The Crystal Structures of Namgp04, Na2camg(P04)2 and Nalsca13mgs(P04hs: New Examples for Glaserite Related Structures

Total Page:16

File Type:pdf, Size:1020Kb

The Crystal Structures of Namgp04, Na2camg(P04)2 and Nalsca13mgs(P04hs: New Examples for Glaserite Related Structures by R. Olden bourg Verlag, Miinchen The crystal structures of NaMgP04, Na2CaMg(P04)2 and NalsCa13Mgs(P04hs: new examples for glaserite related structures J. Alkemper and H. Fuess * Technische Universitar Darmstadt, Fachbereich Materialwissenschaft, Petersenstr. 23, D-64287 Darmstadt, Germany Received October 2nd, 1997; accepted in revised form February 2nd, 1998 Abstract. Three phosphates with (NaMIIp04), composi- polymorphs of NaMgP04 were described (Kapralik, Po- tion have been synthesized and characterized structurally. tancok 1971; Majling 1973; U st'yantsev, Tretnikova, Ke- The low temperature modifications of NaMgP04 and lareva 1976). Na2CaMg(P04h crystallize in the orthorhombic space Brianite, Na2CaMg(P04h. the only intermediate phase group P2j2j2" and the monoclinic space group P21/c, re- in the system NaMgP04-NaCaP04 known by now, was spectively. The phase transitions at high temperature were first described by Fuchs, Olsen and Henderson (1967). investigated by thermal analysis and powder diffractome- Moore (1975) proposed isomorphism with merwinite try. The high-temperature modification of Na2CaMg(P04h (Ca3Mg(Si04h). Ust'yantsev and Tretnikova (1976) de- is isotypic with glaserite, K3Na(S04h as determined by tected a reversible phase transformation at 1113 K and an Rietveld refinement. NajsCa13MgS(P04)IS crystallizes in incongruent melting point at 1493 K. the trigonal space group R3m. The structures of all of Na4Ca4Mg21 (P04) IS, a quarternary oxide with a stoi- these phosphates can be related to the arrangement of ca- chiometry different from the general NaMIIP04 com- tions and phosphate tetrahedra in the glaserite structure. pounds, was synthesized and structurally characterized by Domanskii et al. (1982). Introduction Experimental Whereas the crystal chemistry of silicates of alkaline and alkaline earth metals has extensively been studied the A starting powder for the synthesis of NaMgP04-crystals knowledge of the crystal structures of the corresponding was obtained by heating an equimolar mixture of NaP03 phosphates is rather scarce. As some important biomate- and MgO to 1273 K, cooling to 873 K (5 Klmin) and rials are based on phosphate glass ceramics this lack of holding for 10 h. The powder contained a-NaMgP04, the information constitutes a considerable drawback for the low-temperature modification, and a small amount of further development of these materials (e.g. Vogel, Holand another phosphate, which could not be identified. This 1987; Schulz, Miehe, Fuess, Wange, Gotz 1994; Alkem- powder was then mixed with Na2Mo04 (1: I), heated to per, Fuess 1997). We therefore carried out a program to 1223 K and cooled slowly (10 K/h). After washing with synthesize and to characterize relevant phases which may water the powder contained platelike single crystals of occur in phosphate glass ceramics. a-NaMgP04. Single phase powders could be obtained In the system Na3P04-Ca3(P04h only the structure of by riddling these crystals. one ternary compound, NaCaP0 , was previously deter- 4 Na2CaMg(P04h single crystals were synthesized by mined (Olsen, Bunch, Moore 1977; Ben Amara, Vlasse, mixing NaP03, CaO and MgO in stoichiometric amounts Le FIem, Hagenmuller 1983 a). In the system with Na2Mo04, heating to 1073 K and cooling slowly to Na3P04 - Mg (P0 h three ternary phosphates