - ARTES Y HUMANIDADES - 97 - La barbarie en la primera guerra carlista - 107 - El “gracioso” de La traición en la amistad de María de Zayas y Sotomayor - 115 - Olvido es nombre de mujer - 123 - Un estudio sobre la existencia de varios tipos de caballería superpesada en el bajo Imperio Romano - 131 - Análisis de las causas de la ocupación de la Isla Formosa por parte de la Corona española - 139 - Neoliberalismo y Darwinismo social.
    [Show full text]
  • FIFTH INTERNATIONAL CONFERENCE on MARS POLAR SCIENCE and EXPLORATION September 12-16, 2011 Fairbanks, Alaska
    FIFTH INTERNATIONAL CONFERENCE ON MARS POLAR SCIENCE AND EXPLORATION September 12-16, 2011 Fairbanks, Alaska Sponsored By Lunar and Planetary Institute University of Alaska-Fairbanks NASA Mars Program Office International Association of Cryospheric Sciences Centre for Research in Earth and Space Sciences, York University Conveners Stephen Clifford, Lunar and Planetary Institute Kenji Yoshikawa, University ofAlaska-Fair banks David Beaty, NASA Mars Program Office-Jet Propulsion Laboratory Shane Byrne, University ofArizona David Fisher, Geological Survey of Canada Francois Forget, Universite Paris 6 Michael Hecht, Jet Propulsion Laboratory Peter Smith, University ofArizona Leslie Tamppari, Jet Propulsion Laboratory Timothy Titus, U.S. Geological Survey-Flagstaff Scientific Organizing Committee Jean-Pierre Bibring, Institut d'Astrophysique Spatiale Denis Lacelle, University of Ottawa Wendy Calvin, University ofNevada Chris McKay, NASA Ames Research Center Francois Costard, IDES Universite Paris-Sud Ii Sarah Milkovich, Jet Propulsion Laboratory Peter Doran, University ofIllinois at Chicago Gian-Gabrielle Ori , International Research School of William Durham, Massachusetts institute a/Technology Planetary Sciences Ralf Greve, Hokkaido University Roger Philips, Southwest Research Institute Robert Haberle. NASA Ames Research Center Jeff Plaut, Jet Propulsion Laboratory Candy Hansen, Planetary Science institute Nathan Putzig, Southwest Research Institute Jim Head, Brown University James Rice Jr., NASA Goddard Space Flight Center Ken Herkenhoff,
    [Show full text]
  • Modern Mars' Geomorphological Activity
    Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, Matthew Chojnacki, Susan Conway, Colin Dundas, Candice Hansen, Alfred Mcewen, et al. To cite this version: Serina Diniega, Ali Bramson, Bonnie Buratti, Peter Buhler, Devon Burr, et al.. Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity. Geomorphology, Elsevier, 2021, 380, pp.107627. 10.1016/j.geomorph.2021.107627. hal-03186543 HAL Id: hal-03186543 https://hal.archives-ouvertes.fr/hal-03186543 Submitted on 31 Mar 2021 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. 1 Title: Modern Mars’ geomorphological activity, driven by wind, frost, and gravity 2 3 Authors: Serina Diniega1,*, Ali M. Bramson2, Bonnie Buratti1, Peter Buhler3, Devon M. Burr4, 4 Matthew Chojnacki3, Susan J. Conway5, Colin M. Dundas6, Candice J. Hansen3, Alfred S. 5 McEwen7, Mathieu G. A. Lapôtre8, Joseph Levy9, Lauren Mc Keown10, Sylvain Piqueux1, 6 Ganna Portyankina11, Christy Swann12, Timothy N. Titus6,
    [Show full text]
  • USGS Scientific Investigations Map 3079, Pamphlet
    Prepared for the National Aeronautics and Space Administration Geologic Map of MTM 35337, 40337, and 45337 Quadrangles, Deuteronilus Mensae Region of Mars By Frank C. Chuang and David A. Crown Pamphlet to accompany Scientific Investigations Map 3079 65° 65° MC–1 MC–3 MC–6 MC–4 MC–5 30° 30° 300° 60° MC–10 MC–11 MC–12 MC–13 270° 315° 0° 45° 90° 0° 0° MC–18 MC–19 MC–20 MC–21 300° 60° –30° –30° MC–26 MC–27 MC–25 MC–28 MC–30 –65° –65° 2009 U.S. Department of the Interior U.S. Geological Survey INTRODUCTION difference between the highlands and lowlands could be ~100 m.y. (Frey, 2006). Furthermore, understanding the origin and age of the dichotomy boundary has been made more compli- Deuteronilus Mensae, first defined as an albedo feature at cated due to significant erosion and deposition that have modi- lat 35.0° N., long 5.0° E., by U.S. Geological Survey (USGS) fied the boundary and its adjacent regions (Skinner and others, and International Astronomical Union (IAU) nomenclature, is 2004; Irwin and others, 2004; Tanaka and others, 2005; Head a gradational zone along the dichotomy boundary (Watters and and others, 2006a; Rodriguez and others, 2006). The resulting McGovern, 2006) in the northern mid-latitudes of Mars. The diversity of terrains and features is likely a combined result of boundary in this location includes the transition from the rugged ancient and recent events. Detailed geologic analyses of dichot- cratered highlands of Arabia Terra to the northern lowland omy boundary zones are important for understanding the spatial plains of Acidalia Planitia (fig.
