Lithostratigraphic and Petrographic Analysis of ICDP Drill Core LB-07A, Bosumtwi Impact Structure, Ghana
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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. -
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. -
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. -
Chapter 5: Shock Metamorphism and Impact Melting
5. Shock Metamorphism and Impact Melting ❖❖❖ Shock-metamorphic products have become one of the diagnostic tools of impact cratering studies. They have become the main criteria used to identify structures of impact origin. They have also been used to map the distribution of shock-pressures throughout an impact target. The diverse styles of shock metamorphism include fracturing of crystals, formation of microcrystalline planes of glass through crystals, conversion of crystals to high-pressure polymorphs, conversion of crystals to glass without loss of textural integrity, conversion of crystals to melts that may or may not mix with melts from other crystals. Shock-metamorphism of target lithologies at the crater was first described by Barringer (1905, 1910) and Tilghman (1905), who recognized three different products. The first altered material they identified is rock flour, which they concluded was pulverized Coconino sandstone. Barringer observed that rock flour was composed of fragmented quartz crystals that were far smaller in size than the unaffected quartz grains in normal Coconino sandstone. Most of the pulverized silica he examined passed through a 200 mesh screen, indicating grain sizes <74 µm (0.074 mm), which is far smaller than the 0.2 mm average detrital grain size in normal Coconino (Table 2.1). Fairchild (1907) and Merrill (1908) also report a dramatic comminution of Coconino, although only 50% of Fairchild’s sample of rock flour passed through a 100 mesh screen, indicating grain sizes <149 µm. Heterogeneity of the rock flour is evident in areas where sandstone clasts survive within the rock flour. The rock flour is pervasive and a major component of the debris at the crater. -
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. -
EPSC2018-833, 2018 European Planetary Science Congress 2018 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2018
EPSC Abstracts Vol. 12, EPSC2018-833, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Impact melt boulder from northern Sweden from an unknown source Timmu Kreitsmann (1), Satu Hietala (2), Tapio Soukka (3), Jüri Plado (1), Jari Nenonen (2) and Lauri J. Pesonen (4) (1) Department of Geology, University of Tartu, Estonia ([email protected], [email protected]), (2) Geological Survey of Finland, Finland ([email protected], [email protected]), (3) Oulu Mining School, University of Oulu, Finland ([email protected]) (4) Solid Earth Geophysics Laboratory, Physics Department, University of Helsinki, Finland ([email protected]) Abstract We report an impact melt rock finding from northern Sweden, near the village of Kitkiöjärvi. There is no confirmed meteorite impact structure nearby, thus, the source is currently undiscovered. The impact origin of the finding was confirmed by the presence of planar deformation features (PDFs) in quartz. 1. Introduction Impact cratering is a common and frequent process that affects the planetary surfaces across the solar system throughout geologic time. On Earth, there are 191 confirmed impact structures which are distributed unevenly around the globe. The Fennoscandian Shield houses around 10% of them. Here, we report an impact melt rock finding that originates from an unknown structure in northern Sweden. The semi-rounded impactite boulder, sized 10 × 7 cm, was found by Tapio Soukka in 2017 from a gravel pit at the western side of village Kitkiöjärvi (67°46'16"N 23°03'06"E; Fig. 1). Figure 1: Proven impact structures in Fennoscandia. -
A Tomography Approach to Investigate Impactite Structure
3rd International Conference on Tomography of Materials and Structures Lund, Sweden, 26-30 June 2017, ICTMS2017-110 A TOMOGRAPHY APPROACH TO INVESTIGATE IMPACTITE STRUCTURE A. Fedrigo*1,2, K. Marstal1,3, A. Bjorholm Dahl1, M. Lyksborg1, C. Gundlach1, M. Strobl2 & C. Bender Koch4 1Danish Technical University, Denmark 2European Spallation Source ESS ERIC, Sweden 3ERASMUS MC, Netherland 4Copenhagen University, Denmark Keywords: Neutron imaging, image registration, bimodal imaging, computed tomography. Summary: We investigate the structure of impactites from the Wabar iron meteorite impact site in Saudi Arabia. In order to understand the physical and chemical processes involved in the formation of the impactite, we applied a non-destructive investigation approach, which combines X-ray and neutron tomography. This bi-modal imaging method allowed for a better understanding of the impactite’s chemical composition. 1. INTRODUCTION Meteorite impacts have recently been recognised among the most important processes able to modify planetary surfaces. It also happens to be one of the least understood in details. In particular it is a challenge to understand both the extent of impacts and the physical and chemical changes that occur during and following the impact, where materials (e.g., rocks, sand, meteorite fragments, etc.) are subjected to temperatures of several thousands degrees and pressures of several GPa. In addition, most accessible Earth impact areas are highly affected by weathering, which causes extensive secondary chemical alterations. Iron meteorites impact on planetary surfaces cause shock-induced rock deformations that happens both at macroscopic and at microscopic level, e.g. shatter cones (macroscopic) and planar deformation features in quartz (microscopic). Another indicator often correlated to meteoritic impacts is the presence of iridium concentration anomalies [1, 2]. -
