DOCSLIB.ORG

The Subglacial Birth of Olympus Mons and Its Aureoles

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Subglacial Birth of Olympus Mons and Its Aureoles VOL. 84, NO. BI4 JOURNAL OF GEOPHYSICAL RESEARCH DECEMBER 30, 1979 The Subglacial Birth of Olympus Mons and Its Aureoles CARROLL ANN HODGES AND HENRY J. MOORE U.S. GeologicalSurvey, Menlo Park, California 94025 The vast volcanic plains and shieldsof Mars, togetherwith the thermal, spectrographic,and morpho- logical evidencefor water ice at the poles,for severalpercent water in Viking soil samples,for ground ice or permafrostover much of the planet, and for the existenceof surfacewater at some time in the past, suggestthat magma and water or ice may have interactedduring evolutionof the planet'slandscape. Rel- atively small mesas and buttes, with and without summit craters, are remarkably similar to the table mountainsof Iceland that formed by subglacialeruption during the late Quaternary period. Table moun- tains typicallycomprise foundations of pillow lava and palagonitizedtuff breccias(m6berg), overlain by subaeriallava flows that commonly culminated in a typical shield volcano;some table mountains,how- ever, failed to reachthe subaerialstage and thus lack the cap rock. Subglacialfissure eruptions produced ridgescomposed of pillow lava and m6berg. Conical knobs on steep-sidedMartian plateausare reminis- cent of the small Icelandic shield volcanoesatop m6berg pedestals.Candidate table mountains on Mars are especiallynumerous in the region betweenlatitude 40øN and the margin of the north polar cap, and interaction of lava with a formerly more extensiveice cap may have occurred.More significantis the pos- sibility that Olympus Mons and the broad lobate aureole depositsaround its base may have had similar subglacialbeginnings. This hypothesisrequires an ice cap severalkilometers thick in the vicinity of this enormous shield during its initial stagesof eruption. The amounts of water ice required do not appear excessive,given the limits to presentknowledge of the water budget throughout the planet's history. A mechanismfor localizing suchice, however, is required. INTRODUCTION [1960, 1966a,b, 1967], Sigvaldason[1968], and Preusser[1976]. The morphologiesof numerous small landforms on Mars These distinctivelandforms may be roughly circular but more are not readily interpretable in terms of conventionalimpact, commonly are subrectangular,with abrupt edges and steep flanks that slopeas much as 35ø or more (Figures 5a and 5b). volcanic, or erosionalprocesses. Such featuresinclude circular to rectangularmesas and buttes, with and without summit The top is flat or gently convex, with or without a crater at the craters(Figures 1 and 2), and 'two-story'structures consisting summit, and is composedof aa and pahoehoe flows which in of conicalor irregularknobs atop broad, flat, steep-sidedped- most cases developed into a small subaerial shield volcano estals(Figure 2a). Somelandforms exhibit morphologies con- [Kjartansson,1960]. Underlying the subaerialflows is a pedes- sistentwith either volcanic or impact origins, so their genetic tal-like foundation of 'm6berg,' the Icelandic term for pala- classificationis not obvious.These types of features are espe- gonitized tuffs and breccias[Kjartansson, 1960]. The m6berg cially abundant in the 'northern plains,' betweenabout lati- mass in turn overlies and is partly intercalated with a basal tude 40øN and the margin of the polar ice cap. Features that core of pillow lava. Some table mountains lack the subaerial are clearly volcanicalso occurin parts of this region, specifi- basalt cap (Figure 6). cally, north of the Tharsis and Elysium volcanicprovinces. The pillow lava and m6berg pedestalsindicate that water Well-defined lava flows on the flanks of Alba Patera are inter- was abundant at the site of extrusion. The prevailing genetic mingled with conical cratered domes a few kilometers across hypothesisis diagramedLn Figure 7 [Einarsson,1968]. Basaltic that resemble small volcanic cones; clusters of such features magma was extruded subglacially into water-filled caverns have been noted elsewhereas well (Figure 2b). melted into or through a late Quaternary ice sheet.The initial If terrestrialanalogs are to be found for theseMartian land- extrusions of pillow lava were emplaced