Tuesday, August 9, 2016 POSTER SESSION: METEORITES, HOW DO THEY GET HERE, and HOW DO WE COLLECT THEM? 5:30 P.M
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Olivine and Pyroxene from the Mantle of Asteroid 4 Vesta ∗ Nicole G
Earth and Planetary Science Letters 418 (2015) 126–135 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Olivine and pyroxene from the mantle of asteroid 4 Vesta ∗ Nicole G. Lunning a, , Harry Y. McSween Jr. a,1, Travis J. Tenner b,2, Noriko T. Kita b,3, Robert J. Bodnar c,4 a Department of Earth and Planetary Sciences and Planetary Geosciences Institute, University of Tennessee, Knoxville, TN 37996, USA b Department of Geosciences, University of Wisconsin, Madison, WI 53706, USA c Department of Geosciences, Virginia Tech, Blacksburg, VA 24061, USA a r t i c l e i n f o a b s t r a c t Article history: A number of meteorites contain evidence that rocky bodies formed and differentiated early in our solar Received 25 September 2014 system’s history, and similar bodies likely contributed material to form the planets. These differentiated Received in revised form 25 February 2015 rocky bodies are expected to have mantles dominated by Mg-rich olivine, but direct evidence for such Accepted 25 February 2015 mantles beyond our own planet has been elusive. Here, we identify olivine fragments (Mg# = 80–92) in Available online 17 March 2015 howardite meteorites. These Mg-rich olivine fragments do not correspond to an established lithology Editor: T. Mather in the howardite–eucrite–diogenite (HED) meteorites, which are thought to be from the asteroid 4 Keywords: Vesta; their occurrence in howardite breccias, combined with diagnostic oxygen three-isotope signatures planetary formation and minor element chemistry, indicates they are vestan. -
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. -
Hydrated Minerals and Carbonaceous Chondrite Fragments in Lohawat Howardite: Astrobiological Implications: M
Astrobiology Science Conference 2015 (2015) 7069.pdf HYDRATED MINERALS AND CARBONACEOUS CHONDRITE FRAGMENTS IN LOHAWAT HOWARDITE: ASTROBIOLOGICAL IMPLICATIONS: M. S. Sisodia, A. Basu Sarbadhikari and R. R. Maha- jan. PLANEX, Physical Reasearch Laboratory, Ahmedabad, India (E-mail: [email protected]; [email protected]) Introduction: Presence of hydrated minerals on nebula caused initial melting and subsequent gradual asteroids, which are remnants of the blocks that formed differentiation of these early accreting bodies into the planets of the solar system has great importance for crust, mantle and core [4]. Dawn’s results confirm that deducing the origin of Earth’s water. Asteroid 4 Vesta Vesta is a differentiated protoplanet and that it is a is the parent body of the howardite-eucrite-diogenite parent body of HED meteorites [5]. The presence of (HED) family of the meteorites that have fallen on hydrated minerals on vesta as revealed by Lohawt Earth [1]. Lohawat howardite that fell in India in the howardite is very significant. Howardites originate year 1994 is a heterogeneous breccia composed of va- from the surface of Vesta nad constitute representative riety of mineral and lithic fragments [2]. We report samples from its crust, mantle and core. The low gravi- here optical study of hydrated minerals that we found ty of Vesta induce lower velocities to the impactors in Lohawat howardite and then discuss their astrobio- resulting into incomplete melting of impacting carbo- logical implications. naceous chondrites [6]. Whether these hydrated miner- Petrography of Lohawat howardite: Lohawat als were contributed on the surface of Vesta by carbo- howardite is an assortment of different minerals and naceous chondrites will be revealed by isotope study clasts. -
Carbonaceous Chondrite-Rich Howardites; the Potential for Hydrous Lithologies on the Hed Parent
