VARIATIONS in the CHEMICAL COMPOSITION of PENTLANDITE in DIFFERENT ORDINARY CHONDRITES. S. V. Berzin, Yu. V. Erokhin, V. V. Khiller and K
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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. -
Accretion of Water in Carbonaceous Chondrites: Current Evidence and Implications for the Delivery of Water to Early Earth
ACCRETION OF WATER IN CARBONACEOUS CHONDRITES: CURRENT EVIDENCE AND IMPLICATIONS FOR THE DELIVERY OF WATER TO EARLY EARTH Josep M. Trigo-Rodríguez1,2, Albert Rimola3, Safoura Tanbakouei1,3, Victoria Cabedo Soto1,3, and Martin Lee4 1 Institute of Space Sciences (CSIC), Campus UAB, Facultat de Ciències, Torre C5-parell-2ª, 08193 Bellaterra, Barcelona, Catalonia, Spain. E-mail: [email protected] 2 Institut d’Estudis Espacials de Catalunya (IEEC), Edif.. Nexus, c/Gran Capità, 2-4, 08034 Barcelona, Catalonia, Spain 3 Departament de Química, Universitat Autònoma de Barcelona, 08193 Bellaterra, Catalonia, Spain. E-mail: [email protected] 4 School of Geographical and Earth Sciences, University of Glasgow, Gregory Building, Lilybank Gardens, Glasgow G12 8QQ, UK. Manuscript Pages: 37 Tables: 2 Figures: 10 Keywords: comet; asteroid; meteoroid; meteorite; minor bodies; primitive; tensile strength Accepted in Space Science Reviews (SPAC-D-18-00036R3, Vol. Ices in the Solar System) DOI: 10.1007/s11214-019-0583-0 Abstract: Protoplanetary disks are dust-rich structures around young stars. The crystalline and amorphous materials contained within these disks are variably thermally processed and accreted to make bodies of a wide range of sizes and compositions, depending on the heliocentric distance of formation. The chondritic meteorites are fragments of relatively small and undifferentiated bodies, and the minerals that they contain carry chemical signatures providing information about the early environment available for planetesimal formation. A current hot topic of debate is the delivery of volatiles to terrestrial planets, understanding that they were built from planetesimals formed under far more reducing conditions than the primordial carbonaceous chondritic bodies. -
Sulfide/Silicate Melt Partitioning During Enstatite Chondrite Melting
61st Annual Meteoritical Society Meeting 5255.pdf SULFIDE/SILICATE MELT PARTITIONING DURING ENSTATITE CHONDRITE MELTING. C. Floss1, R. A. Fogel2, G. Crozaz1, M. Weisberg2, and M. Prinz2, 1McDonnell Center for the Space Sciences and Department of Earth and Planetary Sciences, Washington University, St. Louis MO 63130, USA ([email protected]), 2American Museum of Natural History, Department of Earth and Planetary Sciences, New York NY 10024, USA. Introduction: Aubrites are igneous rocks thought (present only in CaS-saturated charges) has a flat REE to have formed from an enstatite chondrite-like pattern with abundances of about 0.5 x CI. precursor [1]. Yet their origin remains poorly Discussion: Oldhamite/glass D values are close to understood, at least partly because of confusion over 1 for most REE, consistent with previous results the role played by sulfides, particularly oldhamite. [4,5,6], and significantly lower than those expected CaS in aubrites contains high rare earth element based on REE abundances in aubritic oldhamite. In (REE) abundances and exhibits a variety of patterns contrast, D values for FeS are surprisingly high (from [2] that reflect, to some extent, those seen in about 0.1 to 1), given the low REE abundances of oldhamite from enstatite chondrites [3]. However, natural troilite. FeS/silicate partition coefficients experimental work suggests that CaS/silicate melt reported by [5] are somewhat lower, but exhibit a REE partition coefficients are too low to account for similar pattern. Alkali loss from the charges, the high abundances observed [4,5] and do not explain resulting in Ca-enriched glass, might provide a partial the variable patterns. -
MACKINAWITE from SOUTH AFRICA W. C J. Van RDNSBU*.O, Geological Surtey Oj Soulh Africa, Preloria, Soulh A.[Ri Co, L. Lrbnunsbyc
