The Secret History of the Tagish Lake Fireball 0
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Experimental and Petrological Constraints on Lunar Differentiation from the Apollo 15 Green Picritic Glasses
Meteoritics & Planetary Science 38, Nr 4, 515–527(2003) Abstract available online at http://meteoritics.org Experimental and petrological constraints on lunar differentiation from the Apollo 15 green picritic glasses Linda T. ELKINS-TANTON,1* Nilanjan CHATTERJEE,2 and Timothy L. GROVE2 1Department of Geological Sciences, Brown University, Providence, Rhode Island, 02912, USA 2Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA *Corresponding author: [email protected] (Received 15 July 2002; revision accepted 23 September 2002) Abstract–Phase equilibrium experiments on the most magnesian Apollo 15C green picritic glass composition indicate a multiple saturation point with olivine and orthopyroxene at 1520°C and 1.3 GPa (about 260 km depth in the moon). This composition has the highest Mg# of any lunar picritic glass and the shallowest multiple saturation point. Experiments on an Apollo 15A composition indicate a multiple saturation point with olivine and orthopyroxene at 1520°C and 2.2 GPa (about 440 km depth in the moon). The importance of the distinctive compositional trends of the Apollo 15 groups A, B, and C picritic glasses merits the reanalysis of NASA slide 15426,72 with modern electron microprobe techniques. We confirm the compositional trends reported by Delano (1979, 1986) in the major element oxides SiO2, TiO2, Al2O3, Cr2O3, FeO, MnO, MgO, and CaO, and we also obtained data for the trace elements P2O5, K2O, Na2O, NiO, S, Cu, Cl, Zn, and F. Petrogenetic modeling demonstrates that the Apollo 15 A-B-C glass trends could not have been formed by fractional crystallization or any continuous assimilation/fractional crystallization (AFC) process. -
FNESS Strategic Plan
Strategic Plan 2013-2015 At a Glance FNESS evolved from the Society of Native Indian Fire Fighters of BC (SNIFF), which was established in 1986. SNIFF’s initial objectives were to help reduce the number of fire-related deaths on First Nations reserves, but it changed its emphasis to incorporate a greater spectrum of emergency services. In 1994, SNIFF changed its name to First Nations’ Emergency Services Society of BC to reflect the growing diversity of services it provides. Today our organization continues to gain recognition and trust within First Nations communities and within Aboriginal Affairs and Northern Development Canada (AANDC) and other organizations. This is reflected in both the growing demand of service requests from First Nations communities and the development of more government-sponsored programs with FNESS. r e v Ri k e s l A Inset 1 Tagish Lake Teslin 1059 Daylu Dena Atlin Lake 501 Taku River Tlingit r e v Liard Atlin Lake i R River ku 504 Dease River K Fort a e Nelson T r t 594 Ts'kw'aylaxw e c iv h R ik River 686 Bonaparte a se a 687 Skeetchestn e D Fort Nelson R i v e First Nations in 543 Fort Nelson Dease r 685 Ashcroft Lake Dease Lake 592 Xaxli'p British Columbia 593 T'it'q'et 544 Prophet River 591 Cayoose Creek 692 Oregon Jack Creek 682 Tahltan er 683 Iskut a Riv kw r s e M u iv R Finlay F R Scale ra e n iv s i er 610 Kwadacha k e i r t 0 75 150 300 Km S 694 Cook's Ferry Thutade R r Tatlatui Lake i e 609 Tsay Keh Dene v Iskut iv 547 Blueberry River e R Lake r 546 Halfway River 548 Doig River 698 Shackan Location -
Chondrule Sizes, We Have Compiled and Provide Commentary on Available Chondrule Dimension Literature Data
Invited review Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups. Jon M. Friedricha,b,*, Michael K. Weisbergb,c,d, Denton S. Ebelb,d,e, Alison E. Biltzf, Bernadette M. Corbettf, Ivan V. Iotzovf, Wajiha S. Khanf, Matthew D. Wolmanf a Department of Chemistry, Fordham University, Bronx, NY 10458 USA b Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024 USA c Department of Physical Sciences, Kingsborough College of the City University of New York, Brooklyn, NY 11235, USA d Graduate Center of the City University of New York, 365 5th Ave, New York, NY 10016 USA e Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York 10964 USA f Fordham College at Rose Hill, Fordham University, Bronx, NY 10458 USA In press in Chemie der Erde – Geochemistry 21 August 2014 *Corresponding Author. Tel: +718 817 4446; fax: +718 817 4432. E-mail address: [email protected] 2 ABSTRACT The examination of the physical properties of chondrules has generally received less emphasis than other properties of meteorites such as their mineralogy, petrology, and chemical and isotopic compositions. Among the various physical properties of chondrules, chondrule size is especially important for the classification of chondrites into chemical groups, since each chemical group possesses a distinct size-frequency distribution of chondrules. Knowledge of the physical properties of chondrules is also vital for the development of astrophysical models for chondrule formation, and for understanding how to utilize asteroidal resources in space exploration. To examine our current knowledge of chondrule sizes, we have compiled and provide commentary on available chondrule dimension literature data. -