CARBONACEOUS CHONDRITE-RICH HOWARDITES; THE POTENTIAL FOR HYDROUS LITHOLOGIES ON THE HED PARENT. J. S. Herrin 1,2 , M. E. Zolensky 2, J. A. Cartwright 3, D. W. Mittle- fehldt 2, and D. K. Ross 1,2 . 1ESCG Astromaterials Research Group, Houston, Texas, USA ( [email protected] ), 2NASA Johnson Space Center, Houston, Texas, USA, 3Max Planck Institut für Chemie, Mainz, Germany. Introduction: Howardites, eucrites, and dioge- clasts texturally resembling CM2 up to 7mm occupy- nites, collectively referred to as the “HED’s”, are a ing nearly half of the sample area accompanied 1-5 clan of meteorites thought to represent three different mm subangular impact melt clasts containing relict lithologies from a common parent body. Collectively eucritic fragments. The remaining medium and fine they are the most abundant type of achondrites in terre- fraction of the specimen consists of mm-to-sub-mm strial collections [1]. Eucrites are crustal basalts and angular-to-subrounded eucritic, diogenitic, carbona- gabbros, diogenites are mostly orthopyroxenites and ceous chondrite clasts set in a medium-to-coarse angu- are taken to represent lower crust or upper mantle ma- lar matrix of same materials. The eucrite/diogenite terials, and howardites are mixed breccias containing ratio of identifiable clasts is approximately 50/50. The both lithologies and are generally regarded as derived total modal abundance of visible carbonaceous chon- from the regolith or near-surface. drite fragments is ~60%. The presence of exogenous chondritic material in PRA 04402 is a howardite breccia consisting of howardite breccias has long been recognized [2,3]. As mm-to-sub-mm subrounded-to-subangular diogenite a group, howardites exhibit divergence in bulk chemi- and eucritic clasts in roughly equal proportions set in a stry from what would be produced by mixing of dioge- medium-to-coarse matrix. -
1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. -
Finegrained Precursors Dominate the Micrometeorite Flux
Meteoritics & Planetary Science 47, Nr 4, 550–564 (2012) doi: 10.1111/j.1945-5100.2011.01292.x Fine-grained precursors dominate the micrometeorite flux Susan TAYLOR1*, Graciela MATRAJT2, and Yunbin GUAN3 1Cold Regions Research and Engineering Laboratory, 72 Lyme Road, Hanover, New Hampshire 03755–1290, USA 2University of Washington, Seattle, Washington 98105, USA 3Geological & Planetary Sciences MC 170-25, Caltech, Pasadena, California 91125, USA *Corresponding author. E-mail: [email protected] (Received 15 May 2011; revision accepted 22 September 2011) Abstract–We optically classified 5682 micrometeorites (MMs) from the 2000 South Pole collection into textural classes, imaged 2458 of these MMs with a scanning electron microscope, and made 200 elemental and eight isotopic measurements on those with unusual textures or relict phases. As textures provide information on both degree of heating and composition of MMs, we developed textural sequences that illustrate how fine-grained, coarse-grained, and single mineral MMs change with increased heating. We used this information to determine the percentage of matrix dominated to mineral dominated precursor materials (precursors) that produced the MMs. We find that at least 75% of the MMs in the collection derived from fine-grained precursors with compositions similar to CI and CM meteorites and consistent with dynamical models that indicate 85% of the mass influx of small particles to Earth comes from Jupiter family comets. A lower limit for ordinary chondrites is estimated at 2–8% based on MMs that contain Na-bearing plagioclase relicts. Less than 1% of the MMs have achondritic compositions, CAI components, or recognizable chondrules. Single mineral MMs often have magnetite zones around their peripheries. -
Hed) Meteorites