TI.IE AMERICAN MINERALOGIST, VOL 52, JULY AUGUST, 1967 MACKINAWITE FROM SOUTH AFRICA W. C J. vAN RDNSBU*.o,Geological Surtey oJ Soulh Africa, Preloria,Soulh A.[rico, AND L. LrBnuNsByc, Deparlment of Geology,Llnit:ersity of Pretoria, Pre!oria,Soul h Africa. ABSTRAcT Mackinawite has been identified in mafic and ultramafic rocks of the Bushveld igneous complex and Insizwa and also in the carbonatite and pegmatoid of Loolekop, Phalaborrva complex in South Africa. The mineral occurs predominantly as somewhat irregular to oriented intergrowths in pentlandite in all these occurrences and less commonly as regular oriented lamellae in chalcopyrite and rarely in cubanite. The textural evidence suggests that mackinawite may represent an exsolution product of pentlandite, chalcopyrite and cubanite. INrnonucrroN The iron sulphide, mackinawite was recently named in a paper by Evans, et al, (1964). Natural occurrencesof this mineral f rom Finland were describedby- Kouvo et al (1963)and from the Muskox intrusion in Canada by Chamberlain and Delabio (1965). During the presentinvestigation mackinawite was distinguishedfrom valleriite in the carbonatite and pegmatoid of Loolekop, Phalaborwa complex, in the Bushveld igneous complex, and from Insizwa, Cape Province.The mode of occurrenceof the mackinawite in the carbonatite difiers somewhatfrom that in the mafic rocks of Insizwa and the Bush- veld complex. MrNnn.q.rocv The physicaland optical propertiesof mackinawitefrom the Bushveid complex,Insizwa and Loolekop are very similar and are in closeagree- ment with the propertiesgiven for the same mineral from the Muskox intrusion by Chamberlain and Delabio (1965). The mineral takes a fairly good polish,particularly after buffing with a chromic oxide slurry. -
Minerals and Mineral Products in Our Bedroom Bed Hematite
Minerals and Mineral Products in our Bedroom Make-Up Kit Muscovite Bed Talc Hematite: hinges, handles, Mica mattress springs Hematite: for color Chromite: chrome plating Bismuth Radio Barite Copper: wiring Plastic Pail Quartz: clock Mica Gold: connections Cassiterite: solder Toilet Bowl / Tub Closet Feldspar: porcelain Chromite: chrome plating Pyrolusite: coloring Hematite: hinges, handles (steel) Chromite: plumbing fixtures Quartz : mirror on door Copper: tubing Desk Toothpaste Hematite: hinges, handles (steel) Apatite: teeth Chromite: chrome plating Fluorite: toothpaste Mirror Rutile: to color false Hematite: handle, frame teeth yellow Chromite: plating Gold: fillings Gold: plating Cinnabar: fillings Quartz: mirror Towels Table Lamp Sphalerite: dyes Brass (an alloy of copper and Chromite: dyes zinc): base Quartz: bulb Water Pipe/Faucet/Shower bulb Wolframite: lamp filament Brass Copper: wiring Iron Nickel Minerals and Mineral Products in our Bedroom Chrome: stainless steel Bathroom Cleaner Department of Environment and Natural Resources Borax: abrasive, cleaner, and antiseptic MINES AND GEOSCIENCES BUREAU Deodorant Spray Can Cassiterite Chromite Copper Carpet Quartz Sphalerite: dyes Telephone Chromite: dyes Drinking Glasses Copper: wiring Sulfur: foam padding Quartz Chromite: plating Gold: red color Clock Silver: electronics Pentlandite: spring Graphite: batteries Refrigerator Quartz: glass, time keeper Hematite Television Chromite: stainless steel Chromite: plating Computer Galena Wolframite: monitor Wolframite: monitor Copper Copper: -
Chondrites and Chondrules Analogous to Sediments Dr
Chondrites and Chondrules Analogous to Sediments Dr. Richard K. Herd Curator, National Meteorite Collection, Geological Survey of Canada, Natural Resources Canada (Retired) 51st Annual Lunar and Planetary Science Conference Houston, Texas March 16-20, 2020 Introduction and Summary • Comparing chondrites and terrestrial conglomerates [1] continues • Meteorites are fragmental rocks, continually subjected to impacts and collisions, whatever their ultimate origin in space and time • Space outside Earth’s atmosphere may be considered a 4D debris field • Of the debris that reaches the surface of Earth and is available for study, > 80 % are