DOCSLIB.ORG

Handbook of Iron Meteorites, Volume 2 (Cape of Good Hope

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Handbook of Iron Meteorites, Volume 2 (Cape of Good Hope Canyon Diablo (Schertz) - Cape of Good Hope 407 lost except one piece of some lW kg (175 pounds), which was adventurer Carl Sternberg, from whom Dankelmann relocated in Yorktown, Texas. acquired a fragment of 84 kg on behalf of the Dutch The collector responsible for the shipment was a Mr. Haberle who government. Sternberg told that he had found the mass was employed by a railroad company and assisted in the construction of water tanks on the line to California. He had himself in 1793 about five miles from the coast between evidently acquired the numerous samples, estimated to consist of two small rivers , Karega and Gasoga. Although Dankelmann five or six large masses and a large number of smaller ones, shortly assumed these to be nonexistent, they may be located on after Foote (1891) had announced the discovery and initiated the systematic search for samples around Meteor Crater. Mr. Haberle Barrow's map (1801: volume 1) as Kareeka and Kasowka, was, however, less successful than Foote in transforming the about 7 50 km straight east of Cape of Good Hope, near the meteorites into money since he was unable to sell them, and they present-day Port Alfred. Dankelmann did not believe were finally abandoned in a storage building which was later demolished. Sternberg's story and discovered later by actual travel and inquiry in the region that the mass had been found by a farmer, Royen, long before 1793, farther west, but still Canyon Diablo (Wickenburg), about 700 km east of Cape of Good Hope. The locality was Arizona, U.S.A. on a plain northeast of Swartkops River between Sondags and Boesmans Rivers. Since this version of the find appears 33 °58'N, ll2°44'W to be the most plausible, the corresponding coordinates are given above. Royen's father had from time to time A mass of 250 g was preliminarily listed as Wickenburg by A.D. dislodged fragments from the mass and forged hoes and Nininger (1940) and Nininger & Nininger (1950). The size, shape and structure suggested, however , that the Wickenburg mass was a plowshares, and the family regretted very much that they transported sample from the vicinity of Meteor Crater. This was had disposed of their iron lump, since iron was difficult to confirmed by Wasson (1968) who reported 7.07% Ni, 82.6 ppm Ga, acquire. 321 ppm Ge and 1.8 ppm Ir, values which are identical to Canyon Diablo, within analytical and sampling error. While 84 kg arrived in Haarlem in 1803 and was described as meteoritic by Marum (1804), another large COLLECTIONS fragment came to London where Tennant (1806) London (50 g), Tempe (47 g). The 1.5 kg sample listed confirmed its meteoritic nature by finding 10% Ni in an by Hey (1966: 519) as being in Chicago is a specimen of analysis. The mass proved to be malleable and very ductile the chondrite Wickenburg (stone). so that James Sowerby in 1814 was able to forge a slightly curved sword, 60 em long and 3.5 em wide , from it. The sword was presented to Czar Alexander in gratitude for Cape of Good Hope, Russia's stand against Napoleon. ''The blade has been Cape Province, South Africa hammered at a red heat, without admixture, out of a single piece of this iron, an inch thick, ground and polished. Its Approximately 33% 0 S, 26°E spring was given it by hammering when cold. The haft was lengthened by welding on a small piece of steel. It was Nickel-rich ataxite, D. Duplex a + 'Y with broad twins and a few 30 J.l wide a-spindles. HV 244±8. found to work very pleasantly, the whole operation taking about ten hours." (Sowerby 1820). An attempt in 1937 to Group !VB . 16.32% Ni, 0.84% Co, 0.12% P, 0.20 ppm Ga, 0.06 ppm Ge, 36 ppm Jr. trace the whereabouts of this sword resulted in a negative reply from Dr. J. Astapowitsch, of the Sternberg HISTORY Astronomical Institute of Moscow (Khan: 1944). In the A mass of about 300 pounds (135 kg) was found in the British Museum , however, a few specimens (no. 15143; Dutch Cape Colony on a plain east of the Great Fish River no . 