DOCSLIB.ORG

METEORITES Ioannis Haranas Dept

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

ROCKS FROM SPACE CALLED METEORITES Ioannis Haranas Dept. of Physics and Computer Science , Wilfrid Laurier University , 75 University Ave. W. Waterloo, ON, N2L 3C5, CANADA e-mail: [email protected] The word meteor is derived from the Greek word Μετέωρος (meteoros) = Suspended in the air Rocks from space can be classified in 4 different categories: 1. Meteorites 2. Meteors (also called shooXng stars) 2 3. Micrometeorides 4. Bolides Meteorite (Earth Fall) Meteorite is a solid debris piece, which survives impact with the Earth's surface aer moving through the Earth’s atmosphere. One of the ~400 meteorites recovered from AntarcXca during the 2012-2013 season. (Image from Planetary Science Research Division at the University of Hawai’i- Manoa) Meteorite: MARS FALL Iron meteorites on the surface of Mars. This is Mars Rover taken picture. Discovery Rover is roboc moving vehicle. METEOROIDS • A meteoroid is a small rocky or metallic body traveling through space. • It is called a meteoroid just before it falls on the surface of the Earth. • Meteoroids are significantly smaller than asteroids, and range in size from small grains to 1 meter-wide objects. • Around 15,000 tones of meteoroids, micrometeoroids and different forms of space dust enter Earth's atmosphere each year. BOLIDES Bolide is either an extraterrestrial body that collides with the Earth, or an excepXonally bright, fireball-like meteor regardless of whether it finally impacts the surface. WHERE METEORITES ORIGINATE FROM? Most meteorites are fragments of small planets shaered by collisions early in the history of the Solar System. They are now called asteroids or comets, that originate in outer space. These remnants form the Asteroid Belt, where many thousands of small objects connuously circle the Sun between the orbits of MARS and JUPITER 230-780 million km away! ORBITS OF KNOWN METEORITES PRIBRAM The first meteorite to have its fall to Earth recorded by a camera network, enabling its inbound trajectory and LOSTCITY orbit to be determined and the meteorite to be recovered. Cameras operated by the Ondrejov Observatory in the Czech LOST CITY Republic recorded a brilliant fireball on Apr. 7, 1959. The second meteorite fall to be recorded by a camera network, thus enabling its trajectory and orbit to be determined and a quick recovery of the fragments, which weighed a total of 17 kg. The Lost City meteorite was found upon analysis to be an H5 chondrite. Jan. 3, 1970 HOW BIG ARE THEY? Meteoroids have a preky big size range. They include any space debris bigger than a molecule and smaller than about 100 meters objects. Anything bigger than 100 m this is considered an Asteroid. HOW MANY DIFFERENT KINDS ARE THERE? WHAT ARE THEY MADE OFF? IRON METEORITES (Fe, Ni & Co (>95%), Ni (5%-25 ) : Most iron meteorites likely originate in the cores of large asteroids, and are composed almost enXrely of nickel-iron alloy, and represent only 5% of the falls. Rancho Gomelia, Mexico, Octahedrite. This iron meteorite has been cut, polished and etched with acid on one face to reveal an interlocking crystal structure of nickel-iron alloys of varying composion. Photo by D. Ball, ASU STONY METEORITES (Mg2SiO4 ): • The most common type of meteorite, are generally composed of approximately 75 to 90 % silicon-based minerals. • Stony meteorites account for 94 % of observed meteorite falls. Warden; an ordinary (H5) chondrite from Western Australia. Photo © D. Ball, ASU STONY – IRON METEORITES (50% nickel-iron and 50% silicate material ): • Stony-iron meteorites contain approximately even amounts of silicates and nickel-iron alloy 1-2% of meteorites. Albin, WY, pallasite. This slice, which is about 18 cenmeters long, has been illuminated from behind to disnguish its olivine content from the surrounding metal. Photo by D. Ball, ASU. HOW FAST DO THEY MOVE? WHY THEY SOMETIMES FALL ON THE EARTH? ARE THEY A PART OF OUR SOLAR SYSTEM? They