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Orbit and Dynamic Origin of the Recently Recovered Annama’S H5 Chondrite
ORBIT AND DYNAMIC ORIGIN OF THE RECENTLY RECOVERED ANNAMA’S H5 CHONDRITE Josep M. Trigo-Rodríguez1 Esko Lyytinen2 Maria Gritsevich2,3,4,5,8 Manuel Moreno-Ibáñez1 William F. Bottke6 Iwan Williams7 Valery Lupovka8 Vasily Dmitriev8 Tomas Kohout 2, 9, 10 Victor Grokhovsky4 1 Institute of Space Science (CSIC-IEEC), Campus UAB, Facultat de Ciències, Torre C5-parell-2ª, 08193 Bellaterra, Barcelona, Spain. E-mail: [email protected] 2 Finnish Fireball Network, Helsinki, Finland. 3 Dept. of Geodesy and Geodynamics, Finnish Geospatial Research Institute (FGI), National Land Survey of Finland, Geodeentinrinne 2, FI-02431 Masala, Finland 4 Dept. of Physical Methods and Devices for Quality Control, Institute of Physics and Technology, Ural Federal University, Mira street 19, 620002 Ekaterinburg, Russia. 5 Russian Academy of Sciences, Dorodnicyn Computing Centre, Dept. of Computational Physics, Valilova 40, 119333 Moscow, Russia. 6 Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302, USA. 7Astronomy Unit, Queen Mary, University of London, Mile End Rd. London E1 4NS, UK. 8 Moscow State University of Geodesy and Cartography (MIIGAiK), Extraterrestrial Laboratory, Moscow, Russian Federation 9Department of Physics, University of Helsinki, P.O. Box 64, 00014 Helsinki University, Finland 10Institute of Geology, The Czech Academy of Sciences, Rozvojová 269, 16500 Prague 6, Czech Republic Abstract: We describe the fall of Annama meteorite occurred in the remote Kola Peninsula (Russia) close to Finnish border on April 19, 2014 (local time). The fireball was instrumentally observed by the Finnish Fireball Network. From these observations the strewnfield was computed and two first meteorites were found only a few hundred meters from the predicted landing site on May 29th and May 30th 2014, so that the meteorite (an H4-5 chondrite) experienced only minimal terrestrial alteration. -
Possible Fluid Rock Interactions on Differentiated Asteroids Recorded in Eucritic Meteorites Jean-Alix Barrat, A
Possible fluid rock interactions on differentiated asteroids recorded in eucritic meteorites Jean-Alix Barrat, A. Yamaguchi, T.E. Bunch, Marcel Bohn, Claire Bollinger, Georges Ceuleneer To cite this version: Jean-Alix Barrat, A. Yamaguchi, T.E. Bunch, Marcel Bohn, Claire Bollinger, et al.. Possible fluid rock interactions on differentiated asteroids recorded in eucritic meteorites. Geochimica et Cosmochimica Acta, Elsevier, 2011, 75 (13), pp.3839-3852. insu-00586415 HAL Id: insu-00586415 https://hal-insu.archives-ouvertes.fr/insu-00586415 Submitted on 15 Apr 2011 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Possible fluid-rock interactions on differentiated asteroids recorded in eucritic meteorites by J.A. Barrat 1,2 , A. Yamaguchi 3,4 , T.E. Bunch 5, M. Bohn 1,2 , 1,2 6 C. Bollinger , and G. Ceuleneer 1Université Européenne de Bretagne, France. 2CNRS UMR 6538 (Domaines Océaniques), U.B.O.-I.U.E.M., Place Nicolas Copernic, 29280 Plouzané Cedex, France. E-Mail: [email protected] . 3National Institute of Polar Research, Tachikawa, Tokyo 190-8518, Japan 4Department of Polar Science, School of Multidisciplinary Science, Graduate University for Advanced Sciences, Tokyo 190-8518, Japan. -
JEM-EUSO: Meteor and Nuclearite Observations
Exp Astron DOI 10.1007/s10686-014-9375-4 ORIGINAL ARTICLE JEM-EUSO: Meteor and nuclearite observations M. Bertaina A. Cellino F. Ronga The JEM-EUSO· Collaboration· · Received: 22 August 2013 / Accepted: 24 February 2014 ©SpringerScience+BusinessMediaDordrecht2014 Abstract Meteor and fireball observations are key to the derivation of both the inven- tory and physical characterization of small solar system bodies orbiting in the vicinity of the Earth. For several decades, observation of these phenomena has only been possible via ground-based instruments. The proposed JEM-EUSO mission has the potential to become the first operational space-based platform to share this capabil- ity. In comparison to the observation of extremely energetic cosmic ray events, which is the primary objective of JEM-EUSO, meteor phenomena are very slow, since their typical speeds are of the order of a few tens of km/sec (whereas cosmic rays travel at light speed). The observing strategy developed to detect meteors may also be applied to the detection of nuclearites, which have higher velocities, a wider range of possible trajectories, but move well below the speed of light and can therefore be considered as slow events for JEM-EUSO. The possible detection of nuclearites greatly enhances the scientific rationale behind the JEM-EUSO mission. Keywords Meteors Nuclearites JEM-EUSO Space detectors · · · M. Bertaina (!) Dipartimento di Fisica, Universit`adiTorino,INFNTorino,viaP.Giuria1,10125Torino,Italy e-mail: [email protected] A. Cellino (!) INAF-Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy e-mail: [email protected] F. Ronga (!) Istituto Nazionale di Fisica Nucleare - Laboratori Nazionali di Frascati, Via E. -