193 5, 4 7) of forged material from Sower by's experi­ close enough to the coast so that it was assumed to be part ments are still preserved. of a ship's anchor carried away by the Kaffers (Barrow Stromeyer (1817) found cobalt in the iron, and 1801 : 225-26). According to Dankelmann (1805) the mass Chladni (1819 : 317; 331-33) reviewed the older literature. had been transported to Capetown by the soldier- In the nineteenth century, Cape of Good Hope was CAPE OF GOOD HOPE - SELECTED CHEMICAL ANALYSES percentage ppm References Ni Co p I c s Cr Cu Zn Ga Ge Ir Pt Wohler in Rose 1864a 16.22 0.73 0.15 Fahrenhorst in Cohen 1900a; l905 15.67 0.95 o.o9 I 3oo 400 300 Goldberg et a!. 1951 16.48 0.43 Nichiporuk & Brown 1965 8.5 11.8 Schaudy eta!. 1972 16.92 0.198 0.059 36 408 Cape of Good Hope Figure 489. Cape of Good Hope (U .S.N .M. no. 985). An etched slice which exhibits the characteristic diffuse streaks of the group !VB ataxites. The streaks are parallel, and often thin out over a length of several centimeters. The dark spotted appearance at top is due to terrestrial corrosion. Etched. Scale bar 10 mm. S.I . neg. M-1369. Figure 490. Cape of Good Hope (U.S.N .M. no. 985). A kamacite spindle with its case of cloudy taenite. Unresolvable transition zones lead to a duplex a + 'Y matrix of the kind which Perry called examined by numerous other workers, among whom Rose "paraeutectoid." Etched. Scale bar 40 p. (Perry 1944: plate 22.) (1864a: 70, plate 3) and Baumhauer (1867: 3 figures) gave important information. The significant mass of 66.2 kg in Etched sections display a dull, fine-grained structure Baumhauer's private collection was, after his death, which is resolvable with a 45x objective. When larger purchased by B. Sturtz in Bonn (Sturtz 1890), together sections are available, it is observed macroscopically that with numerous other meteorites and minerals. The mass the structure is composed of parallel, 1-30 mm wide bands was later acquired for the Hungarian National Collection which reflect the light differently . Only one section is (Tokody&Dudich 1951: 66;Ravasz 1969 : 22). known to the author (Vienna, a 500 g specimen) that shows Cohen (1900a) gave an extensive summary of previous two intersecting sets of parallel bands. A close examination work and added several observations and a new analysis. of the various bands shows that they consist of an ultrafine, Brezina (1896) printed a picture, and Berwerth (1918) gave rhythmic aggregate of Q and 'Y particles elongated parallel to two photomicrographs. Further . structural pictures were the bands visible to the naked eye. The irregular, vermicular presented by Vogel (1928) and Perry (1944: plate 22). taenite particles are generally 0.5-2 J1. wide, and separated Owen & Burns (1939) determined the lattice parameter of by somewhat broader, winding channels of kamacite. The the Q-phase as 2.8630A but found the ')'-phase diffuse. Reed structure, which is more fine-grained than in Kokomo, is (1965b) found an average concentration of 17% Ni in the perhaps best observed in the corroded rim zones where the fine plessite. Schultz & Hintenberger (1967) measured the taenite phase is distinctly yellow on a background of concentrations of noble gases, and Voshage (1967) found a purplish-gray oxides originating from selectively corroded cosmic ray exposure age of 630±70 million years. kamacite. In the optical microscope no structural difference between "dull" and "bright" bands can be observed; COLLECI'IONS Baumhauer (1867) had already found that their chemical Budapest (66 kg+ two slices : 900 g), Vienna (947 g), composition was the same. Also the hardness is the same, Berlin (744 g), London (318 g), Paris (230 g) , Washington within experimental error, being 244±8. The author is (207 g), Gottingen (205 g), Amherst (200 g) , Chicago inclined to think that the bands are parts of the original (196 g), New York (119 g), Harvard (101 g), Stockholm austenite monocrystal that were in twin position and (88 g), Bonn (86 g), Rome (69 g), Tempe (64 g), Ann which, therefore , now possess slightly different orientations Arbor (59 g), Cape Town (55 g), Strasbourg (48 g), of the Q and 'Y grains from band to band. However, since Ti.ibingen (47 g), Ottawa (36 g), Calcutta (26 g), Oslo (13 g, the grains are so fine-grained , this hypothesis is difficult to worked), Chicago (12 g). prove for Cape of Good Hope. DESCRIPTION A few kamacite spindles, typically 30 x 300 JJ., occur The mass received by van Marum ( 1804) was a scattered through the matrix. They have 3-5 J1. wide, flattened fragment of 84 kg with the dimensions 64 x 41 x yellowish taenite rims that gradually merge with the (9-12) em. It was corroded and covered by rounded surrounding plessite. Some of the spindles have tiny cavities, 4-9 em in diameter and 1-3 em deep, as is well schreibersite nuclei, others have daubreelite or troilite shown in the two lithographs reproduced by Baumhauer nuclei, but many are apparently inclusion-free. However, it (1867). No fusion crust or heat-affected rim zone are is believed that inclusions are present above or below the preserved.
