FIRST OCCURRENCES of Nisvsco PHOSPHIDES in CHROMITITE
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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. -
Comprehensive Bibliography on Martian Meteorites (Compiled by C
Comprehensive Bibliography on Martian Meteorites (compiled by C. Meyer, March 2008) Abu Aghreb A.E., Ghadi A.M., Schlüter J., Schultz L. and Thiedig F. (2003) Hamadah al Hamra and Dar al Gani: A comparison of two meteorite fields in the Libyan Sahara (abs). Meteoritics & Planet. Sci. 38, A48. Agee Carl B. (2002) Garnet and majorite fractionation in the early Earth and Mars (abs#1862). Lunar Planet. Sci. XXXIII Lunar Planetary Institute, Houston. (CD-ROM). (see address of LPI in Appendix III) Agee C.B., Bogard Don D., Draper D.S., Jones J.H., Meyer Chuck and Mittlefehldt D.W. (2000) Proposed science requirements and acquisition priorities for the first Mars sample return (abs). In Concept and Approaches for Mars Exploration. Part 1 (ed. S. Hubbard) LPI Contribution # 1062. Lunar Planetary Institute, Houston. Agee C.B. and Draper Dave S. (2003) Melting of model Martian mantle at high pressure: Implications for the composition of the Martian basalt source region (abs#1408). Lunar Planet. Sci. Conf. 34th, Lunar Planetary Institute, Houston (CD-ROM). Agerkvist D.P. and Vistisen L. (1993) Mössbauer spectroscopy of the SNC meteorite Zagami (abs). Lunar Planet. Sci. XXIV, 1-2. Lunar Planetary Institute, Houston. Zagami Agerkvist D.P., Vistisen L., Madsen M.B. and Knudsen J.M. (1994) Magnetic properties of Zagami and Nakhla (abs). Lunar Planet. Sci. XXV, 1-2. Lunar Planetary Institute, Houston. Zagami Nakhla Akai J. (1997) Characteristics of iron-oxide and iron-sulfide grains in meteorites and terrestrial sediments, with special references to magnetite grains in Allan Hills 84001 (abs). Meteoritics & Planet. Sci. -
8. Projectile ˜˜˜
8. Projectile ˜˜˜ Meteoritic remnants of the impacting asteroid that produced Barringer Crater littered the landscape when exploration began ~115 years ago. As described in Chapter 1, meteoritic irons are what initially captured Foote’s interest and spurred Barringer’s interest in a possibly rich natural source of native metal. After Foote’s description was published, samples were collected by F. W. Volz at a nearby trading post and sold widely. Gilbert (1896) estimated that 10 tons of meteoritic debris had already been recovered by the time of his visit. Similarly, Barringer (1905) estimated that 10 to 15 tons of it were circulating around the world by the time his exploration work began. Fortunately, he tried to document the geographic and mass distribution of that debris in a detailed map, which is reproduced in Fig. 8.1. The map indicates that meteoritic irons were recovered from distances approaching 10 km. Gilbert (1896) apparently recovered a sample nearly 13 km beyond the crater rim. A lot of the meteoritic material was oxidized. It is sometimes simply called oxidized iron, but large masses are also called shale balls. A concentrated deposit of small oxidized iron fragments was found northeast of the crater, although those types of fragments are distributed in all directions around the crater. The current estimate of the recovered meteoritic iron mass is 30 tons (Nininger, 1949; Grady, 2000), although this is a highly uncertain number. Specimens were transported in pre-historical times and have been found scattered throughout Arizona (see, for example, Wasson, 1968). Specimens have also been illicitly removed in recent times, without any documentation of the locations or masses recovered. -
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. -
Using Oxygen and Carbon Stable Isotopes, 53Mn-53Cr Isotope Systematics, and Petrology to Constrain the History of Carbonates
