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  • 1
    Monograph available for loan
    Monograph available for loan
    Washington, D.C. : Mineralogical Society of America
    Associated volumes
    Call number: 11/M 99.0429 ; 11/M 98.0500 ; 11/M 00.0101
    In: Reviews in mineralogy
    Description / Table of Contents: We seek to understand the timing and processes by which our solar system formed and evolved. There are many ways to gain this understanding including theoretical calculations and remotely sensing planetary bodies with a number of techniques. However, there are a number of measurements that can only be made with planetary samples in hand. These samples can be studied in laboratories on Earth with the full range of high-precision analytical instruments available now or available in the future. The precisions and accuracies for analytical measurements in modern Earth-based laboratories are phenomenal. However, despite the fact that certain types of measurements can only be done with samples in hand, these samples will always be small in number and not necessarily representative of an entire planetary surface. Therefore, it is necessary that the planetary material scientists work hand-in-hand with the remote sensing community to combine both types of data sets. This exercise is in fact now taking place through an initiative of NASA's Curation and Analysis Planning Team for Extraterrestrial Materials (CAPTEM). This initiative is named "New Views of the Moon: Integrated Remotely Sensed, Geophysical, and Sample Datasets." As preliminary results of the Lunar Prospector mission become available, and with the important results of the Galileo and Clementine missions now providing new global data sets of the Moon, it is imperative that the lunar science community synthesize these new data and integrate them with one another and with the lunar-sample database. Integrated approaches drawing upon multiple data sets can be used to address key problems of lunar origin, evolution, and resource definition and utilization. The idea to produce this Reviews in Mineralogy (RIM) volume was inspired by the realization that many types of planetary scientists and, for that matter, Earth scientists will need access to data on the planetary sample suite. Therefore, we have attempted to put together, under one cover, a comprehensive coverage of the mineralogy and petrology of planetary materials. The book is organized with an introductory chapter that introduces the reader to the nature of the planetary sample suite and provides some insights into the diverse environments from which they come. Chapter 2 on Interplanetary Dust Particles (IDPs) and Chapter 3 on Chondritic Meteorites deal with the most primitive and unevolved materials we have to work with. It is these materials that hold the clues to the nature of the solar nebula and the processes that led to the initial stages of planetary formation. Chapter 4, 5, and 6 consider samples from evolved asteroids, the Moon and Mars respectively. Chapter 7 is a brief summary chapter that compares aspects of melt-derived minerals from differing planetary environments.
    Type of Medium: Monograph available for loan
    Pages: xv, 864 S.
    ISBN: 0-939950-46-4 , 978-0-939950-46-1
    ISSN: 1529-6466
    Series Statement: Reviews in Mineralogy 36
    Classification:
    Mineralogy
    Language: English
    Note: Chapter 1. The Planetary Sample Suite and Environments of Origin by Charles K. Shearer, James J. Papike., and Frans J.M. Rietmeijer, p. 1-01 - 1-28 Chapter 2. Interplanetary Dust Particles by Frans J.M. Rietmeijer, p. 2-01 - 2-96 Chapter 3. Chondritic Meteorites by Adrian J. Brearley and Rhian H. Jones, p. 3-001 - 3-398 Chapter 4. Non-Chondritic Meteorites from Asteroidal Bodies by David Wayne Mittlefehldt, Timothy J. McCoy, Cyrena Anne Goodrich, and Alfred Kracher, p.4-001 - 4-196 Chapter 5. Lunar Samples by James J. Papike, G. Ryder, and Charles K. Shearer, p. 5-001 - 5-234 Chapter 6. Martian Meteorites by Harry Y. McSween, Jr. and Allan H. Treiman, p. 6-01 - 6-54 Chapter 7. Comparative Planetary Mineralogy: Chemistry of Melt- Derived Pyroxene, Feldspar, and Olivine by James J. Papike, p. 7-01 - 7-12
    Location: Reading room
    Location: Reading room
    Location: Reading room
    Branch Library: GFZ Library
    Branch Library: GFZ Library
    Branch Library: GFZ Library
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  • 2
    Description / Table of Contents: The pyroxene and amphibole mineral groups have been the focal points of numerous experimental, theoretical, and field-oriented studies in recent years. Many exciting new results have been obtained since the 1966 International Mineralogical Association Symposium on Pyroxenes and Amphiboles held at the University of Cambridge, England. During September 7-11, 1969, another pyroxene-amphibole symposium will be held at the Virginia Polytechnic Institute, Blacksburg, Virginia. Pyroxenes and Amphiboles: Crystal Chemistry and Phase Petrology is published to coincide with this symposium and is intended to make generally available some of the current research in this field. Formal papers given at the symposium will include new research results not currently at the manuscript stage, and abstracts for these papers will be published in the January-February, 1970, issue of The American Mineralogist.
