Australian Aborigines and Meteorites
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Cross-References ASTEROID IMPACT Definition and Introduction History of Impact Cratering Studies
18 ASTEROID IMPACT Tedesco, E. F., Noah, P. V., Noah, M., and Price, S. D., 2002. The identification and confirmation of impact structures on supplemental IRAS minor planet survey. The Astronomical Earth were developed: (a) crater morphology, (b) geo- 123 – Journal, , 1056 1085. physical anomalies, (c) evidence for shock metamor- Tholen, D. J., and Barucci, M. A., 1989. Asteroid taxonomy. In Binzel, R. P., Gehrels, T., and Matthews, M. S. (eds.), phism, and (d) the presence of meteorites or geochemical Asteroids II. Tucson: University of Arizona Press, pp. 298–315. evidence for traces of the meteoritic projectile – of which Yeomans, D., and Baalke, R., 2009. Near Earth Object Program. only (c) and (d) can provide confirming evidence. Remote Available from World Wide Web: http://neo.jpl.nasa.gov/ sensing, including morphological observations, as well programs. as geophysical studies, cannot provide confirming evi- dence – which requires the study of actual rock samples. Cross-references Impacts influenced the geological and biological evolu- tion of our own planet; the best known example is the link Albedo between the 200-km-diameter Chicxulub impact structure Asteroid Impact Asteroid Impact Mitigation in Mexico and the Cretaceous-Tertiary boundary. Under- Asteroid Impact Prediction standing impact structures, their formation processes, Torino Scale and their consequences should be of interest not only to Earth and planetary scientists, but also to society in general. ASTEROID IMPACT History of impact cratering studies In the geological sciences, it has only recently been recog- Christian Koeberl nized how important the process of impact cratering is on Natural History Museum, Vienna, Austria a planetary scale. -
Acadia Geology Alumni/Ae Newsletter
Acadia Geology Alumni/ae Newsletter Issue 21 December, 2009 Department of Earth and Environmental Science, Acadia University, Wolfville, Nova Scotia, B4P 2R6 [email protected] VIEW FROM ACADIA As I write this message, my term as the “acting head” course, it costs less to deliver. Another aspect of of Earth and Environmental Science is rapidly budgetary constraints is a lack of replacements for drawing to a close. Rob Raeside returns as head faculty on sabbatical. In the “good old days” such beginning Jan. 1, 2010, and it is probably a “toss-up” absences were typically covered by a full-time faculty as to which one of us is happier about that! To be replacement, but now we are lucky to receive one honest, however, I found many aspects of being “per-course replacement”. Such replacements have department head to be rewarding, and if we did not been great but they are paid specifically to teach the have a capable and willing incumbent returning to the single course assigned to them, and hence do not job, continuing in the role would have been OK. provide any coverage for other activities integral to running a department, such as counselling students, The past year at Acadia has more than lived up to the supervising honours and special project students, supposed ancient Chinese curse “may you live in serving on committees, and so on. This ripple-down interesting times”. The main topic occupying effect hits especially hard in a small department such everyone’s mind on campus has been the university as ours. Fortunately, faculty in E&ES have been budget. -
Metal-Silicate Fractionation and Chondrule Formation
A756 Goldschmidt 2004, Copenhagen 6.3.12 6.3.13 Metal-silicate fractionation and Fe isotopes fractionation in chondrule formation: Fe isotope experimental chondrules 1 2 2,3 constraints S. LEVASSEUR , B. A. COHEN , B. ZANDA , 2 1 1 1 1 2 2 R.H. HEWINS AND A.N. HALLIDAY X.K. ZHU , Y. GUO , S.H. TANG , A. GALY , R.D. ASH 2 AND R.K O’NIONS 1 ETHZ, Dep. of Earth Sciences, Zürich, Switzerland ([email protected]) 1 Lab of Isotope Geology, MLR, Chinese Academy of 2 Rutgers University, Piscataway, NJ, USA Geological Sciences, 26Baiwanzhuang Road, Beijing, 3 Muséum National d’Histoire Naturelle, Paris, France China ([email protected]) 2 Department of Earth Sciences, Oxford University, Parks Road, Oxford, OX1 3PR, UK Natural chondrules show an Fe-isotopic mass fractionation range of a few δ-units [1,2] that is interpreted either as the result of Fe depletion