Load more

Recommended publications
  • 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.
    [Show full text]
  • Meteorites on Mars Observed with the Mars Exploration Rovers C
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113, E06S22, doi:10.1029/2007JE002990, 2008 Meteorites on Mars observed with the Mars Exploration Rovers C. Schro¨der,1 D. S. Rodionov,2,3 T. J. McCoy,4 B. L. Jolliff,5 R. Gellert,6 L. R. Nittler,7 W. H. Farrand,8 J. R. Johnson,9 S. W. Ruff,10 J. W. Ashley,10 D. W. Mittlefehldt,1 K. E. Herkenhoff,9 I. Fleischer,2 A. F. C. Haldemann,11 G. Klingelho¨fer,2 D. W. Ming,1 R. V. Morris,1 P. A. de Souza Jr.,12 S. W. Squyres,13 C. Weitz,14 A. S. Yen,15 J. Zipfel,16 and T. Economou17 Received 14 August 2007; revised 9 November 2007; accepted 21 December 2007; published 18 April 2008. [1] Reduced weathering rates due to the lack of liquid water and significantly greater typical surface ages should result in a higher density of meteorites on the surface of Mars compared to Earth. Several meteorites were identified among the rocks investigated during Opportunity’s traverse across the sandy Meridiani plains. Heat Shield Rock is a IAB iron meteorite and has been officially recognized as ‘‘Meridiani Planum.’’ Barberton is olivine-rich and contains metallic Fe in the form of kamacite, suggesting a meteoritic origin. It is chemically most consistent with a mesosiderite silicate clast. Santa Catarina is a brecciated rock with a chemical and mineralogical composition similar to Barberton. Barberton, Santa Catarina, and cobbles adjacent to Santa Catarina may be part of a strewn field. Spirit observed two probable iron meteorites from its Winter Haven location in the Columbia Hills in Gusev Crater.
    [Show full text]
  • A New Sulfide Mineral (Mncr2s4) from the Social Circle IVA Iron Meteorite
    American Mineralogist, Volume 101, pages 1217–1221, 2016 Joegoldsteinite: A new sulfide mineral (MnCr2S4) from the Social Circle IVA iron meteorite Junko Isa1,*, Chi Ma2,*, and Alan E. Rubin1,3 1Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, California 90095, U.S.A. 2Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, U.S.A. 3Institute of Geophysics and Planetary Physics, University of California, Los Angeles, California 90095, U.S.A. Abstract Joegoldsteinite, a new sulfide mineral of end-member formula MnCr2S4, was discovered in the 2+ Social Circle IVA iron meteorite. It is a thiospinel, the Mn analog of daubréelite (Fe Cr2S4), and a new member of the linnaeite group. Tiny grains of joegoldsteinite were also identified in the Indarch EH4 enstatite chondrite. The chemical composition of the Social Circle sample determined by electron microprobe is (wt%) S 44.3, Cr 36.2, Mn 15.8, Fe 4.5, Ni 0.09, Cu 0.08, total 101.0, giving rise to an empirical formula of (Mn0.82Fe0.23)Cr1.99S3.95. The crystal structure, determined by electron backscattered diffraction, is aFd 3m spinel-type structure with a = 10.11 Å, V = 1033.4 Å3, and Z = 8. Keywords: Joegoldsteinite, MnCr2S4, new sulfide mineral, thiospinel, Social Circle IVA iron meteorite, Indarch EH4 enstatite chondrite Introduction new mineral by the International Mineralogical Association (IMA 2015-049) in August 2015. It was named in honor of Thiospinels have a general formula of AB2X4 where A is a divalent metal, B is a trivalent metal, and X is a –2 anion, Joseph (Joe) I.