University of New Mexico UNM Digital Repository Earth and Planetary Sciences ETDs Electronic Theses and Dissertations 7-10-2013 Using oxygen and carbon stable isotopes, 53Mn-53Cr isotope systematics, and petrology to constrain the history of carbonates and water in the CR and CM chondrite parent bodies Mark Tyra Follow this and additional works at: https://digitalrepository.unm.edu/eps_etds Recommended Citation Tyra, Mark. "Using oxygen and carbon stable isotopes, 53Mn-53Cr isotope systematics, and petrology to constrain the history of carbonates and water in the CR and CM chondrite parent bodies." (2013). https://digitalrepository.unm.edu/eps_etds/93 This Dissertation is brought to you for free and open access by the Electronic Theses and Dissertations at UNM Digital Repository. It has been accepted for inclusion in Earth and Planetary Sciences ETDs by an authorized administrator of UNM Digital Repository. For more information, please contact [email protected]. Mark Anthony Tyra Candidate Earth and Planetary Sciences Department This dissertation is approved, and it is acceptable in quality and form for publication: Approved by the Dissertation Committee: Adrian J. Brearley , Chairperson Ian D. Hutcheon Rhian H. Jones Zachary D. Sharp Charles K. Shearer i USING OXYGEN AND CARBON STABLE ISOTOPES, 53MN-53CR ISOTOPE SYSTEMATICS, AND PETROLOGY TO CONSTRAIN THE HISTORY OF CARBONATES AND WATER IN THE CR AND CM CHONDRITE PARENT BODIES by MARK ANTHONY TYRA B.S., Geology, University of Kentucky, 2000 M.S., Geology, University of Maryland, 2005 DISSERTATION Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Earth and Planetary Sciences The University of New Mexico Albuquerque, New Mexico May, 2013 ii DEDICATION Education, on the other hand, means emancipation. -
Magnetite Plaquettes Are Naturally Asymmetric Materials in Meteorites
1 (Revision 2) 2 Magnetite plaquettes are naturally asymmetric materials in meteorites 3 Queenie H. S. Chan1, Michael E. Zolensky1, James E. Martinez2, Akira Tsuchiyama3, and Akira 4 Miyake3 5 1ARES, NASA Johnson Space Center, Houston, Texas 77058, USA. 6 2Jacobs Engineering, Houston, Texas 77058, USA. 7 3Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 8 606-8502, Japan. 9 10 Correspondence to: Queenie H. S. Chan. Correspondence and requests for materials should be 11 addressed to Q.H.S.C. (Email: [email protected]) 12 13 Abstract 14 Life on Earth shows preference towards the set of organics with particular spatial configurations. 15 Enantiomeric excesses have been observed for α-methyl amino acids in meteorites, which 16 suggests that chiral asymmetry might have an abiotic origin. A possible abiotic mechanism that 17 could produce chiral asymmetry in meteoritic amino acids is their formation under the influence 18 of asymmetric catalysts, as mineral crystallization can produce spatially asymmetric structures. 19 Although magnetite plaquettes have been proposed to be a possible candidate for an asymmetric 20 catalyst, based on the suggestion that they have a spiral structure, a comprehensive description of 21 their morphology and interpretation of the mechanism associated with symmetry-breaking in 22 biomolecules remain elusive. Here we report observations of magnetite plaquettes in 1 23 carbonaceous chondrites (CCs) which were made with scanning electron microscopy and 24 synchrotron X-ray computed microtomography (SXRCT). We obtained the crystal orientation of 25 the plaquettes using electron backscatter diffraction (EBSD) analysis. SXRCT permits 26 visualization of the internal features of the plaquettes. -
Oxygen Isotope Compositions of the Kaidun Meteorite – Indications for Aqueous Alteration of E-Chondrites
OXYGEN ISOTOPE COMPOSITIONS OF THE KAIDUN METEORITE – INDICATIONS FOR AQUEOUS ALTERATION OF E-CHONDRITES. K. Ziegler1,*, M. Zolensky2, E. D. Young1,3, A. Ivanov4. 