Geophysical Methods in Impact Crater Hunting – Case Summanen
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Cross-References ASTEROID IMPACT Definition and Introduction History of Impact Cratering Studies
18 ASTEROID IMPACT Tedesco, E. F., Noah, P. V., Noah, M., and Price, S. D., 2002. The identification and confirmation of impact structures on supplemental IRAS minor planet survey. The Astronomical Earth were developed: (a) crater morphology, (b) geo- 123 – Journal, , 1056 1085. physical anomalies, (c) evidence for shock metamor- Tholen, D. J., and Barucci, M. A., 1989. Asteroid taxonomy. In Binzel, R. P., Gehrels, T., and Matthews, M. S. (eds.), phism, and (d) the presence of meteorites or geochemical Asteroids II. Tucson: University of Arizona Press, pp. 298–315. evidence for traces of the meteoritic projectile – of which Yeomans, D., and Baalke, R., 2009. Near Earth Object Program. only (c) and (d) can provide confirming evidence. Remote Available from World Wide Web: http://neo.jpl.nasa.gov/ sensing, including morphological observations, as well programs. as geophysical studies, cannot provide confirming evi- dence – which requires the study of actual rock samples. Cross-references Impacts influenced the geological and biological evolu- tion of our own planet; the best known example is the link Albedo between the 200-km-diameter Chicxulub impact structure Asteroid Impact Asteroid Impact Mitigation in Mexico and the Cretaceous-Tertiary boundary. Under- Asteroid Impact Prediction standing impact structures, their formation processes, Torino Scale and their consequences should be of interest not only to Earth and planetary scientists, but also to society in general. ASTEROID IMPACT History of impact cratering studies In the geological sciences, it has only recently been recog- Christian Koeberl nized how important the process of impact cratering is on Natural History Museum, Vienna, Austria a planetary scale. -
Detecting and Avoiding Killer Asteroids
Target Earth! Detecting and Avoiding Killer Asteroids by Trudy E. Bell (Copyright 2013 Trudy E. Bell) ARTH HAD NO warning. When a mountain- above 2000°C and triggering earthquakes and volcanoes sized asteroid struck at tens of kilometers (miles) around the globe. per second, supersonic shock waves radiated Ocean water suctioned from the shoreline and geysered outward through the planet, shock-heating rocks kilometers up into the air; relentless tsunamis surged e inland. At ground zero, nearly half the asteroid’s kinetic energy instantly turned to heat, vaporizing the projectile and forming a mammoth impact crater within minutes. It also vaporized vast volumes of Earth’s sedimentary rocks, releasing huge amounts of carbon dioxide and sulfur di- oxide into the atmosphere, along with heavy dust from both celestial and terrestrial rock. High-altitude At least 300,000 asteroids larger than 30 meters revolve around the sun in orbits that cross Earth’s. Most are not yet discovered. One may have Earth’s name written on it. What are engineers doing to guard our planet from destruction? winds swiftly spread dust and gases worldwide, blackening skies from equator to poles. For months, profound darkness blanketed the planet and global temperatures dropped, followed by intense warming and torrents of acid rain. From single-celled ocean plank- ton to the land’s grandest trees, pho- tosynthesizing plants died. Herbivores starved to death, as did the carnivores that fed upon them. Within about three years—the time it took for the mingled rock dust from asteroid and Earth to fall out of the atmosphere onto the ground—70 percent of species and entire genera on Earth perished forever in a worldwide mass extinction. -
Shatter Cone and Its Surface Mesh-Structure Formed by Impact
