Goat Paddock, Western Australia: an Impact Crater Near the Simple – Complex Transition
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3-D Seismic Characterization of a Cryptoexplosion Structure
Cryptoexplosion structure 3-D seismic characterization of a eryptoexplosion structure J. Helen Isaac and Robert R. Stewart ABSTRACT Three-quarters of a circular structure is observed on three-dimensional (3-D) seismic data from James River, Alberta. The structure has an outer diameter of 4.8 km and a raised central uplift surrounded by a rim synform. The central uplift has a diameter of 2.4 km and its crest appears to be uplifted about 400 m above regional levels. The structure is at a depth of about 4500 m. This is below the zone of economic interest and the feature has not been penetrated by any wells. The disturbed sediments are interpreted to be Cambrian. We infer that the structure was formed in Late Cambrian to Middle Devonian time and suffered erosion before the deposition of the overlying Middle Devonian carbonates. Rim faults, probably caused by slumping of material into the depression, are observed on the outside limb of the synform. Reverse faults are evident underneath the feature and the central uplift appears to have coherent internal reflections. The amount of uplift decreases with increasing depth in the section. The entire feature is interpreted to be a cryptoexplosion structure, possibly caused by a meteorite impact. INTRODUCTION Several enigmatic circular structures, of different sizes and ages, have been observed on seismic data from the Western Canadian sedimentary basin (WCSB) (e.g., Sawatzky, 1976; Isaac and Stewart, 1993) and other parts of Canada (Scott and Hajnal, 1988; Jansa et al., 1989). The structures present startling interruptions in otherwise planar seismic features. -
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. -
Hydrothermal Alteration at the Lonar Lake Impact Structure, India: Implications for Impact Cratering on Mars
Meteoritics & Planetary Science 38, Nr 3, 365–381 (2003) Abstract available online at http://meteoritics.org Hydrothermal alteration at the Lonar Lake impact structure, India: Implications for impact cratering on Mars Justin J. HAGERTY* and Horton E. NEWSOM Institute of Meteoritics, Department of Earth & Planetary Sciences, University of New Mexico, Albuquerque, New Mexico 87131, USA *Corresponding author. E-mail: [email protected] (Received 12 June 2002; revision accepted 20 February 2003) Abstract–The 50,000 year old, 1.8 km diameter Lonar crater is one of only two known terrestrial craters to be emplaced in basaltic target rock (the 65 million year old Deccan Traps). The composition of the Lonar basalts is similar to martian basaltic meteorites, which establishes Lonar as an excellent analogue for similarly sized craters on the surface of Mars. Samples from cores drilled into the Lonar crater floor show that there are basaltic impact breccias that have been altered by post-impact hydrothermal processes to produce an assemblage of secondary alteration minerals. Microprobe data and X-ray diffraction analyses show that the alteration mineral assemblage consists primarily of saponite, with minor celadonite, and carbonate. Thermodynamic modeling and terrestrial volcanic analogues were used to demonstrate that these clay minerals formed at temperatures between 130°C and 200°C. By comparing the Lonar alteration assemblage with alteration at other terrestrial craters, we conclude that the Lonar crater represents a lower size limit for impact-induced hydrothermal activity. Based on these results, we suggest that similarly sized craters on Mars have the potential to form hydrothermal systems, as long as liquid water was present on or near the martian surface. -
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. -
3D Seismic Expression of a Cryptoexplosion Structure
CANADUN JOURNAL OF EXPLORATION GEOPH”SICS “OLD 29. Pm 2 ,tECEMBER 19931, P 429~439 3-D SEISMIC EXPRESSION OF A CRYPTOEXPLOSION STRUCTURE’ J. HELEN ISAAC~AND ROEERTR. SSEWART~ Mclosh, 1989: Sharpton and Ward, 1990). Impact craters can AWTRACT he termed either simple or complex, the main difference being the presence of multiple ring structures and central An enigmaticcircular itr”Ct”ce is observedon three-*immsionai uplift in a complex crater. The morphological change takes (3-D, ,eimlic d&mfrom Jilmcs River. Alberta It hasan uuter diammr uf 4.8 km anda raisedcentral uplift mrruundrdby a ring ,ynform. place at an excavation cavity diameter of ahout 2 km in sedi- The Centraluplift hasB diameter“1 2.4 km and if6 crestappears to mentary rocks and 4 km in crystalline rocks (Dence. 1972). he aho”, 400 m abovercgkml levels.The top of ihe StmClllr~ii ill B The principal feature of a complex impact crater is a central depth“f aho”, 4500,” and is belowtile LOW“f previousrc”n”“lic interest.Consequently. the featurehas ll”L beenpcnctrated by any peak, or group of peaks. surrounded by a llat tloor inside a wc,,s in the surveyarea. me seismic&lra inteqmation indicatr, terraced rim (Dencr, 1965). Complex crater central peaks are that the dimrbed scdimmtrare Cambrian in age.tt ii cstimilledIhat composed of def(mned and fractured rocks which arc uftcn the structure was formed during the Late CambrianIu Middle older than the country rock surrounding the structure. Partial Devonianlime petid andsuffered SeYcre W”bi,,” Mrw ,llCdrpositim “1 ,hCwcrlying Middle andUpper “ev”“ian carbonares.Rim fml,5, collapse of the central peak may he the source of some of the prohahiycaused by slumpingOf mmria, iill the dqmsion. -
