Tardi-Magmatic Precipitation of Martian Fe/Mg-Rich Clay Minerals Via Igneous Differentiation
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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). -
New Mars Meteorite Fall in Marocco: Final Strewn Field
Available online at www.ilcpa.pl International Letters of Chemistry, Physics and Astronomy 11 (2013) 20-25 ISSN 2299-3843 New Mars meteorite fall in Marocco: final strewn field Abderrahmane Ibhi Laboratory of Geo-heritage and Geo-materials Science, Ibn Zohr University, Agadir, Morocco E-mail address: [email protected] ABSTRACT The Tissint fireball is the only fireball to have been observed and reported by numerous witnesses across the south-east of Morocco. The event was extremely valuable to the scientific community; show an extraordinary and rare event and were also the brightest and most comprehensively observed fireball in Morocco’s known astronomical history. Since the abstract of A. Ibhi (2011) [1]. In 1012-2013 concerning a number of Martian meteorite fragments found in the region of Tata (Morocco), a number of expeditions have been made to the area. A. ibhi has done a great amount of field work. He discovered the strewn field and collected the fragments of this Martian meteorite and many information. Each expedition has had the effect of expanding the size of the strewn field which is now documented to cover more than 70 sq. kilometers. The size of the strewn field is now estimated to be about a 17 km long. Keywords: fireball; Martian meteorite; Shergottite; Strewn field; Tissint; Morocco. 1. INTRODUCTION A meteoritic body entered the earth’s atmosphere in the south-east skies of Tata, Morocco, On Sunday July, 18th, 2011 at 2 o’clock in the morning. Its interaction with the atmosphere led to brilliant light flashes accompanied with detonations. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Lunar Silica-Bearing Diorite: a Lithology from the Moon with Implications for Igneous Differentiation
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 2008.pdf LUNAR SILICA-BEARING DIORITE: A LITHOLOGY FROM THE MOON WITH IMPLICATIONS FOR IGNEOUS DIFFERENTIATION. T. J. Fagan1* and S. Ohkawa1, 1Dept. Earth Sci., Waseda Univ., 1-6-1 Nishi- waseda, Shinjuku, Tokyo, 169-8050, Japan (*[email protected]). Introduction: Silica-rich igneous (“granitic”) ratios and relatively high F concentrations indicate that rocks are rare on the Moon, but have been detected by the analyzed grains are apatite (not merrillite). remote sensing on the lunar surface [e.g., 1], and in Results: The silica-bearing diorite (Sil-Di) is dom- Apollo samples and lunar meteorites [e.g., 2-5]. To date, inated by pyroxene (55 mode%), plagioclase feldspar lunar granitic samples have been characterized by high (36%), silica (4.4%), ilmenite (3.9%) and K-feldspar concentrations of incompatible elements and/or mafic (0.3%) (Fig. 2). Apatite and troilite also occur. The Sil- silicates with high Fe# (atomic Fe/[Fe+Mg]x100) [2-5], Di exhibits interlocking, igneous textures with elongate both features consistent with origin from late-stage re- plagioclase feldspar (Fig. 2). Plagioclase feldspar has sidual liquids or very low degree partial melting. Fur- nearly constant composition of An88Ab11, but pyroxene thermore, silica-rich rocks detected by remote sensing has a wide range of zoning (Fig. 3). often combine the Christiansen feature in infra-red spec- The modal composition of the Sil-Di is plagioclase- tra with high incompatible element concentrations (e.g., rich compared to many silica-bearing igneous rocks Th detected by gamma-ray spectroscopy [1]), again re- from the Moon (Fig. -
3.18 Oneviewofthegeochemistryof Subduction-Related Magmatic Arcs
3.18 OneView of the Geochemistry of Subduction-Related Magmatic Arcs, with an Emphasis on Primitive Andesite and Lower Crust P. B. Ke l e m e n Columbia University, Palisades, NY, USA K. HanghÖj Lamont-Doherty Earth Observatory of Columbia University, Palisades, NY,USA and A. R. Greene University of British Columbia,Vancouver, BC, Canada 3.18.1 INTRODUCTION 2 3.18.1.1 Definition of Terms Used in This Chapter 2 3.18.2 ARC LAVA COMPILATION 3 3.18.3 CHARACTERISTICS OF ARC MAGMAS 7 3.18.3.1 Comparison with MORBs 7 3.18.3.1.1 Major elements 7 3.18.3.1.2 We are cautious about fractionation correction of major elements 9 3.18.3.1.3 Distinctive, primitive andesites 11 3.18.3.1.4 Major elements in calc-alkaline batholiths 11 3.18.3.2 Major and Trace-Element Characteristics of Primitive Arc Magmas 18 3.18.3.2.1 Primitive basalts predominate 18 3.18.3.2.2 Are some low Mgx basalts primary melts? Perhaps not 22 3.18.3.2.3 Boninites, briefly 22 3.18.3.2.4 Primitive andesites: a select group 23 3.18.3.2.5 Three recipes for primitive andesite 23 3.18.3.3 Trace Elements, Isotopes, and Source Components in Primitive Magmas 29 3.18.3.3.1 Incompatible trace-element enrichment 29 3.18.3.3.2 Tantalum and niobium depletion 36 3.18.3.3.3 U-series isotopes 37 3.18.3.3.4 Geodynamic considerations 40 3.18.4 ARC LOWER CRUST 43 3.18.4.1 Talkeetna Arc Section 43 3.18.4.1.1 Geochemical data from the Talkeetna section 45 3.18.4.1.2 Composition, fractionation, and primary melts in the Talkeetna section 49 3.18.4.2 Missing Primitive Cumulates: Due to Delamination 52 3.18.4.3 -
Can Mars' Current Atmosphere Land Block Island Sized Meteorites?
