105. Titanium Stable Isotopic Variations in Chondrites
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
New Major and Trace Element Data from Acapulcoite-Lodranite Clan
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1307.pdf New Major and Trace Element Data from Acapulcoite-Lodranite Clan Meteorites: Evidence for Melt-Rock Reaction Events and Early Collisional Fragmentation of the Parent Body Michael P. Lucas1, Nick Dygert1, Nathaniel R. Miller2, and Harry Y. McSween1, 1Department of Earth & Planetary Sciences, University of Tennessee, Knoxville, [email protected], 2Department of Geological Sciences, Univer- sity of Texas at Austin. Introduction: New major and trace element data illumi- patterns exhibit negative Eu anomalies. REE patterns are nate the magmatic and thermal evolution of the acapul- generally consistent among the three groups, however coite-lodranite parent body (ALPB). We observe major comparison of calculated equilibrium melts for acapulco- and trace element disequilibrium in the acapulcoite and ite and transitional cpx and opx demonstrates disequilib- transitional groups that provide evidence for melt infil- rium partitioning in those samples, especially for light- tration and melt-rock reaction processes. In lodranites, REEs in cpx. In contrast, lodranites are in apparent trace which represent sources of the infiltrating melts, we ob- element equilibrium (Fig 1b). They are depleted in serve rapid cooling from high temperatures (hereafter REE+Y relative to acapulcoite-transitional samples in temps), consistent with collisional fragmentation of the cpx (Fig. 1a), and display consistent REE abundances parent body during differentiation. except NWA 5488, which -
Hf–W Thermochronometry: II. Accretion and Thermal History of the Acapulcoite–Lodranite Parent Body
Earth and Planetary Science Letters 284 (2009) 168–178 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl Hf–W thermochronometry: II. Accretion and thermal history of the acapulcoite–lodranite parent body Mathieu Touboul a,⁎, Thorsten Kleine a, Bernard Bourdon a, James A. Van Orman b, Colin Maden a, Jutta Zipfel c a Institute of Isotope Geochemistry and Mineral Resources, ETH Zurich, Clausiusstrasse 25, 8092 Zurich, Switzerland b Department of Geological Sciences, Case Western Reserve University, Cleveland, OH, USA c Forschungsinstitut und Naturmuseum Senckenberg, Frankfurt am Main, Germany article info abstract Article history: Acapulcoites and lodranites are highly metamorphosed to partially molten meteorites with mineral and bulk Received 11 November 2008 compositions similar to those of ordinary chondrites. These properties place the acapulcoites and lodranites Received in revised form 8 April 2009 between the unmelted chondrites and the differentiated meteorites and as such acapulcoites–lodranites are Accepted 9 April 2009 of special interest for understanding the initial stages of asteroid differentiation as well as the role of 26Al Available online 3 June 2009 heating in the thermal history of asteroids. To constrain the accretion timescale and thermal history of the Editor: R.W. Carlson acapulcoite–lodranite parent body, and to compare these results to the thermal histories of other meteorite parent bodies, the Hf–W system was applied to several acapulcoites and lodranites. Acapulcoites Dhofar 125 Keywords: – Δ chronology and NWA 2775 and lodranite NWA 2627 have indistinguishable Hf W ages of tCAI =5.2±0.9 Ma and Δ isochron tCAI =5.7±1.0 Ma, corresponding to absolute ages of 4563.1±0.8 Ma and 4562.6±0.9 Ma. -
Mineralogy and Petrology of the Angrite Northwest Africa 1296 Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D
Mineralogy and petrology of the angrite Northwest Africa 1296 Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D. Badia, C. Göpel, Marcel Bohn To cite this version: Albert Jambon, Jean-Alix Barrat, Omar Boudouma, Michel Fonteilles, D. Badia, et al.. Mineralogy and petrology of the angrite Northwest Africa 1296. Meteoritics and Planetary Science, Wiley, 2005, 40 (3), pp.361-375. hal-00113853 HAL Id: hal-00113853 https://hal.archives-ouvertes.fr/hal-00113853 Submitted on 2 May 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. Meteoritics & Planetary Science 40, Nr 3, 361–375 (2005) Abstract available online at http://meteoritics.org Mineralogy and petrology of the angrite Northwest Africa 1296 A. JAMBON,1 J. A. BARRAT,2 O. BOUDOUMA,3 M. FONTEILLES,4 D. BADIA,1 C. GÖPEL,5 and M. BOHN6 1Laboratoire Magie, Université Pierre et Marie Curie, CNRS UMR 7047, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 2UBO-IUEM, CNRS UMR 6538, Place Nicolas Copernic, F29280 Plouzané, France 3Service du MEB, UFR des Sciences de la Terre, Université Pierre et Marie Curie, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 4Pétrologie, Modélisation des Matériaux et Processus, Université Pierre et Marie Curie, case 110, 4 place Jussieu, 75252 Paris cedex 05, France 5Laboratoire de Géochimie et Cosmochimie, Institut de Physique du Globe, CNRS UMR 7579, 4 place Jussieu, 75252 Paris cedex 05, France 6Ifremer-Centre de Brest, CNRS-UMR 6538, BP70, 29280 Plouzané Cedex, France *Corresponding author. -
