Mineralogy of the Martian Surface
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MODELED CATASTROPHIC OUTFLOW at ARAM CHAOS CHANNEL, MARS. DA Howard, Earth & Planetary Sciences, University of Tennessee
40th Lunar and Planetary Science Conference (2009) 2179.pdf MODELED CATASTROPHIC OUTFLOW AT ARAM CHAOS CHANNEL, MARS. D. A. Howard, Earth & Planetary Sciences, University of Tennessee, 306 Earth & Planetary Sciences Bldg., 1412 Circle Drive, Knoxville, TN 37996, [email protected]. Introduction: The Aram Chaos channel located at tional algorithms relied on in this study were devel- 2.8°N, 18.5°W, is approximately 100 km long, ranges oped by Komar [1] and I have adapted them for use from 8 to 14 km wide, and has a maximum depth of with the Hydrologic Engineering Center’s River Anal- 2000 m (Figure 1). The confined innermost approx- ysis System (HEC-RAS) based on solution of the con- imately 67 km reach selected for this study includes tinuity and momentum equations [2]. HEC-RAS ad- the area of the channel where the trimline is evident justed for Mars’ gravitational acceleration was only for the stream head at the time of initial catastrophic applied to Mars channels once previously by Burr [3] flow and the outflow height at the channel’s mouth. at Athabasca Vallis and therefore provides the oppor- tunity to further develop the method here. The HEC- RAS model used for both Earth and Mars are identical except that the Mars version was adjusted for the gra- vitational acceleration and the specific weight of water differences between the two planets. Using the HEC- Ares Valles GeoRAS ArcGIS geospatial tool to generate the chan- nel geometry for input to the HEC-RAS flow model, Aram Chaos the hypothesized output potentially quantifies the hy- draulics of the channels more accurately than previous orders-of-magnitude estimates reported in the litera- ture. -
Mars Impact Crater Or Supervolcano? 12 April 2018
Mars impact crater or supervolcano? 12 April 2018 floor, which is covered by flat, icy deposits that show signs of flow and movement – these are likely akin to rocky, ice-rich glaciers, which have built up over time in the cold and arid climate. Mars Express view of Ismenia Patera. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO These images from ESA's Mars Express show a crater named Ismenia Patera on the Red Planet. Its origin remains uncertain: did a meteorite smash into the surface or could it be the remnants of a supervolcano? Ismenia Patera – patera meaning 'flat bowl' in Latin – sits in the Arabia Terra region on Mars. This a transition area between the planet's northern and southern regions – an especially intriguing part of the surface. Ismenia Patera in context within Arabia Terra. Credit: NASA MGS MOLA Science Team Mars' topography is clearly split into two parts: the northern lowlands and the southern highlands, the latter sitting up to a few kilometres higher. This These images were taken on 1 January by the high- divide is a key topic of interest for scientists resolution stereo camera on Mars Express, which studying the Red Planet. Ideas for how this has been circling the planet since 2003. dramatic split formed suggest either a massive single impact, multiple impacts or ancient plate Such high-resolution and detailed images shed light tectonics as seen on Earth, but its origin remains on numerous aspects of Mars – for example, how unclear. the features seen scarring the surface formed in the first place, and how they have evolved in the many Ismenia Patera is some 75 km across. -
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). -
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. -
Columbus Crater HLS2 Hangout: Exploration Zone Briefing
Columbus Crater HLS2 Hangout: Exploration Zone Briefing Kennda Lynch1,2, Angela Dapremont2, Lauren Kimbrough2, Alex Sessa2, and James Wray2 1Lunar and Planetary Institute/Universities Space Research Association 2Georgia Institute of Technology Columbus Crater: An Overview • Groundwater-fed paleolake located in northwest region of Terra Sirenum • ~110 km in diameter • Diversity of Noachian & Hesperian aged deposits and outcrops • High diversity of aqueous mineral deposits • Estimated 1.5 km depth of sedimentary and/or volcanic infill • High Habitability and Biosignature Preservation Potential LZ & Field Station Latitude: 194.0194 E Longitude: 29.2058 S Altitude: +910 m SROI #1 RROI #1 LZ/HZ SROI #4 SROI #2 SROI #5 22 KM HiRISE Digital Terrain Model (DTM) • HiRISE DTMs