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Structure Characterization of Impact Natural Diamond from Popigai Crater
80th Annual Meeting of the Meteoritical Society 2017 (LPI Contrib. No. 1987) 6191.pdf STRUCTURE CHARACTERIZATION OF IMPACT NATURAL DIAMOND FROM POPIGAI CRATER Mara Murri1, Adrian P. Jones2, Paul F. McMillan3, Christoph G. Salzmann3, Matteo Alvaro1, M. Chiara Domeneghetti1, Fabrizio Nestola4, Mauro Prencipe5, David Dobson2, Rachael Hazael3, Moreton Moore6, Sergei A. Vishnevsky7, Alla M. Logvinova7, Nikolay V. Sobolev7 1 Earth and Environmental Science University of Pavia, Via Ferrata 1, Italy ([email protected]), 2 Department of Earth Sciences, University College London, WC1E 6BT, UK ([email protected]), 3 Department of Chemistry, University College London, WC1E 6BT, UK, 4 Department of Geosciences, University of Padua, Italy 5 Earth Sciences Department, University of Torino, Italy, 6 Royal Holloway, University of London, TW20 0EX, UK, 7 Institute of Geology and Mineralogy, Siberian Branch of Russian Academy of Sciences, Koptyug Ave., 3, 630090, Novosibirsk, Russia Introduction: Impact cratering is undoubtedly one of the most frequent high-energetic and potentially catastrophic event occurring at the earth surface and in the planetary system. For example, the energy released from an impact occurring on the Earth’s surface as calculated even for a small impact crater appears to be 3 orders of magnitudes higher than the Hiroshima atomic bomb. These enormous energies and the very short duration can cause unique irreversible changes to rocks and minerals (eg. deformations, phase transformations, melting and vaporization) and are compatible with P and T conditions required to transform graphite into diamond (4.5GPa at 1000°C) and are also enough to induce deformation in the newly formed diamonds. -
The Popigai Crater in the Capacity of Interplanetary Structural Analog
EPSC Abstracts Vol. 5, EPSC2010-217, 2010 European Planetary Science Congress 2010 c Author(s) 2010 The Popigai crater in the capacity of interplanetary structural analog. G.Dolnikov (1), O.Korablev (1), O.Roste (1) and N. Evdokimova (1) (1) Space Research Institute (IKI), Russia, ([email protected] / Fax: +7-495-3332566) Abstract Popigai crater was formed into two-layer target of Archaean crystalline rocks of the Anabar Shields, In central Arctic Siberia of Russia is situated one of and overlying Proterozoic to Mesozoic sedimentary interesting placing our planet crater Popigai. It is the sequences. Basement rocks are represented by the 4th largest impact crater on Earth but the best Verkhne-Anabar (lower layer up to 10 km thick) and exposed, the three other craters are larger, but they the Khapchan (about 800-1200 m) series [3]. are either buried (Chicxulub), strongly deformed (Sudbury), or deformed and severely eroded (Vredefort). The crater is filled with melted and shuttered material, including microdiamonds and other high pressure minerals characteristic of ultra- high pressure formed during the catastrophic impact. 1. Introduction One of very interesting astroblem of Earth is one hundred kilometres Popigai structure, centred at 7134'N, 11112'E in central Arctic Siberia (Fig. 1, 2), that has been ascribed as nature conservation Figure 2: Space image of Popigai meteorite crater. object of our planet of significant first value [1], [2]. Сlearly showed the inner part about 80 km with a darker tone of forest. In Western and North-Western 2. Popigai astroblem sectors of crater clearly showed exits fragments of bottom old crater and melt rocks (tagamites). -
Earth in Upheaval – Velikovsky
