Sedimentation Rate of Salt Determined by Micrometeorite Analysis
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New Insects from the Earliest Permian of Carrizo Arroyo (New Mexico, USA) Bridging the Gap Between the Carboniferous and Permian Entomofaunas
Insect Systematics & Evolution 48 (2017) 493–511 brill.com/ise New insects from the earliest Permian of Carrizo Arroyo (New Mexico, USA) bridging the gap between the Carboniferous and Permian entomofaunas Jakub Prokopa,* and Jarmila Kukalová-Peckb aDepartment of Zoology, Faculty of Science, Charles University, Viničná 7, CZ-128 43 Praha 2, Czech Republic bEntomology, Canadian Museum of Nature, Ottawa, ON, Canada K1P 6P4 *Corresponding author, e-mail: [email protected] Version of Record, published online 7 April 2017; published in print 1 November 2017 Abstract New insects are described from the early Asselian of the Bursum Formation in Carrizo Arroyo, NM, USA. Carrizoneura carpenteri gen. et sp. nov. (Syntonopteridae) demonstrates traits in hindwing venation to Lithoneura and Syntonoptera, both known from the Moscovian of Illinois. Carrizoneura represents the latest unambiguous record of Syntonopteridae. Martynovia insignis represents the earliest evidence of Mar- tynoviidae. Carrizodiaphanoptera permiana gen. et sp. nov. extends range of Diaphanopteridae previously restricted to Gzhelian. The re-examination of the type speciesDiaphanoptera munieri reveals basally coa- lesced vein MA with stem of R and RP resulting in family diagnosis emendation. Arroyohymen splendens gen. et sp. nov. (Protohymenidae) displays features in venation similar to taxa known from early and late Permian from the USA and Russia. A new palaeodictyopteran wing attributable to Carrizopteryx cf. arroyo (Calvertiellidae) provides data on fore wing venation previously unknown. Thus, all these new discoveries show close relationship between late Pennsylvanian and early Permian entomofaunas. Keywords Ephemeropterida; Diaphanopterodea; Megasecoptera; Palaeodictyoptera; gen. et sp. nov; early Asselian; wing venation Introduction The fossil record of insects from continental deposits near the Carboniferous-Permian boundary is important for correlating insect evolution with changes in climate and in plant ecosystems. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Space Resources Roundtable II : November 8-10, 2000, Golden, Colorado
SPACE RESOURCES RouNDTABLE II November 8-10, 2000 Colorado School of Mines Golden, Colorado LPI Contribution No. 1070 SPACE RESOURCES ROUNDTABLE II November 8-10, 2000 Golden, Colorado Sponsored by Colorado School of Mines Lunar and Planetary Institute National Aeronautics and Space Administration Steering Committee Joe Burris, WorldTradeNetwork.net David Criswell, University of Houston Michael B. Duke, Lunar and Planetary Institute Mike O'Neal, NASA Kennedy Space Center Sanders Rosenberg, InSpace Propulsion, Inc. Kevin Reed, Marconi, Inc. Jerry Sanders, NASA Johnson Space Center Frank Schowengerdt, Colorado School of Mines Bill Sharp, Colorado School of Mines LPI Contribution No. 1070 Compiled in 2000 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Matenal in this volume may be copied wnhout restraint for library, abstract service, education. or personal research purposes; however, republication of any paper or portion thereof requ1res the wriuen permission of the authors as well as the appropnate acknowledgment of this publication. Abstracts in this volume may be cited as Author A B. (2000) Title of abstract. In Space Resources Roundtable II. p x.x . LPI Contnbuuon No. 1070. Lunar and Planetary Institute. Houston. This repon is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Phone: 281-486-2172 Fax: 281-486-2186 E-mail: [email protected] Mail order requestors will be invoiced for the cost of shipping and handling. LPI Contribution No 1070 iii Preface This volume contains abstracts that have been accepted for presentation at the Space Resources Roundtable II, November 8-10, 2000. -
High Survivability of Micrometeorites on Mars: Sites with Enhanced Availability of Limiting Nutrients
