Gale Crater: the Mars Science Laboratory/ Curiosity Rover Landing Site
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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. -
Curiosity's Candidate Field Site in Gale Crater, Mars
Curiosity’s Candidate Field Site in Gale Crater, Mars K. S. Edgett – 27 September 2010 Simulated view from Curiosity rover in landing ellipse looking toward the field area in Gale; made using MRO CTX stereopair images; no vertical exaggeration. The mound is ~15 km away 4th MSL Landing Site Workshop, 27–29 September 2010 in this view. Note that one would see Gale’s SW wall in the distant background if this were Edgett, 1 actually taken by the Mastcams on Mars. Gale Presents Perhaps the Thickest and Most Diverse Exposed Stratigraphic Section on Mars • Gale’s Mound appears to present the thickest and most diverse exposed stratigraphic section on Mars that we can hope access in this decade. • Mound has ~5 km of stratified rock. (That’s 3 miles!) • There is no evidence that volcanism ever occurred in Gale. • Mound materials were deposited as sediment. • Diverse materials are present. • Diverse events are recorded. – Episodes of sedimentation and lithification and diagenesis. – Episodes of erosion, transport, and re-deposition of mound materials. 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 2 Gale is at ~5°S on the “north-south dichotomy boundary” in the Aeolis and Nepenthes Mensae Region base map made by MSSS for National Geographic (February 2001); from MOC wide angle images and MOLA topography 4th MSL Landing Site Workshop, 27–29 September 2010 Edgett, 3 Proposed MSL Field Site In Gale Crater Landing ellipse - very low elevation (–4.5 km) - shown here as 25 x 20 km - alluvium from crater walls - drive to mound Anderson & Bell -
Supervolcanoes Within an Ancient Volcanic Province in Arabia Terra, Mars 2 3 4 Joseph
EMBARGOED BY NATURE 1 1 Supervolcanoes within an ancient volcanic province in Arabia Terra, Mars 2 3 4 Joseph. R. Michalski 1,2 5 1Planetary Science Institute, Tucson, Arizona 85719, [email protected] 6 2Dept. of Earth Sciences, Natural History Museum, London, United Kingdom 7 8 Jacob E. Bleacher3 9 3NASA Goddard Space Flight Center, Greenbelt, MD, USA. 10 11 12 Summary: 13 14 Several irregularly shaped craters located within Arabia Terra, Mars represent a 15 new type of highland volcanic construct and together constitute a previously 16 unrecognized martian igneous province. Similar to terrestrial supervolcanoes, these 17 low-relief paterae display a range of geomorphic features related to structural 18 collapse, effusive volcanism, and explosive eruptions. Extruded lavas contributed to 19 the formation of enigmatic highland ridged plains in Arabia Terra. Outgassed sulfur 20 and erupted fine-grained pyroclastics from these calderas likely fed the formation of 21 altered, layered sedimentary rocks and fretted terrain found throughout the 22 equatorial region. Discovery of a new type of volcanic construct in the Arabia 23 volcanic province fundamentally changes the picture of ancient volcanism and 24 climate evolution on Mars. Other eroded topographic basins in the ancient Martian 25 highlands that have been dismissed as degraded impact craters should be 26 reconsidered as possible volcanic constructs formed in an early phase of 27 widespread, disseminated magmatism on Mars. 28 29 30 EMBARGOED BY NATURE 2 31 The source of fine-grained, layered deposits1,2 detected throughout the equatorial 32 region of Mars3 remains unresolved, though the deposits are clearly linked to global 33 sedimentary processes, climate change, and habitability of the surface4. -
The Evolution of a Heterogeneous Martian Mantle: Clues from K, P, Ti, Cr, and Ni Variations in Gusev Basalts and Shergottite Meteorites
Earth and Planetary Science Letters 296 (2010) 67–77 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites Mariek E. Schmidt a,⁎, Timothy J. McCoy b a Dept. of Earth Sciences, Brock University, St. Catharines, ON, Canada L2S 3A1 b Dept. of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119, USA article info abstract Article history: Martian basalts represent samples of the interior of the planet, and their composition reflects their source at Received 10 December 2009 the time of extraction as well as later igneous processes that affected them. To better understand the Received in revised form 16 April 2010 composition and evolution of Mars, we compare whole rock compositions of basaltic shergottitic meteorites Accepted 21 April 2010 and basaltic lavas examined by the Spirit Mars Exploration Rover in Gusev Crater. Concentrations range from Available online 2 June 2010 K-poor (as low as 0.02 wt.% K2O) in the shergottites to K-rich (up to 1.2 wt.% K2O) in basalts from the Editor: R.W. Carlson Columbia Hills (CH) of Gusev Crater; the Adirondack basalts from the Gusev Plains have more intermediate concentrations of K2O (0.16 wt.% to below detection limit). The compositional dataset for the Gusev basalts is Keywords: more limited than for the shergottites, but it includes the minor elements K, P, Ti, Cr, and Ni, whose behavior Mars igneous processes during mantle melting varies from very incompatible (prefers melt) to very compatible (remains in the shergottites residuum). -