Exploring the Geology of a New Differentiated Basaltic Asteroid
BUNBURRA ROCKHOLE: EXPLORING THE GEOLOGY OF A NEW DIFFERENTIATED BASALTIC ASTEROID. G.K. Benedix1,7, P.A. Bland1,7, J. M. Friedrich2,3, D.W. Mittlefehldt4, M.E. Sanborn5, Q.-Z. Yin5, R.C. Greenwood6, I.A. Franchi6, A.W.R. Bevan7, M.C. Towner1 and Grace C. Perotta2. 1Dept. Applied Geology, Curtin University, GPO Box U1987, Perth, WA, 6845 Australia ([email protected]), 2Dept. Chem., Fordham University, 441 East Fordham Road, Bronx, NY 10458 USA, 3Dept. Earth & Planetary Sciences, American Museum of Natural History, New York, NY 10024, USA, 4NASA/Johnson Space Center, Houston, TX, USA, 5Dept. of Earth and Planetary Sciences, University of California at Davis, Davis, CA 95616, USA, 6Planetary & Space Sci., The Open University, Milton Keynes, MK7 6AA, UK, 7Western Australia Museum, Locked Bag 49, Welshpool, WA, 6986, Australia. Introduction: Bunburra Rockhole (BR) is the first versity for chemical analysis. Four of these were ana- recovered meteorite of the Desert Fireball Network [1]. lysed for major and trace elements and two for trace It was initially classified as a basaltic eucrite, based on elements only. Two of these subsamples (A/1 and texture, mineralogy, and mineral chemistry [2] but C/A/2) were analysed at UC Davis to investigate the Cr subsequent O isotopic analyses showed that BR’s isotopic systematics. Homogenized powders from the composition lies significantly far away from the HED two chips were dissolved in Parr bombs for a 96 hour group of meteorites (fig. 1) [1]. This suggested that period at 200°C to insure complete dissolution of re- BR was not a piece of the HED parent body (4 Vesta), fractory minerals such as spinel. -
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 New Polymict Eucrite Dar Al Gani 983: Petrography, Chemical Composition, Noble Gas Record, and Evolution
Meteoritics & Planetary Science 40, Nr 6, 869–879 (2005) Abstract available online at http://meteoritics.org The new polymict eucrite Dar al Gani 983: Petrography, chemical composition, noble gas record, and evolution Andrea PATZER1*, Jochen SCHL‹TER2, Ludolf SCHULTZ3, Dolores H. HILL1, and William V. BOYNTON1 1Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721, USA 2Mineralogisches Museum der Universit‰t Hamburg, D-20146 Hamburg, Germany 3Max-Planck-Institut f¸r Chemie, D-55020 Mainz, Germany *Corresponding author. E-mail: [email protected] (Received 24 September 2004; revision accepted 07 April 2005) Abstract–Mineralogical and chemical studies of Dar al Gani 983 show that this meteorite is a eucrite. Its texture is that of an impact breccia. It contains cumulate pyroxene and feldspar megacrysts, a variety of recrystallized melt clasts, clasts of subophitic basalt, and mesostasis. These components are embedded in a matrix of fragmental pyroxene and plagioclase. In addition, the entire rock is penetrated by glassy melt veins and patches, and displays features of strong shock. The mineralogical and chemical evidence obtained for DaG 983 indicates that this meteorite experienced a complex evolutionary history. The presence of cumulate silicate crystals implies substantial, large scale cratering events on the HED asteroid. As a result of these impacts, rocks from different intrusive bodies to extrusive surface layers were laterally and vertically transported to form a thoroughly mixed megaregolith. DaG 983 represents a sample of this megabreccia. INTRODUCTION provide an outline of the geological settings involved in its formation. Our constraints on the evolutionary path of this Eucrites are differentiated achondrites and share a meteorite were derived from electron microprobe, common provenance with howardites and diogenites (e.g., instrumental neutron activation analysis (INAA), and noble Tschermak 1885; Stolper 1977; Clayton and Mayeda 1996). -
The Comet's Tale