RESEARCH ARTICLE High Survivability of Micrometeorites on Mars: Sites With 10.1029/2019JE006005 Enhanced Availability of Limiting Nutrients Key Points: Andrew G. Tomkins1 , Matthew J. Genge2,3 , Alastair W. Tait1,4 , Sarah L. Alkemade1, • Micrometeorites are predicted to be 1 1 5 far more abundant on Mars than on Andrew D. Langendam , Prudence P. Perry , and Siobhan A. Wilson Earth 1 2 • Micrometeorites are concentrated in School of Earth, Atmosphere and Environment, Melbourne, Victoria, Australia, Impact and Astromaterials Research the residue of aeolian sediment Centre, Department of Earth Science and Engineering, Imperial College London, London, UK, 3Department of removal, such as at bedrock cracks Mineralogy, The Natural History Museum, London, UK, 4Department of Biological and Environmental Sciences, and gravel accumulations University of Stirling, Scotland, UK, 5Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, • Micrometeorite accumulation sites are enriched in key nutrients for Alberta, Canada primitive microbes: reduced phosphorus, sulfur, and iron Abstract NASA's strategy in exploring Mars has been to follow the water, because water is essential for life, and it has been found that there are many locations where there was once liquid water on the surface. Now perhaps, to narrow down the search for life on a barren basalt‐dominated surface, there needs to be a Correspondence to: A. G. Tomkins, refocusing to a strategy of “follow the nutrients.” Here we model the entry of metallic micrometeoroids [email protected] through the Martian atmosphere, and investigate variations in micrometeorite abundance at an analogue site on the Nullarbor Plain in Australia, to determine where the common limiting nutrients available in Citation: these (e.g., P, S, Fe) become concentrated on the surface of Mars. -
Connection Between Micrometeorites and Wild 2 Particles: from Antarctic Snow to Cometary Ices
Meteoritics & Planetary Science 44, Nr 10, 1643–1661 (2009) Abstract available online at http://meteoritics.org Connection between micrometeorites and Wild 2 particles: From Antarctic snow to cometary ices E. DOBRIC√1,*, C. ENGRAND1, J. DUPRAT1, M. GOUNELLE2, H. LEROUX3, E. QUIRICO4, and J.-N. ROUZAUD5 1Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse, CNRS-Univ. Paris Sud, 91405 Orsay Campus, France 2Laboratoire de Minéralogie et de Cosmochimie, Muséum National d’Histoire Naturelle, 57 rue Cuvier, CP52, 75005 Paris, France 3Laboratoire de Structure et Propriétés de l’Etat Solide, CNRS-Univ. des Sciences et Technologies de Lille, 59655 Villeneuve d’Ascq, France 4Laboratoire de Planétologie de Grenoble, Univ. J. Fourier CNRS-INSU 38041 Grenoble Cedex 09, France 5Laboratoire de Géologie, Ecole Normale Supérieure, CNRS, 75231 Paris Cedex 5, France *Corresponding author. E-mail: [email protected] (Received 17 March 2009; revision accepted 21 September 2009) Abstract–We discuss the relationship between large cosmic dust that represents the main source of extraterrestrial matter presently accreted by the Earth and samples from comet 81P/Wild 2 returned by the Stardust mission in January 2006. Prior examinations of the Stardust samples have shown that Wild 2 cometary dust particles contain a large diversity of components, formed at various heliocentric distances. These analyses suggest large-scale radial mixing mechanism(s) in the early solar nebula and the existence of a continuum between primitive asteroidal and cometary matter. The recent collection of CONCORDIA Antarctic micrometeorites recovered from ultra-clean snow close to Dome C provides the most unbiased collection of large cosmic dust available for analyses in the laboratory. -
Xenacanthus (Chondrichthyes: Xenacanthiformes) from North America