were re- 3 4 773 K (5 K/h). The Na2Mo04 was removed by washing ported (Majling, Hanic 1976): NaMg (P0 4 4h, with water. In this way a powder with hexagonal Na4Mg(P04h and NaMgP0 . Whereas the structure of the 4 Na2CaMg(P04h- and rhombohedral NalsCaI3Mgs(P04)j8- first is completely known (Ben Amara et al. 1983b), the crystals was obtained. Single phase powders resulted from others were only identified by their powder diffraction pat- riddling the larger Na2CaMg(P04h-crystals. A suitable terns. Indexing for Na4Mg(P04h indicated tetragonal sys- crystal for structure determination had to be selected tem (Ghorbel, d'Yvoire, Dorernieux-Morin 1974) but carefully because the plates were often twinned. failed for NaMgP0 . Using thermal analysis and high-tem- 4 X-ray powder patterns were collected on a STOE perature powder diffraction, up to five high-temperature powder diffractometer in transmission geometry using CuK," I radiation. A position sensitive detector allowed fast * Correspondence author (e-mail: [email protected]) measurements. Structure refinements were performed by Rietveld analysis using FULLPROF (Rodriguez-Carvajal The final atomic coordinates and displacement parameters 1990) for phases with supposed or known structure. Phase are collected in Tables 2-4 I. transformations were observed in-situ using a high tempera- a-NaMgP04 crystallizes in the orthorhombic space tureattachment with Debye-Scherrer geometry. group P2,2,21• The phosphate tetrahedra are near! y re- The data acquisition for single crystal structure deter- gular. Mg is coordinated quadratic pyramidal by five mination was performed using a STOE-STADI-4 diffract- oxygen atoms with distances 1.97 A - 2.18 A. A sixth oxy- ometer with MoKa radiation (scan mode: 28/w = 1/1) at gen atom is shifted to a distance of 2.48 A-2.97 A. The 293 K. Due to the small size of the crystals, long measur- structure is closely related to that of maricite, NaFeP04 ing times and limitations in 28max were inevitable. The (Le Page, Donnay 1977), but there the Fe coordination is structure determination and the refinement were performed slightly distorted but centrosymmetric octahedral. This is with SHELX-86 and SHELXL-93, respectively. the main reason for the symmetry reduction from Pnma Phase transformation temperatures of powders were in the case of NaFeP04 to the subgroup P2,2,2j of detected with heating rates of 5 Klmin using a Setaram NaMgP04. differential scanning calorimeter. a-Na2CaMg(P04h is isotypic with merwmite, Ca2CaMg(Si04h as suggested by Moore (1975). Although Results I Additional material to this paper can be ordered referring to the The crystal structures of NaMgP04, no. CSD 408374 (NaMgP04), CSD 408373 (Na2CaMg(P04)2) and CSD 408372 (NaISCa13Mgs(P04)IS), names of the authors and cita- Na2CaMg(P04h and NalsCa13Mgs(P04hs tion of the paper at the Fachinformationszentrum, Karlsruhe, Ge- sellschaft fur wissenschaftlich-technische Information mbH, D-76344 The details of the single crystal structure data collection Eggenstcin-Leopoldshafen, Germany. The list of Fa/Fe-data is avail- and the structure determination are summarized in Table I. able from the author up to one year after the publication has appeared. Table 1. Details and results of single crystal a-NaMgP0 structure analysis of NaMgP04, 4 Na2CaMg(P04)2 and NalsCa13Mgs(P04)IS. Crystal colorless prism colorless hexagon colorless rhombohedron Crystal size 0.14 x 0.20 x 0.24 mm 0.20 x 0.20 x 0.07 mm 0.12xO.18xO.21 mm 1 I f1 9.35cm- 17.46 cm- 17.39 cm-I 28max 70° 70° 60° N (hkl) unique 3982 2792 1674 N (param )refined 190 128 135 Crystal system, SG orthorhombic, monoclinic, trigonal P212121 (No. 19) P21/c (No. 14) R3m (No. 166) a 8.828(2) A 9.120(3) A 15.811(3) A b 6.821(2) A 5.198(2) A 15.811(3) A c 15.250(4) A 13.370(4) A 21.499(4) A 90.78° 918.3(4) A3 633.8(4) A3 4644(4) A3 4 4 3 0.049 0.040 0.039 0.167 0.119 0.135 Table 2. Final atomic coordinates (- 104) 2 Atom x y c , U Un U U23 UI3 UI2 and displacement parameters (A . 