Constraining the Source Regions of Lunar Meteorites Using Orbital Geochemical Data
Meteoritics & Planetary Science 50, Nr 2, 214–228 (2015) doi: 10.1111/maps.12412 Constraining the source regions of lunar meteorites using orbital geochemical data A. CALZADA-DIAZ1,2*, K. H. JOY3, I. A. CRAWFORD1,2, and T. A. NORDHEIM2,4 1Department of Earth and Planetary Sciences, Birkbeck College, London WC1E 7HX, UK 2Centre for Planetary Sciences UCL/Birkbeck, London WC1E 6BT, UK 3School of Earth, Atmospheric and Environmental Sciences, University of Manchester, Manchester M13 9PL, UK 4Mullard Space Science Laboratory, University College London, Dorking RH5 6NT, UK *Corresponding author. E-mail: [email protected] (Received 30 July 2014; revision accepted 06 November 2014) Abstract–Lunar meteorites provide important new samples of the Moon remote from regions visited by the Apollo and Luna sample return missions. Petrologic and geochemical analysis of these meteorites, combined with orbital remote sensing measurements, have enabled additional discoveries about the composition and age of the lunar surface on a global scale. However, the interpretation of these samples is limited by the fact that we do not know the source region of any individual lunar meteorite. Here, we investigate the link between meteorite and source region on the Moon using the Lunar Prospector gamma ray spectrometer remote sensing data set for the elements Fe, Ti, and Th. The approach has been validated using Apollo and Luna bulk regolith samples, and we have applied it to 48 meteorites excluding paired stones. Our approach is able broadly to differentiate the best compositional matches as potential regions of origin for the various classes of lunar meteorites. Basaltic and intermediate Fe regolith breccia meteorites are found to have the best constrained potential launch sites, with some impact breccias and pristine mare basalts also having reasonably well-defined potential source regions. -
Lifetimes of Interstellar Dust from Cosmic Ray Exposure Ages of Presolar Silicon Carbide
Lifetimes of interstellar dust from cosmic ray exposure ages of presolar silicon carbide Philipp R. Hecka,b,c,1, Jennika Greera,b,c, Levke Kööpa,b,c, Reto Trappitschd, Frank Gyngarde,f, Henner Busemanng, Colin Madeng, Janaína N. Ávilah, Andrew M. Davisa,b,c,i, and Rainer Wielerg aRobert A. Pritzker Center for Meteoritics and Polar Studies, The Field Museum of Natural History, Chicago, IL 60605; bChicago Center for Cosmochemistry, The University of Chicago, Chicago, IL 60637; cDepartment of the Geophysical Sciences, The University of Chicago, Chicago, IL 60637; dNuclear and Chemical Sciences Division, Lawrence Livermore National Laboratory, Livermore, CA 94550; ePhysics Department, Washington University, St. Louis, MO 63130; fCenter for NanoImaging, Harvard Medical School, Cambridge, MA 02139; gInstitute of Geochemistry and Petrology, ETH Zürich, 8092 Zürich, Switzerland; hResearch School of Earth Sciences, The Australian National University, Canberra, ACT 2601, Australia; and iEnrico Fermi Institute, The University of Chicago, Chicago, IL 60637 Edited by Mark H. Thiemens, University of California San Diego, La Jolla, CA, and approved December 17, 2019 (received for review March 15, 2019) We determined interstellar cosmic ray exposure ages of 40 large ago. These grains are identified as presolar by their large isotopic presolar silicon carbide grains extracted from the Murchison CM2 anomalies that exclude an origin in the Solar System (13, 14). meteorite. Our ages, based on cosmogenic Ne-21, range from 3.9 ± Presolar stardust grains are the oldest known solid samples 1.6 Ma to ∼3 ± 2 Ga before the start of the Solar System ∼4.6 Ga available for study in the laboratory, represent the small fraction ago. -
Magnetite Biomineralization and Ancient Life on Mars Richard B Frankel* and Peter R Buseckt