Neutron Activation Analyses and Half-Life Measurements at the Usgs Triga Reactor
NEUTRON ACTIVATION ANALYSES AND HALF-LIFE MEASUREMENTS AT THE USGS TRIGA REACTOR by Robert E. Larson A thesis submitted to the Faculty and the Board of Trustees of the Colorado School of Mines in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Applied Physics). Golden, Colorado Date Signed: Robert E. Larson Signed: Dr. Uwe Greife Thesis Advisor Golden, Colorado Date Signed: Dr. Thomas E. Furtak Professor and Head Department of Physics ii ABSTRACT Neutron activation of materials followed by gamma spectroscopy using high-purity ger- manium detectors is an e↵ective method for making measurements of nuclear beta decay half-lives and for detecting trace amounts of elements present in materials. This research explores applications of neutron activation analysis (NAA) in two parts. Part 1. High Precision Methods for Measuring Decay Half-Lives, Chapters 1 through 8 Part one develops research methods and data analysis techniques for making high pre- cision measurements of nuclear beta decay half-lives. The change in the electron capture half-life of 51Cr in pure chromium versus chromium mixed in a gold lattice structure is ex- plored, and the 97Ru electron capture decay half-life are compared for ruthenium in a pure crystal versus ruthenium in a rutile oxide state, RuO2.Inaddition,thebeta-minusdecay half-life of 71mZn is measured and compared with new high precision findings. Density Func- tional Theory is used to explain the measured magnitude of changes in electron capture half-life from changes in the surrounding lattice electron configuration. Part 2. Debris Collection Nuclear Diagnostic at the National Ignition Facility, Chapters 9 through 11 Part two explores the design and development of a solid debris collector for use as a diagnostic tool at the National Ignition Facility (NIF). -
Sulfide/Silicate Melt Partitioning During Enstatite Chondrite Melting
61st Annual Meteoritical Society Meeting 5255.pdf SULFIDE/SILICATE MELT PARTITIONING DURING ENSTATITE CHONDRITE MELTING. C. Floss1, R. A. Fogel2, G. Crozaz1, M. Weisberg2, and M. Prinz2, 1McDonnell Center for the Space Sciences and Department of Earth and Planetary Sciences, Washington University, St. Louis MO 63130, USA ([email protected]), 2American Museum of Natural History, Department of Earth and Planetary Sciences, New York NY 10024, USA. Introduction: Aubrites are igneous rocks thought (present only in CaS-saturated charges) has a flat REE to have formed from an enstatite chondrite-like pattern with abundances of about 0.5 x CI. precursor [1]. Yet their origin remains poorly Discussion: Oldhamite/glass D values are close to understood, at least partly because of confusion over 1 for most REE, consistent with previous results the role played by sulfides, particularly oldhamite. [4,5,6], and significantly lower than those expected CaS in aubrites contains high rare earth element based on REE abundances in aubritic oldhamite. In (REE) abundances and exhibits a variety of patterns contrast, D values for FeS are surprisingly high (from [2] that reflect, to some extent, those seen in about 0.1 to 1), given the low REE abundances of oldhamite from enstatite chondrites [3]. However, natural troilite. FeS/silicate partition coefficients experimental work suggests that CaS/silicate melt reported by [5] are somewhat lower, but exhibit a REE partition coefficients are too low to account for similar pattern. Alkali loss from the charges, the high abundances observed [4,5] and do not explain resulting in Ca-enriched glass, might provide a partial the variable patterns. -
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. -
Laboratory Spectroscopy of Meteorite Samples at UV-Vis-NIR Wavelengths: Analysis and Discrimination by Principal Components Analysis
