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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. -
Extraordinary Rocks from the Peak Ring of the Chicxulub Impact Crater: P-Wave Velocity, Density, and Porosity Measurements from IODP/ICDP Expedition 364 ∗ G.L
Earth and Planetary Science Letters 495 (2018) 1–11 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Extraordinary rocks from the peak ring of the Chicxulub impact crater: P-wave velocity, density, and porosity measurements from IODP/ICDP Expedition 364 ∗ G.L. Christeson a, , S.P.S. Gulick a,b, J.V. Morgan c, C. Gebhardt d, D.A. Kring e, E. Le Ber f, J. Lofi g, C. Nixon h, M. Poelchau i, A.S.P. Rae c, M. Rebolledo-Vieyra j, U. Riller k, D.R. Schmitt h,1, A. Wittmann l, T.J. Bralower m, E. Chenot n, P. Claeys o, C.S. Cockell p, M.J.L. Coolen q, L. Ferrière r, S. Green s, K. Goto t, H. Jones m, C.M. Lowery a, C. Mellett u, R. Ocampo-Torres v, L. Perez-Cruz w, A.E. Pickersgill x,y, C. Rasmussen z,2, H. Sato aa,3, J. Smit ab, S.M. Tikoo ac, N. Tomioka ad, J. Urrutia-Fucugauchi w, M.T. Whalen ae, L. Xiao af, K.E. Yamaguchi ag,ah a University of Texas Institute for Geophysics, Jackson School of Geosciences, Austin, USA b Department of Geological Sciences, Jackson School of Geosciences, Austin, USA c Department of Earth Science and Engineering, Imperial College, London, UK d Alfred Wegener Institute Helmholtz Centre of Polar and Marine Research, Bremerhaven, Germany e Lunar and Planetary Institute, Houston, USA f Department of Geology, University of Leicester, UK g Géosciences Montpellier, Université de Montpellier, France h Department of Physics, University of Alberta, Canada i Department of Geology, University of Freiburg, Germany j SM 312, Mza 7, Chipre 5, Resid. -
Multiple Fluvial Reworking of Impact Ejecta—A Case Study from the Ries Crater, Southern Germany
Multiple fluvial reworking of impact ejecta--A case study from the Ries crater, southern Germany Item Type Article; text Authors Buchner, E.; Schmieder, M. Citation Buchner, E., & Schmieder, M. (2009). Multiple fluvial reworking of impact ejecta—A case study from the Ries crater, southern Germany. Meteoritics & Planetary Science, 44(7), 1051-1060. DOI 10.1111/j.1945-5100.2009.tb00787.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 06/10/2021 20:56:07 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656594 Meteoritics & Planetary Science 44, Nr 7, 1051–1060 (2009) Abstract available online at http://meteoritics.org Multiple fluvial reworking of impact ejecta—A case study from the Ries crater, southern Germany Elmar BUCHNER* and Martin SCHMIEDER Institut für Planetologie, Universität Stuttgart, 70174 Stuttgart, Germany *Corresponding author. E-mail: [email protected] (Received 21 July 2008; revision accepted 12 May 2009) Abstract–Impact ejecta eroded and transported by gravity flows, tsunamis, or glaciers have been reported from a number of impact structures on Earth. Impact ejecta reworked by fluvial processes, however, are sparsely mentioned in the literature. This suggests that shocked mineral grains and impact glasses are unstable when eroded and transported in a fluvial system. As a case study, we here present a report of impact ejecta affected by multiple fluvial reworking including rounded quartz grains with planar deformation features and diaplectic quartz and feldspar glass in pebbles of fluvial sandstones from the “Monheimer Höhensande” ~10 km east of the Ries crater in southern Germany. -
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. -
Nonlinear Mixed Integer Based Optimization Technique for Space Applications