    [Show full text]
  • 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.
    [Show full text]
  • Nonchondritic Meteorites Posters
    Lunar and Planetary Science XXXIX (2008) sess608.pdf Thursday, March 13, 2008 POSTER SESSION II: NONCHONDRITIC METEORITES 6:30 p.m. Fitness Center Greenwood R. C. Franchi I. A. Gibson J. M. How Useful are High-Precision Δ 17O Data in Defining the Asteroidal Sources of Meteorites?: Evidence from Main-Group Pallasites, Primitive and Differentiated Achondrites [#2445] High-precision oxygen isotope analysis is capable of revealing important information about the relationship between different meteorite groups. New data confirm that the main-group pallasites are from a distinct source to either the HEDs or mesosiderites. Dobrica E. Moine B. Poitrasson F. Toplis M. J. Bascou J. Rare Earth Element Insight into the Petrologic Evolution of the Acapulcoite-Lodranite Parent Body [#1327] In this study we present petrological and geochemical constraints on the evolution of the acapulcoite-lodranite (A-L) parent body with emphasis on new rare earth element (REE). Bascou J. Dobrica E. Maurice C. Moine B. Toplis M. J. Texture Analysis in Acapulco and Lodran Achondrites [#1317] EBSD-measured lattice-preferred orientation of minerals of both Acapulco and Lodran achondrites have been analyzed and combined with petrological and geochemical investigations providing new constraints on the melt extraction and migration processes. Rumble D. III Irving A. J. Bunch T. E. Wittke H. J. Kuehner S. M. Oxygen Isotopic and Petrological Diversity Among Brachinites NWA 4872, NWA 4874, NWA 4882 and NWA 4969: How Many Ancient Parent Bodies? [#1974] Brachinites, related ultramafic achondrites and Graves Nunataks 06128 may derive from an incompletely-heated, heterogeneous “planetary” parent body. Petitat M. Kleine T. Touboul M.
    [Show full text]
  • Evolution of Asteroidal Cores 747
    Chabot and Haack: Evolution of Asteroidal Cores 747 Evolution of Asteroidal Cores N. L. Chabot The Johns Hopkins Applied Physics Laboratory H. Haack University of Copenhagen Magmatic iron meteorites provide the opportunity to study the central metallic cores of aster- oid-sized parent bodies. Samples from at least 11, and possibly as many as 60, different cores are currently believed to be present in our meteorite collections. The cores crystallized within 100 m.y. of each other, and the presence of signatures from short-lived isotopes indicates that the crystallization occurred early in the history of the solar system. Cooling rates are generally consistent with a core origin for many of the iron meteorite groups, and the most current cooling rates suggest that cores formed in asteroids with radii of 3–100 km. The physical process of core crystallization in an asteroid-sized body could be quite different than in Earth, with core crystallization probably initiated by dendrites growing deep into the core from the base of the mantle. Utilizing experimental partitioning values, fractional crystallization models have ex- amined possible processes active during the solidification of asteroidal cores, such as dendritic crystallization, assimilation of new material during crystallization, incomplete mixing in the molten core, the onset of liquid immiscibility, and the trapping of melt during crystallization. 1. INTRODUCTION ture of the metal and the presence of secondary minerals, are also considered (Scott and Wasson, 1975). In the first From Mercury to the moons of the outer solar system, attempt to classify iron meteorites, groups I–IV were de- central metallic cores are common in the planetary bodies fined on the basis of their Ga and Ge concentrations.