THE COMET’S TALE Newsletter of the Comet Section of the British Astronomical Association Volume 9, No 1 (Issue 17), 2002 April JOEL HASTINGS METCALF MINISTER, HUMANITARIAN, ASTRONOMER Richard R Didick Joel Hastings Metcalf was born in The following account, taken used with either a single prism or Meadville, Pennsylvania, on from a newspaper article about a grating, both of which were January 4th, 1866, the son of him when he lived in Taunton, is provided. Lewis Herbert and Anna (Hicks) somewhat dubious since he Metcalf. Lewis was a Civil War actually bought the 7-inch In the observatory at Keesville, Veteran, a soldier who lost a leg refractor. "When but 14 years old the instrument was mounted in a at the first battle of "Bull Run" he built a telescope and ground very substantial dome, being and was held at Libby prison until out a lens with which he was able fastened to a fine cut granite base exchanged and discharged. to observe with success all the weighting about a ton. In a principal heavenly bodies. This February when Lake Champlain At the approximate age of 14, Joel was a small two-inch lens. His had frozen over, the whole outfit Metcalf borrowed Richard next attempt was a three-inch lens was loaded on sleds and started Proctor's book, Other Worlds and he later made one of three across the Lake on the ice. The Than Ours, from his Sunday and a half inches, which he ice was thick enough - but there school library which led him to an subsequently sold to Harvard are always long cracks in the interest in astronomy. -
19740026181.Pdf
DYNAMIC& AND PHOTOMETRIC INVESTIGATION OF COMETARY TYPE I1 TAILS Grant NGR 09-015-159 Semiannual Progress Report No. 6 For the period March 15 to September 14, 1974 Principal Investigator Dr. Zdenek Sekanina Prepared for . .-- National Aeronautics and Space Administration ; . Washington, D.C. 20546 q, ' ';'.. ',. : , , , - , .., ,: .,M, ._I _, . ..!..' , , .. ".. .,;-'/- Smithsonian Institution Astrophysical Observatory Cambridge, Massachusetts 02138 DYNAMICAL AND PHOTOMETRIC INVESTIGATION OF COMETARY TYPE 11 TAILS Grant NGR 09-015-159 Semiannual Progress Report No. 6 For the period March 15 to September 14, 1974 Principal Investigator Dr. Zdenek Sekanina Pre-ared for National Aeronautics and Space Administration Washington, D. C. 20546 Smithsonian Institut ion Astrophysical Observatory Sambridge, Massachusetts 02138 TABLE OF CONTENTS ABSTRACT ........................... iii PART A. COMPARISON OF THE WORKING MODEL FOR THE ANTITAIL OF COMET KOHOUTEK (1973f) WITH GROUND-BASED PHOTOGRAPHIC OBSERVATIONS . 1 1. Introduction ....................... 1 11. The Cerro Tololo photographs ............... 1 111. Photographic photometry of the Cerro Tololo plates. The technique ........................ 4 IV. Photographic photometry of the Cerro Tololo plates. The results ......................... V. Calibration stars for the Cerro Tololo plates ....... VI. Preliminary physical interpretation of the observed radial profiles of the antitail ................. VII. References ....................... PART B. OTHER ACTIVITIES IN THE REPORTED PERIOD ........... -
The Meteoritical Society Newsletter 2011
The Meteoritical Society Newsletter (November 2011) IN THIS ISSUE Important reminders From the President Annual Meetings Renew your membership by Jan. 1! Don’t risk From the Treasurer missing issues of MAPS. And, mailing you Publications Reports reminders is expensive. Renew online at http://metsoc.meteoriticalsociety.net. MAPS GCA Nominate your colleagues and students for Elements awards! Deadlines are in January. See From the Nomenclature Committee Awards section for details. From the Membership Committee Awards Nominations for new fellows are due in Recently Announced Awards January. Nominations are welcome. Call for Nominations From the Secretary Proposals to host the 2016 MetSoc meeting Election of New Council are due in March. Contact the secretary for MetSocCom - Electronic Discussion procedures. Group Vote in the Elements Poll if you haven’t Website Is Moving voted already. I am pleased to report on the some of the major PRESIDENT’S EDITORIAL accomplishments of the past year and some plans for the future. The reports by the treasurer and chairs of I am honored to take over as president from major committees that follow provide many more Hiroko Nagahara and can report that the new council details. has operated successfully for nine months. The new council has met twice, in Houston in March and in Annual Meetings Greenwich in August. One subtheme of our meetings has been to look for new ways to maintain the interest The 74th annual meeting of the Meteoritical and participation of all society members. Another has Society was held at the University of Greenwich in the been to call the attention of the broader scientific Old Royal Naval College on the banks of the River community to our activities. -
Meteorites: an Overview