Magnetite biomineralization and ancient life on Mars Richard B Frankel* and Peter R Buseckt Certain chemical and mineral features of the Martian meteorite with a mass distribution unlike terrestrial PAHs or those from ALH84001 were reported in 1996 to be probable evidence of other meteorites; thirdly, bacterium-shaped objects (BSOs) ancient life on Mars. In spite of new observations and up to several hundred nanometers long that resemble fos interpretations, the question of ancient life on Mars remains silized terrestrial microorganisms; and lastly, 10-100 nm unresolved. Putative biogenic, nanometer magnetite has now magnetite (Fe304), pyrrhotite (Fel_xS), and greigite (Fe3S4) become a leading focus in the debate. crystals. These minerals were cited as evidence because of their similarity to biogenic magnetic minerals in terrestrial Addresses magnetotactic bacteria. *Department of Physics, California Polytechnic State University, San Luis Obispo, California 93407, USA; e-mail: [email protected] The ancient life on Mars hypothesis has been extensively tDepartments of Geology and Chemistry/Biochemistry, Arizona State challenged, and alternative non-biological processes have University, Tempe, Arizona 85287-1404, USA; e-mail: [email protected] been proposed for each of the four features cited by McKay et al. [4]. In this paper we review the current situa tion regarding their proposed evidence, focusing on the Abbreviations putative biogenic magnetite crystals. BCM biologically controlled mineralization BIM biologically induced mineralization BSO bacterium-shaped object Evidence for and against ancient Martian life PAH polycyclic aromatic hydrocarbon PAHs and BSOs Reports of contamination by terrestrial organic materials [5°,6°] and the similarity of ALH84001 PAHs to non-bio genic PAHs in carbonaceous chondrites [7,8] make it Introduction difficult to positively identify PAHs of non-terrestrial, bio A 2 kg carbonaceous stony meteorite, designated genic origin. -
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. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Organic Matter in Meteorites Department of Inorganic Chemistry, University of Barcelona, Spain
REVIEW ARTICLE INTERNATIONAL MICROBIOLOGY (2004) 7:239-248 www.im.microbios.org Jordi Llorca Organic matter in meteorites Department of Inorganic Chemistry, University of Barcelona, Spain Summary. Some primitive meteorites are carbon-rich objects containing a vari- ety of organic molecules that constitute a valuable record of organic chemical evo- lution in the universe prior to the appearance of microorganisms. Families of com- pounds include hydrocarbons, alcohols, aldehydes, ketones, carboxylic acids, amino acids, amines, amides, heterocycles, phosphonic acids, sulfonic acids, sugar-relat- ed compounds and poorly defined high-molecular weight macromolecules. A vari- ety of environments are required in order to explain this organic inventory, includ- ing interstellar processes, gas-grain reactions operating in the solar nebula, and hydrothermal alteration of parent bodies. Most likely, substantial amounts of such Received 15 September 2004 organic materials were delivered to the Earth via a late accretion, thereby provid- Accepted 15 October 2004 ing organic compounds important for the emergence of life itself, or that served as a feedstock for further chemical evolution. This review discusses the organic con- Address for correspondence: Departament de Química Inorgànica tent of primitive meteorites and their relevance to the build up of biomolecules. Universitat de Barcelona [Int Microbiol 2004; 7(4):239-248] Martí i Franquès, 1-11 08028 Barcelona, Spain Tel. +34-934021235. Fax +34-934907725 Key words: primitive meteorites · prebiotic chemistry · chemical evolution · E-mail: [email protected] origin of life providing new opportunities for scientific advancement. One Introduction of the most important findings regarding such bodies is that comets and certain types of meteorites contain organic mole- Like a carpentry shop littered with wood shavings after the cules formed in space that may have had a relevant role in the work is done, debris left over from the formation of the Sun origin of the first microorganisms on Earth. -
For a Larger Version of the First Nations in British
