Handbook of Iron Meteorites, Volume 2 (Canyon Diablo, Part 2)
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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. -
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. -
THE American Museum Journal
T ///^7; >jVvvscu/n o/ 1869 THE LIBRARY THE American Museum Journal VOLUME VII, 1907 NEW YORK: PUBLISHED BY THE AMERICAN MUSEUM OF NATURAL HISTORY 1907 Committee of Publication EDMUND OTIS HOVF.Y, Ediior. FRANK M. ( IIAPMAN ] LOUIS P. GHATACAP \ .l<lris-on/ linanl WILLIAM K. GREGOIlvJ THE AMERICAN MUSEUM OF NATURAL HISTORY. 77th Street and Central Park West, New York. OFFICERS AND COMMITTEES PRESIDEXT MORRIS K. JESUP FIRST VICE-PRESIDENT SECOND VICE-PRESIDENT J. PIERPONT MORGAN HENRY F. OSBORN TREASURER SECRETARY CHARLES LANIER J. HAMPDEN ROBB ASSISTANT SECRETARY AND DIRECTOR ASSISTANT TREASURER HERMON C. BUMPUS GEORGE H. SHERWOOD BOARD OF TRUSTEES Class of 1907 D. O. :\IILLS ALBERT S. BICKMORE ARCHIBALD ROGERS CORNELIUS C. CUYLER ADRIAN ISELIN, Jr. Class of 1908 H. o. have:\ieyer Frederick e. hyde A. I). JUHJJAIU) GEORCiE S. BOWDOIN (TEVELANl) H. DOIXJE Class of 1909 MORRIS K. JESUP J. PIERPONT MORGAN JOSEPH H. CHOATE GEORGE G. HAVEN HENRY F. OSBORN Class of 1910 J. HAMPDEN ROBB PERCY R. PYNE ARTHUR CURTISS JAMES Class of 1911 CHARLES LANIER WILLIAISI ROCKEFELLER ANSON W. HARD GUSTAV E. KISSEL SETH LOW Scientific Staff DIRECTOR Hermon C. Bumpus, Ph.D., Sc. D. DEPARTMENT OF PUBLIC INSTRUCTION Prof. Albert S. Bickmore, B. S., Ph.D., LL.D., Curator Emeritus George H. Shehwood, A.B., A.M., Curator DEPARTMENT OF GEOLOGY AND INVERTEBRATE PALEONTOLOGY Prof. R. P. Whitfield, A.M., Curator Edmund Otis Hovey, A.B., Ph.D., Associate Curator DEPARTMENT OF MAMMALOGY AND ORNITHOLOGY Prof. J. A. Allen, Ph.D., Curator Frank M. Chapman, Associate Curator DEPARTMENT OF VERTEBRATE PALAEONTOLOGY Prof. -
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. -
Lunar and Planetary Science XXX 1753.Pdf
Lunar and Planetary Science XXX 1753.pdf INTERSTELLAR DIAMOND. II. GROWTH AND IDENTIFICATION. Andrew W. Phelps, University of Dayton Research Institute, Materials Engineering Division (300 College Park, Dayton OH, 45469-0130, [email protected]). likely form clumps of carbon that look much like the Introduction: The first abstract in this series starting material – hydrogen rich sp3 bound clusters. suggested that many types of diamond are found in many types of meteoritic material and that the The compounds that fit the requirements above variation in polytype abundance appears to reflect the include the cycloalkanes such as adamantane [21-30] nature of the host. How the diamonds got there and (C10H16) and bicyclooctane (C6H8) (BCO) . what they mean will now be examined. Opinions These compounds ‘look’ like small cubic diamonds regarding the formation mechanism(s) of meteoritic and lonsdaleite respectively. If these particular and interstellar diamond grains have changed over compounds are suggested as models for diamond the years as new methods of making synthetic nuclei then a number of structural and diamond were developed[1,2]. Meteoritic diamonds thermodynamic predictions can be made about the were once believed to be the result of high pressure - types of diamond that can form and its relative temperature processes in the interior of planetary abundance with regard to the physics and chemistry bodies[3,4]. Impact formation of diamond became of its growth environment. A few examples of this popular after the development of shock wave are: Adamantane is a lower energy form and would diamond synthesis[5] because shock synthesis was tend to form in an environment of sufficient thermal able to form lonsdaleite and meteorites were full of energy to allow the molecule to organize into this lonsdaleite. -