KANSAS CITY, MO PUBLIC LIBRARY MAR 1989 JALS DATE DUE Earth in upheaval. 1 955 . Books by Immarvjel Velikoviky Earth in Upheaval Worlds in Collision Published by POCKET BOOKS Most Pot Ian Books arc available at special quantify discounts for hulk purchases for sales promotions premiums or fund raising SpeciaJ books* or txx)k e\( erj)ts can also tx.' created to ht specific needs FordetaJs write the office of the Vice President of Special Markets, Pocket Books, 12;K) Avenue of the Arm-mas New York New York 10020 EARTH IN UPHEAVAL Smnianue! Velikovsky F'OCKET BOOKS, a division of Simon & Schuster, IMC 1230 Avenue of the Americas, New York, N Y 10020 Copyright 1955 by Immanuel Vehkovskv Published by arrangement with Doubledav tx Compauv, 1m Library of Congiess Catalog Card Number 55-11339 All rights reserved, including the right to reproduce this book or portions thereof in any form whatsoever For information address 6r Inc. Doubledav Company, , 245 Park Avenue, New York, N Y' 10017 ISBN 0-fi71-524f>5-tt Fust Pocket Books punting September 1977 10 9 H 7 6 POCKET and colophon ae registered trademarks of Simon & Schuster, luc Printed in the USA ACKNOWLEDGMENTS WORKING ON Earth in Upheaval and on the essay (Address before the Graduate College Forum of Princeton University) added at the end of this volume, I have incurred a debt of gratitude to several scientists. Professor Walter S. Adams, for many years director of Mount Wilson Observatory, gave me all the in- formation and instruction for which I asked concern- ing the atmospheres of the planets, a field in which he is the outstanding authority. -
Shocked Quartz, Ir, Sr, and OS Anomalies Found in the Late
LPS XXVII 239 Shocked Quartz, Ir, Sr, and 0sanomalies found in the Late Eocene at Massignano (Ancona, Italy): clear evidence of a bolide impact. Aron K. Clymer, Dept. of Geology and Geophysics, University of California, Berkeley, California 94720; Hubert B. Vonhof, Research School of Sedimentary Geology (NSG), Inst. of Earth Sciences, Vrije Universiteit, de Boelelaan 1085, 1018 HV, Amsterdam, Netherlands; Thomas Meisel, Dept. of Geology, University of Maryland, College Park, MD 20742; David M. Bice, Dept. of Geology, Carleton College, Northfield, MN 55057; Alessandm Montanari, Osservatorio Geologico di Coldigioco, 62020 Frontale (MC), Italy. Shock metamorphosed quartz grains coincident with a positive Ir anomaly of 199 +I- 19 ppb, a positive 87Srl86Sr anomaly, and a negative 187W 1880s anomaly of about 0.3 5 have been found in a marly layer of the Late Eocene Scagha Variegata formation at Massignano (Ancona), which clearly indicates a large impact with an interpolated radiometric age of 35.7 +I- 0.4 Ma. The Popigai crater (Siberia, - 100 km diameter) and the recently discovered Chesapeake Bay Crater (Eastern U. S., - 80 km diameter) are the only known giant craters from the Late Eocene and are prime candidates for the event that distributed the shocked quartz and geochemical anomalies found at Massignano. Although the Middle and Late Eocene are characterized by signrficant stepwise extinctions, the only evidence of a biotic response at Massignano to an impact is a cooler water shift in the dinocyst assemblage associated with the impact layer. Therefore the effects of the impact on this region of the Late Eocene Tethys appears mild, and the global ramification s of the Late Eocene impacts on climate and life remains unclear. -
Candidates for Multiple Impact Craters: Popigai and Chicxulub As Seen by EGM08, a Global 50×50 Gravitational Model
Solid Earth Discuss., 2, 69–103, 2010 Solid Earth www.solid-earth-discuss.net/2/69/2010/ Discussions © Author(s) 2010. This work is distributed under the Creative Commons Attribution 3.0 License. This discussion paper is/has been under review for the journal Solid Earth (SE). Please refer to the corresponding final paper in SE if available. Candidates for multiple impact craters: popigai and chicxulub as seen by EGM08, a global 50×50 gravitational model J. Klokocnˇ ´ık1, J. Kostelecky´ 2,3, I. Pesekˇ 3, P. Novak´ 2,4, C. A. Wagner5, and J. Sebera1,3 1Astronomical Institute, Academy of Sciences of the Czech Republic, Czech Republic 2Research Institute for Geodesy, Topography and Cartography, Czech Republic 3Department of Advanced Geodesy, Czech Technical University, Czech Republic 4Department of Math, Faculty of Applied Sciences, University of West Bohemia, Czech Republic 5Laboratory for Satellite Altimetry, NOAA, USA Received: 15 January 2010 – Accepted: 25 February 2010 – Published: 9 March 2010 Correspondence to: J. Klokocnˇ ´ık ([email protected]) Published by Copernicus Publications on behalf of the European Geosciences Union. 69 Abstract In 2008 the new Earth Gravitational Model (EGM08) was released. It contains a com- plete set of spherical harmonic coefficients of the Earth’s gravitational potential (Stokes parameters) to degree 2190 and order 2159 that can be used for evaluation of various 5 potential quantities with both the unprecedented accuracy and high spatial resolution. Two such quantities, the gravity anomaly and second-order radial derivative of the dis- turbing potential, were computed over selected areas with known impact craters. The displays of these derivatives for two such sites clearly show not only the strong circular- like features known to be associated with them but also other symmetrical structures 10 which appear to make them multiple impact sites. -