are made from two images of the same area on the ground, taken from different look angles (known as a stereo-pair) • DTM’s are powerful research tools that allow researchers to take terrain measurements and model geological processes • For our traversability analysis of Columbus: • The HiRISE DTM was processed and completed by the University of Arizona HiRISE Operations Center. • DTM data were imported into ArcMap 10.5 software and traverses were acquired and analyzed using the 3D analyst tool. • A slope map was created in ArcMap to assess slope values along traverses as a supplement to topography observations. Slope should be ≤30°to meet human mission requirements. Conclusions Traversability • 9 out of the 17 traverses analyzed met the slope criteria for human missions. • This region of Columbus Crater is traversable and allows access to regions of astrobiological interest. It is also a possible access point to other regions of Terra Sirenum. -
NASA Mars Exploration Strategy: “Follow the Water”
Gullies on Mars -- Water or Not? Allan H. Treiman NASA Mars Exploration Strategy: “Follow the Water” Life W Climate A T Geology E Resources R Evidence of Water on Mars Distant Past Crater Degradation and Valley Networks ‘River’ Channels Flat Northern Lowlands Meteorites Carbonate in ALH84001 Clay in nakhlites MER Rover Sites Discoveries Hydrous minerals: jarosite! Fe2O3 from water (blueberries etc.) Silica & sulfate & phosphate deposits Recent Past (Any liquid?) Clouds & Polar Ice Ground Ice Valley Networks and Degraded Craters 1250 km River Channels - Giant Floods! 225 km 10 km craters River Channels - ‘Normal’ Flows 14 km 1 km River Channels from Rain? 700 km Science, July 2, 2004 19 km Ancient Martian Meteorite ALH84001 MER Opportunity - Heatshield and parachute. Jarosite - A Water-bearing Mineral Formed in Groundwater 3+ KFe3 (SO4)2(OH)6 2 Jarosite = K2SO4 + 3 Fe2O3 + 3 H2SO4 Hematite is in “Blueberries,” which still suggest water. Stone Mountain MER Spirit: Columbia Hills H2O Now: Clouds & Polar Caps Ground Ice – Mars Orbiter GRS Water abundances within a few meters depth of the Martian surface. Wm. Feldman. AAAS talk & Los Alamos Nat’l. Lab. Press Release, 15 Feb. 2003. (SPACE.com report, 16 Feb. 2003) So, Water on Mars !! So? Apparently, Mars has/had lots of water. Lots of evidence for ancient liquid water (> ~2 billion years ago), both surface and underground. Martian Gullies - Liquid Water or Not? Material flows down steep slopes, most commonly interpreted as water-bearing debris flows [Malin and Edgett (2000) Science 288, 2330]. Liquid water is difficult to produce and maintain near Mars’ surface, now. -
Downselection of Landing Sites Proposed for the Mars 2020 Rover Mission
47th Lunar and Planetary Science Conference (2016) 2324.pdf DOWNSELECTION OF LANDING SITES PROPOSED FOR THE MARS 2020 ROVER MISSION. M. P. Golombek1, J. A. Grant2, K. A. Farley3, K. Williford1, A. Chen1, R. E. Otero1, and J. W. Ashley1, 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109; 2Smithsonian Institution, Center for Earth and Planetary Sciences, Washington, D.C. 20560, 3Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125. Introduction: The Mars 2020 mission would ex- suitable for addressing key planetary evolution ques- plore a site likely to have been habitable, seek signs of tions if and when they are returned to Earth. past life, prepare a returnable cache with the most Results of the voting were presented as the compelling samples, take the first steps towards in-situ weighted average (assigning 5 points to each green resource utilization on Mars, and demonstrate technol- vote, 3 to each yellow vote, and 1 to each red vote that ogy needed for future human and robotic exploration were then summed and divided by the total number of of Mars. The first landing site workshop identified and votes) and the mode (color receiving the most votes). prioritized 27 landing sites proposed by the science This ensured that participants could not skew the re- community according to science objectives that also sults by withholding votes from some sites. Both met the engineering constraints [1]. This abstract de- methods yield similar results and reveal a fall-off in scribes the downselection of landing sites that occurred support for sites ranked lower than the top nine or ten at the second landing site workshop and associated based on mode and average, respectively [2]. -
Understanding the History of Arabia Terra, Mars Through Crater-Based Tests Karalee Brugman University of Colorado Boulder
