Earth's Phosphides in Levant and Insights Into the Source of Archean
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Podiform Chromite Deposits—Database and Grade and Tonnage Models
Podiform Chromite Deposits—Database and Grade and Tonnage Models Scientific Investigations Report 2012–5157 U.S. Department of the Interior U.S. Geological Survey COVER View of the abandoned Chrome Concentrating Company mill, opened in 1917, near the No. 5 chromite mine in Del Puerto Canyon, Stanislaus County, California (USGS photograph by Dan Mosier, 1972). Insets show (upper right) specimen of massive chromite ore from the Pillikin mine, El Dorado County, California, and (lower left) specimen showing disseminated layers of chromite in dunite from the No. 5 mine, Stanislaus County, California (USGS photographs by Dan Mosier, 2012). Podiform Chromite Deposits—Database and Grade and Tonnage Models By Dan L. Mosier, Donald A. Singer, Barry C. Moring, and John P. Galloway Scientific Investigations Report 2012-5157 U.S. Department of the Interior U.S. Geological Survey U.S. Department of the Interior KEN SALAZAR, Secretary U.S. Geological Survey Marcia K. McNutt, Director U.S. Geological Survey, Reston, Virginia: 2012 This report and any updates to it are available online at: http://pubs.usgs.gov/sir/2012/5157/ For more information on the USGS—the Federal source for science about the Earth, its natural and living resources, natural hazards, and the environment—visit http://www.usgs.gov or call 1–888–ASK–USGS For an overview of USGS information products, including maps, imagery, and publications, visit http://www.usgs.gov/pubprod To order this and other USGS information products, visit http://store.usgs.gov Suggested citation: Mosier, D.L., Singer, D.A., Moring, B.C., and Galloway, J.P., 2012, Podiform chromite deposits—database and grade and tonnage models: U.S. -
Handbook of Iron Meteorites, Volume 3
Sierra Blanca - Sierra Gorda 1119 ing that created an incipient recrystallization and a few COLLECTIONS other anomalous features in Sierra Blanca. Washington (17 .3 kg), Ferry Building, San Francisco (about 7 kg), Chicago (550 g), New York (315 g), Ann Arbor (165 g). The original mass evidently weighed at least Sierra Gorda, Antofagasta, Chile 26 kg. 22°54's, 69°21 'w Hexahedrite, H. Single crystal larger than 14 em. Decorated Neu DESCRIPTION mann bands. HV 205± 15. According to Roy S. Clarke (personal communication) Group IIA . 5.48% Ni, 0.5 3% Co, 0.23% P, 61 ppm Ga, 170 ppm Ge, the main mass now weighs 16.3 kg and measures 22 x 15 x 43 ppm Ir. 13 em. A large end piece of 7 kg and several slices have been removed, leaving a cut surface of 17 x 10 em. The mass has HISTORY a relatively smooth domed surface (22 x 15 em) overlying a A mass was found at the coordinates given above, on concave surface with irregular depressions, from a few em the railway between Calama and Antofagasta, close to to 8 em in length. There is a series of what appears to be Sierra Gorda, the location of a silver mine (E.P. Henderson chisel marks around the center of the domed surface over 1939; as quoted by Hey 1966: 448). Henderson (1941a) an area of 6 x 7 em. Other small areas on the edges of the gave slightly different coordinates and an analysis; but since specimen could also be the result of hammering; but the he assumed Sierra Gorda to be just another of the North damage is only superficial, and artificial reheating has not Chilean hexahedrites, no further description was given. -
New Major and Trace Element Data from Acapulcoite-Lodranite Clan
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1307.pdf New Major and Trace Element Data from Acapulcoite-Lodranite Clan Meteorites: Evidence for Melt-Rock Reaction Events and Early Collisional Fragmentation of the Parent Body Michael P. Lucas1, Nick Dygert1, Nathaniel R. Miller2, and Harry Y. McSween1, 1Department of Earth & Planetary Sciences, University of Tennessee, Knoxville, [email protected], 2Department of Geological Sciences, Univer- sity of Texas at Austin. Introduction: New major and trace element data illumi- patterns exhibit negative Eu anomalies. REE patterns are nate the magmatic and thermal evolution of the acapul- generally consistent among the three groups, however coite-lodranite parent body (ALPB). We observe major comparison of calculated equilibrium melts for acapulco- and trace element disequilibrium in the acapulcoite and ite and transitional cpx and opx demonstrates disequilib- transitional groups that provide evidence for melt infil- rium partitioning in those samples, especially for light- tration and melt-rock reaction processes. In lodranites, REEs in cpx. In contrast, lodranites are in apparent trace which represent sources of the infiltrating melts, we ob- element equilibrium (Fig 1b). They are depleted in serve rapid cooling from high temperatures (hereafter REE+Y relative to acapulcoite-transitional samples in temps), consistent with collisional fragmentation of the cpx (Fig. 1a), and display consistent REE abundances parent body during differentiation. except NWA 5488, which -
