DOCSLIB.ORG

Ablation, 259, 260 Acid Rains, 217 Acoustic Gravity Waves, 148, 218

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Ablation, 259, 260 Acid Rains, 217 Acoustic Gravity Waves, 148, 218 INDEX Ablation, 259, 260 fluctuation, 348 Acid rains, 217 temperature, 348, 349 Acoustic gravity waves, 148, 218, 236 Atmospheric darkening, 207 Acoustic signals, 149 Atmospheric winds, 239 Acoustic system, 148 Auroral phenomena, 238 Active Geophysical Rocket Experiments, 328 Australasian strewn field, 272 Advective motion, 341 Australian-Asian tektites, 268 Aerial shock waves, 229 Australites, 267 Aerodynamic forces, 10 Air-blast, 16 Baikonur cosmodrome, 238 Alfven velocity, 314, 322 Ballistic motion, 270 Aluminium jet, 328 Barents Sea, 293 Alvarez, Luis, 1 Barium vapor streams, 325 ANEOS equation of state, 62, 269, 293 10Be, 271, 272 Angara River, 232 Benesov bolide, 135 Annealing of meteorite samples, 340 Bishop’s rings, 234 Annealing of minerals, 245 Block structure, 33 Anomalies of elements and isotopes Bodaibo, 232 in peat, 242 Bohemia, 273 Anomalous atmospheric phenomena, 235, 236 Bolides, 131 Antipodal point, 216, 217, 219 Bottom relief, 41 Apollo lunar samples, 268 Brazil, 228 Apparent strength, 145 Breakup, 9 Arago neutral polarization points, 234 Brightness, 233 Archean, 175, 187 Bronze Age, 228 Artificial air cloud, 328, 329 Buried explosions, 31, 56 Asteroidal hypothesis, 259 Butterfly-shaped tree fall pattern, 240 Asteroids, 120 2002 EM7, 5 99942 Apophis, 5 Carbon, 208 Eros, 61 Carbonaceous chondrites, 242, 243 Gaspra, 92 Carbonates terrestrial, 340, 346 Hermes, 5 Carbon isotopes 13C, 14C, 243 Ida, 92 Casualties, 19, 23 Itokawa, 57, 92 Cenomanian-Turonian boundary, 208 Mathilde, 7, 61, 92, 244 Central European tektite strewn field, 271 Toutatis, 5 Charcoal, 207 Atmosphere, 9 Chemical energy of explosives, 327, 328 composition, 348 Chemical plants, 52 density, 9 Chronology 351 352 Index lunar impact craters, 93 Deuterium, 243 terrestrial impact craters, 109 Devastation area, 18, 229 Clinopyroxenites, 279 Diamagnetic cavern, 329 Clouds, 23, 46 Diamagnetic cavity, 329 CO2,46 Differentiation, 340 Coastal areas, 39, 40 primary, 340, 348 Collapse Dinosaurs, 1, 72, 313 transient cavity, 106, 173, 174, 178, 179, Disruptive collisions, 124 181, 185, 190 Distal ejecta, 267, 297 underwater bench, 185 Don Quijote mission, 66 Colorful sunsets, 234 Double craters, 7 Comet(s), 117 Drag coefficient, 138, 247 Borelly, 61, 244 Dunite, 281 C/2000 A2, 8 Dust, 45 Encke, 126 Dust spreading, 235 Halley, 60 Dusty mantle, 119, 124 Jaccobini-Zinner, 60 Dynamic mass, 139 Shoemaker-Levy 9, 68, 236 Tempel 1, 61 Early Earth, 333, 346 Wild-2, 61 Early Mars, 347, 348 Comet albedos, 120 Early upper geospheres, 334 Cometary bodies, 118, 340 Earth’s material, 339, 347 accumulation, 336, 342, 348 Cometary hypothesis, 258 “tail”, 348 Comet fading time, 119 atmosphere, 333, 344 Comet nuclei, 118, 120 inert gases, 345 Comet population, 119 modern, 346 Concrete dams, 54 primitive, 339, 340, 347 Cosmic rays, 124, 281, 320 mass, 349 Criosphere, 346 pressure, 349 early, 347, 348 core, 333, 339, 341, 345 Critical ionization velocities, 330 crust Crown fires, 210 evolution, 333 CSS (Catalina Sky Survey), 2 formation, 333, 336, 340 Cumulative distribution of fragments, 270 growth, 333, 335, 341, 342, 348 