1Institute of Geophysics and Planetary Physics, University of California Los Angeles (UCLA), Los Angeles, CA 90095, U.S.A., 2ARES, NASA Johnson Space Center, Houston, TX 77058, U.S.A., 3Department of Earth and Space Sciences, UCLA, Los Angeles, CA 90095, U.S.A., 4Vernadsky Institute, Moscow, Russia. *Current address: Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, U.S.A., ([email protected], [email protected], [email protected], [email protected]). Introduction: The Kaidun microbreccia is a Results: The clasts are comprised of the following unique meteorite due to the diversity of its constituent lithologies: altered enstatite chondrites or aubrites, clasts. Fragments of various types of carbonaceous (CI, CM2, C1 (most likely CI1), C2, and a microbreccia. CM, CV, CR), enstatite (EH, EL), and ordinary chon- Surviving E-chondrite or aubrite primary minerals drites, basaltic achondrites, and impact melt products include enstatite, augite, diopside, silica, plagioclase have been described, and also several unknown clasts (albite to anorthite), ilmenite and heideite. Alteration [1, and references therein]. The small mm-sized clasts products of the enstatite material are: poorly-crystalline represent material from different places and times in enstatite, calcite, phyllosilicates, neoformed albite, and the early solar system, involving a large variety of par- amphiboles (actinolite) (Fig. 1). Alteration mineralogy ent bodies [2]; meteorites are of key importance to the of the CM2 clast include Ca carbonates, tochilinite, study of the origin and evolution of the solar system, serpentine, sulfides, and chromite. -
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. -
General Index Vols. XLI-L, Third Series
GENERAL INDEX OF VOLUMES XLI-L OF THE THIRD SERIES. WInthe references to volumes xli to I, only the numerals i to ir we given. NOTE.-The names of mineral8 nre inaerted under the head ol' ~~IBERALB:all ohitllary notices are referred to under OBITUARY. Under the heads BO'PANY,CHK~I~TRY, OEOLO~Y, Roo~s,the refereuces to the topics in these department8 are grouped together; in many cases, the same references appear also elsewhere. Alabama, geological survey, see GEOL. REPORTSand SURVEYS. Abbe, C., atmospheric radiation of Industrial and Scientific Society, heat, iii, 364 ; RIechnnics of the i. 267. Earth's Atmosphere, v, 442. Alnska, expedition to, Russell, ii, 171. Aberration, Rayleigh, iii, 432. Albirnpean studies, Uhler, iv, 333. Absorption by alum, Hutchins, iii, Alps, section of, Rothpletz, vii, 482. 526--. Alternating currents. Bedell and Cre- Absorption fipectra, Julius, v, 254. hore, v, 435 ; reronance analysis, ilcadeiny of Sciences, French, ix, 328. Pupin, viii, 379, 473. academy, National, meeting at Al- Altitudes in the United States, dic- bany, vi, 483: Baltimore, iv, ,504 : tionary of, Gannett, iv. 262. New Haven, viii, 513 ; New York, Alum crystals, anomalies in the ii. 523: Washington, i, 521, iii, growth, JIiers, viii, 350. 441, v, 527, vii, 484, ix, 428. Aluminum, Tvave length of ultra-violet on electrical measurements, ix, lines of, Runge, 1, 71. 236, 316. American Association of Chemists, i, Texas, Transactions, v, 78. 927 . Acoustics, rrsearchesin, RIayer, vii, 1. Geological Society, see GEOL. Acton, E. H., Practical physiology of SOCIETYof AMERICA. plants, ix, 77. Nuseu~nof Sat. Hist., bulletin, Adams, F. -
Handbook of Iron Meteorites, Volume 3 (Willow Creek – Wood's Mountian)
Willamette - Willow Creek 1321 Stage four would be the penetration of the atmos Williamstown. See Kenton County phere. However, no remnants of the associated sculpturing (Williamstown) are to be seen today. The fusion crust and heat-affected o:2 zones are all removed by weathering. Immediately after its landing, the external shape of Willamette may have re Willow Creek, Wyoming, U.S.A. sembled that of Morito rather closely. Stage five is the final long-term exposure in the humid 43°26'N, 106° 46'W; about 1,800 m Oregon valley forest during which the deep cavities, partially penetrating and generally perpendicular to the Coarse octahedrite, Og. Bandwidth 1.40±0.25 mm. Partly recrystal topside of the mass, were formed. While no large-scale lized . HV 152±6. texture, such as silicate inclusions, can be considered Group IIIE. 8.76% Ni, about 0.35% P, 16.9 ppm Ga, 36.4 ppm Ge, responsible for the curious corrosion progress, it is possible 0 .05 ppm lr. that the very distinct troilite filaments have aided in the weathering. These lanes of fine-grained troilite, kamacite HISTORY and taenite would probably provide easy diffusion paths A mass of 112.5 pounds (51 kg) was found by John studded with electrochemical cells and with dilute sulfuric Forbes of Arminto, Wyoming, near Willow Creek, Natrona acid from decomposed troilite, where the kamacite phase County, about 1914. For a long time it was in the would provide the anodic areas and dissolve first. The final possession of the Forbes family, but in 1934 the meteorite product, the deeply carved Willamette mass, must, however, be seen to be believed. -
