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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. -
Some Will Go Far to Catch a Falling Star Henner Busemann Enjoys a Hymn to the Passionate Collectors Who Fuelled the Science of Meteorites
Vol 462|26 November 2009 BOOKS & ARTS Some will go far to catch a falling star Henner Busemann enjoys a hymn to the passionate collectors who fuelled the science of meteorites. The Fallen Sky: An Intimate History of into legal disputes. Farmer Ellis Hughes, for and he is considered one of the leaders of Shooting Stars example, was convicted of theft after ‘recov- modern meteorite research. Yet Nininger’s by Christopher Cokinos ering’ the famous Willamette iron meteor ite hopes for an appointment as a professor for Tarcher/Penguin: 2009. 528 pp. $27.95 from private land in 1902. The 14-tonne main meteoritics never materialized. Traduced as chunk of this is now in the American Museum a collector with merely commercial interests, of Natural History, New York. Nininger struggled to earn enough to sup- Meteorites — rocks that ‘fall from the sky’ — Cokinos’s efforts culminate in three splendid port his family yet managed to accumulate an fascinate and inspire. The origin of these dark, chapters. One concerns pioneer Harvey Ninin- impressive private collection of meteorites. often strangely sculpted boulders that might ger, a biologist from Kansas who was the first Cokinos conveys his excitement at visiting suddenly dent a ploughed field or demolish to systematically trace and collect meteorites Nördlingen, a picturesque medieval town in a roof has long been disputed. Yet the global in the United States. Cokinos gives a thrilling the south of Germany, built within a meteorite consequences of meteorite impacts have only description of Nininger’s crater of some 20 kilome- recently been accepted. It took the efforts of a epic fight to raise aware- “Jealousy, personal tres in diameter that formed few visionaries — mostly non-academics who ness of the importance of animosity and a struggle around 15 million years had to endure scholastic resistance, sarcasm meteor ites as extraterrestrial ago. -
Comet and Meteorite Traditions of Aboriginal Australians
Encyclopaedia of the History of Science, Technology, and Medicine in Non-Western Cultures, 2014. Edited by Helaine Selin. Springer Netherlands, preprint. Comet and Meteorite Traditions of Aboriginal Australians Duane W. Hamacher Nura Gili Centre for Indigenous Programs, University of New South Wales, Sydney, NSW, 2052, Australia Email: [email protected] Of the hundreds of distinct Aboriginal cultures of Australia, many have oral traditions rich in descriptions and explanations of comets, meteors, meteorites, airbursts, impact events, and impact craters. These views generally attribute these phenomena to spirits, death, and bad omens. There are also many traditions that describe the formation of meteorite craters as well as impact events that are not known to Western science. Comets Bright comets appear in the sky roughly once every five years. These celestial visitors were commonly seen as harbingers of death and disease by Aboriginal cultures of Australia. In an ordered and predictable cosmos, rare transient events were typically viewed negatively – a view shared by most cultures of the world (Hamacher & Norris, 2011). In some cases, the appearance of a comet would coincide with a battle, a disease outbreak, or a drought. The comet was then seen as the cause and attributed to the deeds of evil spirits. The Tanganekald people of South Australia (SA) believed comets were omens of sickness and death and were met with great fear. The Gunditjmara people of western Victoria (VIC) similarly believed the comet to be an omen that many people would die. In communities near Townsville, Queensland (QLD), comets represented the spirits of the dead returning home. -
Tubular Symplectic Inclusions in Olivine from the Fukang Pallasite