Cumulative explosive devices, 325 early stage, 333, 334, 335, Cumulative number of impacts, 154 336, 348 Czech Republic, 274 final stage, 333, 343, 348 main stage, 335 rate, 334, 334 Daily solar currents, 237 time, 334, 335 Dangerous objects, 3, 19, 52, 54 primitive, 333, 339, 340, 342, 344, 347 Darwin, Charles, 267 hydrosphere Debris, 124, 126 modern, 346 Deceleration, 9, 13 primitive, 333, 339, 340, 344 Deep Impact Mission, 61, 64, 65 magnetic field, 314, 328 Deep water, 34, 37 mantle, 333, 339, 340, 341, 345 Deflection, 55 mass, 336, 337 Deformation, 11 mean density, 334, 335 Degassing, 340 Earthquake(s), 29, 34, 39, 40 Desert Network, 131 Earthquake magnitude(s), 29, 74 Deserts, 49 Ejecta, 25, 44, 59, 164, 172, 176, 180, 183, Destruction of dams, 54 191, 268 Index 353 Ejecta blanket, 26, 298 Fragmentation, 41, 58, 59, 134 Ejecta curtain, 41, 303 Fragment–vapor cloud, 135 Ejecta motion, 269 Ejecta return, 216 Galileo spacecraft, 70 Ejection, 346 Gas hydrates, 345, 346, 347 efficiency, 347 in the early earth, 346 of impact material, 340, 347 layers, 347, 348 to geocentric orbits, 339 Geo-chronometer, 333 Electromagnetic impulse, 66 Hf-W, 336, 348 Energy U-Pb, 348 balance, 340 Geomagnetic cavern, 322 equipartition, 337 Geomagnetic effect, 237 flux, 342 Geomagnetic field, 68 gravitational, 340 Geophysical experiments, 325 differentiation, 341 Ghana, 274 of impact, 340, 342, 343 Global fire, 207, 215, 223 kinetic, 334 Grady-Kipp distribution, 278 potential, 342 Gravity-dominated regime, 62, 63 of random motion, 335 Grazing impact, 213 of short-living isotopes, 340 Greenland bolide, 151 sources, 341 Ground telescopes, 70, 229 Energy–frequency distribution, 156 Ground water, 210 Eocene-Oligocene boundary, 208 Growing planet (Earth), 333, 334, 335, 336, Epicenter zone, 230 337, 338, 339, 342, 343 Erosion, 166, 292, 304 root-mean-square velocity, 337 ESA, 61, 66 Gullies, 292, 304 Escape, 216, 283, 313 Gyro radius of ions, 330 Europe, 55, 236 Explosive type generators, 325 Eyewitness reports, 212, 230 Hadean, 334, 340 Halley-type comets, 117, 122 Hayabusa mission, 57 F layer of the ionosphere, 320 2 Hazard mitigation, 21 Fading of comets, 119 Heat transfer coefficient, 212 Fading rate, 119 High-velocity jets, 325 Falling bodies, 336, 337, 343 Hiroshima, 19, 23 composition, 348 Hubble Space Telescope, 70 flow, 342, 346 Hydrodynamic instabilities, 255 frequency, 333, 338, 342, 348 Hydroelectric dams, 52 masses, 335 mass spectrum, 333, 348 velocity spectrum, 333, 348 Icy bodies, 17, 35, 233, 316 Feeding zone, 334, 335, 336, 337, 342 Ignition, 22, 23, 25, 210, 215 expanding, 335 Impact crater(s) Ferromagnetic material, 245 accumulation rate, 109, 165 Final crater, 26 formation, 35 Fire(s), 22 mode of formation Fireball, 16, 23, 210 strength/gravity, 105, 106, 110 Fire propagation, 211 morphology Flares, 154 simple/complex, 105, 106, 168 Flattened trees, 210 lunar Fluxus experiments, 328 Orientale basin, 107 Focused solar light, 56 terrestrial 354 Index Arkenu, 50 Ivory Coast strewn fields, 271 Barringer Meteorite Crater, 229 Ivory Coast tektites, 271, 275 Bosumtwi, 271, 275 Chesapeake Bay impact structure, 271 Chicxulub, 180, 208, 217 Jena, 237 Elgygytgyn, 27, 283 Jet engine, 56 Eltanin impact structure, 293, 304, 307 Jiotto spaceship, 60 Henbury, 229 Jovian moons, 122 Kaali, 10 Jupiter, 