chondrites • Chondrites and chondrules are generally considered the product of heating of dust in the early Solar System, and therefore effectively igneous in origin • Modelling these abundant and important space rocks as analogous to terrestrial detrital sediments, specifically conglomerates, is innovative, can help derive data on their true origins and history, and provide con text for ongoing analyses Chondrites and Chondrules • Chondrites are rocks made of rocks • They are composed of chondrules and chondrule-like objects from which they take their name • Chondrules are roughly spheroidal pebble-like rocks predominantly composed of olivine, pyroxene, feldspar, iron-nickel minerals, chromite, magnetite, sulphides etc. • They range from nanoscale to more than a centimetre, with some size variation by chondrite type. There are thousands/millions of them available for study • Hundreds of chondrules fill the area of a single 3.5 x 2.5 cm standard thin section What is Known ? • Adjacent chondrules may be millions of years different in age • They date from the time of earliest solar system objects (viz. -
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. -
The Moon After Apollo
ICARUS 25, 495-537 (1975) The Moon after Apollo PAROUK EL-BAZ National Air and Space Museum, Smithsonian Institution, Washington, D.G- 20560 Received September 17, 1974 The Apollo missions have gradually increased our knowledge of the Moon's chemistry, age, and mode of formation of its surface features and materials. Apollo 11 and 12 landings proved that mare materials are volcanic rocks that were derived from deep-seated basaltic melts about 3.7 and 3.2 billion years ago, respec- tively. Later missions provided additional information on lunar mare basalts as well as the older, anorthositic, highland rocks. Data on the chemical make-up of returned samples were extended to larger areas of the Moon by orbiting geo- chemical experiments. These have also mapped inhomogeneities in lunar surface chemistry, including radioactive anomalies on both the near and far sides. Lunar samples and photographs indicate that the moon is a well-preserved museum of ancient impact scars. The crust of the Moon, which was formed about 4.6 billion years ago, was subjected to intensive metamorphism by large impacts. Although bombardment continues to the present day, the rate and size of impact- ing bodies were much greater in the first 0.7 billion years of the Moon's history. The last of the large, circular, multiringed basins occurred about 3.9 billion years ago. These basins, many of which show positive gravity anomalies (mascons), were flooded by volcanic basalts during a period of at least 600 million years. In addition to filling the circular basins, more so on the near side than on the far side, the basalts also covered lowlands and circum-basin troughs. -
Pyrrhotite and Pentlandite in Ll3 to Ll6 Chondrites: Determining Compositional and Microstructural Indicators of Formation Conditions
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2621.pdf PYRRHOTITE AND PENTLANDITE IN LL3 TO LL6 CHONDRITES: DETERMINING COMPOSITIONAL AND MICROSTRUCTURAL INDICATORS OF FORMATION CONDITIONS. D. L. Schrader1 and T. J. Zega2, 1Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State Uni- versity, Tempe, AZ 85287-1404, USA ([email protected]), 2Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721, USA ([email protected]). Introduction: The compositions, textures, and electron microscope (FIB-SEM) at UAz and the JEOL crystal structures of sulfides can be used to constrain JXA-8530F Hyperprobe EPMA at Arizona State Uni- oxygen fugacity, aqueous, thermal, and cooling history versity (ASU). The FIB-SEM was also used to extract [e.g., 1–5]. The most abundant sulfides in extraterres- ~10 × 5 µm sections transecting the pyrrhotite- trial samples are the pyrrhotite group [(Fe,Ni,Co,Cr)1– pentlandite interfaces within sulfide grains from each xS], which can occur with pentlandite [(Fe,Ni,Co,Cr)9– meteorite, which were thinned to electron transparency