The Recognition of Terrestrial Impact Structures
Bulletin of the Czech Geological Survey, Vol. 77, No. 4, 253–263, 2002 © Czech Geological Survey, ISSN 1210-3527 The recognition of terrestrial impact structures ANN M. THERRIAULT – RICHARD A. F. GRIEVE – MARK PILKINGTON Natural Resources Canada, Booth Street, Ottawa, Ontario, KIA 0ES Canada; e-mail: [email protected] Abstract. The Earth is the most endogenically active of the terrestrial planets and, thus, has retained the poorest sample of impacts that have occurred throughout geological time. The current known sample consists of approximately 160 impact structures or crater fields. Approximately 30% of known impact structures are buried and were initially detected as geophysical anomalies and subsequently drilled to provide geologic samples. The recognition of terrestrial impact structures may, or may not, come from the discovery of an anomalous quasi-circular topographic, geologic or geo- physical feature. In the geologically active terrestrial environment, anomalous quasi-circular features, however, do not automatically equate with an impact origin. Specific samples must be acquired and the occurrence of shock metamorphism, or, in the case of small craters, meteoritic fragments, must be demonstrated before an impact origin can be confirmed. Shock metamorphism is defined by a progressive destruction of the original rock and mineral structure with increasing shock pressure. Peak shock pressures and temperatures produced by an impact event may reach several hundreds of gigaPascals and several thousand degrees Kelvin, which are far outside the range of endogenic metamorphism. In addition, the application of shock- wave pressures is both sudden and brief. Shock metamorphic effects result from high strain rates, well above the rates of norma l tectonic processes. -
Appendix a Recovery of Ejecta Material from Confirmed, Probable
Appendix A Recovery of Ejecta Material from Confirmed, Probable, or Possible Distal Ejecta Layers A.1 Introduction In this appendix we discuss the methods that we have used to recover and study ejecta found in various types of sediment and rock. The processes used to recover ejecta material vary with the degree of lithification. We thus discuss sample processing for unconsolidated, semiconsolidated, and consolidated material separately. The type of sediment or rock is also important as, for example, carbonate sediment or rock is processed differently from siliciclastic sediment or rock. The methods used to take and process samples will also vary according to the objectives of the study and the background of the investigator. We summarize below the methods that we have found useful in our studies of distal impact ejecta layers for those who are just beginning such studies. One of the authors (BPG) was trained as a marine geologist and the other (BMS) as a hard rock geologist. Our approaches to processing and studying impact ejecta differ accordingly. The methods used to recover ejecta from unconsolidated sediments have been successfully employed by BPG for more than 40 years. A.2 Taking and Handling Samples A.2.1 Introduction The size, number, and type of samples will depend on the objective of the study and nature of the sediment/rock, but there a few guidelines that should be followed regardless of the objective or rock type. All outcrops, especially those near industrialized areas or transportation routes (e.g., highways, train tracks) need to be cleaned off (i.e., the surface layer removed) prior to sampling. -
Geochemistry of Darwin Glass and Target Rocks from Darwin Crater, Tasmania, Australia