enter Earth’s atmosphere at velocity from 11 to 70 km per second (km/s). Meteors can fall on Earth for any sort of reason. The main reason is that they are loose bits of rock which have escaped gravitational pull of a planet and the earth has more mass and therefore pulls them into our planet. They are part of the original material that formed the Solar System. Apophis NASA is tracking over 800 objects of more than 1km across, and anything with a diameter of over 3km is considered a global catastrophic risk. The biggest recent scare was from APOPHIS which is around 325 meters across. When it was discovered in 2004, it was esXmated there was a 2.7% chance of impact in 2029, and it Close approach of Apophis on will create a crater of a diameter April 13, 2029 (as known in 4.3 km. February 2005 New informaon has shown we're safe aer all! Is a near-Earth asteroid that caused a brief period of concern in December 2004 because initial observations indicated a probability of up to 2.7% that it would hit Earth on April 13, 2029. The white bar indicates uncertainty in the range of positions (as known in February 2005) Apophis HypotheCcal Impact Scenario θ APOPHIS EARTH IMPACT: HYPOTHETICAL SCENARIO COMPUTER INPUT MODEL SIMULATION PARAMETERS • Distance from Impact: 120.00 km ( = 74.50 miles ) Toronto –Waterloo distance • Projectile diameter: 325.00 meters ( = 1070.00 feet ) • Projectile Density: 3200 kg/m3 • Impact Velocity: 30.70 km per second ( = 19.10 miles per second ) • Impact Angle: 10 degrees • Target Density: 1000 kg/m3 • Target Type: Liquid water of depth 5.0 km ( = 3.1 miles ), over crystalline rock. ENERGY CALCULATION AND ATMOSPHERIC ENTRY • Energy before atmospheric entry: 2.72 x 1019 Joules = 6.49 x 103 MegaTons TNT • The average interval between impacts of this size somewhere on Earth during the last 4 billion years is 9.5 x 104years • The projectile begins to breakup at an altitude of 61.50 km • The projectile bursts into a cloud of fragments at an altitude of 16.5 meters • The residual velocity of the projectile fragments after the burst is 5.99 km/s • The energy of the airburst is 2.61 x 1019 Joules = 6.24 x 103 MegaTons. • No crater is formed, although large fragments may strike the surface. MAJOR GLOBAL CHANGES • The Earth is not strongly disturbed by the impact and loses negligible mass. • The impact does not make a noticeable change in the tilt of Earth's axis (< 5/100 = 0.05 of a degree). • The impact does not shift the Earth's orbit noticeably. AIR BLAST • The air blast will arrive approximately 6.06 minutes after impact. • Peak Overpressure: 17100 Pa = 0.171 bars = 2.43 psi • Max wind velocity: 37.6 m/s = 84.1 mph • Sound Intensity: 85 dB (Loud as heavy traffic) • Damage Description: Glass windows will shatter. TSUNAMI WAVE The impact-generated tsunami wave arrives approximately 21.3 minutes after impact. Tsunami wave amplitude is less than 4.7 meters ( = 15.4 feet). HOW IS THE EARTH PROTECTED? YOU CAN CALL EARTHS NATURAL PROTECTION MECHANISM! HOW IS THIS POSSIBLE? This is Earth’s strange companion: Near-Earth asteroid 3753 Cruithne. Its orbit was first Xme predicted in 1997 by two Canadian York University astronomers , Dr. P.Weigert and Dr. K. Innanen, and Dr. S. Mikkola from Univ. of Turku, Finland . This curious 5 km in diameter companion it takes 770 years for the to complete a horseshoe-shaped. Every 385 years, it comes to its closest point around the Earth. GRUINTHE THROUGH TELESCOPE Gruithne: historical people known to have lived in the British Isles during the Iron Age vARIOUS METEORITE SAMPLES THA HAVE FALLEN ON THE EARTH This is a close up picture of our Campo del Cielo Meteorite from surface cut (Patrick Herman, Toronto 2014) Campo del Cielo 1,000 kilometers northwest of Buenos Aires, Argentina. El Chaco: The 37 ton Main Mass of the Campo del Cielo Iron Meteorite 1 ton= 1000 kilogram THANK YOU!!! .
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.
  • Tree-Ring Dating of Meteorite Fall in Sikhote-Alin, Eastern Siberia – Russia