from metal-silicate Recent studies have shown that considerable variations of fractionation during chondrule formation [1] or as the Fe isotopes exist in both meteoritic and terrestrial materials, reflection of the fractionation range of chondrule precursors and that they are related, through mass-dependent [2]. In order to better understand the iron isotopic fractionation, to a single isotopically homogeneous source[1]. compositions of chondrules we conducted experiments to This implies that the Fe isotope variations recorded in the study the effects of reduction and evaporation of iron on iron solar system materials must have resulted from mass isotope systematics. fractionation incurred by the processes within the solar system About 80mg of powdered slag fayalite was placed in a itself. -
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. -
Compilation of Minimum and Maximum Isotope Ratios of Selected Elements in Naturally Occurring Terrestrial Materials and Reagents by T
U.S. Department of the Interior U.S. Geological Survey Compilation of Minimum and Maximum Isotope Ratios of Selected Elements in Naturally Occurring Terrestrial Materials and Reagents by T. B. Coplen', J. A. Hopple', J. K. Bohlke', H. S. Reiser', S. E. Rieder', H. R. o *< A R 1 fi Krouse , K. J. R. Rosman , T. Ding , R. D. Vocke, Jr., K. M. Revesz, A. Lamberty, P. Taylor, and P. De Bievre6 'U.S. Geological Survey, 431 National Center, Reston, Virginia 20192, USA 2The University of Calgary, Calgary, Alberta T2N 1N4, Canada 3Curtin University of Technology, Perth, Western Australia, 6001, Australia Institute of Mineral Deposits, Chinese Academy of Geological Sciences, Beijing, 100037, China National Institute of Standards and Technology, 100 Bureau Drive, Stop 8391, Gaithersburg, Maryland 20899 "institute for Reference Materials and Measurements, Commission of the European Communities Joint Research Centre, B-2440 Geel, Belgium Water-Resources Investigations Report 01-4222 Reston, Virginia 2002 U.S. Department of the Interior GALE A. NORTON, Secretary U.S. Geological Survey Charles G. Groat, Director The use of trade, brand, or product names in this report is for identification purposes only and does not imply endorsement by the U.S. Government. For additional information contact: Chief, Isotope Fractionation Project U.S. Geological Survey Mail Stop 431 - National Center Reston, Virginia 20192 Copies of this report can be purchased from: U.S. Geological Survey Branch of Information Services Box 25286 Denver, CO 80225-0286 CONTENTS Abstract...................................................... -
Abstract: Investigation of the Form and Age of the Bloody Creek Crater
Atlantic Geology . Volume 48 . 2012 40 Investigation of the form and age of the Bloody Creek Crater, southwestern Nova Scotia Mariella Nalepa1, Ian Spooner1, and Peter Williams2 1. Department of Earth and Environmental Science, Acadia Uni- versity, Wolfville, Nova Scotia B4P 2R6, Canada <[email protected]> ¶ 2. Department of Physics, Acadia Uni- versity, Wolfville, Nova Scotia B4P 2R6, Canada Virtually all terrestrial impact craters exhibit a circular geometry in plan-form; only three impact sites exhibiting non-circular, elongate forms have been identified on Earth. One of these exceptional sites is the Bloody Creek Crater located in southwestern Nova Scotia, an approximately 0.42 km long-axis elliptical crater first identified in 1987 during a regional air photo survey. It was confirmed as an impact crater in 2009 through integrated geomorphic, geophysical, and petrographic data. The structure’s rare ellipticity, pristine definition, preservation through shock metamorphic features of anomalously high pressures at the rim, low depth-to-diameter ratio, as well as age remain ambiguous and complicate the interpretation of the origin and evolution of the crater. The purpose of this study is to quantify the form of the feature in order to better understand the nature and age of impact. To achieve this objective, analytical software was used to assess the shape of the crater rim. An extensive review of the literature was also performed to understand the controls on crater formation as well as to synthesize a model for the geological evolution of the site which would aid in the interpretation of the age of the structure. Results demonstrate that the form of the crater rim is best approximated by an ellipse, as illustrated by comparison of the RMSE (Root-Mean-Square Error) calculated for various geometric models. -