41st Lunar and Planetary Science Conference (2010) 2351.pdf CAN MARS’ CURRENT ATMOSPHERE LAND BLOCK ISLAND SIZED METEORITES? J.E.Chappelow1 and M.P. Golombek2, 1SAGA Inc., 1148 Sundance Loop, Fairbanks, AK 99709 (john.chap- [email protected]), 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109. Introduction: In 2005-6 Chappelow and Sharpton mass and vf is the final velocity, were used to sort the showed that iron meteorites up to a few kg in mass BI meteorite outcomes out of the results. should be expected on Mars [1,2] and that even irons Results: We found that Mars’ current atmosphere the mass of Heat Shield Rock (hereafter HSR, also can decelerate iron meteoroids as large as Block Is- named Meridiani Planum) (50 – 60 kg) could be land below 2 km/s, but only if they start with very spe- landed, even under as low-density a martian atmo- cific masses, speeds, and (especially) entry angles. All sphere as the one that exists today, though only rarely. of the positive results for BI that were found followed They would have to encounter the planet within nar- the type 3 flight path shown on Fig. 1 (termed “fall- row limits of initial mass, entry velocity, and entry back” trajectories in the caption). On this type of tra- angle [3] to have their velocity reduced sufficiently be- jectory, the meteoroid enters the atmosphere, initially low hypervelocity impact speeds (< 2 km/s) to land a descends, but then ascends briefly as the planet curves meteorite as opposed to forming a primary crater and away beneath it, before finally slowing and redescend- being destroyed or severely deformed. -
The Mars 2020 Candidate Landing Sites: a Magnetic Field Perspective
The Mars 2020 Candidate Landing Sites: A Magnetic Field Perspective The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Mittelholz, Anna et al. “The Mars 2020 Candidate Landing Sites: A Magnetic Field Perspective.” Earth and Space Science 5, 9 (September 2018): 410-424 © 2018 The Authors As Published http://dx.doi.org/10.1029/2018EA000420 Publisher American Geophysical Union (AGU) Version Final published version Citable link http://hdl.handle.net/1721.1/118846 Terms of Use Creative Commons Attribution-NonCommercial-NoDerivs License Detailed Terms http://creativecommons.org/licenses/by-nc-nd/4.0/ Earth and Space Science RESEARCH ARTICLE The Mars 2020 Candidate Landing Sites: A Magnetic 10.1029/2018EA000420 Field Perspective Key Points: • Mars 2020 offers the opportunity Anna Mittelholz1 , Achim Morschhauser2 , Catherine L. Johnson1,3, to acquire samples that record the Benoit Langlais4 , Robert J. Lillis5 , Foteini Vervelidou2 , and Benjamin P. Weiss6 intensity and direction of the ancient Martian magnetic field 1 • Laboratory paleomagnetic Department of Earth, Ocean and Atmospheric Sciences, The University of British Columbia, Vancouver, British Columbia, 2 3 measurements of returned samples Canada, GFZ German Research Center for Geosciences, Potsdam, Germany, Planetary Science Institute, Tucson, AZ, USA, can address questions about the 4Laboratoire de Planétologie et Geodynamique, UMR 6112 CNRS & Université de Nantes, Nantes, France, 5Space Science history of the -
The Tennessee Meteorite Impact Sites and Changing Perspectives on Impact Cratering
UNIVERSITY OF SOUTHERN QUEENSLAND THE TENNESSEE METEORITE IMPACT SITES AND CHANGING PERSPECTIVES ON IMPACT CRATERING A dissertation submitted by Janaruth Harling Ford B.A. Cum Laude (Vanderbilt University), M. Astron. (University of Western Sydney) For the award of Doctor of Philosophy 2015 ABSTRACT Terrestrial impact structures offer astronomers and geologists opportunities to study the impact cratering process. Tennessee has four structures of interest. Information gained over the last century and a half concerning these sites is scattered throughout astronomical, geological and other specialized scientific journals, books, and literature, some of which are elusive. Gathering and compiling this widely- spread information into one historical document benefits the scientific community in general. The Wells Creek Structure is a proven impact