103) for II 33 a-NaMgP0 . 4 Na(l) 1427(1) 2941(2) 5938(1 ) 8(1) 12(1) 9(1) -2(1) 0(1) -1(1) Na(2) 1494(2) 2196(2) 2617(1 ) 12(1) 17(1) 7(1)7 0(1) -1(1) -1(1) Na(3) 1484(2) 2324(2) -715(1) lI(1) 20(1) 9(1) 2(1) 0(1) 3(1) Mg(l) 4867(1 ) 4529(1 ) 2604(1 ) 7(1) 6(1) 6(1) -2(1) -2(1) 0(1) Mg(2) 4804(1) 415(1) 5960(1 ) 8(1) II (I) 8(1) 2(1) -3(1) -2(1) Mg(3) 4959(1 ) 247(1 ) 9218(1 ) 6(1) 13(1) 6(1) 3(1) -2(1) -2(1) P(I) 3204(1) 2184(1 ) 992(1) 2(1) 5(1) 3(1) 0(1) -1(1) -1(1) P(2) 3200(1) 2755(1 ) 7646(1 ) 3(1) 5(1) 2(1) 0(1) 0(1) 0(1) P(3) 3163(1 ) 2559(1) 4332(1 ) 3(1) 10(1) 3(1) 2(1) 0(1) 0(1) 0(1) 3845(2) 3964(3) 1476(1) 12(1) 5(1) 5(1) 0(1) -3(1) -2(1) 0(2) 3559(2) 4435(3) 4835(1) 8(1) II (1) 8(1) -2(1) -3(1) -2(1) 0(3) 3839(2) 4581(3) 8093(1) II (I) 9(1) 7(1) -3(1) -4(1) -4(1) 0(4) 1439(2) 2294(3) 1016(1) 3(1) 13(1) 7(1) 1(1) 1(1) 2(1) 0(5) 3805(2) 2157(3) 49(1) 6(1) 14(1) 5(1) -2(1) 1(1) 1(1) 0(6) 1439(2) 2861(2) 7665(1 ) 2(1) 5(1) 9(1) 0(1) -1(1) 0(1) 0(7) 3782(2) 2581(3) 3388(1 ) 7(1) 17(1) 4(1) 1(1) 2(1) 0(1) 0(8) 1404(2) 2347(3) 4334(1 ) 3(1) 12(1) 7(1) 2(1) 1(1) 3(1) 0(9) 3677(2) 939(3) 8160(1 ) II (I) 10(1) 10(1) 2(1) -4(1) 3(1) 0(10) 3666(2) 327(3) 1490(1) II (I) 5(1) 13(1) 1(1) -6(1) -1(1) 0(11) 3860(2) 817(3) 4810(1 ) 8(1) 13(1) 9(1) 4(1) -3(1) 1(1) 0(12) 3812(2) 2688(3) 6693(1 ) 6(1) 13(1) 6(1) -2(1) 2(1) 1(1) Table 3.
Recommended publications
  • CRYSTAL STRUCTURE of NATURAL STANFIELDITE from the IMILAC PALLASITE; Ian M
    LPSC XXIII 1355 CRYSTAL STRUCTURE OF NATURAL STANFIELDITE FROM THE IMILAC PALLASITE; Ian M. Steele and Edward Olsen, Department of Geophysical Sciences, 5734 S. Ellis Ave., Chicago, IL 60637. Stanfieldite, ideally Ca4Mg5P6024,was first recognized by Fuchs (1) and has since been described from some 15 pallasites (1 $2)and at least one mesosiderite (1). It is one of several phosphates including farringtonite, brianite and panethite which have not been recognized in terrestrial samples. Stanfieldite commonly coexists with whitlockite (Ca3(P04)2), but in two pallasites, Springwater and Rawlinna, farringtonite (Mg3(P04)2)is present in addition to whitlockite. According to the phase diagram determined by Ando (3) the three phosphates should not occur but rather only farringtonite-stanfieldite or whitlockite-stanfieldite. This is especially true as the pallasites have cooled very slowly and equilibrium should be expected. Fuchs (1) described the space group of stanfieldite from the Estherville mesosiderite as either Pcor PUcwhile Dickens and Brown (4) gave the space group of synthetic Ca7Mg9(Ca,Mg)2(P04),2 as C2/c and determined the structure within this space group. To resolve the apparent discrepancy in space group and to verify that natural stanfieldite has the same structure as the synthetic material, we selected a single crystal of stanfieldite from the lmilac pallasite and determined both the space group and structure from single crystal intensity data. Particular attention is given to the possibility of ordering of Mg, Fe and Mn with a possible effect on the space group. S~acearoup: A single crystal study using precession techniques showed systematic - absences of hkl diffractions with h+k = odd and h01 diffractions with h = odd and I = odd.
