Cosmic History and a Candidate Parent Asteroid for the Quasicrystal-Bearing Meteorite Khatyrka
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ESO's VLT Sphere and DAMIT
ESO’s VLT Sphere and DAMIT ESO’s VLT SPHERE (using adaptive optics) and Joseph Durech (DAMIT) have a program to observe asteroids and collect light curve data to develop rotating 3D models with respect to time. Up till now, due to the limitations of modelling software, only convex profiles were produced. The aim is to reconstruct reliable nonconvex models of about 40 asteroids. Below is a list of targets that will be observed by SPHERE, for which detailed nonconvex shapes will be constructed. Special request by Joseph Durech: “If some of these asteroids have in next let's say two years some favourable occultations, it would be nice to combine the occultation chords with AO and light curves to improve the models.” 2 Pallas, 7 Iris, 8 Flora, 10 Hygiea, 11 Parthenope, 13 Egeria, 15 Eunomia, 16 Psyche, 18 Melpomene, 19 Fortuna, 20 Massalia, 22 Kalliope, 24 Themis, 29 Amphitrite, 31 Euphrosyne, 40 Harmonia, 41 Daphne, 51 Nemausa, 52 Europa, 59 Elpis, 65 Cybele, 87 Sylvia, 88 Thisbe, 89 Julia, 96 Aegle, 105 Artemis, 128 Nemesis, 145 Adeona, 187 Lamberta, 211 Isolda, 324 Bamberga, 354 Eleonora, 451 Patientia, 476 Hedwig, 511 Davida, 532 Herculina, 596 Scheila, 704 Interamnia Occultation Event: Asteroid 10 Hygiea – Sun 26th Feb 16h37m UT The magnitude 11 asteroid 10 Hygiea is expected to occult the magnitude 12.5 star 2UCAC 21608371 on Sunday 26th Feb 16h37m UT (= Mon 3:37am). Magnitude drop of 0.24 will require video. DAMIT asteroid model of 10 Hygiea - Astronomy Institute of the Charles University: Josef Ďurech, Vojtěch Sidorin Hygiea is the fourth-largest asteroid (largest is Ceres ~ 945kms) in the Solar System by volume and mass, and it is located in the asteroid belt about 400 million kms away. -
The Impact Crater at the Origin of the Julia Family Detected with VLT/SPHERE??,?? P
A&A 618, A154 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833477 & © ESO 2018 Astrophysics The impact crater at the origin of the Julia family detected with VLT/SPHERE??,?? P. Vernazza1, M. Brož2, A. Drouard1, J. Hanuš2, M. Viikinkoski3, M. Marsset4, L. Jorda1, R. Fetick1, B. Carry5, F. Marchis6, M. Birlan7, T. Fusco1, T. Santana-Ros8, E. Podlewska-Gaca8,9, E. Jehin10, M. Ferrais10, P. Bartczak8, G. Dudzinski´ 8, J. Berthier7, J. Castillo-Rogez11, F. Cipriani12, F. Colas7, C. Dumas13, J. Durechˇ 2, M. Kaasalainen3, A. Kryszczynska8, P. Lamy1, H. Le Coroller1, A. Marciniak8, T. Michalowski8, P. Michel5, M. Pajuelo7,14, P. Tanga5, F. Vachier7, A. Vigan1, B. Warner15, O. Witasse12, B. Yang16, E. Asphaug17, D. C. Richardson18, P. Ševecekˇ 2, M. Gillon10, and Z. Benkhaldoun19 1 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), Marseille, France e-mail: [email protected] 2 Institute of Astronomy, Charles University, Prague, V Holešovickᡠch 2, 18000, Prague 8, Czech Republic 3 Department of Mathematics, Tampere University of Technology, PO Box 553, 33101 Tampere, Finland 4 Astrophysics Research Centre, Queen’s University Belfast, BT7 1NN, UK 5 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06304 Nice Cedex 4, France 6 SETI Institute, Carl Sagan Center, 189 Bernado Avenue, Mountain View CA 94043, USA 7 IMCCE, Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris Cedex, France 8 Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, -
Earth and Planetary Science Letters 490 (2018) 122–131