SHATTER CONE AND ITS SURFACE MESHED- STRUCTURE FORMED BY IMPACT MELT-GASIFICATION IN XISHAN TAIHU LAKE CHINA H.N. Wang1, Y. Chen1, X.F. Shen1 L.Y. Zhou1 and Y.W. Wang2 11Department of Earth & Planetary Sciences, Nanjing University, Nanjing, China 210093 ([email protected]) 2 Department of Natural Resources and Environmental Sciences, University of Illinois at Urbana-Champaign, Champaign Introduction: Meshed--structure shatter cone: Discuss ion: Shatter cones are represented by a range of curved to The height of these cones is generally 50 to 70 cm. The 1. Meshed-structure are related to the melt- curvilinear fractures decorated with divergent striations. striation radiates from the original point at the top of cone, gasification of carbonates target rock: Striations radiate from an apex of a conical feature or from a similar to the longitude meridian. Meanwhile, cone surface Carbonates are brittle, fusible and volatile. Under the narrow apical area. Shatter cones are the only distinct meso shock wave, it is easy to be granulated. Its melting point presents hoopline around the cone. (Fig.D) The grid on is as low as 500-600°C. When the shock wave pass to macroscopic recognition criterion for impact structures. cone surface is generally in centimeter scale (2-4cm x Despite being known for 110 yrs, the formation mechanism through, it melts instantly and forms the atherosclerotic 2-3cm), latitude and longitude lines form a grid meshed- fluid, leaving a meshed structure and imprints after of shatter cone remains unclear. Different hypotheses for structure. This is an important and unique phenomenon cooling. -
The Scientific Method an Investigation of Impact Craters
National Aeronautics and Space Administration The Scientific Method: An Investigation of Impact Craters Recommended for Grades 5,6,7 www.nasa.gov Table of Contents Digital Learning Network (DLN) .................................................................................................... 3 Overview................................................................................................................................................. 3 National Standards............................................................................................................................. 4 Sequence of Events........................................................................................................................... 5 Videoconference Outline ................................................................................................................. 6 Videoconference Event .................................................................................................................... 7 Vocabulary...........................................................................................................................................10 Videoconference Guidelines........................................................................................................11 Pre- and Post-Assessment ...........................................................................................................12 Post-Conference Activity...............................................................................................................14 -
Impact Structures and Events – a Nordic Perspective
107 by Henning Dypvik1, Jüri Plado2, Claus Heinberg3, Eckart Håkansson4, Lauri J. Pesonen5, Birger Schmitz6, and Selen Raiskila5 Impact structures and events – a Nordic perspective 1 Department of Geosciences, University of Oslo, P.O. Box 1047, Blindern, NO 0316 Oslo, Norway. E-mail: [email protected] 2 Department of Geology, University of Tartu, Vanemuise 46, 51014 Tartu, Estonia. 3 Department of Environmental, Social and Spatial Change, Roskilde University, P.O. Box 260, DK-4000 Roskilde, Denmark. 4 Department of Geography and Geology, University of Copenhagen, Øster Voldgade 10, DK-1350 Copenhagen, Denmark. 5 Division of Geophysics, University of Helsinki, P.O. Box 64, FIN-00014 Helsinki, Finland. 6 Department of Geology, University of Lund, Sölvegatan 12, SE-22362 Lund, Sweden. Impact cratering is one of the fundamental processes in are the main reason that the Nordic countries are generally well- the formation of the Earth and our planetary system, as mapped. reflected, for example in the surfaces of Mars and the Impact craters came into the focus about 20 years ago and the interest among the Nordic communities has increased during recent Moon. The Earth has been covered by a comparable years. The small Kaalijärv structure of Estonia was the first impact number of impact scars, but due to active geological structure to be confirmed in northern Europe (Table 1; Figures 1 and processes, weathering, sea floor spreading etc, the num- 7). First described in 1794 (Rauch), the meteorite origin of the crater ber of preserved and recognized impact craters on the field (presently 9 craters) was proposed much later in 1919 (Kalju- Earth are limited. -