    Pages: Online-Ressource (VIII, 332 Seiten)
    Language: English
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  • 3
    Electronic Resource
    Electronic Resource
    Springer
    Contributions to mineralogy and petrology 20 (1968), S. 81-85 
    ISSN: 1432-0967
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences
    Notes: Abstract Bond distances and angles in isostructural, ordered clinopyroxenes are compared for eight compositions, based on five new and three published crystal-structure refinements from X-ray diffraction data. Unit-cell parameters and configuration of the silicate chains are directly correlated with cation composition and distribution in the M2 and M1 sites.
    Type of Medium: Electronic Resource
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  • 4
    ISSN: 1432-0967
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences
    Notes: Abstract The Jurassic Notch Peak granitic stock, western Utah, discordantly intrudes Cambrian interbedded pure limestones and calcareous argillites. Contact metamorphosed argillite and limestone samples, collected along traverses away from the intrusion, were analyzed for δ 18O, δ 13C, and δD. The δ 13C and δ 18O values for the limestones remain constant at about 0.5 (PDB) and 20 (SMOW), respectively, with increasing metamorphic grade. The whole rock δ 18O values of the argillites systematically decrease from 19 to as low as 8.1, and the δ 13C values of the carbonate fraction from 0.5 to −11.8. The change in δ 13C values can be explained by Rayleigh decarbonation during calcsilicate reactions, where calculated $$\Delta ^{13} {\text{C}}_{\left( {{\text{CO}}_{\text{2}} - {\text{cc}}} \right)}$$ is about 4.5 permil for the high-grade samples and less for medium and low-grade samples suggesting a range in temperatures at which most decarbonation occurred. However, the amount of CO2 released was not anough to decrease the whole rock δ 18O to the values observed in the argillites. The low δ 18O values close to the intrusion suggest interaction with magmatic water that had a δ 18O value of 8.5. The extreme lowering of δ 13C by fractional devolatilization and the lowering of δ 18O in argillites close to the intrusion indicates oxgen-equivalent fluid/rock ratios in excess of 1.0 and X(CO2)F of the fluid less than 0.2. Mineral assemblages in conjunction with the isotopic data indicate a strong influence of water infiltration on the reaction relations in the argillites and separate fluid and thermal fronts moving thru the argillites. The different stable isotope relations in limestones and argillites attest to the importance of decarbonation in the enhancement of permeability. The flow of fluids was confined to the argillite beds (argillite aquifers) whereas the limestones prevented vertical fluid flow and convective cooling of the stock.
    Type of Medium: Electronic Resource
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  • 5
    Publication Date: 2015-10-02
    Description: Spinel is a very important rock-forming mineral that is found in basalts from Earth, Mars, the Earth’s Moon, and basaltic meteorites. Spinel can be used as a sensitive indicator of petrologic and geochemical processes that occur in its host rock. This paper highlights the role of increasing f O 2 (from IW-1 to FMQ+2) in converting a 〉90% normal spinel to an ~25% magnetite (inverse) spinel, the trajectory of D V spinel/melt as it relates to the ratio of V 3+ /V 4+ in the melt, and the crystal chemical attributes of the spinel that control the intrinsic compatibility of both V 3+ and V 4+ . This work examines the nuances of the V partitioning and provides a crystal chemical basis for understanding Fe 3+ , Cr, and V substitution into the octahedral sites of spinel. Understanding this interplay is critical for using spinels as both indicators of planetary parentage and reconstructing the redox history of magmatic systems on the terrestrial planets. Three potential examples for this use are provided. In addition, this work helps explain the ubiquitous miscibility gap between spinels with changing ülvospinel contents.