Meteorites: An Overview Edward R. D. Scott* 1811-5209/11/0007-0047$2.50 DOI: 10.2113/gselements.7.1.47 eteorites come from numerous parent bodies with a wide variety chondrites are the most pristine, of geological histories. A few (~0.5%) come from Mars or the Moon; type 6 are the most metamor- phosed, and type 1 are the most Mthe rest are impact debris from collisions between asteroids orbiting aqueously altered. between Mars and Jupiter. Unlike terrestrial, Martian, and lunar rocks, the Asteroids that melted supply us asteroidal meteorites contain minerals that formed before the Sun and the with three major classes of mete- Solar System, during the growth of planetesimals and planets from the disk orites: irons, which are Fe–Ni of dust and gas around the Sun (“the solar nebula”), and during the first samples from the cores of aster- oids; metal-free silicate rocks from half-billion years of Solar System evolution. asteroidal mantles and crusts, Meteorites from unmelted asteroids are called chondrites; which are called achondrites as they are cosmic sediments composed of particles that were they lack chondrules; and stony irons, which are impact- generated mixtures of achondrites and Fe–Ni metal (Fig. present in the solar nebula (Fig. 1). The most abundant particles are millimeter-sized objects called chondrules, 2). Most irons (85%) are divided into thirteen groups which are solidified droplets of silicate magma. The chon- (called IAB, IIAB, IIC, etc.), which come from separate drules, associated grains of Fe–Ni metal, and a few volume parent bodies. The remaining ~15% probably come from percent or less of calcium–aluminum-rich inclusions another 50-odd parent bodies. -
Identification of Meteorite Source Regions in the Solar System
Icarus 311 (2018) 271–287 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Identification of meteorite source regions in the Solar System ∗ Mikael Granvik a,b, , Peter Brown c,d a Department of Physics, P.O. Box 64, 0 0 014 University of Helsinki, Finland b Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, Kiruna, Box 848, S-98128, Sweden c Department of Physics and Astronomy, University of Western Ontario, London N6A 3K7, Canada d Centre for Planetary Science and Exploration, University of Western Ontario, London N6A 5B7, Canada a r t i c l e i n f o a b s t r a c t Article history: Over the past decade there has been a large increase in the number of automated camera networks that Received 27 January 2018 monitor the sky for fireballs. One of the goals of these networks is to provide the necessary information Revised 6 April 2018 for linking meteorites to their pre-impact, heliocentric orbits and ultimately to their source regions in the Accepted 13 April 2018 solar system. We re-compute heliocentric orbits for the 25 meteorite falls published to date from original Available online 14 April 2018 data sources. Using these orbits, we constrain their most likely escape routes from the main asteroid belt Keywords: and the cometary region by utilizing a state-of-the-art orbit model of the near-Earth-object population, Meteorites which includes a size-dependence in delivery efficiency. While we find that our general results for escape Meteors routes are comparable to previous work, the role of trajectory measurement uncertainty in escape-route Asteroids identification is explored for the first time. -
Citizen Science with the Desert Fireball Network
EPSC Abstracts Vol. 13, EPSC-DPS2019-1178-2, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Fireballs in the Sky: Citizen Science with the Desert Fireball Network Brian Day (1), Phil Bland (2), Renae Sayers (2) (1) NASA Solar System Exploration Research Virtual Institute. NASA Ames Research Center. Moffett Field, CA, USA. ([email protected]) (2) Curtin University. Perth, WA, Australia. ([email protected]) ([email protected]) Abstract Curtin University in Western Australia. It is led by Phil Bland of Curtin University. Fireballs in the Sky is an innovative Australian citizen science program that connects the public with 2. Observatory Design and Network the research of the Desert Fireball Network (DFN). The observatories are fully autonomous intelligent This research aims to understand the early workings imaging systems, capable of operating for 12 months of the solar system, and Fireballs in the Sky invites in a harsh environment without maintenance, and people around the world to learn about this science, storing all imagery collected over that period. Each contributing fireball sightings via a user-friendly observatory uses a 36MP consumer DSLR camera augmented reality mobile app. Tens of thousands of equipped with a fisheye lens providing spatial people have downloaded the app world-wide and precision of approximately one arcminute. The participated in the science of meteoritics. The DSLR is modified with a liquid crystal (LC) shutter. Fireballs in the Sky app allows users to get involved The LC shutter is used to break the fire-ball trail into with the Desert Fireball Network research, dashes for velocity calculation, after triangulation.