Nonlinear mixed integer based Optimization Technique for Space Applications by Martin Schlueter A thesis submitted to The University of Birmingham for the degree of Doctor of Philosophy School of Mathematics The University of Birmingham May 2012 University of Birmingham Research Archive e-theses repository This unpublished thesis/dissertation is copyright of the author and/or third parties. The intellectual property rights of the author or third parties in respect of this work are as defined by The Copyright Designs and Patents Act 1988 or as modified by any successor legislation. Any use made of information contained in this thesis/dissertation must be in accordance with that legislation and must be properly acknowledged. Further distribution or reproduction in any format is prohibited without the permission of the copyright holder. Abstract In this thesis a new algorithm for mixed integer nonlinear programming (MINLP) is developed and applied to several real world applications with special focus on space ap- plications. The algorithm is based on two main components, which are an extension of the Ant Colony Optimization metaheuristic and the Oracle Penalty Method for con- straint handling. A sophisticated implementation (named MIDACO) of the algorithm is used to numerically demonstrate the usefulness and performance capabilities of the here developed novel approach on MINLP. An extensive amount of numerical results on both, comprehensive sets of benchmark problems (with up to 100 test instances) and several real world applications, are presented and compared to results obtained by concurrent methods. It can be shown, that the here developed approach is not only fully competi- tive with established MINLP algorithms, but is even able to outperform those regarding global optimization capabilities and cpu runtime performance. -
High Resolution Electron Backscatter Diffraction Mapping of Shock-Deformation in Apatite from the Chicxulub Impact Structure
Large Meteorite Impacts VI 2019 (LPI Contrib. No. 2136) 5041.pdf High Resolution Electron Backscatter Diffraction Mapping of Shock-Deformation in Apatite from the Chicxulub Impact Structure. Morgan A. Cox1,2, Timmons M. Erickson1,3, Martin Schmieder2, and David A. Kring2, 1Space Science and Technology Centre (SSTC), School of Earth and Planetary Science, Curtin University, Perth, WA 6102, Australia. 2Lunar and Planetary Institute (LPI) – USRA, 3600 Bay Area Boulevard, Houston, TX 77058, USA 3Jacobs- JETS, Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, Texas, 77058, USA. (Email: [email protected]) Introduction: The phosphate apatite, 2-36-37.5, 237-2-60-61.5, 273-1-58-59.5, 276-1-85-87, Ca5(PO4)3(F,Cl,OH), is a ubiquitous accessory mineral 285-2-3-5, 299-2-10-12.5, 303-2-71-72.5) consist of found in both terrestrial and extraterrestrial rocks. It is plagioclase, quartz, alkali feldspar, biotite, with minor commonly used to study planetary volatile abundances muscovite, apatite, zircon, titanite, epidote, garnet, and, because it is a U–Pb carrier, to determine the ages ilmenite, and magnetite. The impact melt rock and melt of geologic events (e.g., [1]). The utility of apatite may veins (89-3-13.5-15, 163-3-52.5-54, 206-3-54-56) are be affected by impact cratering processes that produce aphanitic and mainly composed of quartz, feldspar, and shock-deformation microstructures within the phase, calcite along with clasts of bedrock. including planar fractures, partial to whole-scale A total of 560 apatite crystals were identified and recrystallization, and low angle grain boundaries, which imaged using optical microscopy at the LPI. -
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. -