    Print ISSN: 0003-004X
    Electronic ISSN: 1945-3027
    Topics: Geosciences
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  • 6
    Publication Date: 2014-07-02
    Description: Whitlockite and merrillite are two Ca-phosphate minerals found in terrestrial and planetary igneous rocks, sometimes coexisting with apatite. Whitlockite has essential structural hydrogen, and merrillite is devoid of hydrogen. Whitlockite components have yet to be discovered in samples of extraterrestrial merrillite, despite evidence for whitlockite-merrillite solid solution in terrestrial systems. The observation of merrillite in meteoritic and lunar samples has led many to conclude that the magmas from which the merrillite formed were "very dry." However, the Shergotty martian meteorite has been reported to contain both apatite and merrillite, and recently the apatite has been shown to contain substantial OH abundances, up to the equivalent of 8600 ppm H 2 O. In the present study, we determined the abundances of F, Cl, H 2 O, and S in merrillite from Shergotty using secondary ion mass spectrometry (SIMS). We determined that the merrillite in Shergotty was properly identified (i.e., no discernible whitlockite component), and it coexists with OH-rich apatite. The absence of a whitlockite component in Shergotty merrillite and other planetary merrillites may be a consequence of the limited thermal stability of H in whitlockite (stable only at T 〈1050 °C), which would prohibit merrillite-whitlockite solid-solution at high temperatures. Consequently, the presence of merrillite should not be used as evidence of dry magmatism without a corresponding estimate of the T of crystallization. In fact, if a whitlockite component in extraterrestrial merrillite is discovered, it may indicate formation by or equilibration with hydrothermal or aqueous fluids.
    Print ISSN: 0003-004X
    Electronic ISSN: 1945-3027
    Topics: Geosciences
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  • 7
    Publication Date: 2014-07-02
    Description: In this work we present a series of experiments that examine the relationship between oxygen fugacity and Cr valence ratio in olivine grown from a basaltic liquid. These experiments are specifically targeted for an olivine-rich martian basalt composition that was modeled after the bulk chemistry of the meteorite Yamato 980459 (i.e., Y-98). The chromium valence ratio in the olivine crystals was measured with X-ray absorption near edge spectroscopy (XANES) at the Advanced Photon Source, Argonne National Laboratory. Results from the XANES measurements indicate that the ratio of divalent to trivalent Cr in the olivine is not only systematically correlated with f O 2 , but is also reflective of the molar Cr 3+ /Cr 2+ in the silicate liquid from which it grew. In this way, measurements of Cr valence in olivine phenocrysts can yield important information about the oxygen fugacity and molar Cr 3+ /Cr 2+ of its parental liquid in the absence of a quenched melt phase. Although the results from the experiments presented in this work specifically apply to the Y-98 parental melt, the concepts and XANES analytical techniques discussed within the text present a novel, generalized methodology that may be applicable to any olivine-bearing basalt. Furthermore, the XANES-based measurements are made on a micrometer-scale, thus potential changes of the Cr 3+ /Cr 2+ in the melt during crystallization could be examined with a great deal of spatial detail.