Meteorites from the Lut Desert (Iran)
Meteorites from the Lut Desert (Iran) Hamed Pourkhorsandi, Jérôme Gattacceca, Pierre Rochette, Massimo d’Orazio, Hojat Kamali, Roberto Avillez, Sonia Letichevsky, Morteza Djamali, Hassan Mirnejad, Vinciane Debaille, et al. To cite this version: Hamed Pourkhorsandi, Jérôme Gattacceca, Pierre Rochette, Massimo d’Orazio, Hojat Kamali, et al.. Meteorites from the Lut Desert (Iran). Meteoritics and Planetary Science, Wiley, 2019, 54 (8), pp.1737-1763. 10.1111/maps.13311. hal-02144596 HAL Id: hal-02144596 https://hal-amu.archives-ouvertes.fr/hal-02144596 Submitted on 31 May 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Distributed under a Creative Commons Attribution - NonCommercial - ShareAlike| 4.0 International License doi: 10.1111/maps.13311 Meteorites from the Lut Desert (Iran) Hamed POURKHORSANDI 1,2*,Jerome^ GATTACCECA 1, Pierre ROCHETTE 1, Massimo D’ORAZIO3, Hojat KAMALI4, Roberto de AVILLEZ5, Sonia LETICHEVSKY5, Morteza DJAMALI6, Hassan MIRNEJAD7, Vinciane DEBAILLE2, and A. J. Timothy JULL8 1Aix Marseille Universite, CNRS, IRD, Coll France, INRA, CEREGE, Aix-en-Provence, France 2Laboratoire G-Time, Universite Libre de Bruxelles, CP 160/02, 50, Av. F.D. Roosevelt, 1050 Brussels, Belgium 3Dipartimento di Scienze della Terra, Universita di Pisa, Via S. -
Impact−Cosmic−Metasomatic Origin of Microdiamonds from Kumdy−Kol Deposit, Kokchetav Massiv, N
11th International Kimberlite Conference Extended Abstract No. 11IKC-4506, 2017 Impact−Cosmic−Metasomatic Origin of Microdiamonds from Kumdy−Kol Deposit, Kokchetav Massiv, N. Kazakhstan L. I. Tretiakova1 and A. M. Lyukhin2 1St. Petersburg Branch Russian Mineralogical Society. RUSSIA, [email protected] 2Institute of remote ore prognosis, Moscow, RUSSIA, [email protected] Introduction Any collision extraterrestrial body and the Earth had left behind the “signature” on the Earth’s surface. We are examining a lot of signatures of an event caused Kumdy-Kol diamond-bearing deposit formation, best- known as “metamorphic” diamond locality among numerous UHP terrains around the world. We are offering new impact-cosmic-metasomatic genesis of this deposit and diamond origin provoked by impact event followed prograde and retrograde metamorphism with metasomatic alterations of collision area rocks that have been caused of diamond nucleation, growth and preserve. Brief geology of Kumdy-Kol diamond-bearing deposit Kumdy-Kol diamond-bearing deposit located within ring structure ~ 4 km diameter, in the form and size compares with small impact crater (Fig. 1). It is important impact event signature. Figure1: Cosmic image of Kumdy-Kol deposit area [http://map.google.ru/]. Diamond-bearing domain had been formed on the peak of UHP metamorphism provoked by comet impact under oblique angle on the Earth surface. As a result, steep falling system of tectonic dislocations, which breakage and fracture zones filling out of impact and host rock breccia with blastomylonitic and blastocataclastic textures have been created. Diamond-bearing domain has complicated lenticular-bloc structure (1300 x 40-200 m size) and lens out with deep about 300 m. -
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. -
Graphic No Vels & Comics
