Handbook of Iron Meteorites, Volume 2 (Kalkaska
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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. -
Disequilibrium Melting and Melt Migration Driven by Impacts: Implications for Rapid Planetesimal Core Formation
Available online at www.sciencedirect.com Geochimica et Cosmochimica Acta 100 (2013) 41–59 www.elsevier.com/locate/gca Disequilibrium melting and melt migration driven by impacts: Implications for rapid planetesimal core formation Andrew G. Tomkins ⇑, Roberto F. Weinberg, Bruce F. Schaefer 1, Andrew Langendam School of Geosciences, P.O. Box 28E, Monash University, Melbourne, Victoria 3800, Australia Received 20 January 2012; accepted in revised form 24 September 2012; available online 12 October 2012 Abstract The e182W ages of magmatic iron meteorites are largely within error of the oldest solar system particles, apparently requir- ing a mechanism for segregation of metals to the cores of planetesimals within 1.5 million years of initial condensation. Cur- rently favoured models involve equilibrium melting and gravitational segregation in a static, quiescent environment, which requires very high early heat production in small bodies via decay of short-lived radionuclides. However, the rapid accretion needed to do this implies a violent early accretionary history, raising the question of whether attainment of equilibrium is a valid assumption. Since our use of the Hf–W isotopic system is predicated on achievement of chemical equilibrium during core formation, our understanding of the timing of this key early solar system process is dependent on our knowledge of the seg- regation mechanism. Here, we investigate impact-related textures and microstructures in chondritic meteorites, and show that impact-generated deformation promoted separation of liquid FeNi into enlarged sulfide-depleted accumulations, and that this happened under conditions of thermochemical disequilibrium. These observations imply that similar enlarged metal accumu- lations developed as the earliest planetesimals grew by rapid collisional accretion. -
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. -
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. -
Handbook of Iron Meteorites, Volume 3
1350 Yenberrie - York (Iron) Specimens in the U.S. National Museum in Washington: 3.54 kg on three slices (no. 607) 290 g part slice (no. 1626) York (Iron), Nebraska, U.S.A. Approximately 40°52'N, 97°35'W; 500 m Medium octahedrite, Om. Bandwidth 1.00±0.15 mm. E-structure. HV 305 ±15 . Probably group III A. About 7.7% Ni and 0.12% P. HISTORY A mass of 835 g was found in 1878 on the farm of ~ - . Robert M. Lytle, near York in York County. The mass was Figure 2007. Yenberric (U.S.N.M. no. 607). Taenite with cloudy plowed up from a edges and martensitic interior in which cloudy patches occasionally depth of 20 em in virgin, black loamy occur. Part of the explanation may be sought in the taenite lamella prairie soil. It was in the fmder's possession until 1895 being parallel to the plane of section. Etched. Scale bar 200 J.L. See when it was acquired by Barbour (1898) who described it also Figures 109 and 119. and gave figures of the exterior and of etched slices. COLLECfiONS \ New York (701 g), Washington (30 g). \ ANALYSES Kunz reported (in Barbour 1898) 7.38% Ni and 0 .74% Co. The sum appears correct, but the present author would expect that some of the nickel has been included with the cobalt. The meteorite is estimated to have the following composition: 7 .7±0.2% Ni, 0.50% Co, 0.12±0.02% P, with trace elements placing it in the chemical group IliA. -
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. -
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. -
TRACE ELEMENT COMPOSITION and CLASSIFICATION of Ni-RICH ATAXITE ONELLO
81st Annual Meeting of The Meteoritical Society 2018 (LPI Contrib. No. 2067) 6176.pdf TRACE ELEMENT COMPOSITION AND CLASSIFICATION OF Ni-RICH ATAXITE ONELLO. K. D. Litasov1,2, A. Ishikawa3, A. G. Kopylova4, N. M. Podgornykh1, 1Sobolev Institute of Geology and Mineralogy, SB RAS, 3 Koptyuga Ave, Novosibirsk, 630090, Russia ([email protected]); 2Novosibirsk State University, 2 Pirogova st, Novosibirsk 630090, Russia; 3Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo, 152- 8550, Japan; 4Institute of Diamond and Precious Metal Geology, 39 Lenina Ave, Yakutsk, 677980, Russia Introduction: Significant amount of iron meteorites remains poorly described and ungrouped. Some of them re- veal anomalous composition, which do not allow classification to the specific known groups [1]. Here we provide new