    Print ISSN: 0003-004X
    Electronic ISSN: 1945-3027
    Topics: Geosciences
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  • 8
    Publication Date: 2016-04-02
    Description: Pyroxene is arguably the most powerful, single-phase geochemical and petrologic recorder of Solar System processes, from nebular condensation through planetary evolution, over a wide range of temperatures, pressures, and f o 2 . It is an important mineral phase in the crusts and mantles of evolved planets, in undifferentiated and differentiated asteroids, and in refractory inclusions—the earliest Solar System materials. Here, we review the valence state partitioning behavior of Cr (Cr 2+ , Cr 3+ ), Ti (Ti 3+ , Ti 4+ ), and V (V 2+ , V 3+ , V 4+ , V 5+ ) among crystallographic sites in pyroxene over a range of f o 2 from approximately fayalite-magnetite-quartz (FMQ) to ~7 log units below iron-wüstite (IW-7), and decipher how pyroxene can be used as a recorder of conditions of planetary and nebular environments and planetary parentage. The most important crystallographic site in pyroxene with respect to its influence on mineral/melt partitioning is M2; its Ca content has a huge effect on partitioning behavior, because the large Ca cation expands the structure. As a result, distribution coefficients ( D s) for Cr and V increase with increasing Ca content from orthopyroxene to pigeonite to augite. In addition, it is noted that V 3+ is favored over V 4+ in olivine and pyroxene. In pyroxene in refractory inclusions, Ti 3+ is favored over Ti 4+ and incorporation of Ti is facilitated by the high availability of Al for coupled substitution. The most important results from analysis of pyroxene in martian meteorites (e.g., QUE 94201) are the oxygen fugacity estimates of IW+0.2 and IW+0.9 derived from partitioning and valence data for Cr and V, respectively, obtained from experiments using appropriate temperatures and melt compositions. In angrites, changes in V valence state may translate to changes in f o 2 , from IW-0.7 during early pyroxene crystallization, to IW+0.5 during later episodes of pyroxene crystallization. In addition to f o 2 , the partitioning behavior of Cr, V, and Ti between pyroxene and melt is also dependent upon availability of other cations, especially Al, for charge-balancing coupled substitutions.
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    Electronic ISSN: 1945-3027
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  • 9
    Publication Date: 2013-11-19
    Description: A spiked (with REE, V, Sc) martian basalt Yamato 980459 (Y98) composition was used to synthesize olivine, spinel, and pyroxene at 1200 °C at five oxygen fugacities: IW–1, IW, IW+1, IW+2, and QFM. These run products were analyzed by electron microprobe, ion microprobe, and X-ray absorption near-edge spectroscopy to establish four oxybarometers based on vanadium partitioning behavior between the following pairs of phases: V spinel-melt, V/(Cr+Al) spinel-melt, olivine-melt, and spinel-olivine. The results for the spinel-melt, olivine-melt, and V/(Cr+Al) spinel-melt are applicable for the entire oxygen fugacity range while the spinel-olivine oxybarometer is only applicable between IW–1 and IW+1. The oxybarometer based on V partitioning between spinel-olivine is restricted to basalts that crystallized under low oxygen fugacities, some martian, all lunar, as well as samples from 4 Vesta. The true potential and power of the new spinel-olivine oxybarometer is that it does not require samples representative of a melt composition or samples with some remnant of quenched melt present. It just requires that the spinel-olivine pairs were in equilibrium when the partitioning of V occurred. We have applied the V spinel-olivine oxybarometer to the Y98 meteorite as a test of the method.
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    Electronic ISSN: 1945-3027
    Topics: Geosciences
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  • 10
    Publication Date: 2017-08-04
    Description: A revised diagram plotting the Fe/Mn ratio of pyroxene and olivine verses the anorthite content of plagioclase indicates that the Angrite Parent Body originated from a solar system reservoir with a similar Mn-Fe signature to that from which the Earth was derived. The major difference in terrestrial and angritic basalts is the extreme volatile depletion (particularly Na and K) in the latter. Considerable research and publication has been focused on angrite meteorites, which are among the oldest objects in the solar system (~4.56 Ga; Keil 2012 ). These meteorites include a silica-undersaturated mafic mineral assemblage. The identity and location of their parent body is still unknown and widely debated. Our new work on angrites SAH 99555, LEW 86010, NWA 10463, LEW 87051, and Angra dos Reis focused on olivine and is interpreted in the context of existing pyroxene and plagioclase data sets. This paper improves the "Mn-Fe in olivine and anorthite content of plagioclase tool for planetary parentage" specifically targeted at finding members of the angrite group of meteorites.
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    Electronic ISSN: 1945-3027
    Topics: Geosciences
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