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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. -
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. -
Re-Os ISOTOPIC CONSTRAINTS on the CRYSTALLIZATION HISTORY of IIAB IRON METEORITES
Lunar and Planetary Science XXVIII 1258.PDF Re-Os ISOTOPIC CONSTRAINTS on the CRYSTALLIZATION HISTORY of IIAB IRON METEORITES. M.I. Smoliar, R.J. Walker, J.W. Morgan. Dept. of Geol., Univ. MD, College Park, MD 20742 The IIAB group represents one of the clearest cases of face bet-ween IIA and IIB subgroups [4]. It also shows an fractional crystallization of metallic magma during core intermediate struc-ture - roughly half of this 2700 kg iron is formation. The Ni-Ir trend in the IIAB group (Fig. 1) has a a single hexahedral crystal of kamasite (typical for IIA sub- very steep negative slope which indicates a correspon- group), while the other part has the coarsest octahedral dingly high Ir distribution coefficient, and, consequently, structure, very similar to Navajo and Mount Joy - the neigh- high sulfur content in the parental metallic magma [1]. Sta- bors of Old Woman from IIB subgroup [5]. Specimens from tistical analyses of the IIAB Ni-Ir trend indicates that the both octahedral and hexahedral parts of Old Woman were observed scatter of datapoints along the ideal crystalli- analyzed. zation line is mostly due to analytical uncertainty. This Fig. 2 shows the Re-Os experimental results for the IIB implies that the Ni-Ir distribution pattern in IIAB irons re- meteorites along with previously publisued IIA isochron flects fractional crystallization, with no significant parallel ([7], age = 4.537 ± 8 Ga, initial 187Os/188Os ratio = 0.09550 or subsequent processes. Originally two separate groups ± 7, MSWD = 1.15). Low age uncertainty and low MSWD were recognized (IIA and IIB) on the basis of their different value imply that the whole IIA subgroup crystallized in a crystallographic structure and the prominent hiatus in the Ir narrow time interval not exceeding 16 m.y. -
Lost Lake by Robert Verish
Meteorite-Times Magazine Contents by Editor Like Sign Up to see what your friends like. Featured Monthly Articles Accretion Desk by Martin Horejsi Jim’s Fragments by Jim Tobin Meteorite Market Trends by Michael Blood Bob’s Findings by Robert Verish IMCA Insights by The IMCA Team Micro Visions by John Kashuba Galactic Lore by Mike Gilmer Meteorite Calendar by Anne Black Meteorite of the Month by Michael Johnson Tektite of the Month by Editor Terms Of Use Materials contained in and linked to from this website do not necessarily reflect the views or opinions of The Meteorite Exchange, Inc., nor those of any person connected therewith. In no event shall The Meteorite Exchange, Inc. be responsible for, nor liable for, exposure to any such material in any form by any person or persons, whether written, graphic, audio or otherwise, presented on this or by any other website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. does not endorse, edit nor hold any copyright interest in any material found on any website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. shall not be held liable for any misinformation by any author, dealer and or seller. In no event will The Meteorite Exchange, Inc. be liable for any damages, including any loss of profits, lost savings, or any other commercial damage, including but not limited to special, consequential, or other damages arising out of this service. © Copyright 2002–2010 The Meteorite Exchange, Inc. All rights reserved. No reproduction of copyrighted material is allowed by any means without prior written permission of the copyright owner. -
September 17, 2010 -- Oregon's Sixth Meteorite, Named Fitzwater Pass