beneath meltwater forms,they are mostprofitably sought where geologic and cli- and ice. As the pile of pillow lava grew upward, confining matic conditions are similar to past or present environments pressuresof the overlying meltwater and ice decreased,and on Mars; Iceland, with its combination of active volcanism the consequentincreased vesiculation of the magma, aug- and glaciation,is a promisinglocale to explore [Allen, 1977, mented by influx of water into the vent, initiated phreatomag- 1978, 1979;Hodges, 1977; Hodges and Moore, 1978a, b; Wil- matic explosions [Jones, 1970]. Sideromelane tuff breccias, liams, 1978].The table mountainsof Iceland (Figures3a and subsequentlyaltered to palagonite,were then depositedatop 3b), whichformed as a resultof subglacialvolcanic extrusion, the pillow lava. If the accumulatingpile reachedthe surfaceof are our major topic of interest here, augmentedby reference the meltwater lake, subaerialflows were emplaced,commonly to oceanic shield volcanoes such as Mauna Loa, which have capped by a shield volcano. As the subaerial flows advanced subaqueouseruptive historiesparallel with the subglacial into the meltwater at the margin of the pile, explosive dis- stagesof the Icelandic table mountains[Kjartansson, 1966a; ruption occurred,and tuff brecciaswere depositedas steeply Moore and Fiske, 1969]. dipping sediments,much like the foreset beds of a delta, but in this caseoverridden by topset beds of lava [Jones,1969]. ICELAND'S TABLE MOUNTAINS With subsequentwithdrawal of the ice, the subaerial flows The relatively small, isolated plateaustermed table moun- formed a resistantcap overlying the less resistantm6berg tains (Figure 4) have been describedin detail by Van Bernrne- foundation. The thicknessof the ice sheet, indicated by the len and Rutten [1955], Jones [1966, 1969, 1970], Kjartansson height of the m6berg pedestals,was apparently 500-1000 m during the Pleistocenestage of table mountain development. Copyright ¸ 1979 by the American GeophysicalUnion. Crateredhills or mesasof m6bergthat are not cappedby lava Paper number 9B 1125. 8061 0148-0227/79/009B- 1125501.00 8062 HODGES AND MOORE: SECOND MARS COLLOQUIUM a b Fig. 1. The small circular plateau with summit crater (arrow) is one of the best candidates for a Martian table mountain. It has a mor- phology and dimensions that are similar to the table mountains in c d Iceland which are formed by subglacial volcanic eruption (compare with Figure 3). Terraces and ridgesoccur near the base.Smaller, simi- lar featuresare nearby. Horizontal and approximate vertical scalesof --- 6 km profile are same scaleas photograph.(Height estimatedfrom shadow length.) Sun at left. (Latitude 49øN, longitude 225ø; Viking photo- graph 009B 15.) Fig. 2a. Rectangular to subcircular Martian mesas that resemble Icelandic table mountains with (arrow a) and without (arrow b) obvi- ous summit craters.Two-story structureand typical impact craters in- (Figure 6) and m6berg ridges (formed by subglacialfissure dicated by arrows c and d. Diagrammatic profiles drawn at ap- eruptions) presumably representextrusions that did not reach proximately twice the scale of photograph;no vertical exaggeration. (Heights estimatedfrom shadowlengths.) Sun at left. (Latitude 45øN, the surfaceof the ice or meltwater [Kjartansson,1960]. longitude 20ø; Viking photograph026A30.) These Icelandic features are relatively small, generally a few kilometers across and a few hundred meters high; the highest,Herdubreid (Figure 5), has over 1000 m of total relief [Van Bemmelenand Rutten, 1955]. The contrast in morphol- ogy between strictly subaerial shieldsand table mountains in . Iceland [Jones, 1969] is readily apparent on topographic maps of the two types of structures(Figure 8). The tuyas of British Columbia also have been interpreted as ..i•' ;•;•i;..;:•::::::::::::::::::::::::::::::::::::::: productsof subglacialPleistocene eruptions [Mathews, 1948], ... ß:'*:i.'*" "'"'::• as have similar volcanic rock successionsin Antarctica [Le Masurier, 1972] and Alaska [Hoare and Coanrad, 1978]. Anal- ...:. yses of subglacial shield-type eruptions and resulting land- "':.