Using the Manicouagan Impact Crater to Calibrate the Cyclostratigraphy Of
Using the Manicouagan Impact Ejecta to Calibrate the Cyclostratigraphy of the Newark Basin Francis D. Winslow III1, E.Troy Rasbury1, Sidney R. Hemming2 1Department of Geosciences, Stony Brook University, Stony Brook, NY 11794-2100, 2Lamont-DohertyEarth Observatory of Columbia University, Palisades, NY 10964 Introduction The Newark Basin, which contains the Triassic-Early Jurassic Newark Supergroup, is one of the best-studied early Mesozoic stratigraphic successions. A high-resolution cyclostratigraphic and magnetostratigraphic framework has been developed for the Newark Basin that encompasses approximately 30 my. When combined with biostratigraphy, this high- resolution record allows for global correlation of the Newark Basin succession with other Mesozoic basins, as well as the marine record. However, the high-resolution framework and the resulting correlations are based upon the assumption that the cyclostratigraphy is periodic and that the periods are known. There are only a few radiometric ages to constrain this cyclostratigraphy, most of which are from sills and basalt flows of the Central Atlantic Magmatic Province (CAMP) that on the basis of biostratigraphy are near the very base of the Jurassic. All other ages are based on extrapolation using the well-developed McLaughlin cycles that are considered to be 404 ky in duration. Our unpublished U-Pb results from stromatolite calcite and phosphate coprolites yield precise ages that support the assumed periodicity of the cycles. However, the occurrence of radiometrically datable syndepositional material in the Newark Basin is barely exploited. The Manicouagan Impact event would have produced a syndepositional horizon that potentially provides an additional test of the age and thus the cycle periods. -
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. -
Nördlingen 2010: the Ries Crater, the Moon, and the Future of Human Space Exploration, P
Program and Abstract Volume LPI Contribution No. 1559 The Ries Crater, the Moon, and the Future of Human Space Exploration June 25–27, 2010 Nördlingen, Germany Sponsors Museum für Naturkunde – Leibniz-Institute for Research on Evolution and Biodiversity at the Humboldt University Berlin, Germany Institut für Planetologie, University of Münster, Germany Deutsches Zentrum für Luft- und Raumfahrt DLR (German Aerospace Center) at Berlin, Germany Institute of Geoscience, University of Freiburg, Germany Lunar and Planetary Institute (LPI), Houston, USA Deutsche Forschungsgemeinschaft (German Science Foundation), Bonn, Germany Barringer Crater Company, Decatur, USA Meteoritical Society, USA City of Nördlingen, Germany Ries Crater Museum, Nördlingen, Germany Community of Otting, Ries, Germany Märker Cement Factory, Harburg, Germany Local Organization City of Nördlingen Museum für Naturkunde – Leibniz- Institute for Research on Evolution and Biodiversity at the Humboldt University Berlin Ries Crater Museum, Nördlingen Center of Ries Crater and Impact Research (ZERIN), Nördlingen Society Friends of the Ries Crater Museum, Nördlingen Community of Otting, Ries Märker Cement Factory, Harburg Organizing and Program Committee Prof. Dieter Stöffler, Museum für Naturkunde, Berlin Prof. Wolf Uwe Reimold, Museum für Naturkunde, Berlin Dr. Kai Wünnemann, Museum für Naturkunde, Berlin Hermann Faul, First Major of Nördlingen Prof. Thomas Kenkmann, Freiburg Prof. Harald Hiesinger, Münster Prof. Tilman Spohn, DLR, Berlin Dr. Ulrich Köhler, DLR, Berlin Dr. David Kring, LPI, Houston Dr. Axel Wittmann, LPI, Houston Gisela Pösges, Ries Crater Museum, Nördlingen Ralf Barfeld, Chair, Society Friends of the Ries Crater Museum Lunar and Planetary Institute LPI Contribution No. 1559 Compiled in 2010 by LUNAR AND PLANETARY INSTITUTE The Lunar and Planetary Institute is operated by the Universities Space Research Association under a cooperative agreement with the Science Mission Directorate of the National Aeronautics and Space Administration. -
Cráteres E Impactos