Acta Geologica Polonica, Vol. 49 (J 999), No.3, pp. 215-266 406 IU S UNES 0 I Dentitions of Late Palaeozoic Orthacanthus species and new species of ?Xenacanthus (Chondrichthyes: Xenacanthiformes) from North America GARY D. JOHNSON Department of Earth Sciences and Physics, University of South Dakota; 414 East Clark Street, Vermillion, SD 57069-2390, USA. E-mail: [email protected] ABSTRACT: JOHNSON, G.D. 1999. Dentitions of Late Palaeozoic Orthacanthus species and new species of ?Xenacanthus (Chondrichthyes: Xenacanthiformes) from North America. Acta Geologica Polonica, 49 (3),215-266. Warszawa. Orthacanthus lateral teeth have paired, variably divergent, smooth, usually carinated labio-lingually compressed principal cusps separated by a central foramen; one or more intermediate cusps; and an api cal button on the base isolated from the cusps. Several thousand isolated teeth from Texas Artinskian bulk samples are used to define the heterodont dentitions of O. texensis and O. platypternus. The O. tex ensis tooth base has a labio-Iingual width greater than the anteromedial-posterolateral length, the basal tubercle is restricted to the thick labial margin, the principal cusps are serrated to varying degrees, and the posterior cusp is larger. The O. platypternus tooth base is longer than wide, its basal tubercle extends to the center, the labial margin is thin, serrations are absent on the principal cusps, the anterior cusp is larger, and a single intermediate cusp is present. More than two hundred isolated teeth from Nebraska (Gzhelian) and Pennsylvania (Asselian) provide a preliminary description of the heterodont dentition of O. compress us . The principal cusps are similar to O. -
By JB Gillespie and GD Hargadine
GEOHYDROLOGY AND SALINE GROUND-WATER DISCHARGE TO THE SOUTH FORK NINNESCAH RIVER IN PRATT AND KINGMAN COUNTIES, SOUTH-CENTRAL KANSAS By J.B. Gillespie and G.D. Hargadine U.S. GEOLOGICAL SURVEY Water-Resources Investigations Report 93-4177 Prepared in cooperation with the CITY OF WICHITA, SEDGWICK COUNTY, and the KANSAS WATER OFFICE Lawrence, Kansas 1994 U.S. DEPARTMENT OF THE INTERIOR BRUCE BABBITT, Secretary U.S. GEOLOGICAL SURVEY Robert M. Hirsch, Acting Director For additional information write to: Copies of this report can be purchased from: U.S. Geological Survey District Chief Earth Science Information Center U.S. Geological Survey Open-File Reports Section Water Resources Division Box 25286, MS 517 4821 Quail Crest Place Denver Federal Center Lawrence, Kansas 66049-3839 Denver, Colorado 80225 CONTENTS Page Definition of terms.......................................................................................................................... vii Abstract............................................................................................................................................. 1 Introduction....................................................................................................................................... 1 Purpose and scope................................................................................................................2 Previous studies................................................................................................................... 4 Acknowledgments ................................................................................................................4 -
Finegrained Precursors Dominate the Micrometeorite Flux
Meteoritics & Planetary Science 47, Nr 4, 550–564 (2012) doi: 10.1111/j.1945-5100.2011.01292.x Fine-grained precursors dominate the micrometeorite flux Susan TAYLOR1*, Graciela MATRAJT2, and Yunbin GUAN3 1Cold Regions Research and Engineering Laboratory, 72 Lyme Road, Hanover, New Hampshire 03755–1290, USA 2University of Washington, Seattle, Washington 98105, USA 3Geological & Planetary Sciences MC 170-25, Caltech, Pasadena, California 91125, USA *Corresponding author. E-mail: [email protected] (Received 15 May 2011; revision accepted 22 September 2011) Abstract–We optically classified 5682 micrometeorites (MMs) from the 2000 South Pole collection into textural classes, imaged 2458 of these MMs with a scanning electron microscope, and made 200 elemental and eight isotopic measurements on those with unusual textures or relict phases. As textures provide information on both degree of heating and composition