68 Kamensk, 292, 304 Jupiter-family comets, 117 Kara, 27 Lockne, 292, 293, 299 K/T (Cretaceous/Tertiary) boundary, 44, 45, 207, Macha crater group, 229 208, 223 Mjølnir, 293 K/T event, 25 Popigai, 27, 175 Kamenskoe, 232 Puchezh-Katunki, 172 Kelvin-Helmholtz instabilities, 11, 14, 73 Ries, 27, 271, 272 Kezhma, 232 Steinheim, 273 Kinetic energy of a jet, 328 Sterlitamak, 164 Kinetic weapon, 56 Sudbury, 193 Krakatau, 218 Ust-Kara, 27 Kuiper belt, 118 Vredefort, 187 Kulik, Leonid, 212 Wabar, 51 Venusian Mead, 165 Laboratory modeling experiments, 239 Sascia, 172 Lake Bosumtwi, 274 Impact frequency, 103, 111, Lamb wave, 218, 219 166, 169 Landing speed, 57 Impact glasses, 271 Large craters, 27 Impact melt, 177, 181, 183, Laser, 56 190, 194 Late heavy bombardment, 93, 95 Impact probability, 99, 102, 103 Lateral velocity, 137 Impact rate, 93, 102 Layers Impacts into water, 39 mixing, 334, 342 Impacts of large bodies, 348 average thickness, 344 Impact velocity, 102–104 near-surface, 334, 347 Indochina, 271 Lena River, 232 Infrasound waves, 148 Libyan desert glass, 50 Injuries, 24 Lifetimes of minor bodies, 127 Innisfree meteorite, 132 Lifetimes of small comets, 126 Integral luminous efficiency, 140 Light curves, 133 Internal waves, 222 Light flashes, 151 International agreements, 56 Lightning, 210, 222, 230 International laws, 60 Light phenomena, 231 Ionization equilibrium, 322 Light twilights, 234 Ionization potential, 322 LINEAR (Lincoln Laboratory’s Near-Earth Ionosphere, 67, 238, 314 Asteroid Research), 2 Ionospheric current system, 238 Lithosphere, 34, 187 Ionospheric disturbances, 315 LONEOS (Lowell Near-Earth Objects Survey), 2 Ionospheric effects, 315 Long-period comets, 117, 122, 127 Iridium, 207, 242 Lost City meteorite, 132 Irkutsk, 237 Luminous efficiency, 137 Isothermal atmosphere, 218 Lunar crust, 283 Index 355 Lunar meteorites, 267, 283 diamonds, 177 Lusatia, 273 gold, 193 oil, 185 Modeling of the Tunguska event, 249 Mach number, 47 Moho boundary, 28, 33 Magnetic diffusion, 328 Moldavites, 273 Magnetic disturbances, 314, 322 Moon, 229, 268, 283 Magnetic field, 322 Moravia, 273 Magnetic field variations, 238 Morávka meteorite, 132 Magnetic storm, 315 Morphologic anomalies, 246 Magnetic susceptibility, 245 Morphometric anomalies, 246 Magnetodynamic disturbances, 238 Mortality, 18, 19 Magnetohydrodynamic waves, 68, 328 Multiphase hydrodynamics, 269 Magnetosphere, 67, 238, 314 Muong Nong tektites, 271 Malyshevka, 232 Mutative changes, 246 Manhattan Project, 56 Mantle, 123 Nagasaki, 18, 19, 23 Mars, 49, 269, 278, 283 NASA, 1, 60, 61 Martian atmosphere, 277 NEAR (Near Earth Asteroid Rendezvous), 61 Martian meteorites, 268, 280 Near-Earth Asteroids, 110, 112 Mass accumulation, 335 Near-Earth Objects, 4, 272 Mass extinctions, 180, 207, 208, NEAT(Near-Earth Asteroid Tracking), 2 218, 312 Neutron, 55 Matter in the feeding zone, 335 Nitrogen isotope, 244 condensed, 335 Nizhnyaya Tunguska River, 232 density, 334 Noctilucent clouds, 235, 236 surface density, 335, 336 Nonuniform atmosphere, 20 Mesosphere, 44 North American strewn field, 271 Meteorite Committee, 241 North Star Active Plasma
Load more

Recommended publications
  • Show Your Parents