    [Show full text]
  • Silicate-Bearing Iron Meteorites and Their Implications for the Evolution Of
    Chemie der Erde 74 (2014) 3–48 Contents lists available at ScienceDirect Chemie der Erde j ournal homepage: www.elsevier.de/chemer Invited Review Silicate-bearing iron meteorites and their implications for the evolution of asteroidal parent bodies ∗ Alex Ruzicka Cascadia Meteorite Laboratory, Portland State University, 17 Cramer Hall, 1721 SW Broadway, Portland, OR 97207-0751, United States a r t a b i c s t l r e i n f o a c t Article history: Silicate-bearing iron meteorites differ from other iron meteorites in containing variable amounts of sili- Received 17 July 2013 cates, ranging from minor to stony-iron proportions (∼50%). These irons provide important constraints Accepted 15 October 2013 on the evolution of planetesimals and asteroids, especially with regard to the nature of metal–silicate Editorial handling - Prof. Dr. K. Heide separation and mixing. I present a review and synthesis of available data, including a compilation and interpretation of host metal trace-element compositions, oxygen-isotope compositions, textures, miner- Keywords: alogy, phase chemistries, and bulk compositions of silicate portions, ages of silicate and metal portions, Asteroid differentiation and thermal histories. Case studies for the petrogeneses of igneous silicate lithologies from different Iron meteorites groups are provided. Silicate-bearing irons were formed on multiple parent bodies under different con- Silicate inclusions Collisions ditions. The IAB/IIICD irons have silicates that are mainly chondritic in composition, but include some igneous lithologies, and were derived from a volatile-rich asteroid that underwent small amounts of silicate partial melting but larger amounts of metallic melting. A large proportion of IIE irons contain fractionated alkali-silica-rich inclusions formed as partial melts of chondrite, although other IIE irons have silicates of chondritic composition.
    [Show full text]
  • Mineral Evolution
    American Mineralogist, Volume 93, pages 1693–1720, 2008 REVIEW PAPER Mineral evolution ROBERT M. HAZEN,1,* DOMINIC PAPINEAU,1 WOUTER BLEEKER,2 ROBERT T. DOWNS,3 JOHN M. FERRY,4 TIMOTHY J. MCCOY,5 DIMITRI A. SVERJENSKY,4 AND HEXIONG YANG3 1Geophysical Laboratory, Carnegie Institution, 5251 Broad Branch Road NW, Washington, D.C. 20015, U.S.A. 2Geological Survey of Canada, 601 Booth Street, Ottawa, Ontario K1A OE8, Canada 3Department of Geosciences, University of Arizona, 1040 East 4th Street, Tucson, Arizona 85721-0077, U.S.A. 4Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, Maryland 21218, U.S.A. 5Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, D.C. 20560, U.S.A. ABSTRACT The mineralogy of terrestrial planets evolves as a consequence of a range of physical, chemical, and biological processes. In pre-stellar molecular clouds, widely dispersed microscopic dust particles contain approximately a dozen refractory minerals that represent the starting point of planetary mineral evolution. Gravitational clumping into a protoplanetary disk, star formation, and the resultant heat- ing in the stellar nebula produce primary refractory constituents of chondritic meteorites, including chondrules and calcium-aluminum inclusions, with ~60 different mineral phases. Subsequent aque- ous and thermal alteration of chondrites, asteroidal accretion and differentiation, and the consequent formation of achondrites results in a mineralogical repertoire limited to ~250 different minerals found in unweathered meteorite samples. Following planetary accretion and differentiation, the initial mineral evolution of Earth’s crust depended on a sequence of geochemical and petrologic processes, including volcanism and degassing, fractional crystallization, crystal settling, assimilation reactions, regional and contact metamorphism, plate tectonics, and associated large-scale fluid-rock interactions.