data on the unique Ni- and P-rich iron meteorite Onello, which contains rare high-pressure phosphide allabogdanite [2]. Onello was found in Yakutia (Russia) in 1997. Preliminary study did not allow its clear classification [3]. Methods: Several 0.5-2 cm fragments of meteorite were cut and polished for investigation by scanning electron microscope (Tescan MYRA 3 LMU) with energy-dispersive system X-Max-80 (Oxford Instr.). Trace elements com- position was obtained by LA-ICP-MS (Thermo Scientific Element XR) method at University of Tokyo (Japan). We used homogenous piece of Campo del Cielo iron and synthetic FeNi-metal [4] as standards. Results and discussion: Onello is fine-grained ataxite with matrix consisting of taenite with 23.0-25.4 wt% Ni. Taenite matrix contains numerous tiny inclusions of schreibersite (22-26 wt% Ni), nickelphosphide (44-52 wt% Ni) and allabogdanite (20.6-21.8 wt% Ni). -
Elastic Properties of Iron Meteorites. Nikolay Dyaur1, Robert R. Stewart1, and Martin Cassidy1, 1University of Houston, Science
51st Lunar and Planetary Science Conference (2020) 3063.pdf Elastic properties of iron meteorites. Nikolay Dyaur1, Robert R. Stewart1, and Martin Cassidy1, 1University of Houston, Science and Research Building 1, 3507 Cullen Boulevard, room 312, Houston, TX 77204, [email protected] Introduction: We investigate the elastic properties of a ture, in the iron meteorites indicates directionality in variety of iron meteorites using ultrasonic (0.5 MHz to 5 physical properties. So, we explored the possibility of MHz) laboratory measurements. Our meteorite samples elastic anisotropy. First, we estimated Vp- and Vs- include Campo de Cielo, Canyon Diablo, Gibeon, and anisotropy from the measured maximum and minimum Nantan. The densities of the meteorites range from 7.15 velocity for each sample. g/cc to 7.85 g/cc. P-wave velocities are from 5.58 km/s to 7.85 km/s, and S-wave velocities are from 2.61 km/s to 3.37 km/s. There is a direct relationship between P-wave velocity and density (approximately quadratic). We find evidence of anisotropy and S-wave splitting in the Gibe- on sample. These measurements may help inform studies related to planetary core properties, asteroid mining, and Earth protection. Iron meteorites are composed of Fe-Ni mixes with Fe content around 90%. The principal minerals are kamacite and taenite with some inclusions mainly repre- sented by troilite, graphite, diamond, gold, quartz, and some others. Iron meteorites are divided into groups based on their structure linked to Ni content: Hexahe- drites (4-6% of Ni), Octahedrites (6-14% of Ni) and Nickel-rich ataxites (>12% of Ni) [1]. -
(2000) Forging Asteroid-Meteorite Relationships Through Reflectance
Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta. -
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 -
Revisiting the Campo Del Cielo, Argentina Crater Field: a New Data Point from a Natural Laboratory of Multiple Low Velocity, Oblique Impacts S.P
Lunar and Planetary Science XXXVII (2006) 1102.pdf Revisiting the Campo del Cielo, Argentina crater field: A new data point from a natural laboratory of multiple low velocity, oblique impacts S.P. Wright1, M.A. Vesconi2, A. Gustin2, K.K. Williams3, A.C. Ocampo4, and W.A. Cassidy5, 1Department of Geological Sciences, Arizona State University, Box 6305, Tempe, AZ 85287-6305, [email protected]; 2Servicios Informaticos Integrales, Resistencia, Chaco Prov- ince, Argentina; 3Center for Earth and Planetary Studies, Smithsonian Institute, Washington, D.C. 20013-7012; 4NASA HQ, Science Mission Directorate, 300 E St. SW, 3C66, Washington, D.C. 20546; 5Department of Geology and Planetary Sciences, University of Pittsburgh, Pittsburgh, PA 15260-3332, [email protected] Introduction: The energy of formation of very Foerster magnetic gradiometer. Gradients over a ver- low angle impact craters in loess targets is not well- tical interval of 60 cm were measured at ground level. known. The Campo del Cielo, Argentina crater field Negative lobes appear deeper than positive ones. There (CdCcf) represents a natural laboratory of at least 22 is a positive/negative pair over the point where the low-angle impact craters formed in loess ~4000 years meteorite was discovered, but the negative lobe is ago. Because of the uniformity of the loess and com- much closer to the location of the meteorite than is the position of the projectiles, as well as a limited range of positive one. This effect may be dictated by the rela- impact velocities, calculation of energies of crater for- tive strength of the negative lobe. Positive/negative mation are simplified.