of MMs, we developed textural sequences that illustrate how fine-grained, coarse-grained, and single mineral MMs change with increased heating. We used this information to determine the percentage of matrix dominated to mineral dominated precursor materials (precursors) that produced the MMs. We find that at least 75% of the MMs in the collection derived from fine-grained precursors with compositions similar to CI and CM meteorites and consistent with dynamical models that indicate 85% of the mass influx of small particles to Earth comes from Jupiter family comets. A lower limit for ordinary chondrites is estimated at 2–8% based on MMs that contain Na-bearing plagioclase relicts. Less than 1% of the MMs have achondritic compositions, CAI components, or recognizable chondrules. Single mineral MMs often have magnetite zones around their peripheries. -
AN ACHONDRITIC MICROMETEORITE from ANTARCTICA: EXPANDING the SOLAR SYSTEM INVENTORY of BASALTIC ASTEROIDS. M. Gounelle1,2,3, C. Engrand2, M
Lunar and Planetary Science XXXVI (2005) 1655.pdf AN ACHONDRITIC MICROMETEORITE FROM ANTARCTICA: EXPANDING THE SOLAR SYSTEM INVENTORY OF BASALTIC ASTEROIDS. M. Gounelle1,2,3, C. Engrand2, M. Chaussidon4, M.E. Zolensky5 and M. Maurette2. 1Université Paris XI, 91 405 Orsay, France ([email protected]), 2CSNSM. Bâtiment 104, 91 405 Orsay, France.3Department of Mineralogy, The Natural History Museum, London, UK. 4CRPG-CNRS, BP20, 54501 Vandoeuvre les Nancy, France. 5KT, NASA Johnson Space Center, Houston, Texas 77058, USA. Introduction: Micrometeorites with sizes below 1 mm 100.0 are collected in a diversity of environments such as deep-sea sediments and polar caps [1]. Chemical, mineralogical and isotopic studies indicate that micrometeorites are closely related to primitive CI / carbonaceous chondrites that amount to only ~2 % of 10.0 meteorite falls [1]. While thousands of REE micrometeorites have been studied in detail, no micrometeorite has been found so far with an unambiguous achondritic composition and texture. 1.0 One melted cosmic spherule has a low Fe/Mn ratio La Ce Pr Nd Sm Eu Gd Dy Er Yb Lu similar to that of eucrites, the most common basaltic Figure 2: REE abundance pattern of pyroxene in meteorite group [2]. Here we report on the texture, MM40 measured with the ims3f ion microprobe at mineralogy, Rare Earth Elements (REEs) abundance CRPG Nancy. and oxygen isotopic composition of the unmelted Antarctic micrometeorite 99-21-40 that has an Pyroxene in MM40 is enriched by a factor of 10 in unambiguous basaltic origin. REEs relative to CI chondrites. The REE abundance pattern is fractionated with a gradual increase from light to heavy REEs. -
Near Earth Asteroid Rendezvous: Mission Summary 351
Cheng: Near Earth Asteroid Rendezvous: Mission Summary 351 Near Earth Asteroid Rendezvous: Mission Summary Andrew F. Cheng The Johns Hopkins Applied Physics Laboratory On February 14, 2000, the Near Earth Asteroid Rendezvous spacecraft (NEAR Shoemaker) began the first orbital study of an asteroid, the near-Earth object 433 Eros. Almost a year later, on February 12, 2001, NEAR Shoemaker completed its mission by landing on the asteroid and acquiring data from its surface. NEAR Shoemaker’s intensive study has found an average density of 2.67 ± 0.03, almost uniform within the asteroid. Based upon solar fluorescence X-ray spectra obtained from orbit, the abundance of major rock-forming elements at Eros may be consistent with that of ordinary chondrite meteorites except for a depletion in S. Such a composition would be consistent with spatially resolved, visible and near-infrared (NIR) spectra of the surface. Gamma-ray spectra from the surface show Fe to be depleted from chondritic values, but not K. Eros is not a highly differentiated body, but some degree of partial melting or differentiation cannot be ruled out. No evidence has been found for compositional heterogeneity or an intrinsic magnetic field. The surface is covered by a regolith estimated at tens of meters thick, formed by successive impacts. Some areas have lesser surface age and were apparently more recently dis- turbed or covered by regolith. A small center of mass offset from the center of figure suggests regionally nonuniform regolith thickness or internal density variation. Blocks have a nonuniform distribution consistent with emplacement of ejecta from the youngest large crater. -