#! Inset 1 Tagish Lake #! Teslin 502 Liard Atlin Lake #!501 Taku River Tlingit L 594 Ts'kw 'aylaxw iard #! Atlin Lake R 687 Skeetchestn ive #! ! 504 Dease River K r 686 Bonaparte # #! e r t e c iv h R ik #! a se a e D Fort Nelson R ! i # ! 592 Xaxli'p #! 685 Ashcroft v # e 543 Fort Nelson Dease r #! 593 T'it'q'et Lake Dease Lake #! First Nations 591 Cayoose Creek #! 692 Oregon Jack Creek 682 Tahltan #! 544 P rophet River r #! a ive in British Colum bia F R in British Colum bia 683 Iskut r #! kw a r s s e M u e iv r R Finlay R e iv n er i 610 Kw ad acha k Scale i t #! ! S R # 694 Cook's Ferry i v 0 75 150 300 km e r Thutade r e Lake I iv Tatlatui 609 Tsay Keh Dene skut R #! 547 Blueberry River Lake #! 698 Shackan #! #! #! #! 696 Nicom en 546 Halfw ay River 548 Doig River 705 Lytton #! #! Location of First Nation's 699 Nooaitch Main Community #! Williston Fort St John 707 Skuppah #! Lake N Indian Reserve a ! s 542 Saulteau # 706 Siska s #! #! 704 Kanaka Bar #! R Takla i 545 W est Moberly v City or Town e Lake r 532 Kispiox 533 Glen Vow ell 608 Takla 677 Nisga'a Village of New Aiyansh 537 Gitanyow 531 Gitanm aax #! #! Park and Protected Area 679 Nisga'a Village of Gitw inksihlkw #! #!!534 Hagw ilget 678 Nisga'a Village of Laxgalt'sap #!#! # #! 700 Boothroyd ! #! #! 535 Gitsegukla 671 Nisga'a Village of Gingolx#! # ! Babine #! 618 McLeod Lake 536 Gitw ar ngak # e 530 W itset v i Sm ithers 674 Lax Kw 'alaam s R Lake 617 Tl'azt'en ! 701 Boston Bar ! # #! Terrace #!680 Kitselas 728 Yekooche ! # #! # #! 730 Binche W hut'en 673 Metlakatla ena -
Meteoroids: the Smallest Solar System Bodies
Passage of Bolides through the Atmosphere 1 O. Popova Abstract Different fragmentation models are applied to a number of events, including the entry of TC3 2008 asteroid in order to reproduce existing observational data. keywords meteoroid entry · fragmentation · modeling 1 Introduction Fragmentation is a very important phenomenon which occurs during the meteoroid entry into the atmosphere and adds more drastic effects than mere deceleration and ablation. Modeling of bolide 6 fragmentation (100 – 10 kg in mass) may be divided into several approaches. Detail fitting of observational data (deceleration and/or light curves) allows the determination of some meteoroid parameters (ablation and shape-density coefficients, fragmentation points, amount of mass loss) (Ceplecha et al. 1993; Ceplecha and ReVelle 2005). Observational data with high accuracy are needed for the gross-fragmentation model (Ceplecha et al. 1993), which is used for the analysis of European and Desert bolide networks data. Hydrodynamical models, which describe the entry of the meteoroid 6 including evolution of its material, are applied mainly for large bodies (>10 kg) (Boslough et al. 1994; Svetsov et al. 1995; Shuvalov and Artemieva 2002, and others). Numerous papers were devoted to the application of standard equations for large meteoroid entry in the attempts to reproduce dynamics and/or radiation for different bolides and to predict meteorite falls. These modeling efforts are often supplemented by different fragmentation models (Baldwin and Sheaffer, 1971; Borovi6ka et al. 1998; Artemieva and Shuvalov, 2001; Bland and Artemieva, 2006, and others). The fragmentation may occur in different ways. For example, few large fragments are formed. These pieces initially interact through their shock waves and then continue their flight independently. -
Meteorite Wis91600: a New Sample Related to a D- Or T-Type Asteroid
Lunar and Planetary Science XXXVI (2005) 1564.pdf METEORITE WIS91600: A NEW SAMPLE RELATED TO A D- OR T-TYPE ASTEROID. T. Hiroi1, E. Tonui2, C. M. Pieters1, M. E. Zolensky3, Y. Ueda4, M. Miyamoto4, and S. Sasaki4,5, 1Dept. of Geological Sci., Brown University, Providence, RI 02912 ([email protected]), 2Dept. of Earth and Space Sci., University of California Los Angeles, 595 Charles Young Drive East, Los Angeles, CA 90095-1567, 3SN2, NASA Johnson Space Center, Houston, TX 77058, 4Dept. of Earth and Planetary Sci., University of Tokyo, Hongo, Tokyo 113- 0033, Japan, 5National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. Introduction: Since the Tagish Lake meteorite On the other hand, WIS91600 shows a very similar fell in January 2000, the assumed one-of-the-kind 3-µm feature to a T/D-type asteroid 308 Polyxo, if one meteorite has become the hottest issue among a peculiar data point of Polyxo at 3.5 µm can be disre- diversity of scientists. Meanwhile, as the physical garded and its VNIR spectrum shows a near-perfect origin of the meteorite in our solar system, D or T match with the average T/D asteroid spectrum as asteroids have been suggested by Hiroi et al. [1, 2] shown in Fig. 1. The VNIR spectrum, especially its based on comparison of their visible-near-infrared continuum slope, is believed to be strongly affected by (VNIR) reflectance spectra. While it is probably still the amount of carbon and other opaque phase, while true that the Tagish Lake meteorite is possibly the first the 3-µm band feature shows characteristics of the recovered sample from a D or T asteroid as a meteorite component hydrous minerals.