Hf–W Thermochronometry: II. Accretion and Thermal History of the Acapulcoite–Lodranite Parent Body
Earth and Planetary Science Letters 284 (2009) 168–178 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl Hf–W thermochronometry: II. Accretion and thermal history of the acapulcoite–lodranite parent body Mathieu Touboul a,⁎, Thorsten Kleine a, Bernard Bourdon a, James A. Van Orman b, Colin Maden a, Jutta Zipfel c a Institute of Isotope Geochemistry and Mineral Resources, ETH Zurich, Clausiusstrasse 25, 8092 Zurich, Switzerland b Department of Geological Sciences, Case Western Reserve University, Cleveland, OH, USA c Forschungsinstitut und Naturmuseum Senckenberg, Frankfurt am Main, Germany article info abstract Article history: Acapulcoites and lodranites are highly metamorphosed to partially molten meteorites with mineral and bulk Received 11 November 2008 compositions similar to those of ordinary chondrites. These properties place the acapulcoites and lodranites Received in revised form 8 April 2009 between the unmelted chondrites and the differentiated meteorites and as such acapulcoites–lodranites are Accepted 9 April 2009 of special interest for understanding the initial stages of asteroid differentiation as well as the role of 26Al Available online 3 June 2009 heating in the thermal history of asteroids. To constrain the accretion timescale and thermal history of the Editor: R.W. Carlson acapulcoite–lodranite parent body, and to compare these results to the thermal histories of other meteorite parent bodies, the Hf–W system was applied to several acapulcoites and lodranites. Acapulcoites Dhofar 125 Keywords: – Δ chronology and NWA 2775 and lodranite NWA 2627 have indistinguishable Hf W ages of tCAI =5.2±0.9 Ma and Δ isochron tCAI =5.7±1.0 Ma, corresponding to absolute ages of 4563.1±0.8 Ma and 4562.6±0.9 Ma. -
Chromite Crystal Structure and Chemistry Applied As an Exploration Tool
Western University Scholarship@Western Electronic Thesis and Dissertation Repository February 2015 Chromite Crystal Structure and Chemistry applied as an Exploration Tool Patrick H.M. Shepherd The University of Western Ontario Supervisor Dr. Roberta L. Flemming The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Patrick H.M. Shepherd 2015 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geology Commons Recommended Citation Shepherd, Patrick H.M., "Chromite Crystal Structure and Chemistry applied as an Exploration Tool" (2015). Electronic Thesis and Dissertation Repository. 2685. https://ir.lib.uwo.ca/etd/2685 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Western University Scholarship@Western University of Western Ontario - Electronic Thesis and Dissertation Repository Chromite Crystal Structure and Chemistry Applied as an Exploration Tool Patrick H.M. Shepherd Supervisor Roberta Flemming The University of Western Ontario Follow this and additional works at: http://ir.lib.uwo.ca/etd Part of the Geology Commons This Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in University of Western Ontario - Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Chromite Crystal Structure and Chemistry Applied as an Exploration Tool (Thesis format: Integrated Article) by Patrick H.M. -
NEW MINEI{AL NAMES Mrcuanr, Frbrscnun Fersilicite, Ferdisilicite L
TFIE AMI'RICAN MINERALOGIST, VOL 54, NOVEMBER DECEMBER, 1969 NEW MINEI{AL NAMES Mrcuanr, FrBrscnun Fersilicite,Ferdisilicite V. Kn. Gnvoar'ven (1969) The occurrence of natural ferrosilicon in the northern Azov region. Dokl. Ahad. Nauh.S.S.SR,185, 4lG+18 (in Russian). V. Ku. Grvonx'veN, A. L. Lrrvrw, .qNo A. S. Povannnny<u (1969) Occurrence of the new minerals fersilicite and ferdisilicate. Geol.Zh. (Lrkraine) 29 No.2,62-71 (in Russian). In placers and in drill-core samples of sandstones of the Poltava series near Zachativsk station, Donets region, fragments 0.1 to 3 mm in size were found of material with strong steely luster, although many of the grains are covered by a dark gray opaque film. Chemical 'I'ananaev analysesby N V. of fractions of size )1 mm and 0.25-0.5 mm gave, resp.; Fe 52.09,50.51; Si 43 25, 41.45;TiOz 0.05,0.55; AI2OB1.30, 2.70; MnO 0.65,2.56; MgO 0.18, O.32;CaO 092,0.42; Na2Onot detd., 0.15; K:O not detd.,0.01;NiO 0.30,not detd., sum 98.74 (given as99.74),98.67 (given as 10O.67a/).Spectrographic analyses by E. S. Nazare- vich showed also Co 0.06, 0 06; V 0.003, 0.003, Cr 0.2, 0 03; Zr 0.O03(?), 0.0a; Cu 0.6, 0.3; 2nO.01,0.02; Sn 0.02,0.027a.The analysescorrespond approximately to I'e2SL. Optical and X-ray data showed that the material consists of two distinct phases, a cubic phase with o 4.48*0.012 A corresponding to synthetic FeSi, and a tetragonal phase with a 2 69+0.012, c 5.08+ 0.02 A, correspondingto synthetic FeSi2 The cubic phase, named {ersilicate, has strongest lines 3.143 (5)(110), 2.566 (5)(111), l.ee1(10)(210), r.8r7 (9)(211), 1.347 (s)(311), 1.196 (10)(321), r.lre (s)(400),1.028 (e) (331), 0.978 (9)(421). -