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1374.pdf COMPARING THE CYSTALLOGRAPHIC STRUCTURES OF THE HOWARDITE, EUCRITE AND DIOGENITE (HED) METEORITES. L.V. Forman1, L. Daly2,1, T. J. Barrett3, 1Space Science and Technology Centre, School of Earth and Planetary Science, Curtin University, Bentley, 6102, Australia. (lu- [email protected]), 2School of Geographical and Earth Sciences, University of Glasgow, Glasgow, G12 8QQ, UK. 3Open University, Milton Keynes, MK7 6AA, UK, Introduction: The Howardite, Eucrite, Diogenite (HED) meteorites are a group of achondrite meteor- ites that likely originate from the same parent body (e.g. [1, 2]), which is believed to be 4 Vesta [3]. As HED meteorites are some of the oldest achondrites in our collections [4], they can provide valuable insights into processes occurring on small bodies early in the Solar System. To provide further constraints of the geological history of the HED parent body, we are undertaking a systematic cryatallographic analysis of a suite of HED meteorites by using electron backscatter diffraction (EBSD) analyses. Preliminary work has focused on the meteorties Allan Hills (ALH) 88135, a howardite polymict breccia, and Camel Donga, a eucrite mo- nomict breccia. Method: Thin sections of each sample were pol- ished using 1 µm and 0.3 µm alluminium sphere sus- pension fluid for 15 minutes each, and a colloidal silica NaOH suspension for 4 hours. The sections Figure 2. An EBSD phase map of ALH 88135. The colours were left uncoated to permit analysis at low vaccum. reveal the distribution of each mineral phase within this EBSD analyses were conducted on the samples using region. -
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. -
Lev A. Muravyev , Viktor I. Grokhovsky
The Chrono List of Bad Meteorites Harmful № Date Name Place Type Fall Description Source 1Ural Federal University, specimen 1,2 Lombardia, Doubtful 2 1 04.09.1511 Crema shwr several killed birds, sheep, and a man (dbt) [3, 7] Lev A. Muravyev , Institute of Geophysics Ural Branch of RAS, Italy meteorite Doubtful 2 04.09.1654 Milan Italy {?} - killed a monk (dbt) [3, 7] 1 Ekaterinburg, Russia; meteorite Aquitaine, crushed cottage, killed farmer and Viktor I. Grokhovsky 3 24.07.1790 Barbotan H5 shwr - [1, 10] [email protected], [email protected] France some cattle (dbt) Uttar Pradesh, [7, 9, Abstract. The problem of the asteroid-comet hazard is now being 4 19.12.1798 Benares (a) LL4 shwr 0,9 kg building India 10] actively discussed, because the consequences of the fall of large cosmic Bayern, 5 13.12.1803 Mässing Howardite U - building struck [1, 10] bodies on the earth can be catastrophic and affect the survival of Germany humanity and all living things. Fragments of smaller celestial bodies - Moscow, 6 05.09.1812 Borodino H5 U 0,5 kg observed by a soldier on guard [7] meteorites, fall to the earth much more often, and they can also emanate Russia a certain danger. In several papers that were published about 20 years Rajasthan, Doubtful killed a men and injured a women 7 16.01.1825 Oriang {?} - [3, 7] ago, attempts were made to compile a list of events related to the India meteorite (dbt) Uttar Pradesh, [3, 7, 9, damage caused by meteorites falling from the sky. -
AGGLUTINATES in HOWARDITE NWA 1769: SPACE WEATHERING on VESTA. Y. Liu1, L.P. Keller2, A.A. Fraeman3, R. Christoffersen4, Z. Rahman4, B.L
46th Lunar and Planetary Science Conference (2015) 1706.pdf AGGLUTINATES IN HOWARDITE NWA 1769: SPACE WEATHERING ON VESTA. Y. Liu1, L.P. Keller2, A.A. Fraeman3, R. Christoffersen4, Z. Rahman4, B.L. Ehlmann1,3, S.K. Noble5, and J.A. Barrat6. 1Jet Propulsion La- boratory, California Institute of Technology, Pasadena, CA 91109, USA. 2ARES, Mail Code KR, NASA JSC, Hou- ston, TX 77058, USA. 3Div. of Geol. & Planet. Sci., California Institute of Technology, Pasadena, CA 91125, USA. 4Jacobs, NASA JSC, Mail Code XI, Houston, TX 77058, USA. 5. NASA GSFC Mail Code 691, Greenbelt MD 20771. USA. 6Université de Brest, CNRS UMR 6538 (Domaines Océaniques), I.U.E.M., Place Nicolas 12 Copernic, 29280 Plouzané, France. (Email: [email protected]). Introduction: The Vestan surface lacks spectral features indicative of the type of space weathering oc- curring on the Moon and other airless bodies [1]. On the Moon, micrometeorite and solar-wind ion bom- bardment