    [Show full text]
  • Greenland Last Ice Area
    kn Greenland Last Ice Area Potentials for hydrocarbon and mineral resources activities Mette Frost, WWF-DK Copenhagen, September 2014 Report Greenland Last Ice Area. Potentials for hydrocarbon and mineral resources activities. The report is written by Mette Frost, WWF Verdensnaturfonden. Published by WWF Verdensnaturfonden, Svanevej 12, 2400 København NV. Denmark. Phone +45 3536 3635 – E-mail: [email protected] WWF Global Arctic Programme, 275 Slater Street, Ottawa, Ontario, K1P 5L4. Canada. Phone: +1 613 232 2535 Project The report has been developed under the Last Ice Area project, a joint project between WWF Canada, WWF Denmark and WWF Global Arctic Programme. Other WWF reports on Greenland – Last Ice Area Greenland Last Ice Area. Scoping study: socioeconomic and socio-cultural use of the Greenland LIA. By Pelle Tejsner, consultant and PhD. and Mette Frost, WWF-DK. November 2012. Seals in Greenland – an important component of culture and economy. By Eva Garde, WWF-DK. November 2013. Front page photo: Yellow house in Kullorsuaq, Qaasuitsup Kommunia, Greenland. July 2012. Mette Frost, WWF Verdensnaturfonden. The report can be downloaded from www.wwf.dk [1] CONTENTS Last Ice Area Introduction 4 Last Ice Area / Sikuusarfiit Nunngutaat 5 Last Ice Area/ Den Sidste Is 6 Summary 7 Eqikkaaneq 12 Sammenfatning 18 1. Introduction – scenarios for resources development within the Greenland LIA 23 1.1 Last Ice Area 23 1.2 Geology of the Greenland LIA 25 1.3 Climate change 30 2. Mining in a historical setting 32 2.1 Experiences with mining in Greenland 32 2.2 Resources development to the benefit of society 48 3.
    [Show full text]
  • THE Hf-W ISOTOPIC SYSTEM and the ORIGIN of the EARTH and MOON
    18 Mar 2005 11:55 AR AR233-EA33-18.tex XMLPublishSM(2004/02/24) P1: KUV 10.1146/annurev.earth.33.092203.122614 Annu. Rev. Earth Planet. Sci. 2005. 33:531–70 doi: 10.1146/annurev.earth.33.092203.122614 Copyright c 2005 by Annual Reviews. All rights reserved First published online as a Review in Advance on February 1, 2005 THE Hf-W ISOTOPIC SYSTEM AND THE ORIGIN OF THE EARTH AND MOON Stein B. Jacobsen Department of Earth and Planetary Sciences, Harvard University, Cambridge, Massachusetts 02138; email: [email protected] KeyWords accretion, tungsten, isotopes, chronometer, core formation ■ Abstract The Earth has a radiogenic W-isotopic composition compared to chon- drites, demonstrating that it formed while 182Hf (half-life 9 Myr) was extant in Earth and decaying to 182W. This implies that Earth underwent early and rapid accretion and core formation, with most of the accumulation occurring in ∼10 Myr, and concluding approximately 30 Myr after the origin of the Solar System. The Hf-W data for lunar samples can be reconciled with a major Moon-forming impact that terminated the ter- restrial accretion process ∼30 Myr after the origin of the Solar System. The suggestion that the proto-Earth to impactor mass ratio was 7:3 and occurred during accretion is inconsistent with the W isotope data. The W isotope data is satisfactorily modeled with a Mars-sized impactor on proto-Earth (proto-Earth to impactor ratio of 9:1) to form the Moon at ∼30 Myr. 1. INTRODUCTION The process of terrestrial planet-building probably began when a large population of small bodies (planetesimals) of roughly similar size coagulated into a smaller population of larger bodies.