New Clues from Earth's Most Elusive Impact Crater: Evidence of Reidite in Australasian Tektites from Thailand
See discussions, stats, and author profiles for this publication at: https://www.researchgate.net/publication/321956231 New clues from Earth's most elusive impact crater: Evidence of reidite in Australasian tektites from Thailand Article in Geology · December 2017 DOI: 10.1130/G39711.1 CITATIONS READS 0 64 4 authors, including: Aaron J. Cavosie Timmons Erickson Curtin University Curtin University 100 PUBLICATIONS 2,285 CITATIONS 27 PUBLICATIONS 159 CITATIONS SEE PROFILE SEE PROFILE All content following this page was uploaded by Aaron J. Cavosie on 16 March 2018. The user has requested enhancement of the downloaded file. New clues from Earth’s most elusive impact crater: Evidence of reidite in Australasian tektites from Thailand Aaron J. Cavosie1, Nicholas E. Timms1, Timmons M. Erickson2, and Christian Koeberl3,4 1The Institute for Geoscience Research (TIGeR), Department of Applied Geology, Curtin University, Perth, WA 6102, Australia 2Lunar and Planetary Institute, Universities Space Research Association, Houston, Texas 77058, USA 3Natural History Museum, 1010 Vienna, Austria 4Department of Lithospheric Research, University of Vienna, 1090 Vienna, Austria ABSTRACT in Australasian tektites from Thailand supports a Australasian tektites are enigmatic drops of siliceous impact melt found in an ~8000 × location for the source crater in Southeast Asia. ~13,000 km strewn field over Southeast Asia and Australia, including sites in both the Indian and Pacific oceans. These tektites formed only 790,000 yr ago from an impact crater estimated MUONG NONG–TYPE TEKTITES to be 40–100 km in diameter; yet remarkably, the young and presumably large structure Muong Nong–type tektites (MN-type, or lay- remains undiscovered. -
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The Ohio Journal of Volume 116 No. 1 April Program ANSCIENCE INTERNATIONAL MULTIDISCIPLINARY JOURNAL Abstracts The Ohio Journal of SCIENCE Listing Services ISSN 0030-0950 The Ohio Journal of Sciencearticles are listed or abstracted in several sources including: EDITORIAL POLICY AcadSci Abstracts Bibliography of Agriculture General Biological Abstracts The Ohio Journal of Scienceconsiders original contributions from members and non-members of the Academy in all fields of science, Chemical Abstracts technology, engineering, mathematics and education. Submission Current Advances in Ecological Sciences of a manuscript is understood to mean that the work is original and Current Contents (Agriculture, Biology & unpublished, and is not being considered for publication elsewhere. Environmental Sciences) All manuscripts considered for publication will be peer-reviewed. Deep Sea Research and Oceanography Abstracts Any opinions expressed by reviewers are their own, and do not Environment Abstracts represent the views of The Ohio Academy of Science or The Ohio Journal of Science. Environmental Information Center Forest Products Abstracts Forestry Abstracts Page Charges Geo Abstracts Publication in The Ohio Journal of Science requires authors to assist GEOBASE in meeting publication expenses. These costs will be assessed at $50 per page for nonmembers. Members of the Academy do not Geology Abstracts pay page charges to publish in The Ohio Journal of Science. In GeoRef multi-authored papers, the first author must be a member of the Google Scholar Academy at the time of publication to be eligible for the reduced Helminthological Abstracts member rate. Papers that exceed 12 printed pages may be charged Horticulture Abstracts full production costs. Knowledge Bank (The Ohio State University Libraries) Nuclear Science Abstracts Submission Review of Plant Pathology Electronic submission only. -
Pliocene Impact Crater Discovered in Colombia: Geological Evidences from Tektites