    Show your parents Saxby and William Pridmore Show your parents is a series of short chapters aimed at helping children (under 12 years) master a little general knowledge and science. Some of this material may need input from an adult – some words and ideas may be a bit difficult. But, the need for a bit of adult/parent input is not a bad thing – such interaction between the generations may be helpful to both. See what you think. It is a not-for-profit endeavour. Editorial Board Rachel & Amelia Allan, Eve Porter, Layla Tanner, Dempsey & Isaac O’Neil, and Julia & Claude Glaetzer Dedicated to Helen Stephen [pictured] [William’s pre-school teacher; many thanks to Sarah Stephen for the photograph] Contents 1. Start here… 2. Here, pussy, pussy… 3. Bones 4. Space opportunity 5. Rainbows 6. Where is New Zealand? 7. The narwhal 8. Kangaroos, what they do… 9. Planets and volcanos 10. Optical illusions 11. First and surprising 12. The marsupials 13. Tree rings and things 14. Flowers and honey 15. Evolution and waterfalls 16. Catalogue 17. Magnets and unrelated 18. Cakes first 19. Take a breath 20. Dolphins and 21. Getting around 22. Geography special 23. Speak up 24. Going around 25. Dragon’s blood 26. Larry 27. More atoms 28. Flags 29. Moscow 30. Some carbon 31. More carbon 32. Photosynthesis 33. Pisa 34. Toes and energy 35. Water and energy 36. Craters 37. Animals, mainly 38. Old rocks Show your parents Chapter 1. [‘Show your parents’ is a series of short chapters aimed at helping children (with input from their parents) learn some stuff.
    [Show full text]
  • The Origin of the Circular K Anomalies at the Bosumtwi Impact Structure
    Large Meteorite Impacts VI 2019 (LPI Contrib. No. 2136) 5008.pdf THE ORIGIN OF THE CIRCULAR K ANOMALIES AT THE BOSUMTWI IMPACT STRUCTURE. C.A.B. Niang1,2,3, D. Baratoux3, D.P. Diallo1, R. Braucher4, P. Rochette4, C. Koeberl5, M.W. Jessell6, W.U. Reimold7, D. Boamah8, G. Faye9, M.S. Sapah10, O. Vanderhaeghe3, S. Bouley11. 1Département de Géologie, Université Cheikh Anta Diop, Dakar, Senegal, [email protected], 2Institut Fon- damental d’Afrique Noire Cheikh Anta Diop, Dakar, Senegal. 3Géosciences Environnement Toulouse, University of Toulouse, CNRS & IRD, 14, Avenue Edouard Belin, 31400, Toulouse, France. 4Centre Européen de Recherche et d’Enseignement des Géosciences et de l’Environnement, Aix-Marseille Université, CNRS, IRD, CEREGE UM34, Aix en Provence, France, 5Department of Lithospheric Research, University of Vienna, 1090 Vienna, Austria, and Natural History Museum 1010 Vienna, Austria. 6Centre for Exploration Targeting, The University of Western Aus- tralia, 35 Stirling Highway, Crawley, WA 6009, Australia. 7Institute of Geosciences, Laboratory of Geodynamics, Geochronology and Environmental Science, University of Brasília, Brasília, Brazil. 8Geological Survey Department, Accra, Ghana. 9Institut des Sciences de la Terre, Université Cheikh Anta Diop de Dakar, Sénégal.10Department of Earth Science, University of Ghana, Accra, Ghana. 11GEOPS - Géosciences Paris Sud, Univ. Paris-Sud, CNRS, Université Paris-Saclay, Rue du Belvédère, Bât. 504-509, 91405 Orsay, France Introduction: Radiometric data are commonly to weathering, erosional and transport processes. Sev- used for geological mapping in mineral exploration, eral samples were also taken at surface and combined particularly in tropical regions where outcrop condi- with samples from shallow boreholes used for cosmo- tions are poor.