•i""•*' *<":' n..... ":'-};:. forms are applicable to the submarine development of larger oceanic shield volcanoes [Kjartansson, 1966a, 1967; Jones, 1966; Moore and Fiske, 1969]. OCEANIC SHIELD VOLCANOES Moore and Fiske [1969] documented a threefold structure analogousto that of the table mountains in the shield volca- noes on the island of Hawaii (Figure 9): (1) pillow lava and fragmentserupted from deepwatervents, overlain by (2) vitric explosiondebris, littoral cone ash and breccia erupted from shallow water vents or at the interface of subaerial lava and water, and (3) the subaerial shield that forms the super- structure of the volcano. As in the table mountains, the con- tact between the'subaerial shield and the submarine pedestal is marked by a distinct break in slope (becauseof the suscepti- bility to masswasting and erosionof the brecciasand pillow Fig. 2b. Small,possibly volcanic, cratered domes (arrow). Dia- lava), but the lower flank is not as steepas in the subglacial grammaticprofile drawn at scalelarger than that of photograph;no case. Kjartansson [1966a] inferred that the same stages and verticalexaggeration. (Height estimated from shadowlength.) Sun at productsof eruption characterizeddevelopment of the Surtsey left. (Latitude40øN,
Load more

Recommended publications
  • Design of Low-Altitude Martian Orbits Using Frequency Analysis A
    Design of Low-Altitude Martian Orbits using Frequency Analysis A. Noullez, K. Tsiganis To cite this version: A. Noullez, K. Tsiganis. Design of Low-Altitude Martian Orbits using Frequency Analysis. Advances in Space Research, Elsevier, 2021, 67, pp.477-495. 10.1016/j.asr.2020.10.032. hal-03007909 HAL Id: hal-03007909 https://hal.archives-ouvertes.fr/hal-03007909 Submitted on 16 Nov 2020 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. Design of Low-Altitude Martian Orbits using Frequency Analysis A. Noulleza,∗, K. Tsiganisb aUniversit´eC^oted'Azur, Observatoire de la C^oted'Azur, CNRS, Laboratoire Lagrange, bd. de l'Observatoire, C.S. 34229, 06304 Nice Cedex 4, France bSection of Astrophysics Astronomy & Mechanics, Department of Physics, Aristotle University of Thessaloniki, GR 541 24 Thessaloniki, Greece Abstract Nearly-circular Frozen Orbits (FOs) around axisymmetric bodies | or, quasi-circular Periodic Orbits (POs) around non-axisymmetric bodies | are of primary concern in the design of low-altitude survey missions. Here, we study very low-altitude orbits (down to 50 km) in a high-degree and order model of the Martian gravity field. We apply Prony's Frequency Analysis (FA) to characterize the time variation of their orbital elements by computing accurate quasi-periodic decompositions of the eccentricity and inclination vectors.
    [Show full text]
  • Variability of Mars' North Polar Water Ice Cap I. Analysis of Mariner 9 and Viking Orbiter Imaging Data
    Icarus 144, 382–396 (2000) doi:10.1006/icar.1999.6300, available online at http://www.idealibrary.com on Variability of Mars’ North Polar Water Ice Cap I. Analysis of Mariner 9 and Viking Orbiter Imaging Data Deborah S. Bass Instrumentation and Space Research Division, Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228-0510 E-mail: [email protected] Kenneth E. Herkenhoff U.S. Geological Survey, 2255 North Gemini Drive, Flagstaff, Arizona 86001 and David A. Paige Department of Earth and Space Sciences, University of California, Los Angeles, 405 Hilgard Avenue, Los Angeles, California 90095-1567 Received May 15, 1998; revised November 17, 1999 1. INTRODUCTION Previous studies interpreted differences in ice coverage between Mariner 9 and Viking Orbiter observations of Mars’ north residual Like Earth, Mars has perennial ice caps and an active wa- polar cap as evidence of interannual variability of ice deposition on ter cycle. The Viking Orbiter determined that the surface of the the cap. However,these investigators did not consider the possibility northern residual cap is water ice (Kieffer et al. 1976, Farmer that there could be significant changes in the ice coverage within et al. 1976). At the south residual polar cap, both Mariner 9 the northern residual cap over the course of the summer season. and Viking Orbiter observed carbon dioxide ice throughout the Our more comprehensive analysis of Mariner 9 and Viking Orbiter summer. Many have related observed atmospheric water vapor imaging data shows that the appearance of the residual cap does not abundances to seasonal exchange between reservoirs such as show large-scale variance on an interannual basis.