Lunar and Planetary Science XLVIII (2017) 2832.pdf PLIOCENE IMPACT CRATER DISCOVERED IN COLOMBIA: GEOLOGICAL EVIDENCES FROM TEKTITES. A. Ocampo1, J. Gómez2, J. A. García3, A. Lindh4, A. Scherstén4, A. Pitzsch5, L. Page4, A. Ishikawa6, 7 8 9 9 10 11 1 K. Suzuki , R. S. Hori , Margarita Buitrago and José Abel Flores , D. Barrero , V. Vajda ; NASA HQ, Science Mission Directorate, US ([email protected]), 2Colombian Geological Survey, Bogotá, Colombia; 3Universidad Libre, Sociedad astronomica ANTARES, Cali, Colombia; 4Department of Geology, Lund University, Sweden; 5MAX–lab, Lund University, Sweden/ Helmholtz Zentrum Berlin, Institute Methods and Instrumentation for Synchrotron Radia- tion Research, Berlin, Germany; 6Department of Earth Science & Astronomy, The University of Tokyo, Japan; 7IFREE/SRRP, Japan Agency for Marine–Earth Science and Technology, Yokosuka, Japan; 8Department of Earth Science, Ehime University, Japan; 9Department of Geology, University of Salamanca, Spain. 10Consultant geologist, Bogotá, Colombia; 11Department of Palaeobiology, Swedish Museum of Natural History, Sweden Introduction: The geological and paleontologi- The impact crater and the local geology: The cal record have revealed that impacts of large extra- Cali Crater is located in the Cauca Sub-Basin between terrestrial bodies may cause ecosystem devastation at a the Western and Central Colombian Cordillera, SE of global scale [1], whereas smaller impacts have more Cali, in a geologically complex and tectonically modify regional consequences depending on their size, impact area Fig 2 [5]. Using seismic data we determine the angle and composition of the target rocks [2]. Approx- outer ring of the buried Cali impact crater has major imately 200 impact structures are currently confirmed axis of 36 km and a minor axis of 26 km. -
Chicxulub and the Exploration of Large Peak- Ring Impact Craters Through Scientific Drilling
Chicxulub and the Exploration of Large Peak- Ring Impact Craters through Scientific Drilling David A. Kring, Lunar and Planetary Institute, Houston, Texas 77058, USA; Philippe Claeys, Analytical, Environmental and Geo-Chemistry, Vrije Universiteit Brussel, Pleinlaan 2, Brussels 1050, Belgium; Sean P.S. Gulick, Institute for Geophysics and Dept. of Geological Sciences, Jackson School of Geosciences, University of Texas at Austin, Austin, Texas 78758, USA; Joanna V. Morgan and Gareth S. Collins, Dept. of Earth Science and Engineering, Imperial College London SW7 2AZ, UK; and the IODP-ICDP Expedition 364 Science Party. ABSTRACT proving the structure had an impact origin. to assess the depth of origin of the peak- The Chicxulub crater is the only well- The buried structure was confirmed by ring rock types and determine how they preserved peak-ring crater on Earth and seismic surveys conducted in 1996 and were deformed during the crater-forming linked, famously, to the K-T or K-Pg mass 2005 to be a large ~180–200-km–diameter event. That information is needed to effec- impact crater with an intact peak ring tively test how peak-ring craters form on extinction event. For the first time, geolo- (Morgan et al., 1997; Gulick et al., 2008). planetary bodies. gists have drilled into the peak ring of that The discovery of the Chicxulub impact The expedition was also designed to crater in the International Ocean structure initially prompted two scientific measure any hydrothermal alteration in Discovery Program and International drilling campaigns. In the mid-1990s, a the peak ring and physical properties of the Continental Scientific Drilling Program series of shallow onshore wells up to 700 m rocks, such as porosity and permeability, (IODP-ICDP) Expedition 364. -
Educator's Guide
educator’s guide Table of Contents INTRODUCTION . 3 ACTIVITY FOR GRADES 3-5 Introduction for Educator . 4 Asteroids in Orbit Student Activity . 5 ACTIVITIES FOR GRADES 6-8 Introduction for Educator . 7 What Are Asteroids? Instructions for Educator . 7 Making a Splash Instructions for Educator . 7 Working Together Instructions for Educator . 8 What Are Asteroids? Student Activity . 9 Making a Splash Student Activity . 11 Working Together Student Activity . 13 ACTIVITIES FOR GRADES 9-12 Introduction for Educator . 15 Tracing the Past Instructions for Educator . 15 Defending the Future Instructions for Educator . 16 Tracing the Past Student Activity . 17 Defending the Future Student Activity . 18 EDUCATIONAL STANDARDS ALIGNMENT . 19 ACKNOWLEDGEMENTS . 