Near-Earth Asteroid 2012 TC4 Observing Campaign Results From
Icarus 326 (2019) 133–150 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Near-Earth asteroid 2012 TC4 observing campaign: Results from a global T planetary defense exercise ⁎ Vishnu Reddya, , Michael S. Kelleyb, Davide Farnocchiac, William H. Ryand, Cristina A. Thomase, Lance A.M. Bennerc, Jessie Dotsonf, Marco Michelig, Melissa J. Bruckera, Schelte J. Bush, Marina Brozovicc, Lorien Wheeleri, Viqar Abbasij, James M. Bauerk, Amber Bonsalll, Zarah L. Browna, Michael W. Buschm, Paul Chodasc, Young-Jun Choin,o, Nicolas Erasmusp, Kelly E. Fastb, John P. Faucherq, Rachel B. Fernandesa, Frank D. Ghigol, David G. Gilbankp, Jon D. Giorginic, Annika Gustafssone, Olivier Hainautr, Walter M. Harrisa, Joseph S. Jaoc, Lindley S. Johnsonb, Theodore Karetaa, Myung-Jin Kimn, Detlef Koschnys, Emily A. Kramerc, Rob R. Landisb, Denis G. Laurinj, Jeffrey A. Larsenq, Clement G. Leec, Cassandra Lejolya, Tim Listert, Robert McMillana, Joseph R. Masieroc, Donovan Mathiasu, Michael Mommertv, Hong-Kyu Moonw, Nicholas A. Moskovitzx, Shantanu P. Naiduc, Ravi Teja Nallapuy, Haris Khan Niaziz, John W. Noonana, David Polishookaa, Eileen V. Ryand, Lauren Schatzab, James V. Scottia, Benjamin Sharkeya, Boris M. Shustovac, Amanda A. Sickafoosep,ad, Marc A. Silvaae, Martin A. Sladec, Lindsay R. Slicka, Lawrence G. Snedekerae, Alessondra Springmanna, David Tholenaf, David E. Trillinge,p, Alberto Q. Vodnizaag, Richard Wainscoataf, Robert Werykaf, Makoto Yoshikawaah a Lunar and Planetary Laboratory, University of Arizona, 1629 E University Blvd, Tucson, AZ 85721, USA b Planetary Defense Coordination Office, Planetary Science Division, NASA Headquarters, 300 E St SW, Washington, DC20546,USA c Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA d Magdalena Ridge Observatory, New Mexico Tech, 801 Leroy Place, Socorro, NM 87801, USA e Dept. -
Comets, Asteroids, and Meteorites
Comets, Asteroids, and Meteorites Clues to the Origin of the Solar System Is Pluto a Planet? Introduction • There is evidence that the small amounts of debris that we observe in our Solar System is a remnant of a previous era of intense bombardment that produced frequent impacts on all of the planets – the Late Heavy Bombardment (~4.1 billion years ago) • Moon and Mercury for example, testify to this episode of intense cratering. • Such bombardment was universal and hammered the Earth as well, later to be disguised by erosion and plate tectonics. • The survivors of this original space debris, still exist today, in the form of asteroids, comets, and meteoroids. The 1908 Tunguska Event • First proposed that the Tunguska event was caused by the collision between the Earth and a small comet. • not a reasonable explanation because an icy comet would have exploded too high in the atmosphere to produce the damage seen from the Tunguska event. • consistent with the Earth colliding with an 80-meter diameter, rocky meteoroid traveling at hypersonic speed, about 79,000 km/h. • Some particles consistent in composition with meteoritic dust were found embedded in tree resin at the impact site. • modeled the impact and found it consistent with the impact of a 70-meter diameter stony meteorite that exploded in the atmosphere. 1969 Chihuahua Mexico Event • In 1969 hundreds of people watched while an intense blue-white light crossed the night sky near Chihuahua, Mexico. • punctuated by an explosion that showered the ground with hundreds of rocks, carbonaceous chondrites, all fragments of what is now known as the Allende meteorite. -
Impactite Stratigraphy and Depositional Processes in the Chicxulub and Ries Impact Structures: What Is a Crater Floor?