    [Show full text]
  • MARS DURING the PRE-NOACHIAN. J. C. Andrews-Hanna1 and W. B. Bottke2, 1Lunar and Planetary La- Boratory, University of Arizona
    Fourth Conference on Early Mars 2017 (LPI Contrib. No. 2014) 3078.pdf MARS DURING THE PRE-NOACHIAN. J. C. Andrews-Hanna1 and W. B. Bottke2, 1Lunar and Planetary La- boratory, University of Arizona, Tucson, AZ 85721, [email protected], 2Southwest Research Institute and NASA’s SSERVI-ISET team, 1050 Walnut St., Suite 300, Boulder, CO 80302. Introduction: The surface geology of Mars appar- ing the pre-Noachian was ~10% of that during the ently dates back to the beginning of the Early Noachi- LHB. Consideration of the sawtooth-shaped exponen- an, at ~4.1 Ga, leaving ~400 Myr of Mars’ earliest tially declining impact fluxes both in the aftermath of evolution effectively unconstrained [1]. However, an planet formation and during the Late Heavy Bom- enduring record of the earlier pre-Noachian conditions bardment [5] suggests that the impact flux during persists in geophysical and mineralogical data. We use much of the pre-Noachian was even lower than indi- geophysical evidence, primarily in the form of the cated above. This bombardment history is consistent preservation of the crustal dichotomy boundary, to- with a late heavy bombardment (LHB) of the inner gether with mineralogical evidence in order to infer the Solar System [6] during which HUIA formed, which prevailing surface conditions during the pre-Noachian. followed the planet formation era impacts during The emerging picture is a pre-Noachian Mars that was which the dichotomy formed. less dynamic than Noachian Mars in terms of impacts, Pre-Noachian Tectonism and Volcanism: The geodynamics, and hydrology. crust within each of the southern highlands and north- Pre-Noachian Impacts: We define the pre- ern lowlands is remarkably uniform in thickness, aside Noachian as the time period bounded by two impacts – from regions in which it has been thickened by volcan- the dichotomy-forming impact and the Hellas-forming ism (e.g., Tharsis, Elysium) or thinned by impacts impact.
    [Show full text]
  • 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.
    [Show full text]
  • Physical Properties of Martian Meteorites: Porosity and Density Measurements
    Meteoritics & Planetary Science 42, Nr 12, 2043–2054 (2007) Abstract available online at http://meteoritics.org Physical properties of Martian meteorites: Porosity and density measurements Ian M. COULSON1, 2*, Martin BEECH3, and Wenshuang NIE3 1Solid Earth Studies Laboratory (SESL), Department of Geology, University of Regina, Regina, Saskatchewan S4S 0A2, Canada 2Institut für Geowissenschaften, Universität Tübingen, 72074 Tübingen, Germany 3Campion College, University of Regina, Regina, Saskatchewan S4S 0A2, Canada *Corresponding author. E-mail: [email protected] (Received 11 September 2006; revision accepted 06 June 2007) Abstract–Martian meteorites are fragments of the Martian crust. These samples represent igneous rocks, much like basalt. As such, many laboratory techniques designed for the study of Earth materials have been applied to these meteorites. Despite numerous studies of Martian meteorites, little data exists on their basic structural characteristics, such as porosity or density, information that is important in interpreting their origin, shock modification, and cosmic ray exposure history. Analysis of these meteorites provides both insight into the various lithologies present as well as the impact history of the planet’s surface. We present new data relating to the physical characteristics of twelve Martian meteorites. Porosity was determined via a combination of scanning electron microscope (SEM) imagery/image analysis and helium pycnometry, coupled with a modified Archimedean method for bulk density measurements. Our results show a range in porosity and density values and that porosity tends to increase toward the edge of the sample. Preliminary interpretation of the data demonstrates good agreement between porosity measured at 100× and 300× magnification for the shergottite group, while others exhibit more variability.
    [Show full text]
  • 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.