    [Show full text]
  • Brianite, Narcamg[Poa]R: a Phosphate Analog of Merwinite
    American Mineralogist, Volume60, pages 717-718, lgTS Brianite,NarCaMg[POa]r: A phosphateAnalog of Merwinite, CarCaMgISiO4], Peur BnrnNMoonn Departmentof the GeophysicalSciences, The (lniuersity of Chicago,Chicago, Illinois 60637 Abstract Brianite,Na,CaMg[po,l,, a t3.36(5)A,t s.zl14e,, c 9.13(3)A,p 91.2(0.2)",space group P2r/a,is structurallyisomorphic to merwinite,CarCaMg[SiOn]r. Fuchs,Olsen, and Henderson(1967) describeda calculationsalong [0] l], [03I], and [100]which are new species,brianite, which occurs as a rare con- comparedwith the earlier study. It is instructiveto stituent in small pocketsin the Dayton octahedrite note that Moore and Araki (1972)pointed out mis- from Montgomery County, Ohio. Brianite was settingsof the same kind in an earlier study on observedto possessfine lamellar structurewith ex- merwinite.The refinedcell data for brianite obtain tinction anglesbetween adjacent lamellae of 2-3". from an indexing of the original powder data in The authors concludedthat the compoundis almost Fuchsel al. The first thirty linesof thesepowder data ideally NarCaMg[POn],on the basis of detailed have been indexed (Table 2) on the basis of a electronmicroprobe study. calculatedpowder pattern derived from merwinite Rotation and Weissenbergphotographs led Fuchs crystal structure data. Brianite is polysynthetically et al to concludethat brianiteis orthorhombic,and twinnedon { 100},explaining the lamellarappearance their resultsare presentedin Table l. A marked of the grains. spatial similarity between brianite and bredigite, Moore (1973), in a topological-geometrical (Ca,Ba)Ca,rMgr[SiOn]r, wasnoted by theseauthors, analysisof alkali sulfate and calcium orthosilicate having been suggested by Dr. A. Kato as a private structures,noted three kinds of large cation communicationin their study.
    [Show full text]
  • Chladniite, Narcamgr(Poo)U: a New Mineral from the Carlton (IIICD) Iron Meteorite
    American Mineralogist, Volume 79, pages 375-380, 1994 Chladniite, NarCaMgr(POo)u: A new mineral from the Carlton (IIICD) iron meteorite Trvrorny J. McCov Planetary Geosciences,Department of Geology and Geophysics,School of Oceanand Earth Scienceand Technology, University of Hawaii at Manoa, Honolulu, Hawaii 96822, U.S.A. I.q,NrM. Srnrr,n Department of the GeophysicalSciences, University of Chicago, 5734 S. Ellis Ave., Chicago,Illinois 60637, U.S.A. Kr,lus Knrr, Planetary Geosciences,Hawaii Center for Volcanology, Department of Geology and Geophysics, School of Ocean and Earth Scienceand Technology, University of Hawaii at Manoa, Honolulu, Hawaii 96822, U.S.A. B. F. Lnoxano U.S. Geological Survey, Box 25046, M.S. 905, Denver FederalCenter, Denver, Colorado 80225, U.S.A. MlcNus ENonns Institut ftir Planetologie,Westflilische Wilhelms-Universit?it, D-4400 Mi.inster,Germany Ansrntcr A new mineral, chladniite, NarcaMgr(Poo)u, occurs as a single grain within a silicate- bearing inclqsion in the Carlton (IIICD) iron meteorite. It is hexagonal, R3, a : 14.967, c : 42.595 A. tt is named for E.F.F.Chladni (1756-1827),who is widely regardedas the founder of the scienceof meteoritics. Chladniite is colorlessand transparent when pow- dered. In polished section, the mineral is gray, dark, weakly bireflecting, and weakly an- isotropic. Cleavage,rarely visible, is rhomboidal in plan. Polishing hardnessis less than low-calcium orthopyroxene, but greater than Fe,Ni metal. Reflectancemeasurements at -- 589 nm give R, : 5.3o/o,R, 5.60/o.Assuming an absorption coefficient k : 0, the cal- culated refractive indices are nt : | .60, n, : | .62.