NEWS RELEASE EMBARGOED UNTIL 1 PM P.S.T., SEPTEMBER 27, 2010 By: Alex Ruzicka, Melinda Hutson, Dick Pugh Source: Cascadia Meteorite Laboratory, Department of Geology, Portland State University, 503- 725-3372, email [email protected] Oregon’s sixth meteorite, named Fitzwater Pass, is discovered to be a rare type of iron. (Portland, Ore.) – September 27, 2010 After spending over 30 years in a Folgers coffee can, a thumb-sized chunk of metal has been identified by researchers as a rare type of iron meteorite. Named Fitzwater Pass, this meteorite adds to five other known meteorites from Oregon. Previous meteorites include Sam’s Valley (found 1894), Willamette (found 1902), Klamath Falls (found 1952), Salem (fell 1981), and Morrow County (recognized 2010). Meteorites are named for the nearest geographical feature. The meteorite was found in the early summer of 1976 by Mr. Paul Albertson of Lakeview, Oregon, while hunting for agate and jasper at Fitzwater Pass in south central Oregon with his high school teacher James Bleakney. Mr. Albertson took the 65 gram (2.3 ounce) teardrop-shaped piece of metal to a local rock shop, where a small amount was ground off. He was told by someone at the rock shop that it was probably a piece of nickel ore. Mr. Albertson placed the rock in a Folgers coffee can, where it remained until 2006. The meteorite made it out of the can and into the hands of Dick Pugh, a member of the Cascadia Meteorite Laboratory (CML) at Portland State University, Portland, Oregon, who recognized it as a probable meteorite. -
The Thermal Conductivity of Meteorites: New Measurements and Analysis
This article appeared in a journal published by Elsevier. The attached copy is furnished to the author for internal non-commercial research and education use, including for instruction at the authors institution and sharing with colleagues. Other uses, including reproduction and distribution, or selling or licensing copies, or posting to personal, institutional or third party websites are prohibited. In most cases authors are permitted to post their version of the article (e.g. in Word or Tex form) to their personal website or institutional repository. Authors requiring further information regarding Elsevier’s archiving and manuscript policies are encouraged to visit: http://www.elsevier.com/copyright Author's personal copy Icarus 208 (2010) 449–454 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The thermal conductivity of meteorites: New measurements and analysis C.P. Opeil a, G.J. Consolmagno b,*, D.T. Britt c a Department of Physics, Boston College, Chestnut Hill, MA 02467-3804, USA b Specola Vaticana, V-00120, Vatican City State c Department of Physics, University of Central Florida, Orlando, FL 32816-2385, USA article info abstract Article history: We have measured the thermal conductivity at low temperatures (5–300 K) of six meteorites represent- Received 6 October 2009 ing a range of compositions, including the ordinary chondrites Cronstad (H5) and Lumpkin (L6), the Revised 21 January 2010 enstatite chondrite Abee (E4), the carbonaceous chondrites NWA 5515 (CK4 find) and Cold Bokkeveld Accepted 23 January 2010 (CM2), and the iron meteorite Campo del Cielo (IAB find). All measurements were made using a Quantum Available online 1 February 2010 Design Physical Properties Measurement System, Thermal Transport Option (TTO) on samples cut into regular parallelepipeds of 2–6 mm dimension. -
Trace Element Inventory of Meteoritic Ca-Phosphates
American Mineralogist, Volume 102, pages 1856–1880, 2017 Trace element inventory of meteoritic Ca-phosphates DUSTIN WARD1,*, ADDI BISCHOFF1, JULIA ROSZJAR2, JASPER BERNDT3, AND MARTIN J. WHITEHOUSE4 1Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany 2Department of Mineralogy and Petrography, Natural History Museum Vienna, Burgring 7, 1010 Vienna, Austria 3Institut für Mineralogie, Westfälische Wilhelms-Universität Münster, Corrensstrasse 24, 48149 Münster, Germany 4Department of Geosciences, Swedish Museum of Natural History, Box 50007, 10405 Stockholm, Sweden ABSTRACT Most extraterrestrial samples feature the two accessory Ca-phosphates (apatite-group minerals and merrillite), which are important carrier phases of the rare earth elements (REE). The trace-element concentrations (REE, Sc, Ti, V, Cr, Mn, Co, As, Rb, Sr, Y, Zr, Nb, Ba, Hf, Ta, Pb, Th, and U) of se- lected grains were analyzed by LA-ICP-MS and/or SIMS (REE only). This systematic investigation includes 99 apatite and 149 merrillite analyses from meteorites deriving from various asteroidal bodies including 1 carbonaceous chondrite, 8 ordinary chondrites, 3 acapulcoites, 1 winonaite, 2 eucrites, 5 shergottites, 1 ureilitic trachyandesite, 2 mesosiderites, and 1 silicate-bearing IAB iron meteorite. Although Ca-phosphates predominantly form in metamorphic and/or metasomatic reactions, some are of igneous origin. As late-stage phases that often incorporate the vast majority of their host’s bulk REE budget, the investigated Ca-phosphates have REE enrichments of up to two orders of magnitude compared to the host rock’s bulk concentrations. Within a single sample, each phosphate species displays a uniform REE-pattern, and variations are mainly restricted to their enrichment, therefore indicating similar formation conditions. -
