Dikes of Distinct Composition Intruded Into Noachian-Aged Crust Exposed in the Walls of Valles Marineris Jessica Flahaut, John F
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The Eastern Outlet of Valles Marineris: a Window Into the Ancient Geologic and Hydrologic Evolution of Mars
First Landing Site/Exploration Zone Workshop for Human Missions to the Surface of Mars (2015) 1054.pdf The Eastern Outlet of Valles Marineris: A Window into the Ancient Geologic and Hydrologic Evolution of Mars Stephen M. Clifford, David A. Kring, and Allan H. Treiman, Lunar and Planetary Institute/USRA, 3600 Bay Area Bvld., Houston, TX 77058 Over its 3,500 km length, Valles Marineris exhibits enormous range of geologic and environmental diversity. At its western end, the canyon is dominated by the tectonic complex of Noctis Labyrinthus while, in the east, it grades into an extensive region of chaos - where scoured channels and streamlined islands provide evidence of catastrophic floods that spilled into the northern plains [1-4]. In the central portion of the system, debris derived from the massive interior layered deposits of Candor, Ophir and Hebes Chasmas spills into the central trough have been identified as possible lucustrine sediments that may have been laid down in long-standing ice-covered lakes [3-6]. The potential survival and growth of Martian organisms in such an environment, or in the aquifers whose disruption gave birth to the chaotic terrain at the east end of the canyon, raises the possibility that fossil indicators of life may be present in the local sediment and rock. In other areas, 6 km-deep exposures of Hesperian and Noachian-age canyon wall stratigraphy have collapsed in massive landslides that extend many tens of kilometers across the canyon floor. Ejecta from interior craters, aeolian sediments, and possible volcanics (which appear to have emanated from structurally controlled vents along the base of the scarps), further contribute to the canyon's geologic complexity [2,3]. -
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. -
Alluvial Fans As Potential Sites for Preservation of Biosignatures on Mars
Alluvial Fans as Potential Sites for Preservation of Biosignatures on Mars Phylindia Gant August 15, 2016 Candidate, Masters of Environmental Science Committee Chair: Dr. Deborah Lawrence Committee Member: Dr. Manuel Lerdau, Dr. Michael Pace 2 I. Introduction Understanding the origin of life Life on Earth began 3.5 million years ago as the temperatures in the atmosphere were cool enough for molten rocks to solidify (Mojzsis et al 1996). Water was then able to condense and fall to the Earth’s surface from the water vapor that collected in the atmosphere from volcanoes. Additionally, atmospheric gases from the volcanoes supplied Earth with carbon, hydrogen, nitrogen, and oxygen. Even though the oxygen was not free oxygen, it was possible for life to begin from the primordial ooze. The environment was ripe for life to begin, but how would it begin? This question has intrigued humanity since the dawn of civilization. Why search for life on Mars There are several different scientific ways to answer the question of how life began. Some scientists believe that life started out here on Earth, evolving from a single celled organism called Archaea. Archaea are a likely choice because they presently live in harsh environments similar to the early Earth environment such as hot springs, deep sea vents, and saline water (Wachtershauser 2006). Another possibility for the beginning of evolution is that life traveled to Earth on a meteorite from Mars (Whitted 1997). Even though Mars is anaerobic, carbonate-poor and sulfur rich, it was warm and wet when Earth first had organisms evolving (Lui et al. -
Pre-Mission Insights on the Interior of Mars Suzanne E
Pre-mission InSights on the Interior of Mars Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, Ulrich Christensen, Véronique Dehant, Mélanie Drilleau, William Folkner, Nobuaki Fuji, et al. To cite this version: Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, et al.. Pre-mission InSights on the Interior of Mars. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.1-72. 10.1007/s11214-018-0563-9. hal-01990798 HAL Id: hal-01990798 https://hal.archives-ouvertes.fr/hal-01990798 Submitted on 23 Jan 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. Open Archive Toulouse Archive Ouverte (OATAO ) OATAO is an open access repository that collects the wor of some Toulouse researchers and ma es it freely available over the web where possible. This is an author's version published in: https://oatao.univ-toulouse.fr/21690 Official URL : https://doi.org/10.1007/s11214-018-0563-9 To cite this version : Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman ,... [et al.]. Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (1). -