Meteoritics & Planetary Science 45, Nr 5, 899–910 (2010) doi: 10.1111/j.1945-5100.2010.01054.x Tubular symplectic inclusions in olivine from the Fukang pallasite Michael R. STEVENS1, David R. BELL1,2, and Peter R. BUSECK1,2* 1School of Earth and Space Exploration, Arizona State University, Tempe, Arizona 85287, USA 2Department of Chemistry and Biochemistry, Arizona State University, Tempe, Arizona 85287, USA *Corresponding author. E-mail: [email protected] (Received 11 June 2009; revision accepted 27 March 2010) Abstract–Olivine from the Fukang meteorite, like that from many other pallasites, contains distinctive arrays of parallel, straight, tubular inclusions. They differ in their extension and linearity from those in terrestrial olivines. They comprise approximately 1% of the total volume. Most have lens-shaped cross-sections, but some are rounded. The major axis of the lens-shaped inclusions is rigorously oriented along olivine [001], and the rounded ones lie along olivine [010] and a few along [100]. The linear nature and orientations of the inclusions suggest that they nucleated on screw dislocations, perhaps formed through shock triggering. High-resolution transmission electron microscopy (TEM) and energy-dispersive x-ray spectroscopy show that the inclusions consist of symplectic intergrowths of chromite, diopside, and silica that appear to have formed by exsolution from the host olivine. The symplectites consist of chromite lamellae with approximately 35-nm spacings that grew outward from a central plane, with interstitial diopside and silica. Contrast modulations having an average spacing of 4.4 nm occur within the chromite lamellae. Using a reaction- front model, we estimate that exsolution occurred over a period of 30 to 100 min, suggesting rapid cooling at high temperature. -
A Catalogue of Large Meteorite Specimens from Campo Del Cielo Meteorite Shower, Chaco Province , Argentina
69th Annual Meteoritical Society Meeting (2006) 5001.pdf A CATALOGUE OF LARGE METEORITE SPECIMENS FROM CAMPO DEL CIELO METEORITE SHOWER, CHACO PROVINCE , ARGENTINA. M. C. L. Rocca , Mendoza 2779-16A, Ciudad de Buenos Aires, Argentina, (1428DKU), [email protected]. Introduction: The Campo del Cielo meteorite field in Chaco Province, Argentina, (S 27º 30’, W 61 º42’) consists, at least, of 20 meteorite craters with an age of about 4000 years. The area is composed of sandy-clay sediments of Quaternary- recent age. The impactor was an Iron-Nickel Apollo-type asteroid (Octahedrite meteorite type IA) and plenty of meteorite specimens survived the impact. Impactor’s diameter is estimated 5 to 20 me- ters. The impactor came from the SW and entered into the Earth’s atmosphere in a low angle of about 9º. As a consequence , the aster- oid broke in many pieces before creating the craters. The first mete- orite specimens were discovered during the time of the Spanish colonization. Craters and meteorite fragments are widespread in an oval area of 18.5 x 3 km (SW-NE), thus Campo del Cielo is one of the largest meteorite’s crater fields known in the world. Crater nº 3, called “Laguna Negra” is the largest (diameter: 115 meters). Inside crater nº 10, called “Gómez”, (diameter about 25 m.), a huge meteorite specimen called “El Chaco”, of 37,4 Tons, was found in 1980. Inside crater nº 9, called “La Perdida” (diameter : 25 x 35 m.) several meteorite pieces were discovered weighing in total about 5200 kg. The following is a catalogue of large meteorite specimens (more than 200 Kg.) from this area as 2005. -
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. -
N Arieuican%Mllsellm
n ARieuican%Mllsellm PUBLISHED BY THE AMERICAN MUSEUM OF NATURAL HISTORY CENTRAL PARK WEST AT 79TH STREET, NEW YORK 24, N.Y. NUMBER 2I63 DECEMBER I9, I963 The Pallasites BY BRIAN MASON' INTRODUCTION The pallasites are a comparatively rare type of meteorite, but are remarkable in several respects. Historically, it was a pallasite for which an extraterrestrial origin was first postulated because of its unique compositional and structural features. The Krasnoyarsk pallasite was discovered in 1749 about 150 miles south of Krasnoyarsk, and seen by P. S. Pallas in 1772, who recognized these unique features and arranged for its removal to the Academy of