Trace Element Chemistry of Cumulus Ridge 04071 Pallasite with Implications for Main Group Pallasites
Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites Item Type Article; text Authors Danielson, L. R.; Righter, K.; Humayun, M. Citation Danielson, L. R., Righter, K., & Humayun, M. (2009). Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites. Meteoritics & Planetary Science, 44(7), 1019-1032. DOI 10.1111/j.1945-5100.2009.tb00785.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 23/09/2021 14:17:54 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656592 Meteoritics & Planetary Science 44, Nr 7, 1019–1032 (2009) Abstract available online at http://meteoritics.org Trace element chemistry of Cumulus Ridge 04071 pallasite with implications for main group pallasites Lisa R. DANIELSON1*, Kevin RIGHTER2, and Munir HUMAYUN3 1Mailcode JE23, NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas 77058, USA 2Mailcode KT, NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas 77058, USA 3National High Magnetic Field Laboratory and Department of Geological Sciences, Florida State University, Tallahassee, Florida 32310, USA *Corresponding author. E-mail: [email protected] (Received 06 November 2008; revision accepted 11 May 2009) Abstract–Pallasites have long been thought to represent samples from the metallic core–silicate mantle boundary of a small asteroid-sized body, with as many as ten different parent bodies recognized recently. This report focuses on the description, classification, and petrogenetic history of pallasite Cumulus Ridge (CMS) 04071 using electron microscopy and laser ablation ICP-MS. -
Meteorite Fall
Meteorite Times Magazine Contents by Editor Featured Monthly Articles Accretion Desk by Martin Horejsi Jim’s Fragments by Jim Tobin Meteorite Market Trends by Michael Blood Bob’s Findings by Robert Verish IMCA Insights by The IMCA Team Micro Visions by John Kashuba Norm’s Tektite Teasers by Norm Lehrman Meteorite Calendar by Anne Black Meteorite of the Month by Editor Tektite of the Month by Editor Terms Of Use Materials contained in and linked to from this website do not necessarily reflect the views or opinions of The Meteorite Exchange, Inc., nor those of any person connected therewith. In no event shall The Meteorite Exchange, Inc. be responsible for, nor liable for, exposure to any such material in any form by any person or persons, whether written, graphic, audio or otherwise, presented on this or by any other website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. does not endorse, edit nor hold any copyright interest in any material found on any website, web page or other cyber location linked to from this website. The Meteorite Exchange, Inc. shall not be held liable for any misinformation by any author, dealer and or seller. In no event will The Meteorite Exchange, Inc. be liable for any damages, including any loss of profits, lost savings, or any other commercial damage, including but not limited to special, consequential, or other damages arising out of this service. © Copyright 2002–2012 The Meteorite Exchange, Inc. All rights reserved. No reproduction of copyrighted material is allowed by any means without prior written permission of the copyright owner. -
Spring 2012 Gem News International
Editor Brendan M. Laurs ([email protected]) Contributing Editors Emmanuel Fritsch, CNRS, Team 6502, Institut des Matériaux Jean Rouxel (IMN), University of Nantes, France ([email protected]) Michael S. Krzemnicki, Swiss Gemmological Institute SSEF, Basel, Switzerland ([email protected]) Franck Notari, GGTL GemLab –GemTechLab, Geneva, Switzerland ([email protected]) Kenneth Scarratt, GIA, Bangkok, Thailand ([email protected]) stones, many rarities such as pallasitic peridot (figure 1) and TUCSON 2012 hibonite (figure 2) were seen at the shows. Cultured pearls continued to have a strong presence, and particularly impres - This year’s Tucson gem and mineral shows saw brisk sales