    [Show full text]
  • A Model for the Hydrologic and Climatic Behavior of Water on Mars
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 98, NO. E6, PAGES 10,973-11,016, JUNE 25, 1993 A Model for the Hydrologicand Climatic Behavior of Water on Mars STEPHEN M. CLIFFORD Lunar and Planetary Institute,Houston, Texas Paststudies of the climaticbehavior of wateron Mars haveuniversally assumed that the atmosphereis the sole pathwayavailable for volatileexchange between the planet'scrustal and polar reservoirs of H20. However,if the planetaryinventory of outgassedH20 exceedsthe pore volume of thecryosphere by morethan a few percent,then a subpermafrostgroundwater system of globalextent will necessarilyresult. The existenceof sucha systemraises the possibilitythat subsurface transport may complementlong-term atmospheric exchange. In thispaper, the hydrologic responseof a water-richMars to climatechange and to the physicaland thermal evolution of its crustis considered. The analysisassumes that the atmosphericleg of the planet'slong-term hydrologic cycle is reasonablydescribed by current models of insolation-drivenexchange. Under the climatic conditionsthat have apparentlyprevailed throughoutmost of Martiangeologic history, the thermalinstability of groundice at low- to mid-latitudeshas led to a netatmospheric transport of H20 fromthe "hot"equatorial region to the colderpoles. Theoretical arguments and variouslines of morphologicevidence suggest that thispoleward flux of H20 hasbeen episodically augmented by additionalreleases of water resultingfrom impacts,catastrophic floods, and volcanism.Given an initially ice- saturatedcryosphere, the deposition of materialat thepoles (or any otherlocation on the planet'ssurface) will result in a situationwhere the local equilibrium depth to the meltingisotherm has been exceeded, melting ice at thebase of the cryosphereuntil thermodynamicequilibrium is once again established.The downwardpercolation of basal meltwaterinto the globalaquifer will resultin the riseof the local watertable in the form of a groundwatermound.
    [Show full text]
  • Timing of Oceans on Mars from Shoreline Deformation Robert I
    Timing of oceans on Mars from shoreline deformation Robert I. Citron1,2, Michael Manga1,2, Douglas J. Hemingway1,2 Abstract Widespread evidence points to the existence of an ancient Martian ocean1,2,3,4,5,6,7,8. Most compelling are the putative ancient shorelines in the northern plains2,7. However, these shorelines fail to follow an equipotential surface, and this has been used to challenge the notion that they formed via an early ocean9 and hence to question the existence of such an ocean. The shorelines’ deviation from a constant elevation can be explained by true polar wander occurring after the formation of Tharsis10, a volcanic province that dominates the gravity and topography of Mars. However, surface loading from the oceans can drive polar wander only if Tharsis formed far from the equator10, and most evidence indicates that Tharsis formed near the equator11,12,13,14,15, meaning that there is no current explanation for the shorelines’ deviation from an equipotential that is consistent with our geophysical understanding of Mars. Here we show that variations in shoreline topography can be explained by deformation caused by the emplacement of Tharsis. We find that the shorelines must have formed before and during the emplacement of Tharsis, instead of afterwards, as previously assumed. Our results imply that oceans on Mars formed early, concurrent with the valley networks 15, and point to a close relationship between the evolution of oceans on Mars and the initiation and decline of Tharsis volcanism, with broad implications for the geology, hydrological cycle and climate of early Mars.