Meteoritics & Planetary Science 43, Nr 3, 479–496 (2008) AUTHOR’S Abstract available online at http://meteoritics.org PROOF Geochemistry of Darwin glass and target rocks from Darwin crater, Tasmania, Australia Kieren T. HOWARD School of Earth Sciences, University of Tasmania, Hobart, Tasmania 7000, Australia Present address: Impacts and Astromaterials Research Centre, Department of Mineralogy, The Natural History Museum, Cromwell Road, London SW7 5BD, UK Corresponding author. E-mail: [email protected] (Received 1 March 2007; revision accepted 25 July 2007) Abstract–Darwin glass formed about 800,000 years ago in western Tasmania, Australia. Target rocks at Darwin crater are quartzites and slates (Siluro-Devonian, Eldon Group). Analyses show 2 groups of glass, Average group 1 is composed of: SiO2 (85%), Al2O3 (7.3%), TiO2 (0.05%), FeO (2.2%), MgO (0.9%), and K2O (1.8%). Group 2 has lower average SiO2 (81.1%) and higher average Al2O3 (8.2%). Group 2 is enriched in FeO (+1.5%), MgO (+1.3%) and Ni, Co, and Cr. Average Ni (416 ppm), Co (31 ppm), and Cr (162 ppm) in group 2 are beyond the range of sedimentary rocks. Glass and target rocks have concordant REE patterns (La/Lu = 5.9–10; Eu/Eu* = 0.55–0.65) and overlapping trace element abundances. 87Sr/86Sr ratios for the glasses (0.80778–0.81605) fall in the range (0.76481–1.1212) defined by the rock samples. ε-Nd results range from −13.57 to −15.86. Nd model ages range from 1.2–1.9 Ga (CHUR) and the glasses (1.2–1.5 Ga) fall within the range defined by the target samples. -
Establishing the Link Between the Chesapeake Bay Impact Structure and the North American Tektite Strewn Field: the Sr-Nd Isotopic Evidence
Meteoritics & Planetary Science 41, Nr 5, 689–703 (2006) Abstract available online at http://meteoritics.org Establishing the link between the Chesapeake Bay impact structure and the North American tektite strewn field: The Sr-Nd isotopic evidence Alexander DEUTSCH1, 2* and Christian KOEBERL3 1Institut f¸r Planetologie (IfP), Westfälische Wilhelms-Universität Münster (WWU), Wilhelm-Klemm-Str. 10, D-48149 M¸nster, Germany 2Zentrallabor f¸r Geochronologie (ZLG), WWU, Corrensstr. 24, D-48149 M¸nster, Germany 3Department of Geological Sciences, University of Vienna, Althanstrasse 14, A-1090 Vienna, Austria *Corresponding author. E-mail: [email protected] (Received 09 November 2004; revision accepted 21 December 2005) Abstract–The Chesapeake Bay impact structure, which is about 35 Ma old, has previously been proposed as the possible source crater of the North American tektites (NAT). Here we report major and trace element data as well as the first Sr-Nd isotope data for drill core and outcrop samples of target lithologies, crater fill breccias, and post-impact sediments of the Chesapeake Bay impact ε t = 35.7 Ma structure. The unconsolidated sediments, Cretaceous to middle Eocene in age, have Sr of + + ε t = 35.7 Ma − − 54 to 272, and Nd ranging from 6.5 to 10.8; one sample from the granitic basement Nd ε t = 35.7 Ma + ε t = 35.7 Ma − with a T CHUR model age of 1.36 Ga yielded an Sr of 188 and an Nd of 5.7. The Exmore breccia (crater fill) can be explained as a mix of the measured target sediments and the granite, plus an as-yet undetermined component. -
Designing Global Climate and Atmospheric Chemistry Simulations for 1 and 10 Km Diameter Asteroid Impacts Using the Properties of Ejecta from the K-Pg Impact
Atmos. Chem. Phys., 16, 13185–13212, 2016 www.atmos-chem-phys.net/16/13185/2016/ doi:10.5194/acp-16-13185-2016 © Author(s) 2016. CC Attribution 3.0 License. Designing global climate and atmospheric chemistry simulations for 1 and 10 km diameter asteroid impacts using the properties of ejecta from the K-Pg impact Owen B. Toon1, Charles Bardeen2, and Rolando Garcia2 1Department of Atmospheric and Oceanic Science, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, USA 2National Center for Atmospheric Research, Boulder, CO, USA Correspondence to: Owen B. Toon ([email protected]) Received: 15 April 2016 – Published in Atmos. Chem. Phys. Discuss.: 17 May 2016 Revised: 28 August 2016 – Accepted: 29 September 2016 – Published: 27 October 2016 Abstract. About 66 million years ago, an asteroid about surface. Nanometer-sized