Earth and Planetary Science Letters 490 (2018) 122–131 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Cosmic history and a candidate parent asteroid for the quasicrystal-bearing meteorite Khatyrka ∗ Matthias M.M. Meier a, , Luca Bindi b,c, Philipp R. Heck d, April I. Neander e, Nicole H. Spring f,g, My E.I. Riebe a,1, Colin Maden a, Heinrich Baur a, Paul J. Steinhardt h, Rainer Wieler a, Henner Busemann a a Institute of Geochemistry and Petrology, ETH Zurich, Zurich, Switzerland b Dipartimento di Scienze della Terra, Università di Firenze, Florence, Italy c CNR-Istituto di Geoscienze e Georisorse, Sezione di Firenze, Florence, Italy d Robert A. Pritzker Center for Meteoritics and Polar Studies, Field Museum of Natural History, Chicago, USA e Department of Organismal Biology and Anatomy, University of Chicago, Chicago, USA f School of Earth and Environmental Sciences, University of Manchester, Manchester, UK g Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Canada h Department of Physics, and Princeton Center for Theoretical Science, Princeton University, Princeton, USA a r t i c l e i n f o a b s t r a c t Article history: The unique CV-type meteorite Khatyrka is the only natural sample in which “quasicrystals” and associated Received 6 October 2017 crystalline Cu, Al-alloys, including khatyrkite and cupalite, have been found. They are suspected to Received in revised form 11 March 2018 have formed in the early Solar System. To better understand the origin of these exotic phases, and Accepted 13 March 2018 the relationship of Khatyrka to other CV chondrites, we have measured He and Ne in six individual, Available online 22 March 2018 ∼40–μm-sized olivine grains from Khatyrka. -
Color Study of Asteroid Families Within the MOVIS Catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia De León1,2
A&A 617, A72 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832780 & © ESO 2018 Astrophysics Color study of asteroid families within the MOVIS catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia de León1,2 1 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 3 Astronomical Institute of the Romanian Academy, 5 Cu¸titulde Argint, 040557 Bucharest, Romania Received 6 February 2018 / Accepted 13 March 2018 ABSTRACT The aim of this work is to study the compositional diversity of asteroid families based on their near-infrared colors, using the data within the MOVIS catalog. As of 2017, this catalog presents data for 53 436 asteroids observed in at least two near-infrared filters (Y, J, H, or Ks). Among these asteroids, we find information for 6299 belonging to collisional families with both Y J and J Ks colors defined. The work presented here complements the data from SDSS and NEOWISE, and allows a detailed description− of− the overall composition of asteroid families. We derived a near-infrared parameter, the ML∗, that allows us to distinguish between four generic compositions: two different primitive groups (P1 and P2), a rocky population, and basaltic asteroids. We conducted statistical tests comparing the families in the MOVIS catalog with the theoretical distributions derived from our ML∗ in order to classify them according to the above-mentioned groups. We also studied the background populations in order to check how similar they are to their associated families. -
Ice& Stone 2020
Ice & Stone 2020 WEEK 51: DECEMBER 13-19 Presented by The Earthrise Institute # 51 Authored by Alan Hale COMET OF THE WEEK: The Great Comet of 1680 Perihelion: 1680 December 18.49, q = 0.006 AU The Great Comet of 1680 over Rotterdam in The Netherlands, during late December 1680 as painted by the Dutch artist Lieve Verschuier. This particular comet was undoubtedly one of the brightest comets of the 17th Century, but it is also one of the most important comets in history from a scientific perspective, and perhaps even from the perspective of overall human history. While there were certainly plenty of superstitions attached to the comet’s appearance, the scientific investigations made of it were among the beginnings of the era in European history we now call The Enlightenment, and indeed, in a sense the Great Comet of 1680 can perhaps be