site, and has been referred to as the ‘syntype’ cryptoexplosion structure for the United State. It was the first impact structure in the United States in which shatter cones were identified and was probably the subject of the first detailed geological report on a cryptoexplosive structure in the United States. The Wells Creek Structure displays bilateral symmetry, and three smaller ‘craters’ lie to the north of the main Wells Creek structure along its axis of symmetry. The question remains as to whether or not these structures have a common origin with the Wells Creek structure. The Flynn Creek Structure, another proven impact site, was first mentioned as a site of disturbance in Safford’s 1869 report on the geology of Tennessee. It has been noted as the terrestrial feature that bears the closest resemblance to a typical lunar crater, even though it is the probable result of a shallow marine impact. -
Chronology of Late Cretaceous Igneous and Hydrothermal Events at the Golden Sunlight Gold-Silver Breccia Pipe, Southwestern Montana
Chronology of Late Cretaceous Igneous and Hydrothermal Events at the Golden Sunlight Gold-Silver Breccia Pipe, Southwestern Montana U.S. GEOLOGICAL SURVEY BULLETIN 2155 T OF EN TH TM E R I A N P T E E D R . I O S . R U M 9 A 8 4 R C H 3, 1 a Chronology of Late Cretaceous Igneous and Hydrothermal Events at the Golden Sunlight Gold-Silver Breccia Pipe, Southwestern Montana By Ed DeWitt, Eugene E. Foord, Robert E. Zartman, Robert C. Pearson, and Fess Foster T OF U.S. GEOLOGICAL SURVEY BULLETIN 2155 EN TH TM E R I A N P T E E D R . I O S . R U M 9 A 8 4 R C H 3, 1 UNITED STATES GOVERNMENT PRINTING OFFICE, WASHINGTON : 1996 a U.S. DEPARTMENT OF THE INTERIOR BRUCE BABBITT, Secretary U.S. GEOLOGICAL SURVEY Gordon P. Eaton, Director For sale by U.S. Geological Survey, Information Services Box 25286, Federal Center Denver, CO 80225 Any use of trade, product, or firm names in this publication is for descriptive purposes only and does not imply endorsement by the U.S. Government Library of Congress Cataloging-in-Publication Data Chronolgy of Late Cretaceous igneous and hydrothermal events at the Golden Sunlight gold-silver breccia pipe, southwestern Montana / by Ed DeWitt . [et al.]. p. cm.—(U.S. Geological Survey bulletin ; 2155) Includes bibliographical references. Supt. of Docs. no. : I 19.3 : 2155 1. Geology, Stratigraphic—Cretaceous. 2. Rocks, Igneous—Montana. 3. Hydrothermal alteration—Montana. 4. Gold ores—Montana. 5. Breccia pipes—Montana. -
The Origin of Ancient Magnetic Activity on Small Planetary Bodies: a Nanopaleomagnetic Study
The Origin of Ancient Magnetic Activity on Small Planetary Bodies: A Nanopaleomagnetic Study James Francis Joseph Bryson Department of Earth Sciences University of Cambridge This dissertation is submitted for the degree of Doctor of Philosophy Selwyn College October 2014 To my family and teachers Declaration I hereby declare that except where specific reference is made to the work of others, the contents of this dissertation are original and have not been submitted in whole or in part for consideration for any other degree or qualification in this, or any other University. This dissertation is the result of my own work and includes nothing which is the outcome of work done in collaboration, except where specifically indicated in the text. This dissertation contains fewer than 225 pages of text, appendices, illustrations, captions and bibliography. James Francis Joseph Bryson October 2014 Acknowledgements First and foremost, I would like to acknowledge my supervisors, Richard Harrison and Simon Redfern. Without Richard’s hard work, dedication, supervision and direction this project would not have been possible, and I feel privileged to have worked with him. Simon should be thanked for his guidance, hours of entertainment and awful jokes. I would like to acknowledge all of my collaborators, in particular Nathan Church, Claire Nichols, Roberts Blukis, Julia Herrero-Albillos, Florian Kronast, Takeshi Kasama and Francis Nimmo. Each has played an invaluable role in acquiring and understanding the data in this thesis and I would not have reached this point without their expertise and help. Martin Walker must be thanked for his assistance and calming influence. I would like to also thank Ioan Lascu for proof-reading this thesis and general advice. -