    [Show full text]
  • Texture, Chemical Composition and Genesis of Schreibersite in Iron Meteorite
    Title Texture, Chemical Composition and Genesis of Schreibersite in Iron Meteorite Author(s) Yoshikawa, Masahide; Matsueda, Hiroharu Citation 北海道大学理学部紀要, 23(2), 255-280 Issue Date 1992-08 Doc URL http://hdl.handle.net/2115/36782 Type bulletin (article) File Information 23-2_p255-280.pdf Instructions for use Hokkaido University Collection of Scholarly and Academic Papers : HUSCAP Jour. Fac. Sci ., Hokkaido Univ., Ser. IV, vol. 23, no. 2, Aug., 1992. pp. 255 -280 TEXTURE, CHEMICAL COMPOSITION AND GENESIS OF SCHREIBERSITE IN IRON METEORITE by Masahide Yoshikawa* and Hiroharu Matsueda (with 13 text-figures, 9 tables and 3 plates) Abstract Thirteen iron meteorites composed of Hexahedrite, Octahedrite and Ataxite were investigated to estimate their cooling history and origin. They are mainly composed of Fe-Ni metals (kamacite and taenite) with smaller amounts of schreibersite (Fe, Ni)3P and sulfides (troilite and sphalerite) . Schreibersite occurs an idiomorphic and xenomorphic crystals and its mode of occurrence is variable in iron meteorites. Xenomorphic schreibersite is subdivided into 6 types on the basis of their textures and relationships with coexisting minerals. Chemical composition of schreibersite varies from 20 to 40 atom. % Ni with textural types among some iron meteorites with different bulk chemical compositions and even in the same meteorite (e. g. Canyon Diablo), while it does not vary so clear with textural types in ALH - 77263. Schreibersite seems to maintain a local equilibrium with coexisting metal phases. Based on the Fe- Ni- P phase diagram, it is estimated that xenomorphic and coarse-grained schreibersite in Y- 75031 and in DRPA 7S007 were crystallized from stability field of taenite and schreibersite at about SOO°C under rapid diffusion conditions.
    [Show full text]
  • Thermal Equilibration of Iron Meteorite and Pallasite Parent Bodies Recorded at the Mineral Scale by Fe and Ni Isotope Systematics
    Available online at www.sciencedirect.com ScienceDirect Geochimica et Cosmochimica Acta 217 (2017) 95–111 www.elsevier.com/locate/gca Thermal equilibration of iron meteorite and pallasite parent bodies recorded at the mineral scale by Fe and Ni isotope systematics Stepan M. Chernonozhkin a,b, Mona Weyrauch c, Steven Goderis a,b,⇑, Martin Oeser c, Seann J. McKibbin b, Ingo Horn c, Lutz Hecht d, Stefan Weyer c, Philippe Claeys b, Frank Vanhaecke a a Ghent University, Department of Analytical Chemistry, Campus Sterre, Krijgslaan 281–S12, 9000 Ghent, Belgium b Vrije Universiteit Brussel, Analytical, Environmental, and Geo-Chemistry, Pleinlaan 2, 1050 Brussels, Belgium c Leibniz Universita¨t Hannover, Institute of Mineralogy, Callinstrasse 3, 30167 Hannover, Germany d Museum fu¨r Naturkunde, Leibniz Institute for Evolution and Biodiversity Science, Invalidenstrasse 43, 10115 Berlin, Germany Received 6 January 2017; accepted in revised form 9 August 2017; Available online 19 August 2017 Abstract In this work, a femtosecond laser ablation (LA) system coupled to a multi-collector inductively coupled plasma-mass spec- trometer (fs-LA-MC-ICP-MS) was used to obtain laterally resolved (30–80 lm), high-precision combined Ni and Fe stable isotope ratio data for a variety of mineral phases (olivine, kamacite, taenite, schreibersite and troilite) composing main group pallasites (PMG) and iron meteorites. The stable isotopic signatures of Fe and Ni at the mineral scale, in combination with the factors governing the kinetic or equilibrium isotope fractionation processes, are used to interpret the thermal histories of small differentiated asteroidal bodies. As Fe isotopic zoning is only barely resolvable within the internal precision level of the isotope ratio measurements within a single olivine in Esquel PMG, the isotopically lighter olivine core relative to the rim 56/54 (D Ferim-core = 0.059‰) suggests that the olivines were largely thermally equilibrated.