University of Colorado, Boulder CU Scholar Undergraduate Honors Theses Honors Program Spring 2014 Understanding the History of Arabia Terra, Mars Through Crater-Based Tests Karalee Brugman University of Colorado Boulder Follow this and additional works at: http://scholar.colorado.edu/honr_theses Recommended Citation Brugman, Karalee, "Understanding the History of Arabia Terra, Mars Through Crater-Based Tests" (2014). Undergraduate Honors Theses. Paper 55. This Thesis is brought to you for free and open access by Honors Program at CU Scholar. It has been accepted for inclusion in Undergraduate Honors Theses by an authorized administrator of CU Scholar. For more information, please contact [email protected]. ! UNDERSTANDING+THE+HISTORY+OF+ARABIA+TERRA,+MARS++ THROUGH+CRATER4BASED+TESTS+ Karalee K. Brugman Geological Sciences Departmental Honors Thesis University of Colorado Boulder April 4, 2014 Thesis Advisor Brian M. Hynek | Geological Sciences Committee Members Charles R. Stern | Geological Sciences Fran Bagenal | Astrophysical and Planetary Sciences Stephen J. Mojzsis | Geological Sciences ABSTRACT' Arabia Terra, a region in the northern hemisphere of Mars, has puzzled planetary scientists because of its odd assemblage of characteristics. This makes the region difficult to categorize, much less explain. Over the past few decades, several hypotheses for the geological history of Arabia Terra have been posited, but so far none are conclusive. For this study, a subset of the Mars crater database [Robbins and Hynek, 2012a] was reprocessed using a new algorithm [Robbins and Hynek, 2013]. Each hypothesis’s effect on the crater population was predicted, then tested via several crater population characteristics including cumulative size-frequency distribution, depth-to-diameter ratio, and rim height. -
Chemin X-Ray Diffraction of the Windjana Sample
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Mineralogy, provenance, and diagenesis of a potassic 10.1002/2015JE004932 basaltic sandstone on Mars: CheMin X-ray diffraction Special Section: of the Windjana sample (Kimberley area, Gale Crater) The Mars Science Laboratory Rover Mission (Curiosity) at The Allan H. Treiman1, David L. Bish2, David T. Vaniman3, Steve J. Chipera4, David F. Blake5, Kimberley, Gale Crater, Mars Doug W. Ming6, Richard V. Morris6, Thomas F. Bristow5, Shaunna M. Morrison7, Michael B. Baker8, Elizabeth B. Rampe6, Robert T. Downs7, Justin Filiberto9, Allen F. Glazner10, Ralf Gellert11, Key Points: Lucy M. Thompson12, Mariek E. Schmidt13, Laetitia Le Deit14, Roger C. Wiens15, Amy C. McAdam16, • First mineralogical analysis of Cherie N. Achilles2, Kenneth S. Edgett17, Jack D. Farmer18, Kim V. Fendrich7, John P. Grotzinger8, sandstone on Mars 19 20 8 21 12 • Windjana sandstone very rich in Sanjeev Gupta , John Michael Morookian , Megan E. Newcombe , Melissa S. Rice , John G. Spray , sanidine, implying a trachyte source Edward M. Stolper8, Dawn Y. Sumner22, Ashwin R. Vasavada20, and Albert S. Yen20 rock • The source of Gale Crater sediments is 1Lunar and Planetary Institute, Houston, Texas, USA, 2Department of Geological Sciences, Indiana University, Bloomington, Indiana, an incredibly diverse igneous terrane USA, 3Planetary Science Institute,Tucson,Arizona,USA,4Chesapeake Energy Corporation, Oklahoma City, Oklahoma, USA, 5NASA Ames Research Center, Moffett Field, California, USA, 6Astromaterials -
Volcanism on Mars
Author's personal copy Chapter 41 Volcanism on Mars James R. Zimbelman Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA William Brent Garry and Jacob Elvin Bleacher Sciences and Exploration Directorate, Code 600, NASA Goddard Space Flight Center, Greenbelt, MD, USA David A. Crown Planetary Science Institute, Tucson, AZ, USA Chapter Outline 1. Introduction 717 7. Volcanic Plains 724 2. Background 718 8. Medusae Fossae Formation 725 3. Large Central Volcanoes 720 9. Compositional Constraints 726 4. Paterae and Tholi 721 10. Volcanic History of Mars 727 5. Hellas Highland Volcanoes 722 11. Future Studies 728 6. Small Constructs 723 Further Reading 728 GLOSSARY shield volcano A broad volcanic construct consisting of a multitude of individual lava flows. Flank slopes are typically w5, or less AMAZONIAN The youngest geologic time period on Mars identi- than half as steep as the flanks on a typical composite volcano. fied through geologic mapping of superposition relations and the SNC meteorites A group of igneous meteorites