Economic Mineral Deposits in Impact Structures: a Review
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Fluid Inclusion Evidence for Impact‐Related Hydrothermal Fluid And
Fluid inclusion evidence for impact-related hydrothermal fluid and hydrocarbon migration in Creataceous sediments of the ICDP-Chicxulub drill core Yax-1 Item Type Article; text Authors Lüders, V.; Rickers, K. Citation Lüders, V., & Rickers, K. (2004). Fluid inclusion evidence for impactrelated hydrothermal fluid and hydrocarbon migration in Creataceous sediments of the ICDPChicxulub drill core Yax1. Meteoritics & Planetary Science, 39(7), 1187-1197. DOI 10.1111/j.1945-5100.2004.tb01136.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 06/10/2021 06:52:32 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656684 Meteoritics & Planetary Science 39, Nr 7, 1187–1197 (2004) Abstract available online at http://meteoritics.org Fluid inclusion evidence for impact-related hydrothermal fluid and hydrocarbon migration in Creataceous sediments of the ICDP-Chicxulub drill core Yax-1 Volker LÜDERS1* and Karen RICKERS1, 2 1GeoForschungsZentrum Potsdam, Department 4, Telegrafenberg, D-14473, Potsdam, Germany 2Hamburger Synchrotronstrahlungslabor HASYLAB at Deutsches Elektronen-Synchrotron DESY, Notkestrasse 85, D-22603 Hamburg, Germany *Corresponding author. E-mail: [email protected] (Received 3 September 2003; revision accepted 31 March 2004) Abstract–Fluid inclusions studies in quartz and calcite in samples from the ICDP-Chicxulub drill core Yaxcopoil-1 (Yax-1) have revealed compelling evidence for impact-induced hydrothermal alteration. Fluid circulation through the melt breccia and the underlying sedimentary rocks was not homogeneous in time and space. The formation of euhedral quartz crystals in vugs hosted by Cretaceous limestones is related to the migration of hot (>200 °C), highly saline, metal-rich, hydrocarbon-bearing brines. -
Railway Employee Records for Colorado Volume Iii
RAILWAY EMPLOYEE RECORDS FOR COLORADO VOLUME III By Gerald E. Sherard (2005) When Denver’s Union Station opened in 1881, it saw 88 trains a day during its gold-rush peak. When passenger trains were a popular way to travel, Union Station regularly saw sixty to eighty daily arrivals and departures and as many as a million passengers a year. Many freight trains also passed through the area. In the early 1900s, there were 2.25 million railroad workers in America. After World War II the popularity and frequency of train travel began to wane. The first railroad line to be completed in Colorado was in 1871 and was the Denver and Rio Grande Railroad line between Denver and Colorado Springs. A question we often hear is: “My father used to work for the railroad. How can I get information on Him?” Most railroad historical societies have no records on employees. Most employment records are owned today by the surviving railroad companies and the Railroad Retirement Board. For example, most such records for the Union Pacific Railroad are in storage in Hutchinson, Kansas salt mines, off limits to all but the lawyers. The Union Pacific currently declines to help with former employee genealogy requests. However, if you are looking for railroad employee records for early Colorado railroads, you may have some success. The Colorado Railroad Museum Library currently has 11,368 employee personnel records. These Colorado employee records are primarily for the following railroads which are not longer operating. Atchison, Topeka & Santa Fe Railroad (AT&SF) Atchison, Topeka and Santa Fe Railroad employee records of employment are recorded in a bound ledger book (record number 736) and box numbers 766 and 1287 for the years 1883 through 1939 for the joint line from Denver to Pueblo. -
2017 ANNUAL REPORT 2017 Annual Report Table of Contents the Michael J