    [Show full text]
  • The Eltanin Impact and Its Tsunami Along the Coast of South America: Insights for Potential Deposits
    Earth and Planetary Science Letters 409 (2015) 175–181 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl The Eltanin impact and its tsunami along the coast of South America: Insights for potential deposits Robert Weiss a, Patrick Lynett b, Kai Wünnemann c a Department of Geosciences, Virginia Tech, VA 24061, USA b Sonny Astani Department of Civil and Environmental Engineering, University of Southern California, Los Angeles, CA 90089-2531, USA c Museum für Naturkunde, Leibniz Institute for Evolution and Biodiversity Science, Invalidenstrasse 43, 10115 Berlin, Germany a r t i c l e i n f o a b s t r a c t Article history: The Eltanin impact occurred 2.15 million years ago in the Bellinghausen Sea in the southern Pacific. Received 21 June 2014 While a crater was not formed, evidence was left behind at the impact site to prove the impact origin. Received in revised form 10 October 2014 Previous studies suggest that a large tsunami formed, and sedimentary successions along the coast of Accepted 19 October 2014 South America have been attributed to the Eltanin impact tsunami. They are characterized by large clasts, Available online xxxx often several meters in diameter. Our state-of-the-art numerical modeling of the impact process and its Editor: J. Lynch-Stieglitz coupling with non-linear wave simulations allows for quantifying the initial wave characteristic and the Keywords: propagation of tsunami-like waves over large distances. We find that the tsunami attenuates quickly with −1.2 Eltanin impact η(r) ∝ r resulting in maximum wave heights similar to those observed during the 2004 Sumatra tsunamis and 2011 Tohoku-oki tsunamis.
    [Show full text]
  • The 3D.Y Knom Example Is /1"<
    t Sixth International Congress on Glass - Washington, D. C., 1962. Fossil Glasses Produced by Inpact of Meteorites, Asteroids 2nd Possibly Comets with the Planet Xarth* A. J. Zzhen :&uon Insticute, Pittsburgh, ?ennsylvania (U. S. A. ) Sunnary / (to be trmslzted izto Frerzh and German) - i in recent thes one of the nost intriging aysteries of geGlogy has ceen the occurrence of aerodgnasicdly-shaped glasses on five continents of the earth. Tnese glasses mder discussion are obviously not of f-d- guritic origin. 3ecent research indicates that these glasses laom as tektites are the result of meteorite, esteroid, or sossibly comet hpact. Lqact glass?s, io generzl, differ Tram volcanic glasses in that they are lo;;.tr in ?,iater zontent, have laver gallium and germiun ccntents, and are rot necessarily ia mgnaticalljr unstable continental areas. These hpac- tites may be divided as follovs: (1)Glasses found in or near terrestrial neteorite craters. These glasses usually contain numerous s-,'nerules 02 nickel-iron, coesite, chunlks of partially melted meteoritic inatter and even stishovite. Shattered or fractured melted mi-nerals such as quarts are comxonly gresent. Aerodpaaic-shaping nay or nay not be present in this t-ne. &m?les are Canyon Diablo and Wabar Crster glasses. (2) Impzct- glasses zssociated with craters uitn no evidence of meteoritic mterial i? the @.ass or surrounding the explosisn site. The 3d.y knom example is /1"< Tnis vork vas supported by Xatiocal A-eroEautizs and Space P.dministretioq,$ 3esezrch Grant NsG-37-6O Supplement 1-62. Page 2 glass associated with AoueUoul Crater in the Western Sahara Desert.
    [Show full text]
  • Early Fracturing and Impact Residue Emplacement: Can Modelling Help to Predict Their Location in Major Craters?