    Tree-Ring Dating of Meteorite Fall in Sikhote-Alin, Eastern Siberia – Russia

    International Journal of Astrobiology, Page 1 of 6 1 doi:10.1017/S1473550411000309 © Cambridge University Press 2011 Tree-ring dating of meteorite fall in Sikhote-Alin, Eastern Siberia – Russia R. Fantucci1, Mario Di Martino2 and Romano Serra3 1Geologi Associati Fantucci e Stocchi, 01027 Montefiascone (VT), Italy e-mail: [email protected] 2INAF-Osservatorio Astronomico di Torino, 10025 Pino Torinese, Italy 3Dipartimento di Fisica, Università di Bologna, via Irnerio 46, 40126 Bologna, Italy Abstract: This research deals with the fall of the Sikhote-Alin iron meteorite on the morning of 12 February 1947, at about 00:38 h Utrecht, in a remote area in the territory of Primorsky Krai in Eastern Siberia (46°09′ 36″N, 134°39′22″E). The area engulfed by the meteoritic fall was around 48 km2, with an elliptic form and thousands of craters. Around the large craters the trees were torn out by the roots and laid radially to the craters at a distance of 10–20 m; the more distant trees had broken tops. This research investigated through dendrocronology n.6 Scots pine trees (Pinus Sibirica) close to one of the main impact craters. The analysis of growth anomalies has shown a sudden decrease since 1947 for 4–8 years after the meteoritic impact. Tree growth stress, detected in 1947, was analysed in detail through wood microsection that confirmed the winter season (rest vegetative period) of the event. The growth stress is mainly due to the lost crown (needle lost) and it did not seem to be caused due to direct damages on trunk and branches (missing of resin ducts).
  • Radar-Enabled Recovery of the Sutter's Mill Meteorite, A

    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.
  • Characteristics of a Bright Fireball and Meteorite Fall at Buzzard Coulee, Saskatchewan, Canada, November 20, 2008

    Characteristics of a Bright Fireball and Meteorite Fall at Buzzard Coulee, Saskatchewan, Canada, November 20, 2008

    40th Lunar and Planetary Science Conference (2009) 2505.pdf CHARACTERISTICS OF A BRIGHT FIREBALL AND METEORITE FALL AT BUZZARD COULEE, SASKATCHEWAN, CANADA, NOVEMBER 20, 2008. A. R. Hildebrand1, E. P. Milley1 , P. G. Brown2, P. J. A. McCausland2, W. Edwards2, M. Beech3, A. Ling4, G. Sarty5, M. D. Paulson4, L. A. Maillet1, S. F. Jones1 and M. R. Stauffer5. 1Department of Geoscience, 2500 University Drive NW, University of Calgary, Calgary, AB T2N 1N4 ([email protected], [email protected]), 2Department of Physics and Astronomy, The University of Western Ontario, London, ON, N6A 3K7, 3Department of Physics, Campion College at the University of Regina, Regina, SK S4S 0A2, 4Edmonton Centre, Royal Astronomical Society of Canada, 5Departments of Physics and En- gineering Physics and Department of Geological Sciences, University of Saskatchewan, Saskatoon, SK S7N 5E2. Introduction: A bright fireball was widely ob- tion surfaces (angular shapes with numerous small served across Alberta, Saskatchewan and Manitoba piezoglypts) presumably reflecting the meteoroids’ during late twilight on November 20, 2008. Interviews significant fragmentation extending deep into the at- of eyewitnesses and crude calibrations of security cam- mosphere; a larger proportion of mature ablation sur- eras constrained the fall region and the first search faces and oriented individuals may occur up range in attempt recovered meteorites off the ice of a manmade the strewn field. Fusion crusts are a typical dark gray pond in Buzzard Coulee, SK, Nov. 27, 2008. for an ordinary chondrite fall with more vitreous crusts Trajectory and Pre-fall Orbit: The fireball and on the back of some oriented specimens. The fall is subsequent dust trail, or shadows cast by the fireball, also distinguished by the large proportion of meteor- were widely recorded by all-sky (4) and security video ites that exhibit freshly broken surfaces with no fusion cameras (at least 19) establishing that its brightest por- crust; broken surfaces with variable amounts of “paint- tion occurred from 17:26:40 to 17:26:45 MST.
  • Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery and Characterization

    Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery and Characterization

    O. P. Popova, et al., Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery and Characterization. Science 342 (2013). Chelyabinsk Airburst, Damage Assessment, Meteorite Recovery, and Characterization Olga P. Popova1, Peter Jenniskens2,3,*, Vacheslav Emel'yanenko4, Anna Kartashova4, Eugeny Biryukov5, Sergey Khaibrakhmanov6, Valery Shuvalov1, Yurij Rybnov1, Alexandr Dudorov6, Victor I. Grokhovsky7, Dmitry D. Badyukov8, Qing-Zhu Yin9, Peter S. Gural2, Jim Albers2, Mikael Granvik10, Läslo G. Evers11,12, Jacob Kuiper11, Vladimir Kharlamov1, Andrey Solovyov13, Yuri S. Rusakov14, Stanislav Korotkiy15, Ilya Serdyuk16, Alexander V. Korochantsev8, Michail Yu. Larionov7, Dmitry Glazachev1, Alexander E. Mayer6, Galen Gisler17, Sergei V. Gladkovsky18, Josh Wimpenny9, Matthew E. Sanborn9, Akane Yamakawa9, Kenneth L. Verosub9, Douglas J. Rowland19, Sarah Roeske9, Nicholas W. Botto9, Jon M. Friedrich20,21, Michael E. Zolensky22, Loan Le23,22, Daniel Ross23,22, Karen Ziegler24, Tomoki Nakamura25, Insu Ahn25, Jong Ik Lee26, Qin Zhou27, 28, Xian-Hua Li28, Qiu-Li Li28, Yu Liu28, Guo-Qiang Tang28, Takahiro Hiroi29, Derek Sears3, Ilya A. Weinstein7, Alexander S. Vokhmintsev7, Alexei V. Ishchenko7, Phillipe Schmitt-Kopplin30,31, Norbert Hertkorn30, Keisuke Nagao32, Makiko K. Haba32, Mutsumi Komatsu33, and Takashi Mikouchi34 (The Chelyabinsk Airburst Consortium). 1Institute for Dynamics of Geospheres of the Russian Academy of Sciences, Leninsky Prospect 38, Building 1, Moscow, 119334, Russia. 2SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA. 3NASA Ames Research Center, Moffett Field, Mail Stop 245-1, CA 94035, USA. 4Institute of Astronomy of the Russian Academy of Sciences, Pyatnitskaya 48, Moscow, 119017, Russia. 5Department of Theoretical Mechanics, South Ural State University, Lenin Avenue 76, Chelyabinsk, 454080, Russia. 6Chelyabinsk State University, Bratyev Kashirinyh Street 129, Chelyabinsk, 454001, Russia.
  • ELEMENTAL ABUNDANCES in the SILICATE PHASE of PALLASITIC METEORITES Redacted for Privacy Abstract Approved: Roman A

    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.
  • Numerical Modeling of the 2013 Meteorite Entry in Lake Chebarkul, Russia

    Numerical Modeling of the 2013 Meteorite Entry in Lake Chebarkul, Russia

    Nat. Hazards Earth Syst. Sci., 17, 671–683, 2017 www.nat-hazards-earth-syst-sci.net/17/671/2017/ doi:10.5194/nhess-17-671-2017 © Author(s) 2017. CC Attribution 3.0 License. Numerical modeling of the 2013 meteorite entry in Lake Chebarkul, Russia Andrey Kozelkov1,2, Andrey Kurkin2, Efim Pelinovsky2,3, Vadim Kurulin1, and Elena Tyatyushkina1 1Russian Federal Nuclear Center, All-Russian Research Institute of Experimental Physics, Sarov, 607189, Russia 2Nizhny Novgorod State Technical University n. a. R. E. Alekseev, Nizhny Novgorod, 603950, Russia 3Institute of Applied Physics, Nizhny Novgorod, 603950, Russia Correspondence to: Andrey Kurkin ([email protected]) Received: 4 November 2016 – Discussion started: 4 January 2017 Revised: 1 April 2017 – Accepted: 13 April 2017 – Published: 11 May 2017 Abstract. The results of the numerical simulation of possi- Emel’yanenko et al., 2013; Popova et al., 2013; Berngardt et ble hydrodynamic perturbations in Lake Chebarkul (Russia) al., 2013; Gokhberg et al., 2013; Krasnov et al., 2014; Se- as a consequence of the meteorite fall of 2013 (15 Febru- leznev et al., 2013; De Groot-Hedlin and Hedlin, 2014): ary) are presented. The numerical modeling is based on the – the meteorite with a diameter of 16–19 m flew into the Navier–Stokes equations for a two-phase fluid. The results of ◦ the simulation of a meteorite entering the water at an angle earth’s atmosphere at about 20 to the horizon at a ve- ∼ −1 of 20◦ are given. Numerical experiments are carried out both locity of 17–22 km s . when the lake is covered with ice and when it is not.
  • The Chelyabinsk Meteorite Fall on February 15, 2013 Attracted Much

