Rok Meteorytu Pu³tusk
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Laboratory Spectroscopy of Meteorite Samples at UV-Vis-NIR Wavelengths: Analysis and Discrimination by Principal Components Analysis
Laboratory spectroscopy of meteorite samples at UV-Vis-NIR wavelengths: Analysis and discrimination by principal components analysis Antti Penttil¨aa,∗, Julia Martikainena, Maria Gritsevicha, Karri Muinonena,b aDepartment of Physics, P.O. Box 64, FI-00014 University of Helsinki, Finland bFinnish Geospatial Research Institute FGI, National Land Survey of Finland, Geodeetinrinne 2, FI-02430 Masala, Finland Abstract Meteorite samples are measured with the University of Helsinki integrating-sphere UV-Vis- NIR spectrometer. The resulting spectra of 30 meteorites are compared with selected spectra from the NASA Planetary Data System meteorite spectra database. The spectral measure- ments are transformed with the principal component analysis, and it is shown that different meteorite types can be distinguished from the transformed data. The motivation is to im- prove the link between asteroid spectral observations and meteorite spectral measurements. Keywords: Meteorites, spectroscopy, principal component analysis 1. Introduction While a planet orbits the Sun, it is subject to impacts by objects ranging from tiny dust particles to much larger asteroids and comet nuclei. Such collisions of small Solar System bodies with planets have taken place frequently over geological time and played an 5 important role in the evolution of planets and development of life on the Earth. Every day approximately 30{180 tons of interplanetary material enter the Earth's atmosphere [1, 2]. This material is mostly represented by smaller meteoroids that undergo rapid ablation in the atmosphere. Under favorable initial conditions part of a meteoroid may survive the atmospheric entry and reach the ground [3]. The fragments recovered on the ground are 10 called meteorites, our valuable samples of the Solar System. -
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. -
The Mineralogical Magazine Journal
THE MINERALOGICAL MAGAZINE AND JOURNAL OF THE MINERALOGICAL SOCIETY. 1~o. 40. OCTOBER 1889. Vol. VIII. On the Meteorites which have been found iu the Desert of Atacama and its neighbourhood. By L. FLETCHER, M.A., F.R.S., Keeper of Minerals in the British Museum. (With a Map of the District, Plate X.) [Read March 12th and May 7th, ]889.J 1. THE immediate object of the present paper is to place on record J- the history and characters of several Atacama meteorites of which no description has yet been published; but incidentally it is con- venient at the same time to consider the relationship of these masses to others from the same region, which either have been already described, or at least are stated to be preserved in one or more of the known Meteo. rite-Collections. 2. The term " Desert of Atacama " is generally applied to that part of western South America which lies between the towns of Copiapo and Cobija, about 330 miles distant from each other, and which extends island as far as the Indian hamlet of Antofagasta, about 180 miles from 224 L. FLETCHER ON THE METEORITES OF ATACAMA. the coast. The Atacama meteorites preserved in the Collections have been found at several places widely separated throughout the Desert. 3. A critical examination of the descriptive literature, and a compari- son of the manuscript and printed meteorite-lists, which have been placed at my service, lead to the conclusion that all the meteoritic frag- ments from Atacama now preserved in the known Collections belong to one or other of at most thirteen meteorites, which, for reasons given below, are referred to in this paper under the following names :-- 1. -
Meteorites: Rocks from Space