UNDERSTANDING the OLYMPUS MONS and VALLES MARINERIS USING THEMIS IMAGERY. S. Mena-Fernandez, H. Xie. to Better Understand Mars A
Lunar and Planetary Science XXXVI (2005) 1056.pdf UNDERSTANDING THE OLYMPUS MONS AND VALLES MARINERIS USING THEMIS IMAGERY. S. Mena-Fernandez, H. Xie. To better understand Mars’ geological features, water resources, possible life, and climate aspects, several spacecrafts such as the Mars Global Survey, Mars Express and Mars Odyssey had been launch into space. The latter, carries a sensor called Thermal Emission Imaging System (THEMIS), which combines a 5-band visible subsystem (VIS) and a 10- band infrared (IR) subsystem with 19m, 100m pixel resolution, respectively. This study aims at developing methods to eventually assess Mars’ mineral and rock composition through the case study of the Olympus Mons and Valles Marineris from THEMIS image analysis. ISIS 3.0 software was utilized to transform individual THEMIS QUEB files to Cub and from Cub to Tiff files. Then, these Tiff images were brought to ENVI for further processing and analyses. All analyses will be based on three geophysical parameters of the two study areas: temperature, radiance, and emissivity. The spectral emissivity of materials in the two areas will be compared with the Earth’s mineral library. This will allow us to finally understand the rock and mineral composition of the Mars surface and the geological and tectonic processes that Mars experienced. Initial results indicate that the temperatures are slightly different between the Olympus Mons (-27°F to 4°F) and the Valles Marineris (-28 to 9 °F), while the spectral radiance of materials in the two areas are obviously different. Further data processing and analyses are still in progress. . -
Are We Martians? Looking for Indicators of Past Life on Mars with the Missions of the European Space Agency
CESAR Scientific Challenge Are we Martians? Looking for indicators of past life on Mars with the missions of the European Space Agency Teacher's Guide 1 Are we Martians? CESAR Scientific Challenge Table of contents: Didactics 5 Phase 0 18 Phase 1 20 Activity 1: Refresh concepts 21 Activity 2: Getting familiar with coordinates 21 Activity 2.1: Identify coordinates on an Earth map 21 Activity 2.2: The Martian zero meridian 24 Activity 2.3: Identify coordinates on a Martian map 25 Activity 2.4: A model of Mars 27 Activity 3: The origin of life 28 Activity 3.1: What is life? 28 Activity 3.2: Traces of extraterrestrial life 29 Activity 3.2.1: Read the following article 30 Activity 3.2.2: Read about Rosalind Franklin and ExoMars 2022 30 Activity 3.3: Experiment for DNA extraction 31 Activity 4: Habitable zones 31 Activity 4.1: Habitable zone of our star 31 Activity 4.2: Study the habitable zones of different stars 34 Activity 4.3: Past, present and future of water on Mars 37 Activity 4.4: Extremophiles 39 Activity 5: What do you know about Mars? 40 Activity 6: Scientific knowledge from Mars’ surface 41 Activity 6.1: Geology of Mars 41 Activity 6.2: Atmosphere of Mars 44 Activity 7: Mars exploration by European Space Agency 45 Activity 7.1: Major Milestones of the European Space Agency on Mars 50 Activity 8: Check what you have learnt so far 52 2 Are we Martians? CESAR Scientific Challenge Phase 2 53 Activity 9: Ask for a videocall with the CESAR Team if needed 54 Phase 3 56 Activity 10: Prepare the Mars landing 57 Activity 10.1: Get used to Google Mars. -
CRISM: Exploring the Geology of Mars
CRISM: Exploring the Geology of Mars Tech Splash Open Music Exploring the geology of Mars is similar to the way that we look at the rock record on Earth. One way we do this is by analyzing stratigraphy – or studying the layers of ancient rocks that record changes through time. The Grand Canyon, for example, exposes over a billion years of the Earth’s history. This history is recorded in the layers of rocks, which tell geologist about the ancient environments that once existed on Earth. Valles Marineris is considered “The Grand Canyon of Mars” and is a planetary geologists’ playground. If we project Valles Marineris onto the Earth’s globe, it would stretch across the entire continental United States. It runs ~4 miles deep and therefore exposes some of the most ancient crust on Mars. How Valles Marineris was formed remains a point of debate among scientists, but would provide