A9 Meteorite Scientists

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METEORITE SCIENTISTS INTRODUCTION In this activity you are going to: Learn about the different types of meteorites, how they form and where they come from Investigate 5 different objects from the meteorite box Use your understanding of meteorites to identify the 5 objects Branding PLANETARY SCIENTISTS Planetary scientists apply the science of geology and space to other worlds. This includes other planets, moons and meteorites! Jane MacArthur, Planetary Scientist – University of Leicester WHAT IS A METEORITE? Simply: A rock from space that hits the Earth Scientifically: A bit more complicated! MANY DIFFERENT NAMES Asteroid A large rocky body found between Mars and Jupiter Atmosphere Meteoroid A smaller fragment of an asteroid outside of the Earth’s atmosphere Meteor A meteoroid that is burning up in the atmosphere Meteorite The fragments that make it to the surface of the Earth WHERE DO THEY COME FROM? Mars Asteroid Belt Jupiter THREE MAIN TYPES STONY NOTE! All asteroid belt meteorites contain some iron I RON STONY - I RON TYPES OF METEORITE Meteorites Stony Iron Stony - iron Some Stony Meteorites have small spherical shapes called chondrules. TheyMeteorite all have type: some iron in. Made of iron Meteorite subtype: Made of: Iron meteorites surrounding Features: are very dense olivine (glass like) (heavy for their crystals size) Chondrules Branding METEORITES ALSO HAVE… What happens to a meteorite as it tears through the Earth’s atmosphere? Fusion crust Dark brown/black surface with ripples, waves or bubbles in from the melted rock and escaping gases The outside of the meteorite heats up as it squashes the air in front of it IMPACTITES Melted material from below a meteorite impact. Gets solid as it cools. Looks like bubbly glass. Can be different colours. Tektite Glass Impactite CHALLENGE! Investigate the samples and use describing words (adjectives) for each one. Can you work out what your sample is? STATION 1 IRON METEORITE STATION 2 CHONDRITE METEORITE STATION 3 LIBYAN GLASS IMPACTITE STATION 4 TEKTITE STATION 5 IRON METEORITE .

Recommended publications

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.
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.
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.
Trace Element Inventory of Meteoritic Ca-Phosphates

American Mineralogist, Volume 102, pages 1856–1880, 2017 Trace element inventory of meteoritic Ca-phosphates DUSTIN WARD1,*, ADDI BISCHOFF1, JULIA ROSZJAR2, JASPER BERNDT3, AND MARTIN J. WHITEHOUSE4 1Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany 2Department of Mineralogy and Petrography, Natural History Museum Vienna, Burgring 7, 1010 Vienna, Austria 3Institut für Mineralogie, Westfälische Wilhelms-Universität Münster, Corrensstrasse 24, 48149 Münster, Germany 4Department of Geosciences, Swedish Museum of Natural History, Box 50007, 10405 Stockholm, Sweden ABSTRACT Most extraterrestrial samples feature the two accessory Ca-phosphates (apatite-group minerals and merrillite), which are important carrier phases of the rare earth elements (REE). The trace-element concentrations (REE, Sc, Ti, V, Cr, Mn, Co, As, Rb, Sr, Y, Zr, Nb, Ba, Hf, Ta, Pb, Th, and U) of se- lected grains were analyzed by LA-ICP-MS and/or SIMS (REE only). This systematic investigation includes 99 apatite and 149 merrillite analyses from meteorites deriving from various asteroidal bodies including 1 carbonaceous chondrite, 8 ordinary chondrites, 3 acapulcoites, 1 winonaite, 2 eucrites, 5 shergottites, 1 ureilitic trachyandesite, 2 mesosiderites, and 1 silicate-bearing IAB iron meteorite. Although Ca-phosphates predominantly form in metamorphic and/or metasomatic reactions, some are of igneous origin. As late-stage phases that often incorporate the vast majority of their host’s bulk REE budget, the investigated Ca-phosphates have REE enrichments of up to two orders of magnitude compared to the host rock’s bulk concentrations. Within a single sample, each phosphate species displays a uniform REE-pattern, and variations are mainly restricted to their enrichment, therefore indicating similar formation conditions.
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.
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.