Chondrule Sizes, We Have Compiled and Provide Commentary on Available Chondrule Dimension Literature Data
Invited review Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups. Jon M. Friedricha,b,*, Michael K. Weisbergb,c,d, Denton S. Ebelb,d,e, Alison E. Biltzf, Bernadette M. Corbettf, Ivan V. Iotzovf, Wajiha S. Khanf, Matthew D. Wolmanf a Department of Chemistry, Fordham University, Bronx, NY 10458 USA b Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024 USA c Department of Physical Sciences, Kingsborough College of the City University of New York, Brooklyn, NY 11235, USA d Graduate Center of the City University of New York, 365 5th Ave, New York, NY 10016 USA e Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York 10964 USA f Fordham College at Rose Hill, Fordham University, Bronx, NY 10458 USA In press in Chemie der Erde – Geochemistry 21 August 2014 *Corresponding Author. Tel: +718 817 4446; fax: +718 817 4432. E-mail address: [email protected] 2 ABSTRACT The examination of the physical properties of chondrules has generally received less emphasis than other properties of meteorites such as their mineralogy, petrology, and chemical and isotopic compositions. Among the various physical properties of chondrules, chondrule size is especially important for the classification of chondrites into chemical groups, since each chemical group possesses a distinct size-frequency distribution of chondrules. Knowledge of the physical properties of chondrules is also vital for the development of astrophysical models for chondrule formation, and for understanding how to utilize asteroidal resources in space exploration. To examine our current knowledge of chondrule sizes, we have compiled and provide commentary on available chondrule dimension literature data. -
Handbook of Iron Meteorites, Volume 2 (Canyon Diablo, Part 2)
Canyon Diablo 395 The primary structure is as before. However, the kamacite has been briefly reheated above 600° C and has recrystallized throughout the sample. The new grains are unequilibrated, serrated and have hardnesses of 145-210. The previous Neumann bands are still plainly visible , and so are the old subboundaries because the original precipitates delineate their locations. The schreibersite and cohenite crystals are still monocrystalline, and there are no reaction rims around them. The troilite is micromelted , usually to a somewhat larger extent than is present in I-III. Severe shear zones, 100-200 J1 wide , cross the entire specimens. They are wavy, fan out, coalesce again , and may displace taenite, plessite and minerals several millimeters. The present exterior surfaces of the slugs and wedge-shaped masses have no doubt been produced in a similar fashion by shear-rupture and have later become corroded. Figure 469. Canyon Diablo (Copenhagen no. 18463). Shock The taenite rims and lamellae are dirty-brownish, with annealed stage VI . Typical matte structure, with some co henite crystals to the right. Etched. Scale bar 2 mm. low hardnesses, 160-200, due to annealing. In crossed Nicols the taenite displays an unusual sheen from many small crystals, each 5-10 J1 across. This kind of material is believed to represent shock annealed fragments of the impacting main body. Since the fragments have not had a very long flight through the atmosphere, well developed fusion crusts and heat-affected rim zones are not expected to be present. The energy responsible for bulk reheating of the small masses to about 600° C is believed to have come from the conversion of kinetic to heat energy during the impact and fragmentation. -
A Fundamental Evaluation of the Atmospheric Pre-Leaching Section of the Nickel-Copper Matte Treatment Process
A FUNDAMENTAL EVALUATION OF THE ATMOSPHERIC PRE-LEACHING SECTION OF THE NICKEL-COPPER MATTE TREATMENT PROCESS by RODRICK MULENGA LAMYA Dissertation presented for the Degree of DOCTOR OF PHILOSOPHY (Extractive Metallurgical Engineering) in the Department of Process Engineering at the University of Stellenbosch, South Africa Promoter Prof. L. Lorenzen STELLENBOSCH March 2007 DECLARATION I the undersigned, hereby declare that the work contained in this dissertation is my own original work and that I have not previously in its entirety or in part submitted it at any university for a degree. Signature: ............................................... Date: ....................................................... Copyright © 2007 Stellenbosch University All rights reserved i SYNOPSIS Nickel-Copper