New Unique Pyroxene Pallasite: Northwest Africa 10019 C
78th Annual Meeting of the Meteoritical Society (2015) 5084.pdf NEW UNIQUE PYROXENE PALLASITE: NORTHWEST AFRICA 10019 C. B. Agee, K. Ziegler, N. Muttik. Institute of Meteoritics and the Department of Earth and Planetary Sciences, University of New Mexico. E-mail: [email protected]. Introduction: Pyroxene pallasites were originally defined by the grouplet of Vermillion and Yamato 8451 [1], which have minor amounts (~1-3 vol%) of pyroxene, with oxygen isotope values that are distinct from the pallasite main group (PMG) and the Eagle Station grouplet (PES). In the meantime, additional pyroxene-bearing pallasites, Zinder, NWA 1911, and Choteau, have been discovered [2,3], however each of these meteorites appears to be unique based on oxygen isotopes and mineralogy -- thus not belonging to the original pyroxene pallasite grouplet. Here we report on yet another unique ungrouped pyroxene pallasite, Northwest Africa 10019, which now brings the total of distinct pyroxene pallasite types – possibly all from different parent bodies – to a total of five. History and Physical Chracteristics: NWA 10019 was purchased by Steve Arnold from Morocco in January 2015 and consisted of one 580 gram fusion crusted individual and 26 grams of several small fusion crusted pieces. Saw cuts and thin slices show angular orange-brown-green, translucent olivines (~50 vol%), the largest 28 mm long, with many smaller (0.5-5 mm) angular grains, some of which are darker colored orthopyroxenes (Fs15.4±0.2Wo1.0±0.2, Fe/Mn=23±1, n=6, ~10 vol %), all set in a matrix of taenite (Fe=72.0±4.0, Ni=27.4±2.4, Co=0.19±0.05 wt%, n=5, ~20 vol%) and kamacite (Fe=93.1±2.0, Ni=6.6±0.2, Co=0.61±0.03 wt%, n=4, ~15 vol %). -
ELEMENTAL ABUNDANCES in the SILICATE PHASE of PALLASITIC METEORITES Redacted for Privacy Abstract Approved: Roman A
AN ABSTRACT OF THE THESIS OF THURMAN DALE COOPER for theMASTER OF SCIENCE (Name) (Degree) in CHEMISTRY presented on June 1, 1973 (Major) (Date) Title: ELEMENTAL ABUNDANCES IN THE SILICATE PHASE OF PALLASITIC METEORITES Redacted for privacy Abstract approved: Roman A. Schmitt The silicate phases of 11 pallasites were analyzed instrumen- tally to determine the concentrations of some major, minor, and trace elements.The silicate phases were found to contain about 98% olivine with 1 to 2% accessory minerals such as lawrencite, schreibersite, troilite, chromite, and farringtonite present.The trace element concentrations, except Sc and Mn, were found to be extremely low and were found primarily in the accessory phases rather than in the pure olivine.An unusual bimodal Mn distribution was noted in the pallasites, and Eagle Station had a chondritic nor- malized REE pattern enrichedin the heavy REE. The silicate phases of pallasites and mesosiderites were shown to be sufficiently diverse in origin such that separate classifications are entirely justified. APPROVED: Redacted for privacy Professor of Chemistry in charge of major Redacted for privacy Chairman of Department of Chemistry Redacted for privacy Dean of Graduate School Date thesis is presented June 1,1973 Typed by Opal Grossnicklaus for Thurman Dale Cooper Elemental Abundances in the Silicate Phase of Pallasitic Meteorites by Thurman Dale Cooper A THESIS submitted to Oregon State University in partial fulfillment of the requirements for the degree of Master of Science June 1974 ACKNOWLEDGMENTS The author wishes to express his gratitude to Prof. Roman A. Schmitt for his guidance, suggestions, discussions, and thoughtful- ness which have served as an inspiration. -
Zac Langdon-Pole Art Basel Hong Kong
Zac Langdon-Pole Art Basel Hong Kong Michael Lett 312 Karangahape Road Cnr K Rd & East St PO Box 68287 Newton Auckland 1145 New Zealand P+ 64 9 309 7848 [email protected] www.michaellett.com Zac Langdon-Pole Passport (Argonauta) (i) 2018 paper nautilus shell, Seymchan meteorite (iron pallasite, landsite: Serbia, Russia) 79 x 25 x 45mm ZL5205 Zac Langdon-Pole Passport (Argonauta) (i) (side view) 2018 paper nautilus shell, Seymchan meteorite (iron pallasite, landsite: Serbia, Russia) 79 x 25 x 45mm ZL5205 Zac Langdon-Pole Passport (Argonauta) (ii) 2018 paper nautilus shell, Sikhote Alin meteorite (iron; coarse octahedrite, landsite: Sikhote Alin mountains, Russia) 103 x 30 x 55mm ZL5209 Zac Langdon-Pole Passport (Argonauta) (ii) (side view) 2018 paper nautilus shell, Sikhote Alin meteorite (iron; coarse octahedrite, landsite: Sikhote Alin mountains, Russia) 103 x 30 x 55mm ZL5209 Zac Langdon-Pole Passport (Argonauta) (iii) (front view and side view) 2018 paper nautilus shell, Nantan meteorite (iron; coarse octahedrite, landsite: Nantan, Peoples Republic of China) 135 x 45 x 95mm ZL5213 Zac Langdon-Pole Passport (Argonauta) (iv) (front view and side view) 2018 paper nautilus shell, Muonionalusta meteorite (iron; fine octahedrite, landsite: Norrbotten, Sweden) 95 x 33 x 65mm ZL5208 Zac Langdon-Pole Passport (Argonauta) (v) 2018 paper nautilus shell, Sericho meteorite (iron pallasite, landsite: Sericho, Kenya) 107 x 33 x 56mm ZL5210 Zac Langdon-Pole Passport (Argonauta) (v) (side view) 2018 paper nautilus shell, Sericho meteorite (iron -
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. -
Analysis of Iron Meteorites by Instrumental Neutron Activation with a Slowpoke Reactor
ANALYSIS OF IRON METEORITES BY INSTRUMENTAL NEUTRON ACTIVATION WITH A SLOWPOKE REACTOR J. Holzbecher and D^ E^ Ryan SLOWPOKE Facility, Dalhousie University Halifax, N. S., Canada, B3H 4J1 R. R. Brooks Department of Chemistry and Biochemistry Massey University Palmerston North, New Zealand In order to devise new methods of chemical classification of iron meteorites - as a refinement of Professor John Wasson's original work [1] - a comprehensive analysis programme has been initiated. The programme involves neutron activation analysis at Dalhousie University; inductively coupled plasma-mass spectrometry (ICP-MS) at the Geological Survey of Canada, Ottawa; mineralogical studies at William Rainey Harper College, Palatine, IL, USA; ICP, graphite furnace, and hydride generatioii atomic absorption spectrometry at Massey University. Analysis of 6 specimens of each of the 14 classes recognized by Professor Wasson are contemplated. This abstract summarizes the experiences in the direct neutron activation analysis of nearly 100 iron meteorites for rhodium, iridium, osmium and gold. At the concentration levels encountered in iron meteorites Rh, Os, Ir, Au, in addition to As and Co, can be readily quantified by direct, instrumental neutron activation analysis thus avoiding more commonly used time - consuming radiochemical separations. Two irradiation, decay and counting time schemes were used: 1) t. =5 min, t, = 1 min, t = 5 min , Samples were irradiated in a Cd-shielded site and counted with an LEP detector; the epithermal irradiation decreases the production of mCo (main activity) much more than that of ^tfi. The LEP detector is advantageous because of the low energies of both nuclides, i.e., 51.5 keV for Rh and 58.6 keV for Co respectively. -
List of Meteorites in the Collections of the Central Siberian Geological Museum at the V.S.Sobolev Institute of Geology and Mineralogy SB RAS (SIGM)
List of meteorites in the collections of the Central Siberian Geological Museum at the V.S.Sobolev Institute of Geology and Mineralogy SB RAS (SIGM). Year Mass in Pieces in Main mass in Indication Meteorite Country Type found SIGM SIGM SIGM in MB Novosibirsk Russia 1978 H5/6 9.628 kg 2 yes 59 Markovka Russia 1967 H4 7.9584 kg 5 yes 48 Ochansk Russia 1887 H4 407 g 1 Kunashak Russia 1949 L6 268 g 1 6 Saratov Russia 1918 L4 183.4 g 1 Elenovka Ukraine 1951 L5 148.7 g 2 6 Zhovtnevyi Ukraine 1938 H6 88.5 g 1 Nikolskoe Russia 1954 L4 39.5 g 1 6 Krymka Ukraine 1946 LL3.2 11.1 g 1 Yurtuk Ukraine 1936 Howardite 5.3 g 1 Pervomaisky Russia 1933 L6 595 g 1 Ivanovka Russia 1983 H5 904 g 1 63 Tsarev Russia 1968 H5 1.91972 kg 3 59 Norton County USA 1948 Aubrite 144 g 1 Stannern Cz. Republic 1808 18.1 g 1 Eucrite-mmict Poland 1868 H5 63.02 g 1 Pultusk Chelyabinsk Russia 2013 LL5 1.55083 kg 28 102 Yaratkulova Russia 2016 H5 25.71 g 1 105 Tobychan Russia 1971 Iron, IIE 41.4998 kg 2 yes 51 Elga Russia 1959 Iron, IIE 10.5 kg 1 16 Sikhote-Alin Russia 1947 Iron, IIAB 37.1626 kg 12 Chebankol Russia 1938 Iron, IAB-sHL 87.1 g 1 Chinga (Chinge) Russia 1912 Iron, ungrouped 5.902 kg 3 13 Kaalijarv (Kaali) Estonia 1937 2.88 g a lot of Iron, IAB-MG Boguslavka Russia 1916 Iron, IIAB 55.57 g 1 Bilibino Russia 1981 Iron, IIAB 570.94 g 1 60 Anyujskij Russia 1981 Iron, IIAB 435.4 g 1 60 Sychevka Russia 1988 Iron, IIIAB 1.581 kg 1 70 Darjinskoe Kazakhstan 1984 Iron, IIC 6 kg 1 yes 78 Maslyanino Russia 1992 Iron, IAB complex 58 kg 2 yes 78 Onello Russia 1998 Iron, ungrouped