The Muonionalusta Iron Meteorites
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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. -
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. -
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. -
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. -
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. -
Geophysical Abstracts, 180-183 January-December 1960
Geophysical Abstracts, 180-183 January-December 1960 GEOLOGICAL SURVEY BULLETIN 1116 Abstracts of current literature pertaining to the physics of the solid earth and to f!eophysical exploration • UNITED STATES GOVERNMENT PRINTING OFFICE, WASHINGTON : 1961 UNITED STATES DEPARTMENT OF THE INTERIOR STEWART L. UDALL, Secretary GEOLOGICAL SURVEY Thomas B. Nolan, Director 1 CONTENTS [The letters in parentheses are those used to designate the chapters for separate publication] Page (A) Geophysical Abstracts 180, January-March--------------------- 1 (B) Geophysical Abstracts 181, April-June------------------------- 129 (C) Geophysical Abstracts 182, July-September--------------------- 281 (D) Geophysical Abstracts 183, October-December------------------ 457 (E) Index to Geophysical Abstracts 180-183, 1960 ------------------- 637 Under department orders, Geophysical Abstracts has been published at different times by the Bureau of Mines orthe Geological Survey as noted below. 1-86, May 1929-June 1936, Bureau of Mines Information Circulars. [Mimeographed] 87, July-December 1936, Geological Survey Bulletin 887. 88-91, 'January-December 1937, Geological Survey Bulletin 895. 92-95, January-December 1938, Geological Survey Bulletin 909. 96-99, January-December 1939, Geological Survey Bulletin 915. 100-103, January-December 1940, Geological Survey Bulletin 925. 104-107, January-December 1941, Geological Survey Bulletin 932. 108-111, January-December 1942, Geological Survey Bulletin 939. 112-127, January 1943-December 1946, Bureau of Mines Information Circu- lars. [Mimeographed] 128-131, January-December 1947, Geological Survey Bulletin 957. 132-135, January-December 1948, Geological Survey Bulletin 959. 136-139, January-December 1949, Geological Survey Bulletin 966. 140-143, January-December 1950, Geological Survey Bulletin 976. 144-147, January-December 1951, Geological Survey Bulletin 981. 148-151, January-December 1952, Geological Survey Bulletin 991. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Ron Hartman and the Lucerne Valley Meteorites by Robert Verish Ron Hartman and the Lucerne Valley Meteorites
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 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 2002–2011 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. -
To Thermal History of Metallic Asteroids
44th Lunar and Planetary Science Conference (2013) 1129.pdf TO THERMAL HISTORY OF METALLIC ASTEROIDS. E.N. Slyuta, Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Sciences, 119991, Kosygin St. 19, Moscow, Russia. [email protected]. Introduction: Physical-mechanical properties of interval of temperatures T-transition from plastic to a iron meteorites depend on structure, chemical and min- fragile condition in iron meteorites is not observed that eralogical composition, from short-term shock loading usually is not characteristic for technical alloys and and from temperature [1]. The yield strength increases, steels at which at decreasing of temperature the plas- if size of kamacite and rhabdites crystals decreases, ticity can decrease down to 0. For example, for iron- and nickel and carbon contents increases. The more Ni nickel alloy at Ni content about 5% the curve T-bend is content, the more taenite, microhardness of which is observed already about 200 K [5]. The mechanism of more than one of kamacite, and accordingly more yield plastic deformation in iron meteorites at low tempera- strength. Short-term shock loading up to 25 GPа also tures varies only. Deformation at 300 K occurs by slid- increases the yield strength. The temperature of small ing, and at 4.2 K and 77 K is accompanied by forma- bodies which unlike planetary bodies have no en- tion and development of static twins, i.e. mechanical dogenic activity and an internal thermal flux, is de- twinning as the basic mechanism of deformation in fined by insolation level and depends on a body posi- iron meteorites at low temperatures dominates [6]. -
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. -
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. -
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.