    [Show full text]
  • The Dichotomy Boundary Deuteronilus Mensae
    First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars (2015) 1033.pdf MARS HUMAN SCIENCE EXPLORATION AND RESOURCE UTILIZATION: THE DICHOTOMY BOUNDARY DEUTERONILUS MENSAE EXPLORATION ZONE James Head1, James Dickson1, John Mustard1, Ralph Milliken1, David Scott1, Brandon Johnson1, David Marchant2, Joseph Levy3, Kjartan Kinch4, Christine Hvidberg4, Francois Forget5, Dale Boucher6, Jill Mikucki7, James Fastook8, Kurt Klaus9. 1Brown University, Providence, RI USA; 2Boston University, Boston, MA USA; 3University of Texas Institute for Geophysics, Austin, TX USA; 4Nils Bohr Institute, University of Copenhagen, Copenhagen, Denmark; 5Laboratoire de Météorologie Dy- namique, Université Pierre et Marie Curie, Paris, France; 6Deltion Innovations, Capreol, Ontario CA; 7Middlebury College, Mid- dlebury, VT USA; 8University of Maine, Orono, ME USA; 9Boeing Company, Houston, TX USA. [email protected] The Dichotomy Boundary Deuteronilus Mensae (DBDM) Exploration Zone (EZ) (39.11˚ N, 23.199˚ E) combines: 1) Fundamental MEPAG scientific objectives for the exploration of Mars (geology, atmos- phere/climate history, hydrology, astrobiology)(1-6; 8-18); 2) Samples/questions from each of the three major geologic eras (Noachian, Hesperian, Amazonian); 3) The certainty of ISRU (I), including access to abundant stores of water ice mapped by SHARAD (16); and 4) Civil Engineering (CE) opportunities, in- cluding manipulating material/ice and reducing reliance on Earth supplies. We combine these four themes into the term Science/ICE. We illustrate the Science/ICE theme in the selection of our current top priority EZ along the DB (Figure 1), among numerous candidate DB EZ sites we have investigated (Figure 2). Figure 1. The Dichotomy Boundary Deuter- onilus Mensae (DBDM) Exploration Zone (EZ) outlined as a circle of 100 km radius, with the Landing Site/Surface Field Station (denoted by star) centrally located and slightly separated to assure safe descent and ascent.
    [Show full text]
  • Geologic Map of the Northern Plains of Mars
    Prepared for the National Aeronautics and Space Administration Geologic Map of the Northern Plains of Mars By Kenneth L. Tanaka, James A. Skinner, Jr., and Trent M. Hare Pamphlet to accompany Scientific Investigations Map 2888 180° E E L Y S I U M P L A N I T I A A M A Z O N I S P L A N I T I A A R C A D I A P L A N I T I A N U T O P I A 0° N P L A N I T I A 30° T I T S A N A S V 60° I S I D I S 270° E 90° E P L A N I T I A B O S R E A L I A C I D A L I A P L A N I T I A C H R Y S E P L A N I T I A 2005 0° E U.S. Department of the Interior U.S. Geological Survey blank CONTENTS Page INTRODUCTION . 1 PHYSIOGRAPHIC SETTING . 1 DATA . 2 METHODOLOGY . 3 Unit delineation . 3 Unit names . 4 Unit groupings and symbols . 4 Unit colors . 4 Contact types . 4 Feature symbols . 4 GIS approaches and tools . 5 STRATIGRAPHY . 5 Early Noachian Epoch . 5 Middle and Late Noachian Epochs . 6 Early Hesperian Epoch . 7 Late Hesperian Epoch . 8 Early Amazonian Epoch . 9 Middle Amazonian Epoch . 12 Late Amazonian Epoch . 12 STRUCTURE AND MODIFICATION HISTORY . 14 Pre-Noachian . 14 Early Noachian Epoch .