    [Show full text]
  • Resource Utilization and Site Selection for a Self-Sufficient Martian Outpost
    NASA/TM-98-206538 Resource Utilization and Site Selection for a Self-Sufficient Martian Outpost G. James, Ph.D. G. Chamitoff, Ph.D. D. Barker, M.S., M.A. April 1998 The NASA STI Program Office... in Profile Since its founding, NASA has been dedicated to CONTRACTOR REPORT. Scientific and the advancement of aeronautics and space technical findings by NASA-sponsored science. The NASA Scientific and Technical contractors and grantees. Information (STI) Program Office plays a key part in helping NASA maintain this important CONFERENCE PUBLICATION. Collected role. papers from scientific and technical confer- ences, symposia, seminars, or other meetings The NASA STI Program Office is operated by sponsored or cosponsored by NASA. Langley Research Center, the lead center for NASA's scientific and technical information. SPECIAL PUBLICATION. Scientific, The NASA STI Program Office provides access technical, or historical information from to the NASA STI Database, the largest NASA programs, projects, and mission, often collection of aeronautical and space science STI concerned with subjects having substantial in the word. The Program Office is also public interest. NASA's institutional mechanism for disseminating the results of its research and • TECHNICAL TRANSLATION. development activities. These results are English-language translations of foreign scientific published by NASA in the NASA STI Report and technical material pertinent to NASA's Series, which includes the following report mission. types: Specialized services that complement the STI TECHNICAL PUBLICATION. Reports of Program Office's diverse offerings include completed research or a major significant creating custom thesauri, building customized phase of research that present the results of databases, organizing and publishing research NASA programs and include extensive results.., even providing videos.
    [Show full text]
  • Mars Field Geology, Biology, and Paleontology Workshop, Summary
    MARS FIELD GEOLOGY, BIOLOGY, AND PALEONTOLOGY WORKSHOP: SUMMARY AND RECOMMENDATIONS November 18–19, 1998 Space Center Houston, Houston, Texas LPI Contribution No. 968 MARS FIELD GEOLOGY, BIOLOGY, AND PALEONTOLOGY WORKSHOP: SUMMARY AND RECOMMENDATIONS November 18–19, 1998 Space Center Houston Edited by Nancy Ann Budden Lunar and Planetary Institute Sponsored by Lunar and Planetary Institute National Aeronautics and Space Administration Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Contribution No. 968 Compiled in 1999 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautcis and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This volume may be cited as Budden N. A., ed. (1999) Mars Field Geology, Biology, and Paleontology Workshop: Summary and Recommendations. LPI Contribution No. 968, Lunar and Planetary Institute, Houston. 80 pp. This volume is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Phone: 281-486-2172 Fax: 281-486-2186 E-mail: [email protected] Mail order requestors will be invoiced for the cost of shipping and handling. _________________ Cover: Mars test suit subject and field geologist Dean Eppler overlooking Meteor Crater, Arizona, in Mark III Mars EVA suit. PREFACE In November 1998 the Lunar and Planetary Institute, under the sponsorship of the NASA/HEDS (Human Exploration and Development of Space) Enterprise, held a workshop to explore the objectives, desired capabilities, and operational requirements for the first human exploration of Mars.
    [Show full text]
  • The Periglacial Landscape of Utopia Planitia; Geologic Evidence for Recent Climate Change on Mars
    Western University Scholarship@Western Electronic Thesis and Dissertation Repository 1-23-2013 12:00 AM The Periglacial Landscape Of Utopia Planitia; Geologic Evidence For Recent Climate Change On Mars. Mary C. Kerrigan The University of Western Ontario Supervisor Dr. Marco Van De Wiel The University of Western Ontario Joint Supervisor Dr. Gordon R Osinski The University of Western Ontario Graduate Program in Geography A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Mary C. Kerrigan 2013 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Climate Commons, Geology Commons, Geomorphology Commons, and the Physical and Environmental Geography Commons Recommended Citation Kerrigan, Mary C., "The Periglacial Landscape Of Utopia Planitia; Geologic Evidence For Recent Climate Change On Mars." (2013). Electronic Thesis and Dissertation Repository. 1101. https://ir.lib.uwo.ca/etd/1101 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. THE PERIGLACIAL LANDSCAPE OF UTOPIA PLANITIA; GEOLOGIC EVIDENCE FOR RECENT CLIMATE CHANGE ON MARS by Mary C. Kerrigan Graduate Program in Geography A thesis submitted in partial fulfillment of the requirements for the degree of Master of Science The School of Graduate and Postdoctoral Studies The University of Western Ontario London, Ontario, Canada © Mary C. Kerrigan 2013 ii THE UNIVERSITY OF WESTERN ONTARIO School of Graduate and Postdoctoral Studies CERTIFICATE OF EXAMINATION Joint Supervisor Examiners ______________________________ Dr.