sive were the relatively new round beaded Chinese freshwater of high-end untreated colored stones (and mineral specimens) products showing bright metallic luster and a variety of natural as well as some low-end goods, but sluggish movement of colors (figure 3). An unusual historic item seen in Tucson is mid-range items. In addition to the more common colored the benitoite necklace suite shown in figure 4. Several additional notable items present at the shows are described in the following pages and will also be documented in future issues of G&G . The theme of this year’s Tucson Gem and Mineral Society show was “Minerals of Arizona” in honor of Arizona’s Centennial, and next year’s theme will be “Fluorite: Colors of the Rainbow.” Figure 2. This exceedingly rare faceted hibonite from Myanmar weighs 0.96 ct and was recently cut from a crystal weighing 0.47 g, which also yielded a 0.26 ct stone. -
Meteorite Finds on Mars – a New Tool to Study Atmosphere and Surface Processes
Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6254.pdf METEORITE FINDS ON MARS – A NEW TOOL TO STUDY ATMOSPHERE AND SURFACE PROCESSES. C. Schröder1, A. W. Tait1, J. W. Ashley2 and the Athena Science Team, 1Biological and Environ- mental Sciences, University of Stirling, Stirling FK9 4LA, UK, [email protected], 2Jet Propulsion La- boratory, California Institute of Technology, Pasadena, CA 91109, USA. Introduction: Mars provides the necessary condi- help provide information on hypervelocity arrival of tions for exogenic rock (meteorite) accumulation and meteoritic materials in the smaller diameter range [13]. preservation, and finding meteorites on Mars has been predicted [1]. The Mars Exploration Rovers (MER), Spirit and Opportunity, are the first to find and charac- terize such meteorites [2-4]. Among those meteorites is the IAB iron complex meteorite Meridiani Planum a.k.a. Heat Shield Rock [2,4] (Fig. 1), the first meteor- ite on Mars that was officially recognized in the MetSoc meteorite database. Heat Shield Rock was the first in a suite of several irons of similar composition found across the Meridiani Plains during Opportunity’s extended traverses. Besides iron meteorites, Opportuni- ty also identified several stony meteorites (Fig. 2) with a composition approaching HED achondrites or poten- tially the silicate fraction of mesosiderite stony irons [2,3], and one putative (based on weathering pattern) but unconfirmed chondritic candidate [5]. The Mars Science Laboratory (MSL) rover Curiosity has since found additional meteorites, most of them irons [6] but Fig. 1. The iron meteorite Meridiani Planum displays a also identified more chondrite candidates [7]. -
Introduction to Meteorites Developed and Compiled by Larry Lebofsky, PSI
Introduction to Meteorites Developed and compiled by Larry Lebofsky, PSI Sikhote-Alin, Iron Meteorite Photo Credit: Larry Lebofsky Created in collaboration with The International Meteorite Collectors Association (IMCA) Big Ideas: • At present, meteorites are our only chance to study material from asteroids, Mars, and much of the Moon. • Meteorites are classified into three groups: stone, stony-iron, and iron. • Primitive stone meteorites come from asteroids that have not changed much since the formation of the Solar System 4.57 billion years ago. • Differentiated stone meteorites come from the surfaces of melted asteroids, the Moon, or Mars. • Stony-iron and iron meteorites come from the interiors of melted asteroids. • Asteroids and comets may have brought water and organics to Earth—the building blocks of life. OSIRIS-REx Asteroid Sample Return Mission Launch Workshop 2016 1 Solar System Objects: • An asteroid is an object that orbits the Sun, but smaller than a planet. They range in size from a few meters to nearly a thousand kilometers across. The image below is of the 525 kilometer diameter asteroid 4 Vesta taken by the Dawn spacecraft. The largest asteroid, 1 Ceres, is 940 kilometers in diameter and is big enough to be “round.” It is also considered to be a dwarf planet. • A meteoroid is an object that orbits the Sun, but is smaller than an asteroid. They range in size from a speck of dust to a few meters across. • A comet is an object that orbits the Sun. Comets are mostly icy and so, when close to the Sun, they display a visible coma and sometimes a tail.