Sciences in St. Petersburg. Chladni (1794) examined it and concluded it must have come from beyond the earth, at a time when the scientific community did not accept the reality of stones falling from the sky. Compositionally, the combination of olivine and nickel-iron in subequal amounts clearly distinguishes the pallasites from all other groups of meteorites, and the remarkable juxtaposition of a comparatively light silicate mineral and heavy metal poses a nice problem of origin. Several theories of the internal structure of the earth have postulated the presence of a pallasitic layer to account for the geophysical data. No apology is therefore required for an attempt to provide a comprehensive account of this remarkable group of meteorites. Some 40 pallasites are known, of which only two, Marjalahti and Zaisho, were seen to fall (table 1). Of these, some may be portions of a single meteorite. It has been suggested that the pallasite found in Indian mounds at Anderson, Ohio, may be fragments of the Brenham meteorite, I Chairman, Department of Mineralogy, the American Museum of Natural History. -
Meteorite Collections: Sample List
Meteorite Collections: Sample List Institute of Meteoritics Department of Earth and Planetary Sciences University of New Mexico October 01, 2021 Institute of Meteoritics Meteorite Collection The IOM meteorite collection includes samples from approximately 600 different meteorites, representative of most meteorite types. The last printed copy of the collection's Catalog was published in 1990. We will no longer publish a printed catalog, but instead have produced this web-based Online Catalog, which presents the current catalog in searchable and downloadable forms. The database will be updated periodically. The date on the front page of this version of the catalog is the date that it was downloaded from the worldwide web. The catalog website is: Although we have made every effort to avoid inaccuracies, the database may still contain errors. Please contact the collection's Curator, Dr. Rhian Jones, ([email protected]) if you have any questions or comments. Cover photos: Top left: Thin section photomicrograph of the martian shergottite, Zagami (crossed nicols). Brightly colored crystals are pyroxene; black material is maskelynite (a form of plagioclase feldspar that has been rendered amorphous by high shock pressures). Photo is 1.5 mm across. (Photo by R. Jones.) Top right: The Pasamonte, New Mexico, eucrite (basalt). This individual stone is covered with shiny black fusion crust that formed as the stone fell through the earth's atmosphere. Photo is 8 cm across. (Photo by K. Nicols.) Bottom left: The Dora, New Mexico, pallasite. Orange crystals of olivine are set in a matrix of iron, nickel metal. Photo is 10 cm across. (Photo by K. -
Sikhote-Alin Meteorite, Elemental Composition Analysis Using CF LIBS
WDS'12 Proceedings of Contributed Papers, Part II, 123–127, 2012. ISBN 978-80-7378-225-2 © MATFYZPRESS Sikhote-Alin Meteorite, Elemental Composition Analysis Using CF LIBS J. Plavčan,1 M. Horňáčková,1 Z. Grolmusová,1,2 M. Kociánová,1 J. Rakovský,1 P. Veis1,2 1 Department of Experimental Physics, Faculty of Mathematics Physics and Informatics Comenius University, Mlynská dolina, 84248 Bratislava, Slovakia. 2 Laboratory of Isotope Geology, State Geological Institute of Dionyz Stur, Mlynská dolina 1, 817 04 Bratislava, Slovakia. Abstract. Calibration free laser induced breakdown spectroscopy (CF-LIBS) method was used for determination of elements presented in meteorite Sikhote Alin as well as its quantities. As a source of ablation, Q-switched Nd: YAG laser operating at 532 nm was used. Emission from plasma was collected by optical fiber that was connected with slit of Echelle spectrometer (ME 5000, Andor) coupled with iCCD camera (iSTAR DH734i-18F- 03, Andor). Optimal experimental conditions, i.e. time delay, gate width, energy per pulse were found. The measured spectra were recorded 2.5 μs after laser pulse and gate width of iCCD camera was set to 0.5 μs. Electron concentration was calculated from broadening of hydrogen Hα line (656 nm).A Saha-Boltzmann plot method was used for determination of electron temperature, assuming the local thermodynamic equilibrium. Apart from iron, which is the main elemental constituent of examined meteorite, elements like nickel, cobalt, phosphor, potassium, sodium, calcium and manganese, were also detected. In comparison with official Sikhote Alin elemental quantitative measurements, some elements like sodium, calcium, potassium and manganese were not mentioned, it is expected that these elements were added to the surface of meteorite after the meteorite fall. -