Magma Mixing Interaction Between Rhyolitic and Basaltic Melt
Magma Mixing Interaction Between Rhyolitic and Basaltic Melt Daniele Morgavi München 2013 Magma Mixing Interaction Between Rhyolitic and Basaltic Melts Daniele Morgavi Dissertation an der Fakultat fur Geowissenschaften der Ludwig-Maximilians-Universität München vorgelegt von Daniele Morgavi aus Roma, Italia München, den May, 2013 Erstgutachter: DONALD B. DINGWELL Zweitgutachter: DIEGO PERUGINI Tag der mündlichen Prüfung: 14. 01. 2014 To all the Friend and lovers that have shared a peace of their life with me In my life (Lennon and McCartney) There are places I remember All my life, though some have changed Some forever not for better Some have gone and some remain All these places have their moments With lovers and friends I still can recall Some are dead and some are living In my life I've loved them all But of all these friends and lovers There is no one compares with you And these memories lose their meaning When I think of love as something new Though I know I'll never lose affection For people and things that went before I know I'll often stop and think about them In my life I love you more Though I know I'll never lose affection For people and things that went before I know I'll often stop and think about them In my life I love you more In my life I love you more i Table of content Table of content……………………………………………………………………ii List of figures………………………………………………………………………iv List of tables………………………………………………………………………..v Preamble…………………………………………………………………………...vi Summary…………………………………………………………………………..vii Zusammenfassung………………………………………………………………...viii Chapter 1. Introduction…………………………………………………………….1 1.1 Magma mixing theory the idea of Bunsen…………………………………2 1.2 Magma mixing in the modern times……………………………………….4 1.3 Numerical and experimental stady a new light for understanding magma mixing………………………………………………………………5 1.4 Chaotic Mixing Experiment………………………………………………..6 Chapter 2. -
Chemical and Isotopic Fractionation of Wet Andesite in a Temperature Gradient: Experiments and Models Suggesting a New Mechanism of Magma Differentiation
Available online at www.sciencedirect.com Geochimica et Cosmochimica Acta 73 (2009) 729–749 www.elsevier.com/locate/gca Chemical and isotopic fractionation of wet andesite in a temperature gradient: Experiments and models suggesting a new mechanism of magma differentiation F. Huang a, C.C. Lundstrom a,*, J. Glessner a, A. Ianno a, A. Boudreau b,J.Lia, E.C. Ferre´ c, S. Marshak a, J. DeFrates a a Department of Geology, University of Illinois at Urbana-Champaign, 245 NHB, 1301 W. Green St., IL 61801, USA b Nicholas School of the Environment and Earth Sciences, Box 90227, Duke University, Durham, NC 27708, USA c Department of Geology, Southern Illinois University, Carbondale, IL 62901-4324, USA Received 6 August 2008; accepted in revised form 4 November 2008; available online 18 November 2008 Abstract Piston–cylinder experiments were conducted to investigate the behavior of partially molten wet andesite held within an imposed temperature gradient at 0.5 GPa. In one experiment, homogenous andesite powder (USGS rock standard AGV-1) with 4 wt.% H2O was sealed in a double capsule assembly for 66 days. The temperature at one end of this charge was held at 950 °C, and the temperature at the other end was kept at 350 °C. During the experiment, thermal migration (i.e., diffusion in a thermal gra- dient) took place, and the andesite underwent compositional and mineralogical differentiation. The run product can be broadly divided into three portions: (1) the top third, at the hot end, contained 100% melt; (2) the middle-third contained crystalline phases plus progressively less melt; and (3) the bottom third, at the cold end, consisted of a fine-grained, almost entirely crystalline solid of granitic composition.