Cometary Micrometeorites and Input of Prebiotic Compounds
BIO Web of Conferences 2, 03003 (2014) DOI: 10.1051/bioconf/20140203003 C Owned by the authors, published by EDP Sciences, 2014 Cometary micrometeorites and input of prebiotic compounds C. Engrand1 1CSNSM CNRS/IN2P3-Univ. Paris Sud, Bat. 104, 91405 Orsay Campus, France Abstract. The apparition of life on the early Earth was probably favored by inputs of extraterrestrial matter brought by carbonaceous chondrite-like objects or cometary material. Interplanetary dust collected nowadays on Earth is related to carbonaceous chondrites and to cometary material. They contain in particular at least a few percent of organic matter, organic compounds (amino-acids, PAHs,…), hydrous silicates, and could have largely contributed to the budget of prebiotic matter on Earth, about 4 Ga ago. A new population of cometary dust was recently discovered in the Concordia Antarctic micrometeorite collection. These "Ultracarbonaceous Antarctic Micro- meteorites" (UCAMMs) are dominated by deuterium-rich and nitrogen-rich organic matter. They seem related to the "CHON" grains identified in the comet Halley in 1986. Although rare in the micrometeorites flux (<5% of the micrometeorites), UCAMMs could have significantly contributed to the input of prebiotic matter. Their content in soluble organic matter is currently under study. 1 Introduction Interplanetary dust originating from asteroids and comets could have contributed to the origin of life on Earth [e.g.1; 2 and references therein]. They could have brought prebiotic material that was used to favor the origin of life on Earth. Cosmic dust also seeded other planetary bodies where life could have emerged as well, such as Mars, Titan, Europa or Enceladus… The origin of interplanetary dust is dual, from asteroids and comets [e.g. -
Science Concept 7: the Moon Is a Natural Laboratory for Regolith Processes and Weathering on Anhydrous Airless Bodies
Science Concept 7: The Moon is a Natural Laboratory for Regolith Processes and Weathering on Anhydrous Airless Bodies Science Concept 7: The Moon is a natural laboratory for regolith processes and weathering on anhydrous airless bodies Science Goals: a. Search for and characterize ancient regolith. b. Determine the physical properties of the regolith at diverse locations of expected human activity. c. Understand regolith modification processes (including space weathering), particularly deposition of volatile materials. d. Separate and study rare materials in the lunar regolith. INTRODUCTION The Moon is unmodified by processes that have changed other terrestrial planets, including Mars, and thus offers a pristine history of evolution of the terrestrial planets. Though Mars demonstrates the evolution of a warm, wet planet, water is an erosive substance that can erase a planet‘s geological history. The Moon, on the other hand, is anhydrous. It has never had liquid water on its surface. The Moon is also airless, as opposed to the Venus, the Earth, and Mars. An atmosphere, too, is a weathering component that can distort a planet‘s geologic history. Thus, the Moon offers a pristine history of the evolution of terrestrial planets that can increase our understanding of the formation of all rocky bodies, including the Earth. Additionally, the Moon offers many resources that can be exploited, from metals like iron and titanium to implanted volatiles like hydrogen and helium. There is evidence for water at the poles in permanently shadowed regions (PSRs) (Nozette et al., 1996). Such volatiles could not only support human exploration and habitation on the Moon, but they could also be the constituents for fuel or fuel cells to propel explorers to farther reaches of the Solar System (NRC, 2007).