Geochemical Constraints on the Origin of the Moon and Preservation of Ancient Terrestrial Heterogeneities
S. J. Lock et al., Space Science Reviews, 216, 109, doi: 10.1007/s11214-020-00729-z, 2020 Geochemical constraints on the origin of the Moon and preservation of ancient terrestrial heterogeneities Simon J. Locka,∗, Katherine R. Berminghamb,c, Rita Paraid, Maud Boyete aDivision of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA. bDepartment of Earth and Planetary Sciences, Rutgers University, Piscataway, NJ 08854, USA cDepartment of Geology, University of Maryland,College Park, MD 20742, USA. dDepartment of Earth and Planetary Sciences, Washington University in St. Louis, Saint Louis, MO 63130, USA. eUniversit´eClermont Auvergne, CNRS, IRD, OPGC, Laboratoire Magmas et Volcans, F-63000 Clermont-Ferrand, France. Abstract The Moon forming giant impact marks the end of the main stage of Earth's accretion and sets the stage for the subsequent evolution of our planet. The giant impact theory has been the accepted model of lunar origin for 40 years, but the parameters of the impact and the mechanisms that led to the formation of the Moon are still hotly debated. Here we review the principal geochemical observations that constrain the timing and parameters of the impact, the mechanisms of lunar formation, and the contemporaneous evolution of Earth. We discuss how chemical and isotopic studies on lunar, terrestrial and meteorite samples relate to physical models and how they can be used to differentiate between lunar origin models. In particular, we argue that the efficiency of mixing during the collision is a key test of giant impact models. A high degree of intra-impact mixing is required to explain the isotopic similarity between the Earth and Moon but, at the same time, the impact did not homogenize the whole terrestrial mantle, as isotopic signatures of pre-impact heterogeneity are preserved. -
Workshop on Oxygen in Asteroids and Meteorites
WOJUCSHOP PIiOGlIAM AND ABSTIIACTS LPI Contribution No. 1267 Workshop on Oxygen in Asteroids and Meteorites June 2-3, 2005 Flagstaff, Arizona Sponsored by Lunar and Planetary Institute National Aeronautics and Space Administration NASA Cosmochemistry Program Conveners David W. Mittlefehldt, NASA Johnson Space Center Thomas Burbine, NASA Goddard Space Flight Center Asteroids and Meteorites Team and Workshop Program Committee David W. Mittlefehldt, NASA Johnson Space Center Thomas Burbine, NASA Goddard Space Flight Center Jeremy Delaney, Rutgers University Ian Franchi, Open University Andrew Rivkin, Massachusetts Institute a/Technology Michael Zolensky, NASA Johnson Space Center Lnnar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Contribution No. 1267 Compiled in 2005 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Agreement No. NCC5-679 issued through the Solar System Exploration Division of the National Aeronautics and Space Administration. Any opinions, findings, and conclusions or recommendations expressed in this volume are those of the author(s) and do not necessarily reflect the views ofthe National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication ofany paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment ofthis publication. Abstracts in this volume may be cited as Author A. B. (2005) Title of abstract. In Workshop on Oxygen in Asteroids and Meteorites, p. XX. LPI Contribution No. 1267, Lunar and Planetary Institute, Houston. This volume is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113, USA Phone: 281-486-2172 Fax: 281-486-2186 E-mail: [email protected] Mail orders requestors will be invoicedfor the cost ofshipping and handling.