4 Asteroids, Comets, and Meteoroids
Name Class Date CHAPTER 28 Minor Bodies of the Solar System SECTION 4 Asteroids, Comets, and Meteoroids KEY IDEAS As you read this section, keep these questions in mind: • What are the physical characteristics of asteroids and comets? • Where is the Kuiper Belt located? • How do meteoroids, meteorites, and meteors differ? • What is the relationship between the Oort cloud and comets? What Are Asteroids? Asteroids are chunks of rock that orbit the sun. READING TOOLBOX Astronomers have discovered more than 300,000 Compare After you read this asteroids, and they think that millions may exist. Like section, create a three-way the orbits of planets, the orbits of asteroids are ellipses. Venn diagram to compare asteroids, comets, and meteoroids. Some of the overlapping spaces in the diagram may be left blank. LOOKING CLOSER 1. Identify On the picture, label which asteroid is Ida and which is Dactyl. Asteroids vary greatly in size. Asteroid Ida is 56 km long. Asteroid Dactyl is 1.5 km across. LOCATION OF ASTEROIDS Most asteroids are located in a region between the orbits of Mars and Jupiter. This region is called the READING CHECK asteroid belt. Some asteroids, however, orbit the sun 2. Describe Where are most more closely. The closest asteroids to the sun are located asteroids located? inside the orbit of Mars. The Trojan asteroids are groups of asteroids found near Jupiter. Copyright © Holt McDougal. All rights reserved. Holt McDougal Earth Science 451 Minor Bodies of the Solar System hq10irna_mbss04.indd 451 4/5/09 10:07:38 AM Name Class Date SECTION 4 Asteroids, Comets, and Meteoroids continued COMPOSITION OF ASTEROIDS The composition of an asteroid is similar to the composition of the inner planets. -
The Fukang Pallasite: Evidence for Non-Equilibrium Shock Processing
Lunar and Planetary Science XXXVII (2006) 2250.pdf THE FUKANG PALLASITE: EVIDENCE FOR NON-EQUILIBRIUM SHOCK PROCESSING. D. S. Lauretta, D. H. Hill, D. N. Della-Giustina, and M. Killgore. Southwest Meteorite Center, Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, [email protected]. Introduction: Pallasites are primarily composed of relatively large (>100 µm) inclusions of silica, Fe- olivine and FeNi-metal. Most researchers agree that metal, and an orthoclase-normative glass (Fig. 2). We this mixture formed after differentiation but before did not observe zoning for Al, Cr, Ca, Mn, or Fe. Ver- solidification of the core of an asteroid. A variety of micular troilite and thin veins of kamacite and troilite origins for pallasites have been put forward, including occur in many olivines. crystallization near the surface of an externally heated The groundmass is mostly kamacite with some oc- asteroid [1]; crystallization of an impact melt [2]; and currences of kamacite mantles surrounding taenite nebular condensation [3]. However, the leading theory cores, rounded taenite adjacent to kamacite, and nu- is that pallasites were generated at the core–mantle merous regions of “comb plessite”. In larger fingers of interface of a differentiated asteroid. Two mechanisms metal, the normal “M”shaped Ni distribution is dis- have been proposed. The first is an equilibrium proc- turbed and chaotic in the center. The trace-element ess, where the intercumulate silicate melt between cu- abundances in bulk Fukang metal are given in Table 1. mulate mantle olivine is replaced by molten metal [4- Schreibersite is enclosed by wide kamacite bands 5]. -
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.