    The Chelyabinsk Meteorite Fall on February 15, 2013 Attracted Much

    46th Lunar and Planetary Science Conference (2015) 2686.pdf MINERALOGY, PETROLOGY, CHRONOLOGY, AND EXPOSURE HISTORY OF THE CHELYABINSK METEORITE AND PARENT BODY. K. Righter1, P. Abell1, D. Agresti2, E. L. Berger3, A.S. Burton1, J.S. Delaney4, M.D. Fries1, E.K. Gibson1, R. Harrington5, G. F. Herzog4, L.P. Keller1, D. Locke6, F. Lindsay4, T.J. McCoy7, R.V. Morris1, K. Nagao8, K. Nakamura-Messenger1, P.B. Niles1, L. Nyquist1, J. Park4, Z.X. Peng9, C.- Y.Shih10, J.I. Simon1, C.C. Swisher, III4, M. Tappa11, and B. Turrin4. 1NASA-JSC, Houston, TX 77058; 2Department of Physics, University of Alabama at Birmingham, Birmingham, AL 35294-1170; 3GeoControl Systems Inc.– Jacobs JETS contract – NASA JSC; 4Rutgers Univ., Wright Labs-Chemistry Dept., Piscataway, NJ; 5UTAS – Jacobs JETS Contract, NASA-JSC; 6HX5 – Jacobs JETS Contract, NASA-JSC; 7Smithsonian Institution, PO Box 37012, MRC 119, Washington, DC; 8Laboratory for Earthquake Chemistry, University of Tokyo, Hongo, Bunkyo- ku, Tokyo 113-0033, Japan; 9Barrios Tech – Jacobs JETS Contract, NASA-JSC; 10Jacobs JETS Contract, NASA- JSC; 11Aerodyne Industries – Jacobs JETS Contract, NASA-JSC. Introduction: The Chelyabinsk meteorite fall in impact melt veins (Figure 2), as compared to on February 15, 2013 attracted much more atten- results of shock experiments [20]. tion worldwide than do most falls [1-3]. A con- Chronology: Portions of light and dark lithol- sortium led by JSC received 3 masses of Chelya- ogies from Chel-101, and the impact melt brecci- binsk (Chel-101, -102, -103) that were collected as (Chel-102 and Chel-103) were prepared and shortly after the fall and handled with care to analyzed for Rb-Sr, Sm-Nd, and Ar-Ar dating.
  • Sikhote-Alin Meteorite, Elemental Composition Analysis Using CF LIBS

    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.
  • Team Studies Rare Meteorite Possibly from the Outer Asteroid Belt 20 December 2012

    Team Studies Rare Meteorite Possibly from the Outer Asteroid Belt 20 December 2012

    Team studies rare meteorite possibly from the outer asteroid belt 20 December 2012 The asteroid approached on an orbit that still points to the source region of CM chondrites. From photographs and video of the fireball, Jenniskens calculated that the asteroid approached on an unusual low-inclined almost comet-like orbit that reached the orbit of Mercury, passing closer to the sun than known from other recorded meteorite falls. "It circled the sun three times during a single orbit of Jupiter, in resonance with that planet," Jenniskens said. Based on the unusually short time that the asteroid was exposed to cosmic rays, there was not much time to go slower or faster around the sun. That puts the original source asteroid very (Phys.org)—Scientists found treasure when they close to this resonance, in a low inclined orbit. studied a meteorite that was recovered April 22, 2012 at Sutter's Mill, the gold discovery site that "A good candidate source region for CM chondrites led to the 1849 California Gold Rush. Detection of now is the Eulalia asteroid family, recently the falling meteorites by Doppler weather radar proposed as a source of primitive C-class asteroids allowed for rapid recovery so that scientists could in orbits that pass Earth," adds Jenniskens. study for the first time a primitive meteorite with little exposure to the elements, providing the most pristine look yet at the surface of primitive asteroids. An international team of 70 researchers reported in today's issue of Science that this meteorite was classified as a Carbonaceous-Mighei or CM-type carbonaceous chondrite and that they were able to identify for the first time the source region of these meteorites.
  • Seismo-Ionospheric Effects Associated with 'Chelyabinsk' Meteorite During