that originated on areal density of impact craters. Mars, as indicated by a relatively young age for most of these caldera An irregular collapse feature formed over the evacuated meteorites, but most importantly because gases trapped within magma chamber within a volcano, which includes the potential glassy parts of the meteorite are identical to the atmosphere of for a significant role for explosive volcanism. Mars. The abbreviation is derived from the names of the three central volcano Edifice created by the emplacement of volcanic meteorites that define major subdivisions identified within the materials from a centralized source vent rather than from along a group: S, Shergotty; N, Nakhla; C, Chassigny. -
Case Fil Copy
NASA TECHNICAL NASA TM X-3511 MEMORANDUM CO >< CASE FIL COPY REPORTS OF PLANETARY GEOLOGY PROGRAM, 1976-1977 Compiled by Raymond Arvidson and Russell Wahmann Office of Space Science NASA Headquarters NATIONAL AERONAUTICS AND SPACE ADMINISTRATION • WASHINGTON, D. C. • MAY 1977 1. Report No. 2. Government Accession No. 3. Recipient's Catalog No. TMX3511 4. Title and Subtitle 5. Report Date May 1977 6. Performing Organization Code REPORTS OF PLANETARY GEOLOGY PROGRAM, 1976-1977 SL 7. Author(s) 8. Performing Organization Report No. Compiled by Raymond Arvidson and Russell Wahmann 10. Work Unit No. 9. Performing Organization Name and Address Office of Space Science 11. Contract or Grant No. Lunar and Planetary Programs Planetary Geology Program 13. Type of Report and Period Covered 12. Sponsoring Agency Name and Address Technical Memorandum National Aeronautics and Space Administration 14. Sponsoring Agency Code Washington, D.C. 20546 15. Supplementary Notes 16. Abstract A compilation of abstracts of reports which summarizes work conducted by Principal Investigators. Full reports of these abstracts were presented to the annual meeting of Planetary Geology Principal Investigators and their associates at Washington University, St. Louis, Missouri, May 23-26, 1977. 17. Key Words (Suggested by Author(s)) 18. Distribution Statement Planetary geology Solar system evolution Unclassified—Unlimited Planetary geological mapping Instrument development 19. Security Qassif. (of this report) 20. Security Classif. (of this page) 21. No. of Pages 22. Price* Unclassified Unclassified 294 $9.25 * For sale by the National Technical Information Service, Springfield, Virginia 22161 FOREWORD This is a compilation of abstracts of reports from Principal Investigators of NASA's Office of Space Science, Division of Lunar and Planetary Programs Planetary Geology Program. -
LAYERED SULFATE-BEARING TERRAINS on MARS: INSIGHTS from GALE CRATER and MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S
Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6316.pdf LAYERED SULFATE-BEARING TERRAINS ON MARS: INSIGHTS FROM GALE CRATER AND MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S. Edwards1, 1Department of Physics & Astrono- my, Northern Arizona University, 2School of Earth & Space Exploration, Arizona State University, 3Department of Earth & Planetary Sciences, Washington University in St. Louis. Introduction: Sulfate species have been detected ronment, with episodes of diagenesis and weathering in late Noachian and Hesperian terrains on Mars lying to form a crystalline hematite lag deposit [4, 5]. The stratigraphically above clay minerals, which has been lag deposit masks the CRISM spectral signature of interpreted as documenting a shift from wetter to more sulfate in most locations. Sulfate minerals including arid environments on the surface. Sulfate detections kieserite and gypsum have been detected in impact are associated with layered deposits in numerous loca- crater walls and windswept regions [6]. The Oppor- tions including Gale Crater, Meridiani Planum, Vallis tunity rover explored southern Meridiani Planum Marineris, and Terra Sirenum, and Aram Chaos [1]. through a campaign of crater-hopping, using craters as These sulfates and clays been identified using their a natural drill to expose strata [6]. The deepest expo- diagnostic absorption features in visible and near- sures explored by Opportunity directly are ~10 meters infrared reflectance (VNIR) data acquired from Mars thick at Victoria Crater. Opportunity results indicate orbit. Additionally, two rover missions have explored that the top layers of Burns formation contain up to sites with massive sulfate deposits. The first, the MER 40% sulfate and included Mg, Ca, and Fe species.