considered as one of the sparks of that era. The significance began with the comet’s discovery, which was made on the morning of November 14, 1680, by a German astronomer residing in Coburg, Gottfried Kirch – the first comet ever to be discovered by means of a telescope. It was already around 4th magnitude at that time, and located near the star Regulus in the constellation Leo; from that point it traveled eastward and brightened rapidly, being closest to Earth (0.42 AU) on November 30. By that time it was a conspicuous naked-eye object with a tail 20 to 30 degrees long, and it remained visible for another week before disappearing into morning twilight. -
Thirty-Fourth List of New Mineral Names
MINERALOGICAL MAGAZINE, DECEMBER 1986, VOL. 50, PP. 741-61 Thirty-fourth list of new mineral names E. E. FEJER Department of Mineralogy, British Museum (Natural History), Cromwell Road, London SW7 5BD THE present list contains 181 entries. Of these 148 are Alacranite. V. I. Popova, V. A. Popov, A. Clark, valid species, most of which have been approved by the V. O. Polyakov, and S. E. Borisovskii, 1986. Zap. IMA Commission on New Minerals and Mineral Names, 115, 360. First found at Alacran, Pampa Larga, 17 are misspellings or erroneous transliterations, 9 are Chile by A. H. Clark in 1970 (rejected by IMA names published without IMA approval, 4 are variety because of insufficient data), then in 1980 at the names, 2 are spelling corrections, and one is a name applied to gem material. As in previous lists, contractions caldera of Uzon volcano, Kamchatka, USSR, as are used for the names of frequently cited journals and yellowish orange equant crystals up to 0.5 ram, other publications are abbreviated in italic. sometimes flattened on {100} with {100}, {111}, {ill}, and {110} faces, adamantine to greasy Abhurite. J. J. Matzko, H. T. Evans Jr., M. E. Mrose, lustre, poor {100} cleavage, brittle, H 1 Mono- and P. Aruscavage, 1985. C.M. 23, 233. At a clinic, P2/c, a 9.89(2), b 9.73(2), c 9.13(1) A, depth c.35 m, in an arm of the Red Sea, known as fl 101.84(5) ~ Z = 2; Dobs. 3.43(5), D~alr 3.43; Sharm Abhur, c.30 km north of Jiddah, Saudi reflectances and microhardness given. -
Aperiodic Mineral Structures
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Infoscience - École polytechnique fédérale de Lausanne EMU Notes in Mineralogy, Vol. 19 (2017), Chapter 5, 213–254 Aperiodic mineral structures L. BINDI1 and G. CHAPUIS2 1 Dipartimento di Scienze della Terra, Universita` di Firenze, Via La Pira 4, I-50121 Firenze, Italy 2 Laboratoire de Cristallographie, E´cole Polytechnique Fe´de´rale de Lausanne, CH-1015 Lausanne, Switzerland The three-dimensional periodic nature of crystalline structures was so strongly anchored in the minds of scientists that the numerous indications that seemed to question this model struggled to acquire the status of validity. The discovery of aperiodic crystals, a generic term including modulated, composite and quasicrystal structures, started in the 1970s with the discovery of incommensurately modulated structures and the presence of satellite reflections surrounding the main reflections in the diffraction patterns. The need to use additional integers to index such diffractograms was soon adopted and theoretical considerations showed that any crystal structure requiring more than three integers to index its diffraction pattern could be described as a periodic object in a higher dimensional space, i.e. superspace, with dimension equal to the number of required integers. The structure observed in physical space is thus a three-dimensional intersection of the structure described as periodic in superspace. Once the symmetry properties of aperiodic crystals were established, the superspace theory was soon adopted in order to describe numerous examples of incommensurate crystal structures from natural and synthetic organic and inorganic compounds even to proteins. Aperiodic crystals thus exhibit perfect atomic structures with long-range order, but without any three-dimensional translational symmetry. -