xS8]. The pyrrhotite group sulfides are largely non- (<100 nm) using methods of [14]. FIB sections were stoichiometric and have a range of compositions then analyzed using the 200 keV aberration-corrected (0<x<0.125) and distinct crystal structures (polytypes). Hitachi HF5000 scanning transmission electron micro- The stoichiometric end members are 2C (troilite; FeS, scope (TEM) at UAz. hexagonal) and 4C (Fe7S8, monoclinic) pyrrhotite. There are also non-integral NC-pyrrhotites with inter- mediate compositions with 0<x<0.125 (all hexagonal); which includes the integral 5C (Fe9S10), 6C (Fe11S12), and 11C (Fe10S11) pyrrhotites [e.g., 6–8]. -
Radar-Enabled Recovery of the Sutter's Mill Meteorite, A
RESEARCH ARTICLES the area (2). One meteorite fell at Sutter’sMill (SM), the gold discovery site that initiated the California Gold Rush. Two months after the fall, Radar-Enabled Recovery of the Sutter’s SM find numbers were assigned to the 77 me- teorites listed in table S3 (3), with a total mass of 943 g. The biggest meteorite is 205 g. Mill Meteorite, a Carbonaceous This is a tiny fraction of the pre-atmospheric mass, based on the kinetic energy derived from Chondrite Regolith Breccia infrasound records. Eyewitnesses reported hearing aloudboomfollowedbyadeeprumble.Infra- Peter Jenniskens,1,2* Marc D. Fries,3 Qing-Zhu Yin,4 Michael Zolensky,5 Alexander N. Krot,6 sound signals (table S2A) at stations I57US and 2 2 7 8 8,9 Scott A. Sandford, Derek Sears, Robert Beauford, Denton S. Ebel, Jon M. Friedrich, I56US of the International Monitoring System 6 4 4 10 Kazuhide Nagashima, Josh Wimpenny, Akane Yamakawa, Kunihiko Nishiizumi, (4), located ~770 and ~1080 km from the source, 11 12 10 13 Yasunori Hamajima, Marc W. Caffee, Kees C. Welten, Matthias Laubenstein, are consistent with stratospherically ducted ar- 14,15 14 14,15 16 Andrew M. Davis, Steven B. Simon, Philipp R. Heck, Edward D. Young, rivals (5). The combined average periods of all 17 18 18 19 20 Issaku E. Kohl, Mark H. Thiemens, Morgan H. Nunn, Takashi Mikouchi, Kenji Hagiya, phase-aligned stacked waveforms at each station 21 22 22 22 23 Kazumasa Ohsumi, Thomas A. Cahill, Jonathan A. Lawton, David Barnes, Andrew Steele, of 7.6 s correspond to a mean source energy of 24 4 24 2 25 Pierre Rochette, Kenneth L. -
Sulfides in Enstate Chondrites
Sulfides in Enstatite Chondrites: Indicators of Impact History Kristyn Hill1,2, Emma Bullock2, Cari Corrigan2, and Timothy McCoy2 1Lock Haven University of Pennsylvania, Lock Haven, PA 17745, USA 2National Museum of Natural History, Department of Mineral Sciences, Washington D.C. 20013, USA Introductton Results Discussion Enstatite chondrites are a class of meteorites. They are Determining the history of the parent body of a referred to as chondrites because of the spherical Impact Melt, Slowly Cooled chondritic meteorite often includes distinguishing whether chondrules found in the matrix of the meteorites. Enstatite aa bb cc d d or not the meteorite was impact melted, and the cooling chondrites are the most highly reduced meteorites and rate. contain iron-nickel metal and sulfide bearing minerals. The Impact melts are distinguishable by the texture of the matrix is made up of silicates, enstatite in particular. There metal and sulfide assemblages. A meteorite that was are usually no oxides found, which supports the idea that impact melted will contain a texture of euhedral to these formed in very oxygen poor environments. The subhedral silicates, like enstatite, protruding into the metal enstatite chondrites in this study are type 3, meaning they or sulfides (figure 2). Some textures will look shattered are unmetamorphosed and not affected by fluids. (figure 2b). Meteorites that contain the mineral keilite are Studying enstatite chondrites will help us determine the PCA 91125 ALHA 77156 PCA 91444 PCA 91085 also an indicator of impact melts (figure 3). Keilite only evolution of their parent bodies which formed at the occurs in enstatite chondrite impact-melt rocks that cooled beginning of our solar system.