Chicxulub Crater - Wikipedia, the Free Encyclopedia
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
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. -
Exceptionally Well-Preserved Fossils in a Middle Ordovician Impact Crater
Downloaded from http://jgs.lyellcollection.org/ by guest on September 29, 2021 Review focus Journal of the Geological Society Published Online First https://doi.org/10.1144/jgs2018-101 The Winneshiek biota: exceptionally well-preserved fossils in a Middle Ordovician impact crater Derek E.G. Briggs1,2*, Huaibao P. Liu3, Robert M. McKay3 & Brian J. Witzke4 1 Department of Geology and Geophysics, Yale University, New Haven, CT 06520, USA 2 Yale Peabody Museum of Natural History, Yale University, New Haven, CT 06520, USA 3 Iowa Geological Survey, IIHR – Hydroscience & Engineering, University of Iowa, 340 Trowbridge Hall, Iowa City, IA 52242, USA 4 Department of Earth and Environmental Sciences, University of Iowa, 115 Trowbridge Hall, Iowa City, IA 52242, USA D.E.G.B., 0000-0003-0649-6417 * Correspondence: [email protected] Abstract: The Winneshiek Shale (Middle Ordovician, Darriwilian) was deposited in a meteorite crater, the Decorah impact structure, in NE Iowa. This crater is 5.6 km in diameter and penetrates Cambrian and Ordovician cratonic strata. It was probably situated close to land in an embayment connected to the epicontinental sea; typical shelly marine taxa are absent. The Konservat-Lagerstätte within the Winneshiek Shale is important because it represents an interval when exceptional preservation is rare. The biota includes the earliest eurypterid, a giant form, as well as a new basal chelicerate and the earliest ceratiocarid phyllocarid. Conodonts, some of giant size, occur as bedding plane assemblages. Bromalites and rarer elements, including a linguloid brachiopod and a probable jawless fish, are also present. Similar fossils occur in the coeval Ames impact structure in Oklahoma, demonstrating that meteorite craters represent a novel and under-recognized setting for Konservat- Lagerstätten. -
Magyar Királyi Földtani Intézet (2006.)
' Copyright Magyar `llami Fldtani IntØzet (Geological Institute of Hungary), 2005 Minden jog fenntartva! All rights reserved! Lektorok Reviewers: BALLA ZOLTÁN, CSÁSZÁRGZA, HAAS JÁNOS, HORVÁTH ISTVÁN, JÁMBOR Á RON, KOVÁCS SÁNDOR, KUBOVICS IMRE, LESS GYRGY, LIEBE PÁL,VICZIÁN ISTVÁN Sorozatszerkesztı Serial editor: BALLA ZOLTÁN Szakszerkesztı Scientific editor: PIROS OLGA Mßszaki szerkesztı Technical editor: SIMONYI DEZS SzÆmtgØpes nyomdai elıkØsztØs DTP: PIROS OLGA, SIMONYI DEZS Bortterv Cover design: SIMONYI DEZS Kiadja a Magyar `llami Fldtani IntØzet Published by the Geological Institute of Hungary Felelıs kiad Responsible editor: KORDOS L`SZL Igazgat Director HU ISSN 03689751 3 Tartalom — Contents Működési jelentés — Activity Report HÁMOR GÉZA (1934–2007) . 7 JÁMBOR ÁRON (összeállító): Dr. Hámor Géza szakirodalmi munkássága . 8 KORDOS LÁSZLÓ: A múlt a jövő kulcsa . 17 BREZSNYÁNSZKY KÁROLY: Igazgatói beszámoló a Magyar Állami Földtani Intézet 2006. évi tevékenységéről . 19 Szakcikkek — Scientific publications RIPSZNÉ JUDIK KATALIN: A Medvednica hegység (Horvátország) és Észak-Magyarország paleozoos és mezozoos kishőmérsékletű metamorf képződményeinek összevetése. — Comparison of Palaeozoic and Mesozoic very low- grade metamorphic formations in the Medvednica Mts (Croatia) and in North Hungary. 47 PELIKÁN PÁL, IVAN FILIPOVIĆ, DIVNA JOVANOVIĆ, MILAN SUDAR, †LJUBINKO PROTIĆ, HIPS KINGA, KOVÁCS SÁNDOR, LESS GYÖRGY: A Bükki-terrénum (É-Magyarország), a Jadari-terrénum (ÉNy-Szerbia) és a Sana-Unai-terrénum (ÉNy-Bosznia) karbon, perm és triász rétegsorainak összehasonlítása. — Correlation of the Carboniferous, Permian and Triassic sequences of the Bükk, Jadar, Sana-Una terrains. 59 BUDAI TAMÁS: Platformok és medencék kialakulása és fejlődése a Bakony középső-triász története során. — Middle Triassic platform and basin evolution of the Bakony Mts, Hungary. 77 HAAS JÁNOS: A bükki és a darnói jura képződmények ősföldrajzi helyzete és kapcsolatai. -
Planetary Surfaces
Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I]. -
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. -
Terrestrial Impact Structures Provide the Only Ground Truth Against Which Computational and Experimental Results Can Be Com Pared