Previously Unknown Quasicrystal Periodic Approximant Found in Space Received: 13 August 2018 Luca Bindi 1, Joyce Pham 2 & Paul J
www.nature.com/scientificreports OPEN Previously unknown quasicrystal periodic approximant found in space Received: 13 August 2018 Luca Bindi 1, Joyce Pham 2 & Paul J. Steinhardt3,4 Accepted: 16 October 2018 We report the discovery of Al Ni Fe , the frst natural known periodic crystalline approximant Published: xx xx xxxx 34 9 2 to decagonite (Al71Ni24Fe5), a natural quasicrystal composed of a periodic stack of planes with quasiperiodic atomic order and ten-fold symmetry. The new mineral has been approved by the International Mineralogical Association (IMA 2018-038) and ofcially named proxidecagonite, which derives from its identity to periodic approximant of decagonite. Both decagonite and proxidecagonite were found in fragments from the Khatyrka meteorite. Proxidecagonite is the frst natural quasicrystal approximant to be found in the Al-Ni-Fe system. Within this system, the decagonal quasicrystal phase has been reported to transform at ~940 °C to Al13(Fe,Ni)4, Al3(Fe,Ni)2 and the liquid phase, and between 800 and 850 °C to Al13(Fe,Ni)4, Al3(Fe,Ni) and Al3(Fe,Ni)2. The fact that proxidecagonite has not been observed in the laboratory before and formed in a meteorite exposed to high pressures and temperatures during impact-induced shocks suggests that it might be a thermodynamically stable compound at high pressure. The most prominent structural motifs are pseudo-pentagonal symmetry subunits, such as pentagonal bipyramids, that share edges and corners with trigonal bipyramids and which maximize shortest Ni–Al over Ni–Ni contacts. 1,2 Te frst decagonal quasicrystalline (QC) phase found in nature, decagonite Al71Ni24Fe5 , was discovered in the Khatyrka meteorite, a CV3 carbonaceous chondrite3–8. -
79Th Annual Meeting of the Meteoritical Society (2016) 6017.Pdf
79th Annual Meeting of the Meteoritical Society (2016) 6017.pdf DISCOVERY OF NEW Al-Cu-Fe MINERALS IN THE KHATYRKA CV3 METEORITE. Chi Ma1,*, Chaney Lin2, Luca Bindi3, Paul J. Steinhardt2. 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA; 2Department of Physics, Princeton University, Princeton, NJ 08544, USA; 3Dipartimento di Scienze della Terra, Università di Firenze, Via La Pira 4, I-50121 Florence, Italy; *Email: [email protected]. Introduction: During a nanomineralogy investigation of the Khatyrka CV3 carbonaceous chondrite, we have identified two new alloy minerals (AlCu with a Pm-3m CsCl structure and Al3Fe with a C2/m structure) and associ- ated icosahedrite (quasicrystal Al63Cu26Fe11 with a five-fold symmetry) at micron scales in section 126A of USNM 7908. The section belongs to the larger Grain 126, which is one of the fragments recovered from an expedition to the Koryak Mountains in far eastern Russia in 2011 [1] as a result of a search for samples that would provide infor- mation on the origin of the quasicrystal mineral icosahedrite [2,3,4]. The recovered fragments have meteoritic (CV3- like) oxygen isotopic compositions and are identified collectively as coming from the Khatyrka meteorite [5], which formed 4.5 billion years ago during the earliest stages of the solar system. Khatyrka is unique, so far being the only meteorite to host metallic Al component. Field-emission scanning electron microscope with energy-dispersive X-ray spectrometer and electron back- scatter diffraction (EBSD), and electron probe microanalyzer (EPMA) were used to characterize chemical composi- tions and structures of the minerals in section 126A. -
Can CO CV Meteorites Come from the Eos Family?