important insight into the history of Mars. It appears to have formed as a result of the enormous stress that the Tharsis bulge –the largest volcanoes in the solar system – places on the crust. This massive load caused stresses that pulled apart the crust and basically ripped it open. Recently, however, it has also been hypothesized that while it was rifting open, it also experienced strike-slip faulting, like we see in California with the San Andreas fault. If Valles Marineris simply pulled apart, we would expect the geology on the North and South side of the canyon to match each other. If significant strike-slip faulting occurred then the rocks would be offset from one another, and the North and South side would not match. -
Growth and Form of the Mound in Gale Crater, Mars: Slope
1 Growth and form of the mound in Gale Crater, Mars: Slope- 2 wind enhanced erosion and transport 3 Edwin S. Kite1, Kevin W. Lewis,2 Michael P. Lamb1 4 1Geological & Planetary Science, California Institute of Technology, MC 150-21, Pasadena CA 5 91125, USA. 2Department of Geosciences, Princeton University, Guyot Hall, Princeton NJ 6 08544, USA. 7 8 Abstract: Ancient sediments provide archives of climate and habitability on Mars (1,2). Gale 9 Crater, the landing site for the Mars Science Laboratory (MSL), hosts a 5 km high sedimentary 10 mound (3-5). Hypotheses for mound formation include evaporitic, lacustrine, fluviodeltaic, and 11 aeolian processes (1-8), but the origin and original extent of Gale’s mound is unknown. Here we 12 show new measurements of sedimentary strata within the mound that indicate ~3° outward dips 13 oriented radially away from the mound center, inconsistent with the first three hypotheses. 14 Moreover, although mounds are widely considered to be erosional remnants of a once crater- 15 filling unit (2,8-9), we find that the Gale mound’s current form is close to its maximal extent. 16 Instead we propose that the mound’s structure, stratigraphy, and current shape can be explained 17 by growth in place near the center of the crater mediated by wind-topography feedbacks. Our 18 model shows how sediment can initially accrete near the crater center far from crater-wall 19 katabatic winds, until the increasing relief of the resulting mound generates mound-flank slope- 20 winds strong enough to erode the mound. Our results indicate mound formation by airfall- 21 dominated deposition with a limited role for lacustrine and fluvial activity, and potentially 22 limited organic carbon preservation. -
Spring 1989 5
MIDDLE EAST LIBRARIANS ASSOCIATION NUMBER 47 SPRING, 1989 TAOLE OF CONTENTS Editor.. ., Note 2 ASSOClA'I ION NEWS Fr°"' ttHt President 3 Librarian of Congress responds to HELA GENERAL NEWS Future Conferences Electronic Addr11sses 7 ARTICLES h1la111 in Canada by Salwa Ferahian B Iraq-Iran Wart a Bibliographical Project by J. Anthony Gardner 14 Conte111porary Pt!r11ian Press in E1till! by Hasan Javadi and Abazar Sepehri lB A Lone Bibliographer at her PC by Priscilla H. Ro~rts 7.b Increa sing Productivity and Public Satisfaction with Middle East and Judaic Library Services through Use of a Personal Co111puter by Oona S. Straley and A111non Zipin 33 BOO!< REVIEW !!I.~irat al-ma•3rif Ta ~hayyu~ reviewed by Abaiar Sepehri :Sb POSITIONS AVAILABLE Princeton Univers ity 38 Sultan Daboos University 39 University of Chicago '10 lntifatlah Publication,,. Available Inside Back Cover l u raeli Fon!ign Relations Documents AvaUablll! Inside Back Cover MH n NIJIHi IU!IN U.U1'1 J410 MIDDLE EAST LIBRARIANS ASSOCIATION EDWARD A. JAJKO PresidP-nt 1989 Moover Ins ti tut ion MEAYLE GASTON Vice-Pr esident & NeH York University Progral'I Chair 1?89 JAMES WEINBERGER Secretary- P~inceta11 ~liver·sity ' Treasurer 1987- 1989 BRENDA E. BICKETT Editor 1900-1990 Georgetown University !:l('ll\ Not•• I• publislurd three ti,.es a year, in ,.inter, "'Pring, and fal I. It i• distributed to ...,,,.bers of the Association and to 11onll'l"'"h"'r ••lh"<: r l born1. M•.,hur•hl11 1h1e11 of US$10.00 for North Afllerican addresses or IJUtl:l.00 fut' •do:Jres!le!& outside North AMerica bring the ~and ..,.' ul:hotr- 111•il !r111•· Bub11criptions are USSl0.00 lUSSl:l.OO outside No rth l'IMlft Ar:al 1nu t.alwlldlit' year, or USS3.00 per issue for 111ost back 11u111hat •, l\ddr••• rnrr••JllHUletir• r11q,11nll11Q •11l111criptioms, dues, or "''"'"b"r""hip In fur111111tiun hll .J•lll!'!!t M• l11l11o·o•r 1 B•cr•tary-Treasurer MELA, l'rtnec•lun llf1iv•r•ily l lhr.,y, lluM 1'10, Princ:•ton, NJ 08:1'10 USA. -
Icelandic Analogs to Martian Flood Lavas