20 2 Introduction AN EXTRAORDINARY FIELD TRIP AND LEARNING EXPERIENCE! Dear Educator, Planetary defense is a relatively new science . Only a few decades ago did we become certain Earth’s history of asteroid impacts was sure to repeat itself . Could we save our world today from a cosmic threat? You bet we can . But to tend to this problem, we must first understand it . That’s where Asteroid Hunters comes in . Asteroid Hunters will take your students on an exciting field trip across the Solar System and to the dawn of time . They’ll watch how gravity spun gas and dust into our Solar System, how rocky debris gathered into worlds, and how the planet-building leftovers became asteroids . They’ll learn that these natural wonders of deep space brought water to planets, and the building blocks of life itself . They will also see how we possess the technological know-how to keep an asteroid from hitting our planet– unlike the doomed dinosaurs of 65 million years ago . -
Shatter Cones of the Haughton Impact Structure, Canada
SHATTER CONES OF THE HAUGHTON IMPACT STRUCTURE, CANADA Gordon R. Osinski(1) and John G. Spray(2) (1)Canadian Space Agency, 6767 Route de l'Aeroport, St-Hubert, QC J3Y 8Y9 Canada, Email: [email protected]: (2)2Planetary and Space Science Centre, Department of Geology, University of New Brunswick, 2 Bailey Drive, Fredericton, NB E3B 5A3, Canada, Email: [email protected] ABSTRACT workers suggested that shatter cones are tensile fractures that form due to interference between the Despite being one of the most distinctive products of incident shock wave and reflected stress waves [5]. hypervelocity impact events, shatter cones remain Two new models have also been proposed. The first enigmatic. Several contrasting models for their model by Baratoux and Melosh [6] builds upon formation have been presented, none of which appear earlier suggestions [4] invoking heterogeneities in to account for all of the observations. In this rocks as initiation points for shatter cone formation. preliminary study, we present an overview of the These authors suggest that the interference of a distribution and characteristics of shatter cones at the scattered elastic wave by heterogeneities results in Haughton impact structure, one of the best preserved tensional stresses, which produces conical fractures. and best exposed terrestrial impact sites. Shatter In contrast, Sagy et al. [7, 8], favour a model in cones are abundant and well developed at Haughton, which shatter cones are fractures produced by due in part to the abundance of fine-grained nonlinear waves that propagate along a fracture front. carbonates in the target sequence. They occur in three main settings: within the central uplift, within 3. -
(S)TEM Analysis of Quartz-Coesite Relations in Impact Ejecta from the Australasian Tektite Strewn Field
EPSC Abstracts Vol. 12, EPSC2018-316-2, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 (S)TEM analysis of quartz-coesite relations in impact ejecta from the Australasian tektite strewn field Fabrizio Campanale (1) ([email protected]), Enrico Mugnaioli (2), Mauro Gemmi (2), Martin R. Lee (3), Billy P. Glass (4) and Luigi Folco (1) (1) Dipartimento di Scienze della Terra, Università di Pisa, Italy (2) Center for Nanotechnology Innovation@NEST, Pisa, Italy (3) Department of Geographical and Earth Sciences, University of Glasgow, UK (4) Department of Geosciences, University of Delaware, Newark, DE, USA Abstract - the largest (~15% of Earth's surface) and the youngest one (~0.8 Myr old) on Earth. Scanning and transmission electron microscopy observations on shocked silica mineral grains from the Australasian tektite/microtektite strewn field suggest that coesite crystals form directly in contact with quartz grains through a subsolidus reconstructive transformation. This finding is in contrast with the current mainstream view, which considers coesite as the product of a rapid crystallization from a dense silica melt or glass during shock unloading. 1. Introduction Quartz is one of the most common mineral in Earth's continental crust. The study of shock metamorphic features in quartz and its shock induced silica polymorphs, i.e., coesite and stishovite, is thus relevant for defining the physical conditions attained during the majority of hypervelocity impacts of cometary or asteroidal bodies on Earth. In endogenic geological processes, which typically involve equilibrium reactions and time-frames from years to thousands of years, coesite forms from quartz Figure 1: Microscopic shocked ejecta composed by at pressures between ~3 and ~10 GPa.