EPSC Abstracts Vol. 14, EPSC2020-928, 2020 https://doi.org/10.5194/epsc2020-928 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Impactite stratigraphy and depositional processes in the Chicxulub and Ries impact structures: What is a crater floor? Sean Gulick1,2,3, Gail Christeson1, Naoma McCall1,2, Joanna Morgan, and Jens Ormö 1Institute for Geophysics, University of Texas at Austin, Austin, Texas, United States of America ([email protected]) 2Department of Geological Sciences, University of Texas at Austin, Austin, Texas, United States of America 3Center for Planetary Systems Habitability, University of Texas at Austin, Austin, Texas, United States of America Introduction: Orbital images of impact crater floors show heterogeneity in texture, relief of central structures, peak rings or terrace zones, and presence or absence of blocks. The absence of the 3rd dimension renders challenges in interpreting the thickness of impactites that fill these craters. Whereas texture in orbital images give clues to emplacement process, terrestrial craters benefit from seismic imaging and scientific drilling. The Cretaceous-Paleogene (K-Pg, 66 Ma), 200 km Chicxulub impact crater, México, provides the unique opportunity to study crater formation processes related to a large impact [1]. Chicxulub is a multi-ring basin with an intact melt sheet, peak ring, and crater floor (Fig. 1) [1,2]. It is well preserved due to its youth and burial beneath 100s of meters of Cenozoic carbonates [1,2]. Figure 1. Northwest orientied, time migrated seismic line (Line B), which was depth converted using 3D seismic refraction velocity model, crosses from near the crater center to inner ring faults of Chicxulub impact structure showing features with 3x vertical exaggeration. -
Asteroids and Dinosaurs: Unexpected Twists and an Unfinished Story
1 Asteroids and dinosaurs: Unexpected twists and an unfinished story Plate tectonics might seem like a routine topic from a 7th grade textbook, but in the 1970s, plate tectonics was cutting-edge science. The theory had only gained widespread acceptance over the previous ten years and subsequently attracted scads of scientists looking to open up new intellectual frontiers. Walter Alvarez was one of them, but his research into plate tectonics was destined to be sidelined. An intriguing observation would eventually lead him, his collaborators, and the rest of science on an intellectual journey across geology, chemistry, paleontology, and atmospheric science—to- Fig. 1. At left, Luis and Walter Alvarez stand by the rock layers near Gubbio, Italy, where unusually high traces of wards solving one of the great mysteries in Earth’s his- iridium were found at the Cretaceous-Tertiary boundary. Was tory: What happened to the dinosaurs (Fig. 1)? this evidence that of an ancient supernova or an ancient asteroid impact? And what, if anything did it have to do with This case study highlights these aspects of the nature the dinosaur extinction? of science: • Science can test hypotheses about events that happened long ago. • Scientific ideas are tested with multiple lines of evidence. • Science relies on communication within a diverse scientific community. • The process of science is non-linear, unpredictable, and ongoing. • Science often investigates problems that require collaboration from those in many different disciplines. From plate tectonics to paleontology One of the key pieces of evidence supporting plate tec- tonic theory was the discovery that rocks on the sea- floor record ancient reversals of the Earth’s magnetic field: as rocks are formed where plates are moving away from one another, they record the current direction of the Earth’s magnetic field, which flip-flops irregularly over very long periods of time (Fig. -
THE RECOVERY of LIFE in the CHICXULUB CRATER FOLLOWING the END CRETACEOUS MASS EXTINCTION. C.M. Lowery1 H. Jones2, J. Smit3, T.J
Lunar and Planetary Science XLVIII (2017) 2156.pdf THE RECOVERY OF LIFE IN THE CHICXULUB CRATER FOLLOWING THE END CRETACEOUS MASS EXTINCTION. C.M. Lowery1 H. Jones2, J. Smit3, T.J. Bralower2, and J.D. Owens4 and Expedition 364 Science Party 1University of Texas Institute for Geophysics, 10100 Burnet Rd., Austin, TX 78759, cmlow- [email protected], 2Department of Geosciences, Penn State University, 535 Deike Building, University Park, PA 16802, 3Faculty of Earth and Life Sciences FALW, de Boelelaan 1085, Amsterdam, Netherlands, 1018HV, 4Department of Earth, Ocean, and Atmospheric Sciences and National High Magnet Field Laboratory, Florida State University, Tallahassee, FL 32306. Introduction: The end Cretaceous mass extinc- Results: The earliest Paleocene post-impact section tion, when approximately 75% of all species on earth is relatively expanded at Site M0077 relative to most went extinct, is widely agreed to have been caused by KPg boundary sections. Syn-impact suevite breccia is the bolide impact that formed the Chicxulub Crater on immediately overlain by a dark brown calcareous silt- Mexico’s Yucatan Platform 66 million years ago [1]. stone between 616.58-617.33 meters below seafloor The rapidity of the KPg extinction is unique in geolog- (mbsf). This unit contains a suite of reworked Maas- ic history, with all other mass extinctions driven by trichtian microfossils well known from the KPg bound- processes that operated on the timescale of hundreds of ary in the Gulf of Mexico, termed the KPg Boundary thousands or millions of years like massive volcanism Cocktail [4]. The top of this unit is enriched in Ni and or continental reconfiguration.