Learning more... Meteorites: rocks from space Meteorites: Rocks from space It has been estimated that 100,000 rocks from space tonnes of extraterrestrial material Every year the Earth is showered by reach the Earth’s surface every year. It extraterrestrial material falling from can be anything from fine dust to space. The Museum’s mineralogy and metallic masses weighing many tonnes. petrology collections include a small Extraterrestrial material that falls towards the holding of meteorites, and a display of Earth is classified by size. The majority of this some of this material is on show in the material is in the form of tiny particles called rocks and minerals aisle of the main micrometeorites. They fall continuously, and court, along with a large touchable arrive unnoticed. specimen that fell in Nantan in China. Meteors or ‘shooting stars’ are often seen in a clear night sky. They are larger dust particles and small rocky fragments, many no more than a gram in weight, which are burnt up by friction as they fall through the Earth’s atmosphere. Meteorites are larger pieces of rock that reach the Earth’s surface without getting burnt up in the atmosphere. A meteorite whose arrival has been witnessed is called a fall. Meteorites discovered without a known time of fall are The Nantan meteorite called finds. All meteorites, falls and finds, are This meteorite comes from either Lihu or Yaozhai town in named after the place where they were picked Nantan County, Guangxi, China, where it fell in 1516. It is an iron meteorite weighing over 155 pounds (71kg), and is up. -
W Numerze: – Wywiad Z Kustoszem Watykańskiej Kolekcji C.D. – Cz¹stki
KWARTALNIK MI£OŒNIKÓW METEORYTÓW METEORYTMETEORYT Nr 3 (63) Wrzesieñ 2007 ISSN 1642-588X W numerze: – wywiad z kustoszem watykañskiej kolekcji c.d. – cz¹stki ze Stardusta a meteorytry – trawienie meteorytów – utwory sp³ywania na Sikhote-Alinach – pseudometeoryty – konferencja w Tucson METEORYT Od redaktora: kwartalnik dla mi³oœników OpóŸnieniami w wydawaniu kolejnych numerów zaczynamy meteorytów dorównywaæ „Meteorite”, którego sierpniowy numer otrzyma³em Wydawca: w paŸdzierniku. Tym razem g³ówn¹ przyczyn¹ by³y k³opoty z moim Olsztyñskie Planetarium komputerem, ale w koñcowej fazie redagowania okaza³o siê tak¿e, i Obserwatorium Astronomiczne ¿e brak materia³u. Musia³em wiêc poczekaæ na mocno opóŸniony Al. Pi³sudskiego 38 „Meteorite”, z którego dorzuci³em dwa teksty. 10-450 Olsztyn tel. (0-89) 533 4951 Przeskok o jeden numer niezupe³nie siê uda³, a zapowiedzi¹ [email protected] dalszych k³opotów jest mi³y sk¹din¹d fakt, ¿e przep³yw materia³ów zacz¹³ byæ dwukierunkowy. W najnowszym numerze „Meteorite” konto: ukaza³ siê artyku³ Marcina Cima³y o Moss z „Meteorytu” 3/2006, 88 1540 1072 2001 5000 3724 0002 a w kolejnym numerze zapowiedziany jest artyku³ o Morasku BOŒ SA O/Olsztyn z „Meteorytu” 4/2006. W rezultacie jednak bêdzie mniej materia³u do Kwartalnik jest dostêpny g³ównie t³umaczenia i trzeba postaraæ siê o dalsze w³asne teksty. Czy mo¿e ktoœ w prenumeracie. Roczna prenu- merata wynosi w 2007 roku 44 z³. chcia³by coœ napisaæ? Zainteresowanych prosimy o wp³a- Z przyjemnoœci¹ odnotowujê, ¿e nabieraj¹ tempa przygotowania cenie tej kwoty na konto wydawcy do kolejnej konferencji meteorytowej, która planowana jest na 18—20 nie zapominaj¹c o podaniu czytel- nego imienia, nazwiska i adresu do kwietnia 2008 r. -
DISTRIBUTION of PULTUSK METEORITE FRAGMENTS. T. Brachaniec1 and J. W. Kosiński2, 1University of Silesia; Faculty of Earth Science; Bedzinska Str
45th Lunar and Planetary Science Conference (2014) 1067.pdf DISTRIBUTION OF PULTUSK METEORITE FRAGMENTS. T. Brachaniec1 and J. W. Kosiński2, 1University of Silesia; Faculty of Earth Science; Bedzinska str. 60, 41-200 Sosnowiec; email: [email protected], 2Comet and Meteor Workshop - Meteorites Section, Warsaw; email: [email protected]. Pultusk meteorite, which is classified as a brec- Modern research of literature and field working ciated H5 chondrite [1] fell at 30th of January 1868 in (Fig. 1) clearly show that the map created by Sam- Central Poland. The bolide was witnessed over a huge sonowicz is only a approximate picture of the distribu- part of Europe, from cities in Hungary and Austria in tion of Pultusk meteorites. The result of a field search- the south, to Gdańsk (Poland), Russia, in the north, ing is an observation that in a small area occur small and big specimens. Author has been claimed that in and from Berlin (Germany), in the west to Grodno the central part of the ellipse should be found speci- (Belarus), in the east. The shock from the bolide re- mens from 0.2 to 2 kg, however, in this area occur portedly collapsed structures in Warsaw, 60 km south small meteorites, weighing a few grams, called “Pul- of where it impacted. Within a few days of the fall, tusk peas”. There are many indications that Sam- about 400 pieces of the meteorite were collected. sonowicz also overestimated the amount of fallen me- After 80 years after the fall Samsonowicz as first teorites [3][4]. published his field working results [2]. -