    Early fracturing and impact residue emplacement: Can modelling help to predict their location in major craters? Item Type Proceedings; text Authors Kearsley, A.; Graham, G.; McDonnell, T.; Bland, P.; Hough, R.; Helps, P. Citation Kearsley, A., Graham, G., McDonnell, T., Bland, P., Hough, R., & Helps, P. (2004). Early fracturing and impact residue emplacement: Can modelling help to predict their location in major craters?. Meteoritics & Planetary Science, 39(2), 247-265. DOI 10.1111/j.1945-5100.2004.tb00339.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 23/09/2021 21:19:20 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/655802 Meteoritics & Planetary Science 39, Nr 2, 247–265 (2004) Abstract available online at http://meteoritics.org Early fracturing and impact residue emplacement: Can modelling help to predict their location in major craters? Anton KEARSLEY,1* Giles GRAHAM,2 Tony McDONNELL,3 Phil BLAND,4 Rob HOUGH,5 and Paul HELPS6 1Department of Mineralogy, The Natural History Museum, Cromwell Road, London SW7 5BD, UK 2Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, California, USA 3Planetary and Space Sciences Research Institute, The Open University, Milton Keynes, MK7 6AA, UK 4Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK 5Museum of Western Australia, Francis Street, Perth, Western Australia 6000, Australia 6School of Earth Sciences and Geography, Kingston University, Kingston-upon-Thames, Surrey, KT1 2EE, UK *Corresponding author. E-mail: [email protected] (Received 30 June 2003; revision accepted 15 December 2003) Abstract–Understanding the nature and composition of larger extraterrestrial bodies that may collide with the Earth is important.
    [Show full text]
  • 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.
    [Show full text]
  • Porosity of Meteorite Impact Rocks: Inferences from Geophysical and Petrophysical Studies from the Lake Bosumtwi Impact Crater, Ghana
    Porosity of Meteorite Impact Rocks: Inferences from Geophysical and Petrophysical Studies from the Lake Bosumtwi Impact Crater, Ghana Damien Meillieux* University of Alberta, Edmonton, Alberta, Canada [email protected] Douglas Schmitt, Meghan Brown, Marek Welz and Tiewei He University of Alberta, Edmonton, Alberta, Canada Bernd Milkereit University of Toronto, Toronto, Ontario, Canada Tobias Karp and Christopher Scholz University of Syracuse, Syracuse, New York, United States and Sylvester Danour Kwame Nkrumah University of Science and Technology, Kumasi, Ghana Abstract Introduction Impact structures have been targets in petroleum exploration primarily due to the structural traps that are created during formation and evolution of the crater basin and rim. Not much is known, however, about the porosity introduced to the rock mass as a result of the high strain rates induced during the impact event itself. This porosity, however, can be of crucial importance both in terms of the storativity and the permeabilty of the remaining rock mass. The Lake Bosumtwi (Ghana) impact crater is a young (~1.1 Ma) structure approximately 10-km in diameter which today remains much intact. Field surface geological investigations of the crater structure are restricted by both Lake Bosumtwi and the thick layer of soft sediments that have accumulated in it since the crater’s formation. Consequently, geophysical methods have played a major role in delineating the structure of the crater. Marine reflection seismic investigations, in particular, showed the existence of a prominent central uplift surrounded by a circular depression [1]. The current study was carried out in 2004 as part of the Lake Bosumtwi Drilling project, under the auspices of the International Continental Drilling Program (ICDP), with two deeper wells drilled into the basin and the central uplift.