Laboratory spectroscopy of meteorite samples at UV-Vis-NIR wavelengths: Analysis and discrimination by principal components analysis Antti Penttil¨aa,∗, Julia Martikainena, Maria Gritsevicha, Karri Muinonena,b aDepartment of Physics, P.O. Box 64, FI-00014 University of Helsinki, Finland bFinnish Geospatial Research Institute FGI, National Land Survey of Finland, Geodeetinrinne 2, FI-02430 Masala, Finland Abstract Meteorite samples are measured with the University of Helsinki integrating-sphere UV-Vis- NIR spectrometer. The resulting spectra of 30 meteorites are compared with selected spectra from the NASA Planetary Data System meteorite spectra database. The spectral measure- ments are transformed with the principal component analysis, and it is shown that different meteorite types can be distinguished from the transformed data. The motivation is to im- prove the link between asteroid spectral observations and meteorite spectral measurements. Keywords: Meteorites, spectroscopy, principal component analysis 1. Introduction While a planet orbits the Sun, it is subject to impacts by objects ranging from tiny dust particles to much larger asteroids and comet nuclei. Such collisions of small Solar System bodies with planets have taken place frequently over geological time and played an 5 important role in the evolution of planets and development of life on the Earth. Every day approximately 30{180 tons of interplanetary material enter the Earth's atmosphere [1, 2]. This material is mostly represented by smaller meteoroids that undergo rapid ablation in the atmosphere. Under favorable initial conditions part of a meteoroid may survive the atmospheric entry and reach the ground [3]. The fragments recovered on the ground are 10 called meteorites, our valuable samples of the Solar System. -
Assessment of the Mesosiderite-Diogenite Connection and an Impact Model for the Genesis of Mesosiderites
45th Lunar and Planetary Science Conference (2014) 2554.pdf ASSESSMENT OF THE MESOSIDERITE-DIOGENITE CONNECTION AND AN IMPACT MODEL FOR THE GENESIS OF MESOSIDERITES. T. E. Bunch1,3, A. J. Irving2,3, P. H. Schultz4, J. H. Wittke1, S. M. Ku- ehner2, J. I. Goldstein5 and P. P. Sipiera3,6 1Dept. of Geology, SESES, Northern Arizona University, Flagstaff, AZ 86011 ([email protected]), 2Dept. of Earth & Space Sciences, University of Washington, Seattle, WA, 3Planetary Studies Foundation, Galena, IL, 4Dept. of Geological Sciences, Brown University, Providence, RI, 5Dept. of Geolo- gy, University of Massachusetts, Amherts, MA, 6Field Museum of Natural History, Chicago, IL. Introduction: Among well-recognized meteorite 34) is the most abundant silicate mineral and in some classes, the mesosiderites are perhaps the most com- clasts contains inclusions of FeS, tetrataenite, merrillite plex and petrogenetically least understood. Previous and silica. Three of the ten norite clasts contain a few workers have contributed important information about tiny grains of olivine (Fa24-32). A single, fine-grained “classic” falls and Antarctic finds, and have proposed breccia clast was found in NWA 5312 (see Figure 2). several different models for mesosiderite genesis [1]. Unlike the case of pallasites, the co-occurrence of met- al and silicates (predominantly orthopyroxene and cal- cic plagioclase) in mesosiderites is inconsistent with a single-stage “igneous” history, and instead seems to demand admixture of at least two separate compo- nents. Here we review the models in light of detailed ex- amination of multiple specimens from a very large mesosiderite strewnfield in Northwest Africa. Many specimens (totaling at least 80 kilograms) from this area (probably in Algeria) have been classified sepa- rately by us and others; however, in most cases the Figure 1. -
Thursday, August 11, 2016 EARLY SOLAR SYSTEM CHRONOLOGY I 8:30 A.M
79th Annual Meeting of the Meteoritical Society (2016) sess701.pdf Thursday, August 11, 2016 EARLY SOLAR SYSTEM CHRONOLOGY I 8:30 a.m. Room B Chairs: Gregory Brennecka Audrey Bouvier 8:30 a.m. Kruijer T. S. * Kleine T. Tungsten Isotope Dichotomy Among Iron Meteorite Parent Bodies: Implications for the Timescales of Accretion and Core Formation [#6449] We report new combined Pt and W isotope data for IC, IIC, IIF, IIIE, and IIIF iron meteorites, with the ultimate aim of better understanding the variable pre-exposure 182W/184W signatures observed among different iron meteorite groups. 8:45 a.m. Tissot F. L. H. * Dauphas N. Grove T. L. Heterogeneity in the 238U/235U Ratios of Angrites [#6104] We report the 238U/235U ratios of six angrites. We find that the angrite-parent body was heterogeneous with regards to U isotopes. We correct the Pb-Pb ages of angrites and test their concordance with ages derived from short-lived chronometers. 9:00 a.m. Brennecka G. A. * Amelin Y. Kleine T. Combined 238U/235U and Pb Isotopics of Planetary Core Material: The Absolute Age of the IVA Iron Muonionalusta [#6296] We report a measured 238U/235U for the IVA iron Muonionalusta. This measured value requires an age correction of ~7 Myr to the previously published Pb-Pb age. This has major implications for our understanding of planetary core formation and cooling. 9:15 a.m. Cartwright J. A. * Amelin Y. Koefoed P. Wadhwa M. U-Pb Age of the Ungrouped Achondrite NWA 8486 [#6231] We report the U-Pb age for ungrouped achondrite NWA 8486 (paired with NWA 7325). -