sulphide ores are the most important Platinum Group Metal bearing ores. The South African deposits are exceptionally rich in the platinum group metals (PGMs) and production of the PGMs is the primary purpose of treating these ores. The methods used in the recovery of the PGMs from the nickel-copper ores generally consists of ore concentration by physical techniques, pyrometallurgical concentration and hydrometallurgical extraction of the base metals followed by the PGMs. Pyrometallurgical concentration produces Ni-Cu matte, which is treated by hydrometallurgical processes to recover the nickel, copper, cobalt and the precious metals. In this study, the leaching behaviour of a Ni–Cu matte in CuSO4–H2SO4 solution during the repulping (pre-leach) stage at Impala Platinum Refineries was studied. The repulping stage is basically a non–oxidative atmospheric leach stage, in which nickel, iron and cobalt are partially dissolved, while the copper is precipitated. To understand the nature of the leaching process during this stage of the base metal refining operation, the effects of variations in the key process variables such as temperature, stirring rate, particle size, pulp density, residence time, initial copper and acid concentrations were investigated. -
Petrogenesis of Acapulcoites and Lodranites: a Shock-Melting Model
Geochimica et Cosmochimica Acta 71 (2007) 2383–2401 www.elsevier.com/locate/gca Petrogenesis of acapulcoites and lodranites: A shock-melting model Alan E. Rubin * Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095-1567, USA Received 31 May 2006; accepted in revised form 20 February 2007; available online 23 February 2007 Abstract Acapulcoites are modeled as having formed by shock melting CR-like carbonaceous chondrite precursors; the degree of melting of some acapulcoites was low enough to allow the preservation of 3–6 vol % relict chondrules. Shock effects in aca- pulcoites include veins of metallic Fe–Ni and troilite, polycrystalline kamacite, fine-grained metal–troilite assemblages, metal- lic Cu, and irregularly shaped troilite grains within metallic Fe–Ni. While at elevated temperatures, acapulcoites experienced appreciable reduction. Because graphite is present in some acapulcoites and lodranites, it seems likely that carbon was the principal reducing agent. Reduction is responsible for the low contents of olivine Fa (4–14 mol %) and low-Ca pyroxene Fs (3–13 mol %) in the acapulcoites, the observation that, in more than two-thirds of the acapulcoites, the Fa value is lower than the Fs value (in contrast to the case for equilibrated ordinary chondrites), the low FeO/MnO ratios in acapulcoite olivine (16–18, compared to 32–38 in equilibrated H chondrites), the relatively high modal orthopyroxene/olivine ratios (e.g., 1.7 in Monument Draw compared to 0.74 in H chondrites), and reverse zoning in some mafic silicate grains. Lodranites formed in a similar manner to acapulcoites but suffered more extensive heating, loss of plagioclase, and loss of an Fe–Ni–S melt. -
Nickel Minerals from Barberton, South Africa: I
American Mineralogist, Volume 58, pages 733-735, 1973 NickelMinerals from Barberton,South Africa: Vl. Liebenbergite,A NickelOlivine SvsneNoA. nn Wnar Nationnl Institute lor Metallurgy, I Yale Road.,Milner Park, I ohannesburg,South Alrica Lnwrs C. ClI.x Il. S. GeologicalSuruey, 345 Middlefield Road, Menlo Park, California 94025 Abstract Liebenbergite, a nickel olivine from the mineral assemblage trevorite-liebenbergite-nickel serpentine-nickel ludwigite-bunsenite-violarite-millerite-gaspeite-nimite, is described mineral- ogically.Ithasa-1.820,P-1.854,7-1.888,ZVa-88",specificgravity-4'60,Mohs hardness- 6 to 6.5, a - 4.727, b - 10.191,c = 5.955A, and Z - 4. X-ray powder data (48 lines) were indexed according to the space grottp Pbnm. The mean chemical composi- tion, calculated from electron microprobe analyses of eight separate liebenbergite grains, gives the mineral formula: (NL eMgoaCoo,sFeo o)Sio "nOn The name is for W. R. Liebenberg, Deputy Director-General of the National Institute for Metallurgy, South Africa. Introduction mission on New Minerals and Mineral Names (rMA). A re-investigationof the trevorite deposit at Bon Accord in the Barberton Mountain Land, South Experimental Methods Africa, led to the discovery of two peculiar but distinct nickel mineral assemblages.Minerals from The refractive indices were determined by the the assemblagewillemseite-nimite-feroan trevorite- conventional liquid immersion method using a reevesite-millerite-violarite-goethitehave been de- sodium lamp as light source.The optical and crystal scribed in earlier papers in this series (de Waal, morphologicalparameters were studiedwith the aid 1969, l97oa, 1970b;de Waal and Viljoen, I97L). of a universal stage. -
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.