    [Show full text]
  • ANIC IMPACTS: MS and IRONMENTAL P ONS Abstracts Edited by Rainer Gersonde and Alexander Deutsch
    ANIC IMPACTS: MS AND IRONMENTAL P ONS APRIL 15 - APRIL 17, 1999 Alfred Wegener Institute for Polar and Marine Research Bremerhaven, Germany Abstracts Edited by Rainer Gersonde and Alexander Deutsch Ber. Polarforsch. 343 (1999) ISSN 01 76 - 5027 Preface .......3 Acknowledgements .......6 Program ....... 7 Abstracts P. Agrinier, A. Deutsch, U. Schäre and I. Martinez: On the kinetics of reaction of CO, with hot Ca0 during impact events: An experimental study. .11 L. Ainsaar and M. Semidor: Long-term effect of the Kärdl impact crater (Hiiumaa, Estonia) On the middle Ordovician carbonate sedimentation. ......13 N. Artemieva and V.Shuvalov: Shock zones on the ocean floor - Numerical simulations. ......16 H. Bahlburg and P. Claeys: Tsunami deposit or not: The problem of interpreting the siliciclastic K/T sections in northeastern Mexico. ......19 R. Coccioni, D. Basso, H. Brinkhuis, S. Galeotti, S. Gardin, S. Monechi, E. Morettini, M. Renard, S. Spezzaferri, and M. van der Hoeven: Environmental perturbation following a late Eocene impact event: Evidence from the Massignano Section, Italy. ......21 I von Dalwigk and J. Ormö Formation of resurge gullies at impacts at sea: the Lockne crater, Sweden. ......24 J. Ebbing, P. Janle, J, Koulouris and B. Milkereit: Palaeotopography of the Chicxulub impact crater and implications for oceanic craters. .25 V. Feldman and S.Kotelnikov: The methods of shock pressure estimation in impacted rocks. ......28 J.-A. Flores, F. J. Sierro and R. Gersonde: Calcareous plankton stratigraphies from the "Eltanin" asteroid impact area: Strategies for geological and paleoceanographic reconstruction. ......29 M.V.Gerasimov, Y. P. Dikov, 0 . I. Yakovlev and F.Wlotzka: Experimental investigation of the role of water in the impact vaporization chemistry.
    [Show full text]
  • Bosumtwi Crater, Ghana
    Detailed structural analysis of the rim of a large, complex impact crater: Bosumtwi Crater, Ghana Wolf U. Reimold Dion Brandt Department of Geology, University of the Witwatersrand, Private Bag 3, P.O. Wits 2050, Johannesburg, South Africa Christian Koeberl Institute of Geochemistry, University of Vienna, Althanstr. 14, A-1090 Vienna, Austria ABSTRACT The 1 Ma Bosumtwi Crater in Ghana is an 11-km-diameter, presumably complex, well- preserved impact structure that is associated with the Ivory Coast tektite strewnfield. Detailed structural geologic studies along a complete traverse through the northwestern rim section indi- cated four zones characterized by distinct deformation styles from just outside of the crater rim to near the crater floor. Zone 1 is dominated by thick deposits of lithic impact breccia, intercalated in places with products of local mass wasting. Zone 2 contains inward-dipping thrust planes, conjugate radial fractures, isoclinal folding, and overturned stratigraphic sequences. Zone 3 represents a megabreccia zone, in which block size decreases upward and outward toward the rim crest. The innermost zone 4 is dominated by intense thrust faulting of multiple orientations, resulting in complex duplex- and lens-shaped bodies. These deformation styles generally corre- spond to those previously reported from the rims of simple bowl-shaped meteorite-impact craters and appear to be characteristic of impact structures in general. INTRODUCTION Bedrock and impact formations outside of the southern rim sectors. A variety of granitoid intru- The geologic structure and macrodeformation crater are only accessible along road cuts and in sions (mainly biotite or amphibole granites) was associated with some small (<2 km), well- stream beds.
    [Show full text]
  • The Subsurface Structure of Oblique Impact Craters
    The subsurface structure of oblique impact craters Dissertation vorgelegt von Dipl.-Geol. Michael H. Poelchau vom Fachbereich Geowissenschaften der Freien Universität Berlin zur Erlangung des akademischen Grades doctor rerum naturalium (Dr. rer. nat.) Berlin, 2010 The subsurface structure of oblique impact craters Dissertation vorgelegt von Dipl.-Geol. Michael H. Poelchau vom Fachbereich Geowissenschaften der Freien Universität Berlin zur Erlangung des akademischen Grades doctor rerum naturalium (Dr. rer. nat.) Berlin, 2010 Gutachter: 1. PD Dr. Thomas Kenkmann 2. Prof. Wolf-Uwe Reimold Tag der Disputation: 23.02.2010 Statement regarding the contributions of the author and others to this thesis This thesis is comprised of three published, peer-reviewed articles and one submitted manuscript, which each form separate chapters within this thesis. The chapters “Introduction” and “General Conclusions” were written especially for this thesis. The PhD candidate is the first author of two of these articles, and the second author of the third article. The PhD candidate is also the first author of a manuscript currently submitted to Earth and Planetary Science Letters. Therefore, these four chapters have their own introduction, methodology, discussion, conclusions and references. The articles and manuscripts used in this thesis are the following: Poelchau, M. H., and T. Kenkmann, 2008. Asymmetric signatures in simple craters as an indicator for an oblique impact direction, Meteoritcal and Planetary Science, 43, 2059-2072. Poelchau M. H., Kenkmann T. and Kring D. A., 2009. Rim uplift and crater shape in Meteor Crater: the effects of target heterogeneities and trajectory obliquity. Journal of Geophysical Research, 114, E01006, doi:10.1029/2008JE003235. Kenkmann, T.