    Seismo-Ionospheric Effects Associated with 'Chelyabinsk' Meteorite During

    Seismo-ionospheric effects associated with 'Chelyabinsk' meteorite during the first 25 minutes after its fall O.I. Berngardt June 27, 2021 Abstract This paper presents the properties of ionospheric irregularities elon- gated with Earth magnetic field during the first 25 minutes after the fall of the meteorite 'Chelyabinsk' experimentally observed with EKB radar of Russian segment of the SuperDARN. It is shown that 40 minutes before meteor fall the EKB radar started to observe powerful scattering from irregularities elongated with the Earth magnetic field in the F-layer. Scattering was observed for 80 minutes and stopped 40 minutes after the meteorite fall. During 9-15 minutes after the meteorite fall at ranges 400-1200 km from the explosion site a changes were observed in the spectral and amplitude characteristics of the scattered signal. This features were the sharp increase in the Doppler frequency shift of the scattered signal corresponding to the Doppler velocities about 600 m/s and the sharp increase of the scattered signal amplitude. This allows us to conclude that we detected the growth of small-scale ionospheric irreg- ularities elongated with the Earth magnetic field at E-layer heights. Joint analysis with the seismic data and numerical modeling shows that the observed effect is connected with the passage of secondary acoustic front formed by supersonic seismic ground wave from the 'Chelyabinsk' meteorite. As a possible explanation the growth of elongated ionospheric ir- arXiv:1409.5927v1 [physics.geo-ph] 21 Sep 2014 regularities may be caused by the passage of the high-speed acoustic wave in the ionosphere in the presence of high enough background electric field.
  • Pre-Fall Orbit of the Buzzard Coulee Meteoroid

    Pre-Fall Orbit of the Buzzard Coulee Meteoroid

    Pre-fall Orbit of the Buzzard Coulee Meteoroid E. P. Milley University of Calgary, Calgary, Alberta [email protected] and A. R. Hildebrand University of Calgary, Calgary, Alberta and P. G. Brown The University of Western Ontario, London, Ontario and M. Noble Royal Astronomical Society of Canada, Edmonton, Alberta and G. Sarty University of Saskatchewan, Saskatoon, Saskatchewan and A. Ling Royal Astronomical Society of Canada, Edmonton, Alberta and L. A. Maillet University of Calgary, Calgary, Alberta Summary A large, bright fireball was widely observed by tens of thousands of eyewitnesses on the evening of November 20, 2008. Subsequently thousands of meteorites fell to the ground and more than 2,500 have been recovered from an area in and near to Buzzard Coulee, Saskatchewan. Many un-calibrated cameras recorded the violent fall of this ~2m boulder. A novel method of calibrating the shadows cast by the fireball has been developed and used to triangulate the atmospheric trajectory. Results show that the rock travelled along a path of 167.5° azimuth at a fairly steep angle of 66.7° altitude. Using timing information with direct measurements of the fireball’s position in the sky an initial velocity of (18.0 ± 0.4) km/s has been determined. An atmospheric trajectory and initial velocity are sufficient data to derive the pre-fall orbit of Buzzard Coulee. The resulting orbit shows that the meteoroid was in a near-Earth Apollo-type orbit before impact. Buzzard Coulee is one of only 14 meteorites worldwide to be associated with a pre-fall orbit. GeoCanada 2010 – Working with the Earth 1 Introduction A bright bolide was observed by tens of thousands of people in Saskatchewan, Alberta, Manitoba and Montana on the night of November 20, 2008.