iron particles are also present glob- 10 km in diameter struck the Yucatan Peninsula creating the ally. Theory suggests these particles might be remnants of the Chicxulub crater. The crater has been dated and found to be vaporized asteroid and target that initially remained as va- coincident with the Cretaceous–Paleogene (K-Pg) mass ex- por rather than condensing on the hundred-micron spherules tinction event, one of six great mass extinctions in the last when they entered the atmosphere. If present in the great- 600 million years. This event precipitated one of the largest est abundance allowed by theory, their optical depth would episodes of rapid climate change in Earth’s history, yet no have exceeded 1000. Clastics may be present globally, but modern three-dimensional climate calculations have simu- only the quartz fraction can be quantified since shock fea- lated the event. -
Pleistocene Organic Matter Modified by the Hiawatha Impact, Northwest Greenland Adam A
https://doi.org/10.1130/G47432.1 Manuscript received 23 January 2020 Revised manuscript received 2 April 2020 Manuscript accepted 8 April 2020 © 2020 The Authors. Gold Open Access: This paper is published under the terms of the CC-BY license. Published online 29 May 2020 Pleistocene organic matter modified by the Hiawatha impact, northwest Greenland Adam A. Garde1, Anne Sofie Søndergaard2, Carsten Guvad1, Jette Dahl-Møller3, Gernot Nehrke4, Hamed Sanei2, Christian Weikusat4, Svend Funder3, Kurt H. Kjær3 and Nicolaj Krog Larsen3 1 Geological Survey of Denmark and Greenland, Øster Voldgade 10, 1350 Copenhagen K, Denmark 2 Lithospheric Organic Carbon (LOC) Group, Department of Geoscience, Aarhus University, Høegh Guldbergs Gade 2, 8000 Aarhus, Denmark 3 Globe Institute, University of Copenhagen, Øster Voldgade 5–7, 1350 Copenhagen K, Denmark 4 Alfred Wegener Institute, Am Handelshafen, 27570 Bremerhaven, Germany ABSTRACT an iron meteorite (Kjær et al., 2018). The bulk The 31-km-wide Hiawatha impact crater was recently discovered under the ice sheet mineral assemblage and chemical composi- in northwest Greenland, but its age remains uncertain. Here we investigate solid organic tion of the sand indicate sourcing from gran- matter found at the tip of the Hiawatha Glacier to determine its thermal degradation, ulite-grade rocks similar to Paleoproterozoic provenance, and age, and hence a maximum age of the impact. Impactite grains of micro- paragneiss exposed in the ice-free foreland brecchia and shock-melted glass in glaciofluvial sand contain abundant dispersed carbon, to the crater (locally including sulfidic parag- and gravel-sized charcoal particles are common on the outwash plain in front of the crater. -
Physical Distribution Trends in Darwin Glass
Physical distribution trends in Darwin glass Item Type Article; text Authors Howard, Kieren T. Citation Howard, K. T. (2009). Physical distribution trends in Darwin glass. Meteoritics & Planetary Science, 44(1), 115-129. DOI 10.1111/j.1945-5100.2009.tb00722.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 11/10/2021 08:24:44 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656530 Meteoritics & Planetary Science 44, Nr 1, 115–129 (2009) Abstract available online at http://meteoritics.org Physical distribution trends in Darwin glass Kieren T. HOWARD Impacts and Astromaterials Research Centre (IARC), Mineralogy Department, The Natural History Museum, Cromwell Road, London SW7 5BD, UK Corresponding author. E-mail: [email protected] (Received 25 January 2008; revision accepted 26 September 2008) Abstract–Darwin glass formed by impact melting, probably during excavation of the 1.2 km diameter Darwin crater, Tasmania, Australia. The glass was ejected up to 20 km from the source crater and forms a strewn field of >400 km2. There is at least 11,250 m3 of glass in the strewn field and relative to the size of the crater this is the most abundant ejected impact glass on Earth. The glass population can be subdivided on the basis of shape (74% irregular, 20% ropy, 0.5% spheroid, 6% droplet, and 0.7% elongate) and color (53% dark green, 31% light green, 11% black, and 5% white). The white glasses contain up to 92 wt% SiO2 and are formed from melting of quartzite.