Roadmaps for Progress 2017 ANNUAL REPORT 2017 Annual Report Table of Contents The Michael J. Fox Foundation is dedicated to finding a cure for 2 A Note from Michael Parkinson’s disease through an 4 Annual Letter from the CEO and the Co-Founder aggressively funded research agenda 6 Roadmaps for Progress and to ensuring the development of 8 2017 in Photos improved therapies for those living 10 2017 Donor Listing 16 Legacy Circle with Parkinson’s today. 18 Industry Partners 26 Corporate Gifts 32 Tributees 36 Recurring Gifts 39 Team Fox 40 Team Fox Lifetime MVPs 46 The MJFF Signature Series 47 Team Fox in Photos 48 Financial Highlights 54 Credits 55 Boards and Councils Milestone Markers Throughout the book, look for stories of some of the dedicated Michael J. Fox Foundation community members whose generosity and collaboration are moving us forward. 1 The Michael J. Fox Foundation 2017 Annual Report “What matters most isn’t getting diagnosed with Parkinson’s, it’s A Note from what you do next. Michael J. Fox The choices we make after we’re diagnosed Dear Friend, can open doors to One of the great gifts of my life is that I've been in a position to take my experience with Parkinson's and combine it with the perspectives and expertise of others to accelerate possibilities you’d improved treatments and a cure. never imagine.’’ In 2017, thanks to your generosity and fierce belief in our shared mission, we moved closer to this goal than ever before. For helping us put breakthroughs within reach — thank you. -
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. -
USGS Open-File Report 2005-1190, Table 1
TABLE 1 GEOLOGIC FIELD-TRAINING OF NASA ASTRONAUTS BETWEEN JANUARY 1963 AND NOVEMBER 1972 The following is a year-by-year listing of the astronaut geologic field training trips planned and led by personnel from the U.S. Geological Survey’s Branches of Astrogeology and Surface Planetary Exploration, in collaboration with the Geology Group at the Manned Spacecraft Center, Houston, Texas at the request of NASA between January 1963 and November 1972. Regional geologic experts from the U.S. Geological Survey and other governmental organizations and universities s also played vital roles in these exercises. [The early training (between 1963 and 1967) involved a rather large contingent of astronauts from NASA groups 1, 2, and 3. For another listing of the astronaut geologic training trips and exercises, including all attending and the general purposed of the exercise, the reader is referred to the following website containing a contribution by William Phinney (Phinney, book submitted to NASA/JSC; also http://www.hq.nasa.gov/office/pao/History/alsj/ap-geotrips.pdf).] 1963 16-18 January 1963: Meteor Crater and San Francisco Volcanic Field near Flagstaff, Arizona (9 astronauts). Among the nine astronaut trainees in Flagstaff for that initial astronaut geologic training exercise was Neil Armstrong--who would become the first man to step foot on the Moon during the historic Apollo 11 mission in July 1969! The other astronauts present included Frank Borman (Apollo 8), Charles "Pete" Conrad (Apollo 12), James Lovell (Apollo 8 and the near-tragic Apollo 13), James McDivitt, Elliot See (killed later in a plane crash), Thomas Stafford (Apollo 10), Edward White (later killed in the tragic Apollo 1 fire at Cape Canaveral), and John Young (Apollo 16). -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Warren and Taylor-2014-In Tog-The Moon-'Author's Personal Copy'.Pdf
This article was originally published in Treatise on Geochemistry, Second Edition published by Elsevier, and the attached copy is provided by Elsevier for the author's benefit and for the benefit of the author's institution, for non- commercial research and educational use including without limitation use in instruction at your institution, sending it to specific colleagues who you know, and providing a copy to your institution’s administrator. All other uses, reproduction and distribution, including without limitation commercial reprints, selling or licensing copies or access, or posting on open internet sites, your personal or institution’s website or repository, are prohibited. For exceptions, permission may be sought for such use through Elsevier's permissions site at: http://www.elsevier.com/locate/permissionusematerial Warren P.H., and Taylor G.J. (2014) The Moon. In: Holland H.D. and Turekian K.K. (eds.) Treatise on Geochemistry, Second Edition, vol. 2, pp. 213-250. Oxford: Elsevier. © 2014 Elsevier Ltd. All rights reserved. Author's personal copy 2.9 The Moon PH Warren, University of California, Los Angeles, CA, USA GJ Taylor, University of Hawai‘i, Honolulu, HI, USA ã 2014 Elsevier Ltd. All rights reserved. This article is a revision of the previous edition article by P. H. Warren, volume 1, pp. 559–599, © 2003, Elsevier Ltd. 2.9.1 Introduction: The Lunar Context 213 2.9.2 The Lunar Geochemical Database 214 2.9.2.1 Artificially Acquired Samples 214 2.9.2.2 Lunar Meteorites 214 2.9.2.3 Remote-Sensing Data 215 2.9.3 Mare Volcanism -