General Vertical Files Anderson Reading Room Center for Southwest Research Zimmerman Library
“A” – biographical Abiquiu, NM GUIDE TO THE GENERAL VERTICAL FILES ANDERSON READING ROOM CENTER FOR SOUTHWEST RESEARCH ZIMMERMAN LIBRARY (See UNM Archives Vertical Files http://rmoa.unm.edu/docviewer.php?docId=nmuunmverticalfiles.xml) FOLDER HEADINGS “A” – biographical Alpha folders contain clippings about various misc. individuals, artists, writers, etc, whose names begin with “A.” Alpha folders exist for most letters of the alphabet. Abbey, Edward – author Abeita, Jim – artist – Navajo Abell, Bertha M. – first Anglo born near Albuquerque Abeyta / Abeita – biographical information of people with this surname Abeyta, Tony – painter - Navajo Abiquiu, NM – General – Catholic – Christ in the Desert Monastery – Dam and Reservoir Abo Pass - history. See also Salinas National Monument Abousleman – biographical information of people with this surname Afghanistan War – NM – See also Iraq War Abousleman – biographical information of people with this surname Abrams, Jonathan – art collector Abreu, Margaret Silva – author: Hispanic, folklore, foods Abruzzo, Ben – balloonist. See also Ballooning, Albuquerque Balloon Fiesta Acequias – ditches (canoas, ground wáter, surface wáter, puming, water rights (See also Land Grants; Rio Grande Valley; Water; and Santa Fe - Acequia Madre) Acequias – Albuquerque, map 2005-2006 – ditch system in city Acequias – Colorado (San Luis) Ackerman, Mae N. – Masonic leader Acoma Pueblo - Sky City. See also Indian gaming. See also Pueblos – General; and Onate, Juan de Acuff, Mark – newspaper editor – NM Independent and -
Evidence for Thermal-Stress-Induced Rockfalls on Mars Impact Crater Slopes
Icarus 342 (2020) 113503 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Evidence for thermal-stress-induced rockfalls on Mars impact crater slopes P.-A. Tesson a,b,*, S.J. Conway b, N. Mangold b, J. Ciazela a, S.R. Lewis c, D. M�ege a a Space Research Centre, Polish Academy of Science, Wrocław, Poland b Laboratoire de Plan�etologie et G�eodynamique UMR 6112, CNRS, Nantes, France c School of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK ARTICLE INFO ABSTRACT Keywords: Here we study rocks falling from exposed outcrops of bedrock, which have left tracks on the slope over which Mars, surface they have bounced and/or rolled, in fresh impact craters (1–10 km in diameter) on Mars. The presence of these Thermal stress tracks shows that these rocks have fallen relatively recently because aeolian processes are known to infill Ices topographic lows over time. Mapping of rockfall tracks indicate trends in frequency with orientation, which in Solar radiation � � turn depend on the latitudinal position of the crater. Craters in the equatorial belt (between 15 N and 15 S) Weathering exhibit higher frequencies of rockfall on their north-south oriented slopes compared to their east-west ones. � Craters >15 N/S have notably higher frequencies on their equator-facing slopes as opposed to the other ori entations. We computed solar radiation on the surface of crater slopes to compare insolation patterns with the spatial distribution of rockfalls, and found statistically significant correlations between maximum diurnal inso lation and rockfall frequency. -
Hirise Camera Views the Mars Rover 'Spirit' at 'Home Plate' 26 November 2007
HiRISE Camera Views the Mars Rover 'Spirit' at 'Home Plate' 26 November 2007 Herkenhoff said. At the time, the camera was flying about 270 kilometers, or about 168 miles, over the surface. At that distance, the camera could resolve objects about 81 centimeters, or about 32 inches, across. The sun was about 56 degrees above the horizon in the winter afternoon sky. The HiRISE image of Home Plate and others are on the HiRISE Website, hirise.lpl.arizona.edu . HiRISE operations are based at The University of Arizona in Tucson. Professor Alfred S. McEwen of the Lunar and Planetary Laboratory is principal investigator for the experiment. The Mars rover "Spirit" is indicated by a circle on "Home Plate" in this new image of Gusev Crater on Mars. This The HiRISE camera is the most powerful camera detail is part of a much larger image the HiRISE camera ever to orbit another planet. It has taken thousands took on Sept. 27, 2007. The rover has since driven of black-and-white images, and hundreds of color north. (Photo: NASA/JPL/University of Arizona) images, since it began science operations in 2006. A single HiRISE image will often be a multigigabyte image that measures 20,000 pixels by 50,000 The High Resolution Imaging Science Experiment, pixels, which includes a 4,000-by-50,000 pixel or HiRISE, camera onboard NASA's Mars region in three colors. It can take a computer up to Reconnaissance Orbiter has taken a new color three hours to process such an image. image of the feature dubbed "Home Plate" in Gusev Crater on Mars. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
11 Fall Unamagazine