    [Show full text]
  • A MARTIAN METEORITE SPECTRAL LIBRARY BASED on in SITU PYROXENE and BULK MARTIAN METEORITE SPECTRA. K. J. Orr1, L. V. Forman1, G. K
    51st Lunar and Planetary Science Conference (2020) 1357.pdf A MARTIAN METEORITE SPECTRAL LIBRARY BASED ON IN SITU PYROXENE AND BULK MARTIAN METEORITE SPECTRA. K. J. Orr1, L. V. Forman1, G. K. Benedix1, M. J. Hackett2 and V. E. Hamilton3. 1Space Science and Technology Centre (SSTC), School of Earth and Planetary Sciences, Curtin Uni- versity, Perth, Western Australia, Australia ([email protected]), 2School of Molecular and Life Sciences, Curtin University, Perth, Western Australia, Australia, 3Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302 USA. Introduction: Thermal infrared spectrometers have tions using four energy dispersive x-ray (EDS) detec- been on board every major space mission to Mars. The tors which allows phase, back-scattered electron Thermal Emission Spectrometer (TES) and the Ther- (BSE) and element x-rays maps to be collected simul- mal Emission Imaging System (THEMIS), on board taneously. The analyses were run with a 70 nm spot Mars Global Survey and Mars Odyssey, respectively, size, 3 µm step size, 15 mm working distance and at have globally mapped the Martian surface in the mid- 25 kV accelerating voltage. infrared (MIR). In the MIR, spectra can be linearly Electron back-scattered diffraction (EBSD) deconvolved to determine modal mineralogy and the analyses were carried out on the sections using a MIR also allows for differentiation between various Tescan Mira3 VP-FESEM (variable pressure field silicates and their constituent phases [1]. This is emission scanning electron microscope) with an Ox- commonly done by deconvolving the Mars acquired fords Instruments Symmetry CMOS detector at the spectra using known terrestrial spectra of rocks and John de Laeter Centre in Curtin University.
    [Show full text]
  • 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).
    [Show full text]
  • FROM WET PLANET to RED PLANET Current and Future Exploration Is Shaping Our Understanding of How the Climate of Mars Changed
    FROM WET PLANET TO RED PLANET Current and future exploration is shaping our understanding of how the climate of Mars changed. Joel Davis deciphers the planet’s ancient, drying climate 14 DECEMBER 2020 | WWW.GEOLSOC.ORG.UK/GEOSCIENTIST WWW.GEOLSOC.ORG.UK/GEOSCIENTIST | DECEMBER 2020 | 15 FEATURE GEOSCIENTIST t has been an exciting year for Mars exploration. 2020 saw three spacecraft launches to the Red Planet, each by diff erent space agencies—NASA, the Chinese INational Space Administration, and the United Arab Emirates (UAE) Space Agency. NASA’s latest rover, Perseverance, is the fi rst step in a decade-long campaign for the eventual return of samples from Mars, which has the potential to truly transform our understanding of the still scientifi cally elusive Red Planet. On this side of the Atlantic, UK, European and Russian scientists are also getting ready for the launch of the European Space Agency (ESA) and Roscosmos Rosalind Franklin rover mission in 2022. The last 20 years have been a golden era for Mars exploration, with ever increasing amounts of data being returned from a variety of landed and orbital spacecraft. Such data help planetary geologists like me to unravel the complicated yet fascinating history of our celestial neighbour. As planetary geologists, we can apply our understanding of Earth to decipher the geological history of Mars, which is key to guiding future exploration. But why is planetary exploration so focused on Mars in particular? Until recently, the mantra of Mars exploration has been to follow the water, which has played an important role in shaping the surface of Mars.
    [Show full text]