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. -
The Civilian Conservation Corps and the National Park Service, 1933-1942: an Administrative History. INSTITUTION National Park Service (Dept
DOCUMENT RESUME ED 266 012 SE 046 389 AUTHOR Paige, John C. TITLE The Civilian Conservation Corps and the National Park Service, 1933-1942: An Administrative History. INSTITUTION National Park Service (Dept. of Interior), Washington, D.C. REPORT NO NPS-D-189 PUB DATE 85 NOTE 293p.; Photographs may not reproduce well. PUB TYPE Reports - Descriptive (141) -- Historical Materials (060) EDRS PRICE MF01/PC12 Plus Postage. DESCRIPTORS *Conservation (Environment); Employment Programs; *Environmental Education; *Federal Programs; Forestry; Natural Resources; Parks; *Physical Environment; *Resident Camp Programs; Soil Conservation IDENTIFIERS *Civilian Conservation Corps; Environmental Management; *National Park Service ABSTRACT The Civilian Conservation Corps (CCC) has been credited as one of Franklin D. Roosevelt's most successful effortsto conserve both the natural and human resources of the nation. This publication provides a review of the program and its impacton resource conservation, environmental management, and education. Chapters give accounts of: (1) the history of the CCC (tracing its origins, establishment, and termination); (2) the National Park Service role (explaining national and state parkprograms and co-operative planning elements); (3) National Park Servicecamps (describing programs and personnel training and education); (4) contributions of the CCC (identifying the major benefits ofthe program in the areas of resource conservation, park and recreational development, and natural and archaeological history finds); and (5) overall -
Stable Isotopes and Hydrothermal Fluid Source in the Yaxcopoil-1 Borehole, Chicxulub Impact Structure, Mexico
Lunar and Planetary Science XXXV (2004) 1261.pdf STABLE ISOTOPES AND HYDROTHERMAL FLUID SOURCE IN THE YAXCOPOIL-1 BOREHOLE, CHICXULUB IMPACT STRUCTURE, MEXICO. L. Zurcher1, D. A. Kring1, D. Dettman2, and M. Rollog2, 1Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., 2Department of Geosciences, University of Arizona, 1040 E. Fourth St., Tucson, Arizona 85721. Introduction: We present new results of a for black glass at the K/T boundary in Haiti (~6‰; detailed C, O, and H stable isotope survey on [7]). A similar but less extensive δ18O shift occurs carbonate and silicate fractions of samples in siliceous samples from the Yucatan-6 (Y-6) collected from the hydrothermally altered borehole (~10-13‰; [1]). δD values from this impactite units at Yaxcopoil-1 (Yax-1). Previous study exhibit a narrow range between -34 and stable isotope studies on Chicxulub crater -54‰, and closely mirror δ18O values. impactites include [1-4]. In this investigation, we Carbonate fraction δ18O values vary between treat stable isotopes in concert with mineralogical 22 and 30‰, and most δ13C values exhibit a and geochemical data. Combined results allowed narrow range between -1 and +2‰. δ18O values are us to place constraints on the physico-chemical heavier than silicate fractions, and some are even parameters of the hydrothermal fluid, which we heavier than local limestone. δ18O and δ13C values used to deduce its most likely source. of carbonate fractions are on average higher in the Hydrothermal Alteration at Yaxcopoil-1: upper part of the impactite section. Yax-1 Petrographic and electron microprobe results carbonate δ18O and δ13C values are also heavier conducted previously [5] suggested a slightly than values of carbonate-dominated samples from alkaline andesitic composition for the impactite Y-6 (11 to 20‰ and -1 to -5‰, respectively; [1]).