Cráteres e Impactos Historia del conocimiento sobre cráteres e impactos Energía y presión de los impactos Mecánica de Cráteres Estructura y tipos de cráteres Leyes de Craterización Meteoritos e impactitas Criterios para la Identificación de Cráteres Consecuencias ambientales de los impactos Conteo de cráteres El evento de Carancas: ejemplo de Geología Planetaria Practicas: Google Earth - cráteres Conteo de cráteres y ajuste de curvas de edad Virtual Lab: Visualización de secciones finas de meteoritos Cut & Paste Impact Cratering Seminar – H. Jay Melosh Geology and Geophysics of the Solar System – Shane Byrne Impact Cratering – Virginia Pasek Explorer's Guide to Impact Craters! http://www.psi.edu/explorecraters/ Terrestrial Impact Structures: Observation and Modeling - Gordon Osinski Environmental Effects of Impact Events - Elisabetta Pierazzo Traces of Catastrophe: A Handbook of Shock-Metamorphic Effects in Terrestrial Meteorite Impact Structures – Bevan French – Smithsonian Institution Effects of Material Properties on Cratering - Kevin Housen - The Boeing Co. Sedimentary rocks in Finnish impact structures -pre-impact or post- impact? - J.Kohonen and M. Vaarma - Geological Survey of Finland History about impact craters The study of impact craters has a well-defined beginning: 1610 Galileo’s small telescope and limited field of view did not permit him to view the entire moon at once, so his global maps were distorted Nevertheless, he recognized a pervasive landform that he termed “spots” He described them as circular, rimmed depressions But declined to speculate on their origin Robert Hooke had a better telescope in 1665 Hooke make good drawings of Hipparchus and speculated on the origin of the lunar “pits”. Hooke considered impact, but dismissed it because he could not imagine a source for the impactors. -
ABSTRACT 1 Terrestrial Impact Craters
MAPPING TERRESTRIAL IMPACT CRATERS WITH THE TANDEM-X DIGITAL ELEVATION MODEL Manfred Gottwald1, Thomas Fritz1, Helko Breit1, Birgit Schättler1, Alan Harris2 1German Aerospace Center, Remote Sensing Technology Institute, Oberpfaffenhofen, D-82234 Wessling, Germany 2German Aerospace Center, Institute of Planetary Research, Rutherfordstr. 2, D-12489 Berlin, Germany ABSTRACT We use the global digital elevation model (DEM) generated in the TanDEM-X mission for map- ping the confirmed terrestrial impact structures in the Earth Impact Database of the Planetary and Space Science Center (PASSC) at the University of New Brunswick, Canada. The TanDEM- X mission generates a global DEM with unprecedented properties. The achieved global coverage together with the improved accuracy (in the sub-10 m range) and spatial resolution (12 m at the equator) opens new opportunities in impact crater research based on terrestrial space-borne remote sensing data. It permits both for simple and complex craters investigations of the mor- phology of the particular structure (rim height, central uplift, ring-like patterns, elevation pro- files) and of the surrounding terrain (local deformation, drainage patterns) of outstanding quali- ty. 1 Terrestrial Impact Craters Earth, in contrast, the crust underwent continuous modification due to various processes such as plate 1.1 Impact Crater Record tectonics, erosion, sedimentation and glaciation. This prevented the development of an unbiased impact Terrestrial impact craters are the relics of collisions of record. Only the ancient continental shields provide the Earth with Solar System objects of different sizes. opportunities for detecting very old impact structures. Such collisions were frequent in the distant past when In other areas, craters of a certain size have remained the Solar System was young but even today solid bod- sufficiently intact only if they were formed rather re- ies from interplanetary space occasionally hit the ter- cently or if their large size has prevented them from restrial surface. -
Impact Crater Morphologies on Vesta
EPSC Abstracts Vol. 7 EPSC2012-700-1 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 Impact crater morphologies on Vesta P. Schenk (1), J.-B. Vincent (2), D.P. O’Brien (3), R. Jaumann (4), D. Williams (5), and the Dawn Science Team, (1) Lunar and Planetary Institute, Texas, USA, (2) Max Planck Institute, Katlenburg-Lindau, Germany, (3) Planetary Science Institute, Arizona, USA, (4) DLR, Inst. of Planetary Research, Germany, (5) Arizona State University, Arizona, USA. ([email protected]/ Fax: +11-281 4862162) Abstract craters have d/D ratios of 0.18 to 0.22, roughly consistent with the established lunar d/D curve for Impact craters on Vesta share some similarities and simple craters. Fresh craters between ~40 and 60 km, differences with other silicate bodies. Fresh craters however are shallower than this trend, corresponding are bowl-shaped though incipient complex features also to the formation of irregular floor mounds in occur at D>40 km. Flow-like features are observed these craters and a putative central peaks and a partial in crater ejecta but inferred volumes of impact melt terrace in these larger craters (Fig. 1). These changes are low compared to lunar craters. Local slopes also are interpreted as incipient or incomplete complex strongly influence crater shape and ejecta formation. crater development, which likely becomes complete only at diameters >60 km. The intersection of the two d/D trends occurs at 25 km, indicating that the 1. Introduction simple-complex transition diameter on Vesta may be -1 Vesta is the first asteroid visited large enough to significantly smaller than predicted from g scaling examine impact craters with potential complex crater from the terrestrial planets.