    [Show full text]
  • ICE TABLES, GLACIERS, and PERIGLACIAL LANDFORMS 8:30 A.M
    41st Lunar and Planetary Science Conference (2010) sess202.pdf Tuesday, March 2, 2010 TERRESTRIAL PLANET CRYOSPHERES: ICE TABLES, GLACIERS, AND PERIGLACIAL LANDFORMS 8:30 a.m. Waterway Ballroom 4 Chairs: Stephen Clifford Douglas Kowalewski 8:30 a.m. Grimm R. E. * Painter S. L. The Secular Loss of Groundwater on Mars [#1329] The instability of ice at low latitudes on Mars also leads to massive groundwater evaporation. If loss has been retarded by lateral heterogeneity, the mid-latitude northern plains may be the last, best hope for accessible groundwater. 8:45 a.m. Clifford S. M. * Lasue J. The Evolution and Fate of Groundwater on Mars: The Influence of Modeling Assumptions and Consistency of Predictions with Observational Constraints [#2739] Two models of the hydrologic evolution of Mars are compared to identify the basis for their differing conclusions regarding the survival and distribution of present-day groundwater. 9:00 a.m. Plaut J. J. * Holt J. W. Head J. W. III Gim Y. Choudhary P. Baker D. M. Kress A. SHARAD Team Thick Ice Deposits in Deuteronilus Mensae, Mars: Regional Distribution from Radar Sounding [#2454] Radar sounding data from SHARAD on MRO are used to map the distribution of mid-latitude ice in the Deuteronilus Mensae region of Mars. Ice is widespread in the region, with thicknesses up to 1 km. 9:15 a.m. Kadish S. J. * Head J. W. Impacts into Ice-rich Deposits on Mars: Excess Ejecta Craters, Perched Craters, and Pedestal Craters [#1017] We compare formation mechanisms based on impacts into ice-rich material for excess ejecta craters, perched craters, and pedestal craters.
    [Show full text]
  • Back Matter (PDF)
    Index Page numbers in italic refer to Figures. Page numbers in bold refer to Tables. Abalos Colles 257, 258, 259 channel networks 5–6 cratered cones 259, 271, 275 formation 9 layered cones 258, 259, 260, 261, Lethe Vallis 206–226 268–271, 273–275 anastomosing patterns 220 erosion 261, 268 outflow 11–12, 12 Abalos Mensa 258, 267 Sulci Gordii 231, 232–255 ablation, solar, Chasma Boreale 277 chaos regions 12 adsorption 146 interior layered deposits 281, 282, 284, 285, Adventdalen, Spitzbergen 113, 114 286, 289–290, 292, 294 periglacial landforms 118 comparison with Valles Marineris 295–296 comparison with Mars 115–118 Chasma Boreale 257, 258, 259, 267 ice-wedge polygons 121 elevation 262–263, 264, 269 aeolian processes 10, 13, 15 formation 276–277 air-fall accumulation, Chasma Boreale 277 air-fall accumulation 277 alases 133, 143 wind erosion 277 Alba Patera Formation 50 outflow event 275, 277 albedo 5, 6 Chryse Planitia, sublimation landforms, ejecta alcove-channel-apron gully morphology 151, 152, 153 blankets 141 alluvial flow clastic forms gully formation 174 blockfields 92, 93, 95, 98, 107 slope–area analysis 185 circles 92, 94, 103 Earth study sites 183, 184, 186, 189 garlands 92, 103 Amazonian epoch 9 islands 90–91, 92, 108 Amazonis Planitia 5 lobate 93–94, 98, 103, 105 thaw 88 Spitzbergen 116, 117 Aorounga Impact Crater, Chad 33 Thaumasia 76, 77–78, 79, 80, 81,82 Arabia Terra 5 nets 91, 92 Aram Chaos, interior layered deposits 282, 285, 286 protalus lobes and ramparts, Arcadia Formation 50 Spitzbergen 117 Ares Vallis stripes 92, 93–94,
    [Show full text]