The Tennessee Meteorite Impact Sites and Changing Perspectives on Impact Cratering
UNIVERSITY OF SOUTHERN QUEENSLAND THE TENNESSEE METEORITE IMPACT SITES AND CHANGING PERSPECTIVES ON IMPACT CRATERING A dissertation submitted by Janaruth Harling Ford B.A. Cum Laude (Vanderbilt University), M. Astron. (University of Western Sydney) For the award of Doctor of Philosophy 2015 ABSTRACT Terrestrial impact structures offer astronomers and geologists opportunities to study the impact cratering process. Tennessee has four structures of interest. Information gained over the last century and a half concerning these sites is scattered throughout astronomical, geological and other specialized scientific journals, books, and literature, some of which are elusive. Gathering and compiling this widely- spread information into one historical document benefits the scientific community in general. The Wells Creek Structure is a proven impact site, and has been referred to as the ‘syntype’ cryptoexplosion structure for the United State. It was the first impact structure in the United States in which shatter cones were identified and was probably the subject of the first detailed geological report on a cryptoexplosive structure in the United States. The Wells Creek Structure displays bilateral symmetry, and three smaller ‘craters’ lie to the north of the main Wells Creek structure along its axis of symmetry. The question remains as to whether or not these structures have a common origin with the Wells Creek structure. The Flynn Creek Structure, another proven impact site, was first mentioned as a site of disturbance in Safford’s 1869 report on the geology of Tennessee. It has been noted as the terrestrial feature that bears the closest resemblance to a typical lunar crater, even though it is the probable result of a shallow marine impact. -
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. -
Geology of the Wabar Meteorite Craters, Saudi Arabia; E
Lunar and Planetary Science XXVIII 1660.PDF GEOLOGY OF THE WABAR METEORITE CRATERS, SAUDI ARABIA; E. M. Shoemaker1 and J.C. Wynn2, 1U.S. Geological Survey and Lowell Observatory, Flagstaff, AZ 86001, 2U.S. Geological Survey, Reston, VA 20192. In March of 1995, we were privileged to accompany an expedition sponsored by the Zahid Corporation of Saudi Arabia to the Wabar Craters in the Rub' Al-Khali desert (The Empty Quarter) of the southern Arabian peninsula (at 21°30.2' N latitude and 50°28.4' E longitude). Transport across the sand sheet of the northern Rub' Al-Khali was by Humvees and a 4 x 4 Volvo truck, which carried a backhoe for the purpose of exposing the structure of the crater rims. Although numerous visitors have examined the Wabar meteorite craters over the 62 years since St. John Philby's first report, no detailed investigation of the geology of the craters had been undertaken prior to our expedition. We spent 5 days during the week of March 12 at the craters carrying out a systematic survey of the craters themselves and the surrounding strewn field of impact glass and impact-formed "instant rock." Parts of three craters were exposed at the time of our visit (Fig. 1). Their diameters are estimated at 11, 64, and 116 m. We refer to these as the 11-m, Philby A, and Philby B craters. Contrary to inferences in a number of previous reports (e.g. [1], [2], [3]), the craters have been formed entirely in loose sand of the active Rub' Al- Khali sand sheet. -
HIGH PRESSURE PHASES in IMPACTITES of the ZWNSHIN CRATER/TTSSR,T1.D.Badyukov
HIGH PRESSURE PHASES IN IMPACTITES OF THE ZWNSHIN CRATER/TTSSR,T1.D.Badyukov. Vernadsky Institute of Geochemistry and Analytical Chemistry, USSR Academy of Science, Moscow, It has been suggested that most rock-forming minerals can be modified in the solid state by shock wave compression (1~2). Recent data suggest a more complicated mechanism of high pres- ure phase transitions: ~Dstallizationof the phases from im- pact melt under shock compression (3.4). In order to investiga- te the problem we looked for high density in impactites of the Zhamanshin crater, The crater was formed in a two-layer target consisting of clays, marls,quartzites, chlorite-epidote-quartz slates and so forth (5). The specimens were collected from the inside part of the crater ring bank. The high density phases were yielded from the samples of impactites by dissolution in hydrofluoric acid. Minerals were identified by optical and X-ray diffraction methods. Mineral and chemical compositions of the investigated samples are shown in table 1. According to the optical microscopy observations corundum, spinel and kyani- te could be formed from the melt but it should be noted that %hisis very difficult to establish exactly because of the sub- micron sizes of c~stallites.Tnvestigation of the shock meta- morphic quartz vein sample, composed of diaplectic quartz, dia- plectic glass and melt glass showed that stishovite i~ only in diaplectic quartz, but coesite is in diaplectic glass and some- times in melt glass in agreement with the data for the Ries crater (6). This could have been si~ggestedby the schenrtic mechanism of formation of the high pressure phases (kyanite and garnet phase). -
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.