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. -
Physical Properties of Martian Meteorites: Porosity and Density Measurements
Meteoritics & Planetary Science 42, Nr 12, 2043–2054 (2007) Abstract available online at http://meteoritics.org Physical properties of Martian meteorites: Porosity and density measurements Ian M. COULSON1, 2*, Martin BEECH3, and Wenshuang NIE3 1Solid Earth Studies Laboratory (SESL), Department of Geology, University of Regina, Regina, Saskatchewan S4S 0A2, Canada 2Institut für Geowissenschaften, Universität Tübingen, 72074 Tübingen, Germany 3Campion College, University of Regina, Regina, Saskatchewan S4S 0A2, Canada *Corresponding author. E-mail: [email protected] (Received 11 September 2006; revision accepted 06 June 2007) Abstract–Martian meteorites are fragments of the Martian crust. These samples represent igneous rocks, much like basalt. As such, many laboratory techniques designed for the study of Earth materials have been applied to these meteorites. Despite numerous studies of Martian meteorites, little data exists on their basic structural characteristics, such as porosity or density, information that is important in interpreting their origin, shock modification, and cosmic ray exposure history. Analysis of these meteorites provides both insight into the various lithologies present as well as the impact history of the planet’s surface. We present new data relating to the physical characteristics of twelve Martian meteorites. Porosity was determined via a combination of scanning electron microscope (SEM) imagery/image analysis and helium pycnometry, coupled with a modified Archimedean method for bulk density measurements. Our results show a range in porosity and density values and that porosity tends to increase toward the edge of the sample. Preliminary interpretation of the data demonstrates good agreement between porosity measured at 100× and 300× magnification for the shergottite group, while others exhibit more variability. -
Magmatic Sulfides in the Porphyritic Chondrules of EH Enstatite Chondrites
Published in Geochimica et Cosmochimica Acta, Accepted September 2016. http://dx.doi.org/10.1016/j.gca.2016.09.010 Magmatic sulfides in the porphyritic chondrules of EH enstatite chondrites. Laurette Piani1,2*, Yves Marrocchi2, Guy Libourel3 and Laurent Tissandier2 1 Department of Natural History Sciences, Faculty of Science, Hokkaido University, Sapporo, 060-0810, Japan 2 CRPG, UMR 7358, CNRS - Université de Lorraine, 54500 Vandoeuvre-lès-Nancy, France 3 Laboratoire Lagrange, UMR7293, Université de la Côte d’Azur, CNRS, Observatoire de la Côte d’Azur,F-06304 Nice Cedex 4, France *Corresponding author: Laurette Piani ([email protected]) Abstract The nature and distribution of sulfides within 17 porphyritic chondrules of the Sahara 97096 EH3 enstatite chondrite have been studied by backscattered electron microscopy and electron microprobe in order to investigate the role of gas-melt interactions in the chondrule sulfide formation. Troilite (FeS) is systematically present and is the most abundant sulfide within the EH3 chondrite chondrules. It is found either poikilitically enclosed in low-Ca pyroxenes or scattered within the glassy mesostasis. Oldhamite (CaS) and niningerite [(Mg,Fe,Mn)S] are present in ! 60 % of the chondrules studied. While oldhamite is preferentially present in the mesostasis, niningerite associated with silica is generally observed in contact with troilite and low-Ca pyroxene. The Sahara 97096 chondrule mesostases contain high abundances of alkali and volatile elements (average Na2O = 8.7 wt.%, K2O = 0.8 wt.%, Cl = 7000 ppm and S = 3700 ppm) as well as silica (average SiO2 = 63.1 wt.%). Our data suggest that most of the sulfides found in EH3 chondrite chondrules are magmatic minerals that formed after the dissolution of S from a volatile-rich gaseous environment into the molten chondrules.