generate nanophase (np) metallic iron (np- Fe0) grains embedded in glassy rims of regolith grains, which subsequently break and melt these rims to form agglutinates in lunar soils. The presence of these com- ponents darkens the surface, increases the slope of the infrared continuum of VIS-NIR spectra, as well as weakens absorption features in lunar spectra. A sys- tematic change of spectra with albedo and surface fea- tures is lacking on the surface of Vesta [1]. However, previous studies of HED samples have found rare ag- glutinates and np-Fe0-bearing glass coatings [2-3], which suggests that limited lunar-style space weather- ing may occur on Vesta. -
Arxiv:1803.02557V2 [Astro-Ph.EP] 30 Apr 2018
Draft version May 1, 2018 Typeset using LATEX default style in AASTeX61 THE DINGLE DELL METEORITE: A HALLOWEEN TREAT FROM THE MAIN BELT Hadrien A. R. Devillepoix,1 Eleanor K. Sansom,1 Philip A. Bland,1 Martin C. Towner,1 Martin Cupak,´ 1 Robert M. Howie,1 Trent Jansen-Sturgeon,1 Morgan A. Cox,1 Benjamin A. D. Hartig,1 Gretchen K. Benedix,1 and Jonathan P. Paxman2 1School of Earth and Planetary Sciences, Curtin University, Bentley, WA 6102, Australia 2School of Civil and Mechanical Engineering, Curtin University, Bentley, WA 6102, Australia ABSTRACT We describe the fall of the Dingle Dell (L/LL 5) meteorite near Morawa in Western Australia on October 31, 2016. The fireball was observed by six observatories of the Desert Fireball Network (DFN), a continental scale facility optimised to recover meteorites and calculate their pre-entry orbits. The 30 cm meteoroid entered at 15.44 km s−1, followed a moderately steep trajectory of 51◦ to the horizon from 81 km down to 19 km altitude, where the luminous flight ended at a speed of 3.2 km s−1. Deceleration data indicated one large fragment had made it to the ground. The four person search team recovered a 1.15 kg meteorite within 130 m of the predicted fall line, after 8 hours of searching, 6 days after the fall. Dingle Dell is the fourth meteorite recovered by the DFN in Australia, but the first before any rain had contaminated the sample. By numerical integration over 1 Ma, we show that Dingle Dell was most likely ejected from the main belt by the 3:1 mean-motion resonance with Jupiter, with only a marginal chance that it came from the nu6 resonance. -
Catching Shooting Stars
PARTNER INSTITUTION PROJECT LEADER @curtin.edu.au SYSTEM XXX TIME ALLOCATED 00 HOURS AREA OF SCIENCE XXX APPLICATIONS USED xx Freshly found 4.5 billion year old meteorite. Credit_Jonathan Paxman, Desert Fireball Network CATCHING SHOOTING STARS Discovering and retrieving newly fallen meteorites can help researchers understand the early workings of the solar system and the origins of our planetary system – including Earth. Over the last fifty years, research attempts to retrieve newly fallen meteorites have met with limited success. Professor Phil Bland, from Curtin University’s Faculty of Science and Engineering, is now leading a team of researchers in a collaborative effort using innovative methodology and supercomputing to achieve results. The Desert Fireball Network (DFN) project uses a network of cameras to detect meteorites or “fireballs” as they fall in the Australian desert. Using the world-class infrastructure at Pawsey Supercomputing Centre, the DFN team stores vast amounts of data and completes trajectory and modelling simulations. The research team can then calculate where a meteorite falls to retrieve, analyze, and trace it back to the parent body in the solar system from where it came. 2016 DESERT FIREBALL NETWORK THE CHALLENGE In November 2015, an 80-kilogram meteor that had been moving at 50 thousand kilometres per hour entered the atmosphere. It created a fireball that streaked across the sky; becoming what some of us refer to as a shooting star. The meteorite then dropped into a remote area of South Australia as a 1.6 kilogram of mottled rock. The Desert Fireball Network had caught the event on camera.