60th Annual Meteoritical Society Meeting 5049.pdf Can CO/CV meteorites come from the Eos family? Eos asteroid family is one of the largest groupings in the main b elt [1] and currently its memb ership consists of more than 480 ob jects [2]. The family is cut by the 9:4 mean-motion resonance with Jupiter, and 5 resonant asteroids have b een found within this resonance [3]. The family memb ers b elong to the rare K taxonomic class and show a sp ectral app earance in b etween C- and S-typ e asteroids [4,5]. Many authors suggest, on the basis of sp ectra and alb edo similarities, that K-typ e asteroids mayhave a mineralogical comp osition close to that of the anhydrous CO/CV carb onaceous chondrites [6,7,8]; however, the sp ec- trum of 221 Eos do es not show clear evidence for the calcium-aluminium-rich inclusions CAI absorption features typical of CO meteorites [9]. In order to test the link b etween CO/CV meteorites and K-typ e aster- oids, in the context of the broader GAPTEC pro ject [10], wehave b egan a massive and long-term numerical integration of a sample of synthetic ob jects aimed at simulating real family memb ers injected into the 9:4 mean-motion resonance. In this analysis, we use the SWIFT RMVS3 integrator package [11,12]. The chaotic region asso ciated with the 9:4 mean-motion resonance spans at least the region b etween 3.026 AU and 3.032 AUatlow eccentricityi.e. -
EXPERIMENTAL IMPACTS of ALUMINUM PROJECTILES INTO QUARTZ SAND: FORMATION 1,2 1,3 of KHATYRKITE (Cual2) and REDUCTION of QUARTZ to SILICON
Bridging the Gap III (2015) 1071.pdf EXPERIMENTAL IMPACTS OF ALUMINUM PROJECTILES INTO QUARTZ SAND: FORMATION 1,2 1,3 OF KHATYRKITE (CuAl2) AND REDUCTION OF QUARTZ TO SILICON. C. Hamann , D. Stöffler , and W. U. Reimold1,3. 1Museum für Naturkunde, Leibniz-Institut für Evolutions- und Biodiversitätsforschung, In- validenstraße 43, 10115 Berlin, Germany ([email protected]; dieter.stö[email protected]; [email protected]); 2Institut für Geologische Wissenschaften, Freie Universität Berlin, Malteserstraße 74– 100, 12249 Berlin, Germany, 3Humboldt-Universität zu Berlin, Unter der Linden 6, 10099 Berlin, Germany. Introduction and Rationale: Impact cratering is a melt particles, shock-lithified sand with and without basic geologic process in the solar system, which was distinct shock effects (PDF, diaplectic glass), and frac- predominant over endogenic geologic processes in the tured quartz grains (for details, see the companion early evolution of geologically active planetary bodies. abstract by Wünnemann et al. [10]). Since this study Since most planetary surfaces are highly porous and/or focuses on chemical projectile–target interaction, we composed of non-cohesive materials (e.g., the lunar will only consider impact melt particles that obviously regolith), understanding the influence of pore space show a crust of projectile melt on their top sides. and non-cohesiveness of materials on the impact pro- The bulk compositions of projectile and target were cess is crucial for gaining insights into the evolution of determined with EMPA and XRF, respectively. Impact planetary regoliths. To this end, numerous theoretical melt particles were studied with optical microscopy, and experimental studies have been conducted (e.g., SEM-EDX, and EMPA. -
Design Rules for Discovering 2D Materials from 3D Crystals
Design Rules for Discovering 2D Materials from 3D Crystals by Eleanor Lyons Brightbill Collaborators: Tyler W. Farnsworth, Adam H. Woomer, Patrick C. O'Brien, Kaci L. Kuntz Senior Honors Thesis Chemistry University of North Carolina at Chapel Hill April 7th, 2016 Approved: ___________________________ Dr Scott Warren, Thesis Advisor Dr Wei You, Reader Dr. Todd Austell, Reader Abstract Two-dimensional (2D) materials are championed as potential components for novel technologies due to the extreme change in properties that often accompanies a transition from the bulk to a quantum-confined state. While the incredible properties of existing 2D materials have been investigated for numerous applications, the current library of stable 2D materials is limited to a relatively small number of material systems, and attempts to identify novel 2D materials have found only a small subset of potential 2D material precursors. Here I present a rigorous, yet simple, set of criteria to identify 3D crystals that may be exfoliated into stable 2D sheets and apply these criteria to a database of naturally occurring layered minerals. These design rules harness two fundamental properties of crystals—Mohs hardness and melting point—to enable a rapid and effective approach to identify candidates for exfoliation. It is shown that, in layered systems, Mohs hardness is a predictor of inter-layer (out-of-plane) bond strength while melting point is a measure of intra-layer (in-plane) bond strength. This concept is demonstrated by using liquid exfoliation to produce novel 2D materials from layered minerals that have a Mohs hardness less than 3, with relative success of exfoliation (such as yield and flake size) dependent on melting point.