    [Show full text]
  • Unbroken Meteorite Rough Draft
    Space Visitors in Kentucky: Meteorites and Asteroid “Ida.” Most meteorites originate from asteroids. Meteorite Impact Sites in Kentucky Meteorite from Clark County, Ky. Mercury Earth Saturn Venus Mars Neptune Jupiter William D. Ehmann Asteroid Belt with contributions by Warren H. Anderson Uranus Pluto www.uky.edu/KGS Special thanks to Collie Rulo for cover design. Earth image was compiled from satellite images from NOAA and NASA. Kentucky Geological Survey James C. Cobb, State Geologist and Director University of Kentucky, Lexington Space Visitors in Kentucky: Meteorites and Meteorite Impact Sites in Kentucky William D. Ehmann Special Publication 1 Series XII, 2000 i UNIVERSITY OF KENTUCKY Collie Rulo, Graphic Design Technician Charles T. Wethington Jr., President Luanne Davis, Staff Support Associate II Fitzgerald Bramwell, Vice President for Theola L. Evans, Staff Support Associate I Research and Graduate Studies William A. Briscoe III, Publication Sales Jack Supplee, Director, Administrative Supervisor Affairs, Research and Graduate Studies Roger S. Banks, Account Clerk I KENTUCKY GEOLOGICAL SURVEY Energy and Minerals Section: James A. Drahovzal, Head ADVISORY BOARD Garland R. Dever Jr., Geologist V Henry M. Morgan, Chair, Utica Cortland F. Eble, Geologist V Ron D. Gilkerson, Vice Chair, Lexington Stephen F. Greb, Geologist V William W. Bowdy, Fort Thomas David A. Williams, Geologist V, Manager, Steven Cawood, Frankfort Henderson office Hugh B. Gabbard, Winchester David C. Harris, Geologist IV Kenneth Gibson, Madisonville Brandon C. Nuttall, Geologist IV Mark E. Gormley, Versailles William M. Andrews Jr., Geologist II Rosanne Kruzich, Louisville John B. Hickman, Geologist II William A. Mossbarger, Lexington Ernest E. Thacker, Geologist I Jacqueline Swigart, Louisville Anna E.
    [Show full text]
  • Fersman Mineralogical Museum of the Russian Academy of Sciences (FMM)
    Table 1. The list of meteorites in the collections of the Fersman Mineralogical Museum of the Russian Academy of Sciences (FMM). Leninskiy prospect 18 korpus 2, Moscow, Russia, 119071. Pieces Year Mass in Indication Meteorite Country Type in found FMM in MB FMM Seymchan Russia 1967 Pallasite, PMG 500 kg 9 43 Kunya-Urgench Turkmenistan 1998 H5 402 g 2 83 Sikhote-Alin Russia 1947 Iron, IIAB 1370 g 2 Sayh Al Uhaymir 067 Oman 2000 L5-6 S1-2,W2 63 g 1 85 Ozernoe Russia 1983 L6 75 g 1 66 Gujba Nigeria 1984 Cba 2..8 g 1 85 Dar al Gani 400 Libya 1998 Lunar (anorth) 0.37 g 1 82 Dhofar 935 Oman 2002 H5S3W3 96 g 1 88 Dhofar 007 Oman 1999 Eucrite-cm 31.5 g 1 84 Muonionalusta Sweden 1906 Iron, IVA 561 g 3 Omolon Russia 1967 Pallasite, PMG 1,2 g 1 72 Peekskill USA 1992 H6 1,1 g 1 75 Gibeon Namibia 1836 Iron, IVA 120 g 2 36 Potter USA 1941 L6 103.8g 1 Jiddat Al Harrasis 020 Oman 2000 L6 598 gr 2 85 Canyon Diablo USA 1891 Iron, IAB-MG 329 gr 1 33 Gold Basin USA 1995 LA 101 g 1 82 Campo del Cielo Argentina 1576 Iron, IAB-MG 2550 g 4 36 Dronino Russia 2000 Iron, ungrouped 22 g 1 88 Morasko Poland 1914 Iron, IAB-MG 164 g 1 Jiddat al Harasis 055 Oman 2004 L4-5 132 g 1 88 Tamdakht Morocco 2008 H5 18 gr 1 Holbrook USA 1912 L/LL5 2,9g 1 El Hammami Mauritani 1997 H5 19,8g 1 82 Gao-Guenie Burkina Faso 1960 H5 18.7 g 1 83 Sulagiri India 2008 LL6 2.9g 1 96 Gebel Kamil Egypt 2009 Iron ungrouped 95 g 2 98 Uruacu Brazil 1992 Iron, IAB-MG 330g 1 86 NWA 859 (Taza) NWA 2001 Iron ungrouped 18,9g 1 86 Dhofar 224 Oman 2001 H4 33g 1 86 Kharabali Russia 2001 H5 85g 2 102 Chelyabinsk
    [Show full text]