FALL 2011 • VOLUME 19 • No. 3 FOR ALUMNI AND FRIENDS OF THE UNIVERSITY OF NORTH ALABAMA Cover Story 10 ..... Thanks a Million, Harvey Robbins Features 3 ..... The Transition 14 ..... From Zero to Infinity 16 ..... Something Special 20 ..... The Sounds of the Pride 28 ..... Southern Laughs 30 ..... Academic Affairs Awards 33 ..... Excellence in Teaching Award 34 ..... China 38 ..... Words on the Breeze Departments 2 ..... President’s Message 6 ..... Around the Campus 45 ..... Class Notes 47 ..... In Memory FALL 2011 • VOLUME 19 • No. 3 for alumni and friends of the University of North Alabama president’s message ADMINISTRATION William G. Cale, Jr. President William G. Cale, Jr. The annual everyone to attend one of these. You may Vice President for Academic Affairs/Provost Handy festival contact Dr. Alan Medders (Vice President John Thornell is drawing large for Advancement, [email protected]) Vice President for Business and Financial Affairs crowds to the many or Mr. Mark Linder (Director of Athletics, Steve Smith venues where music [email protected]) for information or to Vice President for Student Affairs is being played. At arrange a meeting for your group. David Shields this time of year Sometimes we measure success by Vice President for University Advancement William G. Cale, Jr. it is impossible the things we can see, like a new building. Alan Medders to go anywhere More often, though, success happens one Vice Provost for International Affairs in town and not hear music. The festival student at a time as we provide more and Chunsheng Zhang is also a reminder that we are less than better educational opportunities. -
Orbital Detection and Implications of Akaganeite on Mars
45th Lunar and Planetary Science Conference (2014) 2364.pdf ORBITAL DETECTION AND IMPLICATIONS OF AKAGANEITE ON MARS. J. Carter1, C. Viviano-Beck2, L. Le Deit3, J. Bishop4, D. Loizeau5, 1IAS (Paris-Sud University, France, [email protected]), 2JHU/APL (Laurel, MD), 3LPGN (Nantes University, France), 4SETI Institute (Mountain View, CA), 5LGL (Lyon 1 University, France). Introduction: Recent orbital and landed investiga- lands, and intertidal marshes; and within hydrothermal tions of the Martian surface have demonstrated that the brines [13,14,15,16]. The main conditions necessary planet underwent a complex geological and aqueous for akaganéite precipitation are high salinity, mild acid- alteration history, fragments of which are recorded in ity (pH ~6), oxidizing conditions, and most important- the mineralogy of the heavily disrupted surface [1,2,3]. ly, high iron (II/III) and chlorine concentrations. On Of particular interest are aqueously altered minerals Earth, the source of Fe in akaganéite formation is typi- that trace warmer and wetter surface environments on cally iron ore or sulfides (the latter also providing acid- Early Mars, some of which also exhibit biogenic for- ity as they dissolve) [15,16]. Highly concentrated chlo- mation pathways [4,5]. rine occurs within volcanic fumaroles or deep sea vents The most abundant alteration minerals on Mars that as well as within evaporating, closed or semi-closed have likely been detected are hydrated silicates, hy- water systems [15,16,17]. drated sulfates, and chloride salts [6,7,8]. The detection of minor phases remains important, however, as they further constrain localized geochemical environments at different epochs in the timeline of Mars’s geological history. -
Widespread Excess Ice in Arcadia Planitia, Mars
Widespread Excess Ice in Arcadia Planitia, Mars Ali M. Bramson1, Shane Byrne1, Nathaniel E. Putzig2, Sarah Sutton1, Jeffrey J. Plaut3, T. Charles Brothers4 and John W. Holt4 Corresponding author: A. M. Bramson, Lunar and Planetary Laboratory, University of Arizona, Kuiper Space Science Building, 1629 E. University Blvd. Tucson, AZ, 85721, USA. ([email protected]) Affiliations: 1Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA. 2Southwest Research Institute, Boulder, Colorado, USA. 3Jet Propulsion Laboratory, Pasadena, California, USA. 4Institute for Geophysics, University of Texas at Austin, Austin, Texas, USA. Accepted for publication July 18, 2015 in Geophysical Research Letters. An edited version of this paper was published by AGU on August 26, 2015. Copyright 2015 American Geophysical Union. Citation: Bramson, A. M., S. Byrne, N. E. Putzig, S. Sutton, J. J. Plaut, T. C. Brothers, and J. W. Holt (2015), Widespread excess ice in Arcadia Planitia, Mars, Geophys. Res. Lett., 42, doi:10.1002/2015GL064844. Key points: • Terraced craters: abundant in Arcadia Planitia, indicate subsurface layering • A widespread subsurface interface is also detected by SHARAD • Combining data sets yields dielectric constants consistent with decameters of excess water ice Abstract: The distribution of subsurface water ice on Mars is a key constraint on past climate, while the volumetric concentration of buried ice (pore-filling versus excess) provides information about the process that led to its deposition. We investigate the subsurface of Arcadia Planitia by measuring the depth of terraces in simple impact craters and mapping a widespread subsurface reflection in radar sounding data. Assuming that the contrast in material strengths responsible for the terracing is the same dielectric interface that causes the radar reflection, we can combine these data to estimate the dielectric constant of the overlying material. -
Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km.