GRAPHIC NOVELS & COMICS SPRING 2020 TITLE Description FRONT COVER X-Men, Vol. 1 The X-Men find themselves in a whole new world of possibility…and things have never been better! Mastermind Jonathan Hickman and superstar artist Leinil Francis Yu reveal the saga of Cyclops and his hand-picked squad of mutant powerhouses. Collects #1-6. 9781302919818 | $17.99 PB Marvel Fallen Angels, Vol. 1 Psylocke finds herself in the new world of Mutantkind, unsure of her place in it. But when a face from her past returns only to be killed, she seeks vengeance. Collects Fallen Angels (2019) #1-6. 9781302919900 | $17.99 PB Marvel Wolverine: The Daughter of Wolverine Wolverine stars in a story that stretches across the decades beginning in the 1940s. Who is the young woman he’s fated to meet over and over again? Collects material from Marvel Comics Presents (2019) #1-9. 9781302918361 | $15.99 PB Marvel 4 Graphic Novels & Comics X-Force, Vol. 1 X-Force is the CIA of the mutant world—half intelligence branch, half special ops. In a perfect world, there would be no need for an X-Force. We’re not there…yet. Collects #1-6. 9781302919887 | $17.99 PB Marvel New Mutants, Vol. 1 The classic New Mutants (Sunspot, Wolfsbane, Mirage, Karma, Magik, and Cypher) join a few new friends (Chamber, Mondo) to seek out their missing member and go on a mission alongside the Starjammers! Collects #1-6. 9781302919924 | $17.99 PB Marvel Excalibur, Vol. 1 It’s a new era for mutantkind as a new Captain Britain holds the amulet, fighting for her Kingdom of Avalon with her Excalibur at her side—Rogue, Gambit, Rictor, Jubilee…and Apocalypse. -
High Survivability of Micrometeorites on Mars: Sites with Enhanced Availability of Limiting Nutrients
RESEARCH ARTICLE High Survivability of Micrometeorites on Mars: Sites With 10.1029/2019JE006005 Enhanced Availability of Limiting Nutrients Key Points: Andrew G. Tomkins1 , Matthew J. Genge2,3 , Alastair W. Tait1,4 , Sarah L. Alkemade1, • Micrometeorites are predicted to be 1 1 5 far more abundant on Mars than on Andrew D. Langendam , Prudence P. Perry , and Siobhan A. Wilson Earth 1 2 • Micrometeorites are concentrated in School of Earth, Atmosphere and Environment, Melbourne, Victoria, Australia, Impact and Astromaterials Research the residue of aeolian sediment Centre, Department of Earth Science and Engineering, Imperial College London, London, UK, 3Department of removal, such as at bedrock cracks Mineralogy, The Natural History Museum, London, UK, 4Department of Biological and Environmental Sciences, and gravel accumulations University of Stirling, Scotland, UK, 5Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, • Micrometeorite accumulation sites are enriched in key nutrients for Alberta, Canada primitive microbes: reduced phosphorus, sulfur, and iron Abstract NASA's strategy in exploring Mars has been to follow the water, because water is essential for life, and it has been found that there are many locations where there was once liquid water on the surface. Now perhaps, to narrow down the search for life on a barren basalt‐dominated surface, there needs to be a Correspondence to: A. G. Tomkins, refocusing to a strategy of “follow the nutrients.” Here we model the entry of metallic micrometeoroids [email protected] through the Martian atmosphere, and investigate variations in micrometeorite abundance at an analogue site on the Nullarbor Plain in Australia, to determine where the common limiting nutrients available in Citation: these (e.g., P, S, Fe) become concentrated on the surface of Mars. -
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. -
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.