Ann. Rev. Earth Planet. Sci. 1987. 15:245-70 Copyright([;; /987 by Annual Reviews Inc. All rights reserved TERRESTRIAL IMI!ACT STRUCTURES ··- Richard A. F. Grieve Geophysics Division, Geological Survey of Canada, Ottawa, Ontario KIA OY3, Canada INTRODUCTION Impact structures are the dominant landform on planets that have retained portions of their earliest crust. The present surface of the Earth, however, has comparatively few recognized impact structures. This is due to its relative youthfulness and the dynamic nature of the terrestrial geosphere, both of which serve to obscure and remove the impact record. Although not generally viewed as an important terrestrial (as opposed to planetary) geologic process, the role of impact in Earth evolution is now receiving mounting consideration. For example, large-scale impact events may hav~~ been responsible for such phenomena as the formation of the Earth's moon and certain mass extinctions in the biologic record. The importance of the terrestrial impact record is greater than the relatively small number of known structures would indicate. Impact is a highly transient, high-energy event. It is inherently difficult to study through experimentation because of the problem of scale. In addition, sophisticated finite-element code calculations of impact cratering are gen erally limited to relatively early-time phenomena as a result of high com putational costs. Terrestrial impact structures provide the only ground truth against which computational and experimental results can be com pared. These structures provide information on aspects of the third dimen sion, the pre- and postimpact distribution of target lithologies, and the nature of the lithologic and mineralogic changes produced by the passage of a shock wave. -
Impact Cratering
6 Impact cratering The dominant surface features of the Moon are approximately circular depressions, which may be designated by the general term craters … Solution of the origin of the lunar craters is fundamental to the unravel- ing of the history of the Moon and may shed much light on the history of the terrestrial planets as well. E. M. Shoemaker (1962) Impact craters are the dominant landform on the surface of the Moon, Mercury, and many satellites of the giant planets in the outer Solar System. The southern hemisphere of Mars is heavily affected by impact cratering. From a planetary perspective, the rarity or absence of impact craters on a planet’s surface is the exceptional state, one that needs further explanation, such as on the Earth, Io, or Europa. The process of impact cratering has touched every aspect of planetary evolution, from planetary accretion out of dust or planetesimals, to the course of biological evolution. The importance of impact cratering has been recognized only recently. E. M. Shoemaker (1928–1997), a geologist, was one of the irst to recognize the importance of this process and a major contributor to its elucidation. A few older geologists still resist the notion that important changes in the Earth’s structure and history are the consequences of extraterres- trial impact events. The decades of lunar and planetary exploration since 1970 have, how- ever, brought a new perspective into view, one in which it is clear that high-velocity impacts have, at one time or another, affected nearly every atom that is part of our planetary system. -
Cretaceous - Tertiary Mass Extinction Meteoritic Versus Volcanic Causes
GENERAL I ARTICLE Cretaceous - Tertiary Mass Extinction Meteoritic Versus Volcanic Causes P V Sukumaran The bolide impact theory for mass extinctions at the Cretaceous-tertiary (K-T) boundary was a revolutionary concept. This theory was contested by short duration global volcanism as a possible alternative cause for the K-T extinction. Though there is a converging evidence for an extra-terrestrial impact coinciding with the P V Sukumaran took his terminal Cretaceous, the causative link between the M Tech degree in impact and the K-T mass extinction is debatable. Thus, Applied Geology from the while the impact theory is re-emerging, available evidence University of Saugar and has been with the is still insufficient to rule out either of the two hypotheses. Geological Survey of India since 1974. His interests Introduction include geochemistry, petrology and palae oceanography. He is It is now widely believed that life on earth began very early in presently posted to the its geological history, probably about 4000 My (million years) Marine