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 -
Report of the United States National Museum
— THE METEORITE COLLECTION IN THE U. S. NATIONAL MUSEUM; A CATALOGUE OF METEORITES REPRESENTED NOVEMBER 1, 1886, By F. W. Clarke. The following catalogue has been prepared mainly to facilitate ex- changes and to aid in the upbuilding of the collection. In addition to the usual information as to title, date of fall, and weight of specimen, it has beeu thought well to give the source from which each example was obtained ; and it may be interesting to note that the meteorites ac- credited to Dr. J. Berrien. Lindsley were mainly received by him from the late Dr. J. Lawrence Smith. In the catalogue of the Shepard col- lection, now on deposit in the Museum, the arrangement of Professor Shepard himself has been followed without change. Including the Shepard meteorites, over 200 falls are now on exhibition, giving the entire collection a very respectable place among the larger collections of the world. The Tucson iron is unique, and therefore a cut of it is inserted. METEORIC IRONS. 1. Scriba, Oswego County, N. Y. Fouud about 1834. Fragment, 9.15 grammes. By exchange from S. C. H. Bailey. 2. Burlington, Otsego County, N. Y. Ploughed up previous to 1819. Weight of specimen, 76.87 grammes. By exchange from Prof. C. U. Shepard. 3. Lockport, Niagara County, N. Y. Ploughed up earlier thau 1845. Slice weigh- ing 155 grammes. By exchange from the cabinet of Yale College. 4. Jenny's Cheek, Wayne County, W. Va. Found in 1884. Several small frag- ments, 25.5 grammes in all; largest fragment, 15.3 grammes. -
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 -
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. -
The Origin of Ancient Magnetic Activity on Small Planetary Bodies: a Nanopaleomagnetic Study
The Origin of Ancient Magnetic Activity on Small Planetary Bodies: A Nanopaleomagnetic Study James Francis Joseph Bryson Department of Earth Sciences University of Cambridge This dissertation is submitted for the degree of Doctor of Philosophy Selwyn College October 2014 To my family and teachers Declaration I hereby declare that except where specific reference is made to the work of others, the contents of this dissertation are original and have not been submitted in whole or in part for consideration for any other degree or qualification in this, or any other University. This dissertation is the result of my own work and includes nothing which is the outcome of work done in collaboration, except where specifically indicated in the text. This dissertation contains fewer than 225 pages of text, appendices, illustrations, captions and bibliography. James Francis Joseph Bryson October 2014 Acknowledgements First and foremost, I would like to acknowledge my supervisors, Richard Harrison and Simon Redfern. Without Richard’s hard work, dedication, supervision and direction this project would not have been possible, and I feel privileged to have worked with him. Simon should be thanked for his guidance, hours of entertainment and awful jokes. I would like to acknowledge all of my collaborators, in particular Nathan Church, Claire Nichols, Roberts Blukis, Julia Herrero-Albillos, Florian Kronast, Takeshi Kasama and Francis Nimmo. Each has played an invaluable role in acquiring and understanding the data in this thesis and I would not have reached this point without their expertise and help. Martin Walker must be thanked for his assistance and calming influence. I would like to also thank Ioan Lascu for proof-reading this thesis and general advice.