    [Show full text]
  • Impact Melt Rocks in the "Cretaceous
    Large Meteorite Impacts (2003) alpha_t-z.pdf Contents — T through Z Locations and Compositions of Mare Ponds in South Pole-Aitken Basin on the Moon and Its Implication to the Impact Tectonics T. Takata and S. Hori ............................................................................................................................. 4058 New Laboratory Results on Field Sections at the Impact Crater of Araguainha (MT, GO, Brazil). Area of Proximal and Distal Impact Ejecta, Including Microspherules Dated from the End of Permian J. M. Théry, A. Crosta, E. Veto Akos, E. Bilal, K. Gal-Solymos, and E. Dransart................................. 4096 Techniques of Shock Wave Experiments and Determination of Hugoniot Data of Solids K. Thoma................................................................................................................................................ 4134 Differential Stress-controlled Deformation of Quartz During and After Hypervelocity Impact — Microstructural Evidence from the Charlevoix Impact Structure, Quebéc, Canada C. A. Trepmann and J. G. Spray............................................................................................................. 4026 Mjølnir Marine Crater Resulting from Oblique Impact: Compelling Evidence F. Tsikalas and J. I. Faleide................................................................................................................... 4005 A New Mid- to Late-Maastrichtian Impact in the Raton Basin 100m Below the K/T Boundary P. Turner, S. C. Sherlock, P. Clarke, and
    [Show full text]
  • Of the Eltanin Asteroid in Rise Peninsula, Site 1096'
    Barker, P.F., Camerlenghi, A., Acton, G.D., and Ramsay, A.T.S. (Eds.) Proceedings of the Ocean Drilling Program, Scientific Results Volume 178 9. DATAREPORT: A SEARCH FOR DEPOSITS OF THE LATE PLIOCENE IMPACT OF THE ELTANIN ASTEROIDIN RISE SEDIMENTS FROM THE ANTARCTIC PENINSULA,SITE 1096' Frank T. Kyte2 ABSTRACT Concentrations of Ir have been measured in 87 sediment samples from Ocean Drilling Program Site 1096 in search of evidence of fallout from the impact of the Eltanin asteroid, which occurred at 2.15 Ma, -1300 km northwest of the site. An additional six samples were mea- Kyte, F.T., 2001. Data report: A search sured from a unique sand layer and adjacent sediments that are dated at for deposits of the late Pliocene impact -1.6 Ma. These 93 sediment samples are all silts and muds that were de- of the Eltanin asteroid in rise posited on a continental rise drift of the Antarctic Peninsula. No evi- sediments from the Antarctic dence of the Eltanin impact deposit was found in this study. Peninsula, Site 1096. In Barker, P.F., Camerlenghi, A., Acton, G.D., and Ramsay, A.T.S. (Eds.), Proc. OD8 Sci. Results, 178, 1-6 [Online]. Available INTRODUCTION from World Wide Web: <http://www- odp.tamu.edu/publications/l78-SR/ One objective of the Ocean Drilling Program (ODP) Leg 178 expedi- VOLUME/CHAM'ERS/SRl78-09.PDF>. tion was to search for sediment deposits related to the late Pliocene im- [Cited YYYY-MM-DD] pact of the Eltanin asteroid. This is a unique deposit in the known ZCenter for Astrobiology, Institute of Geophysics and Planetary Physics, sedimentary record.
    [Show full text]