Wing of the ago (Mojzsis and others, 1996). Since then it underwent Department and has participated in many several evolutionary branchings to the complex diversity as scientific cruises both as we see today. Nevertheless, it was not a smooth voyage for life Chief Scientist and as a all along, the evolution was punctuated by geologically participating scientist. ins tan taneous events of mass mortality. New species emerged at the expense of their predecessors following each extinction event and life went on evolving ever more vibrantly. In the geologic record of rock strata, such mass extinction events are identifiable based on sudden absence and reduction in diversity of fossil assemblage across stratigraphic boundaries. -
Color Study of Asteroid Families Within the MOVIS Catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia De León1,2
A&A 617, A72 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832780 & © ESO 2018 Astrophysics Color study of asteroid families within the MOVIS catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia de León1,2 1 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 3 Astronomical Institute of the Romanian Academy, 5 Cu¸titulde Argint, 040557 Bucharest, Romania Received 6 February 2018 / Accepted 13 March 2018 ABSTRACT The aim of this work is to study the compositional diversity of asteroid families based on their near-infrared colors, using the data within the MOVIS catalog. As of 2017, this catalog presents data for 53 436 asteroids observed in at least two near-infrared filters (Y, J, H, or Ks). Among these asteroids, we find information for 6299 belonging to collisional families with both Y J and J Ks colors defined. The work presented here complements the data from SDSS and NEOWISE, and allows a detailed description− of− the overall composition of asteroid families. We derived a near-infrared parameter, the ML∗, that allows us to distinguish between four generic compositions: two different primitive groups (P1 and P2), a rocky population, and basaltic asteroids. We conducted statistical tests comparing the families in the MOVIS catalog with the theoretical distributions derived from our ML∗ in order to classify them according to the above-mentioned groups. We also studied the background populations in order to check how similar they are to their associated families. -
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. -
"Ringing" from an Asteroid Collision Event Which Triggered the Flood?
The Proceedings of the International Conference on Creationism Volume 6 Print Reference: Pages 255-261 Article 23 2008 Is the Moon's Orbit "Ringing" from an Asteroid Collision Event which Triggered the Flood? Ronald G. Samec Bob Jones University Follow this and additional works at: https://digitalcommons.cedarville.edu/icc_proceedings DigitalCommons@Cedarville provides a publication platform for fully open access journals, which means that all articles are available on the Internet to all users immediately upon publication. However, the opinions and sentiments expressed by the authors of articles published in our journals do not necessarily indicate the endorsement or reflect the views of DigitalCommons@Cedarville, the Centennial Library, or Cedarville University and its employees. The authors are solely responsible for the content of their work. Please address questions to [email protected]. Browse the contents of this volume of The Proceedings of the International Conference on Creationism. Recommended Citation Samec, Ronald G. (2008) "Is the Moon's Orbit "Ringing" from an Asteroid Collision Event which Triggered the Flood?," The Proceedings of the International Conference on Creationism: Vol. 6 , Article 23. Available at: https://digitalcommons.cedarville.edu/icc_proceedings/vol6/iss1/23 In A. A. Snelling (Ed.) (2008). Proceedings of the Sixth International Conference on Creationism (pp. 255–261). Pittsburgh, PA: Creation Science Fellowship and Dallas, TX: Institute for Creation Research. Is the Moon’s Orbit “Ringing” from an Asteroid Collision Event which Triggered the Flood? Ronald G. Samec, Ph. D., M. A., B. A., Physics Department, Bob Jones University, Greenville, SC 29614 Abstract We use ordinary Newtonian orbital mechanics to explore the possibility that near side lunar maria are giant impact basins left over from a catastrophic impact event that caused the present orbital configuration of the moon.