Edinburgh Research Explorer Icelandic analogs to Martian flood lavas Citation for published version: Keszthelyi, L, Thordarson, T, McEwen, A, Haack, H, Guilbaud, MN, Self, S & Rossi, MJ 2004, 'Icelandic analogs to Martian flood lavas', Geochemistry, Geophysics, Geosystems, vol. 5, no. 11, Q11014, pp. 1-32. https://doi.org/10.1029/2004GC000758 Digital Object Identifier (DOI): 10.1029/2004GC000758 Link: Link to publication record in Edinburgh Research Explorer Document Version: Publisher's PDF, also known as Version of record Published In: Geochemistry, Geophysics, Geosystems Publisher Rights Statement: Published in Geochemistry, Geophysics, Geosystems by the American Geophysical Union (2004) General rights Copyright for the publications made accessible via the Edinburgh Research Explorer is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. Take down policy The University of Edinburgh has made every reasonable effort to ensure that Edinburgh Research Explorer content complies with UK legislation. If you believe that the public display of this file breaches copyright please contact [email protected] providing details, and we will remove access to the work immediately and investigate your claim. Download date: 06. Oct. 2021 Article Geochemistry 3 Volume 5, Number 11 Geophysics 23 November 2004 Q11014, doi:10.1029/2004GC000758 GeosystemsG G ISSN: 1525-2027 AN ELECTRONIC JOURNAL OF THE EARTH -
Cerberus.Pdf
(lP,IIP,U' By Gaynor Borade Greek mythology comprises a huge pantheon, extensive use of anthropomorphism and mythical creatures that ore symbotic. Cerberus, the three headed dog was believed to be the guardian of the reotm of death, or Hades. Cerberus, it was believed, prevented those who crossed the river of death, Styx, from escoping. River Styx was supposed to be the boundory belween the Underworld and Earth. Greek mythology propounded thot Hodes or ihe Underworld wos encircled nine times by River Styx and thot the rivers Phlegethon, Cocytus, Lelhe, Eridanos and Acheron converged with Styx on the 'Great Marsh'. Cerberus guorded the Great Marsh. Importance of Styx in Greek Mythotogy: Hades ond Persephone were believed to be the mortol portals in the Underworld. This reotm wos atso home to Phlegyos or guardian of the River Phlegethon, Charon or Kharon, the ferrymon, ond the living waters of Styx. Styx wos believed to have miraculous powers thot could make o person immorfol, resulting in the grove need for it to be guorded. This reolm relates to the concept of 'hel[' in Christianity and the 'Paradise losf', in the Iiterary genius of 'The Divine Comedy'. In Greek myihology, the ferrymon Charon was in charge of iransporting souls across the Styx, into the Underworld. Here, it was believed thaf the sullen were drowned in Sfyx's muddy waters. Cerberus:The Guardion Cerberus, the mythical guordian of River Styx has been immorlalized through many works of ancient Greek liferoture, ort ond orchitecture. Cerberus is easity recognizabte among the other members of the pontheon due to his three heads. -
Chapter Vi Report of Divisions, Commissions, and Working
CHAPTER VI REPORT OF DIVISIONS, COMMISSIONS, AND WORKING GROUPS Downloaded from https://www.cambridge.org/core. IP address: 170.106.33.42, on 24 Sep 2021 at 09:23:58, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0251107X00011937 DIVISION I FUNDAMENTAL ASTRONOMY Division I provides a focus for astronomers studying a wide range of problems related to fundamental physical phenomena such as time, the intertial reference frame, positions and proper motions of celestial objects, and precise dynamical computation of the motions of bodies in stellar or planetary systems in the Universe. PRESIDENT: P. Kenneth Seidelmann U.S. Naval Observatory, 3450 Massachusetts Ave NW Washington, DC 20392-5100, US Tel. + 1 202 762 1441 Fax. +1 202 762 1516 E-mail: [email protected] BOARD E.M. Standish President Commission 4 C. Froeschle President Commisison 7 H. Schwan President Commisison 8 D.D. McCarthy President Commisison 19 E. Schilbach President Commisison 24 T. Fukushima President Commisison 31 J. Kovalevsky Past President Division I PARTICIPATING COMMISSIONS: COMMISSION 4 EPHEMERIDES COMMISSION 7 CELESTIAL MECHANICS AND DYNAMICAL ASTRONOMY COMMISSION 8 POSITIONAL ASTRONOMY COMMISSION 19 ROTATION OF THE EARTH COMMISSION 24 PHOTOGRAPHIC ASTROMETRY COMMISSION 31 TIME Downloaded from https://www.cambridge.org/core. IP address: 170.106.33.42, on 24 Sep 2021 at 09:23:58, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0251107X00011937 COMMISSION 4: EPHEMERIDES President: H. Kinoshita Secretary: C.Y. Hohenkerk Commission 4 held one business meeting.