    [Show full text]
  • Compiled Thesis
    SPACE ROCKS: a series of papers on METEORITES AND ASTEROIDS by Nina Louise Hooper A thesis submitted to the Department of Astronomy in partial fulfillment of the requirement for the Bachelor’s Degree with Honors Harvard College 8 April 2016 Of all investments into the future, the conquest of space demands the greatest efforts and the longest-term commitment, but it also offers the greatest reward: none less than a universe. — Daniel Christlein !ii Acknowledgements I finished this senior thesis aided by the profound effort and commitment of my thesis advisor, Martin Elvis. I am extremely grateful for him countless hours of discussions and detailed feedback on all stages of this research. I am also grateful for the remarkable people at Harvard-Smithsonian Center for Astrophysics of whom I asked many questions and who took the time to help me. Special thanks go to Warren Brown for his guidance with spectral reduction processes in IRAF, Francesca DeMeo for her assistance in the spectral classification of our Near Earth Asteroids and Samurdha Jayasinghe and for helping me write my data analysis script in python. I thank Dan Holmqvist for being an incredibly helpful and supportive presence throughout this project. I thank David Charbonneau, Alicia Soderberg and the members of my senior thesis class of astrophysics concentrators for their support, guidance and feedback throughout the past year. This research was funded in part by the Harvard Undergraduate Science Research Program. !iii Abstract The subject of this work is the compositions of asteroids and meteorites. Studies of the composition of small Solar System bodies are fundamental to theories of planet formation.
    [Show full text]
  • Schreibersite Growth and Its Influence on the Metallography of Coarse-Structured Iron Meteorites
    SMITHSONIAN CONTRIBUTIONS TO THE EARTH SCIENCES • NUMBER 21 Schreibersite Growth and Its Influence on the Metallography of Coarse-Structured Iron Meteorites Roy S. Clarke, Jr. and Joseph I. Goldstein SMITHSONIAN INSTITUTION PRESS City of Washington 1978 ABSTRACT Clarke, Roy S., Jr., and Joseph I. Goldstein. Schreibersite Growth and Its Influence on the Metallography of Coarse-Structured Iron Meteorites. Smithson- ian Contributions to the Earth Sciences, number 21, 80 pages, 28 figures, 20 tables, 1978. —The role that schreibersite growth played in the structural development process in coarse-structured iron meteorites has been examined. The availability of many large meteorite surfaces and an extensive collection of metallographic sections made it possible to undertake a comprehensive survey of schreibersite petrography. This study was the basis for the selection of samples for detailed electron microprobe analysis. Samples containing representative structures from eight chemical Groups I and IIAB meteorites were selected. Electron microprobe traverses were made across structures representative of the observed range of schreibersite associations. Particular emphasis was placed on schreibersite-kamacite interface compositions. An analysis of these data has led to a comprehensive description of the structural development process. Massive schreibersite, one of the four major types of schreibersite encoun- tered, may be accounted for by equilibrium considerations. Subsolidus nuclea- tion and growth with slow cooling from temperatures at least as high as 850° C, and probably much higher, explain the phase relationships that one sees in meteorite specimens. The retention of taenite in the octahedrites establishes that bulk equilibrium did not extend as low as 550° C. Schreibersite undoubtedly continued in equilibrium with its enclosing kamacite to lower temperatures.
    [Show full text]
  • Mccoy, T. J. Mineralogical Evolution of Meteorites. Elements
    Mineralogical Evolution of Meteorites Halite crystals from the Monahans chondrite contain fl uid inclusions, which indicate Timothy J. McCoy* signifi cant water–rock interactions in the 1811-5209/10/0006-0019$2.50 DOI: 10.2113/gselements.6.1.19 meteorite’s parent body. Image width ~5 mm. COURTESY OF M. he approximately 250 mineral species found in meteorites record the ZOLENSKY AND R. BODNAR earliest stages of the birth of our solar system. Refractory minerals but eventually transformed some that formed during the violent deaths of other stars and during conden- T asteroids into molten worlds that sation of our own solar nebula mixed with a wide range of silicates, sulfi des, formed crusts, mantles, and cores and metals to form the most primitive chondritic meteorites. Subsequent reminiscent of our own planet. It aqueous alteration, thermal metamorphism, and shock metamorphism further is this history—from the earliest beginnings to the melting of diversifi ed the minerals found in meteorites. Asteroidal melting at fi rst planets—that we explore in this increased and then dramatically decreased mineralogical diversity, before a article. new phase of igneous differentiation that presaged the processes that would occur in terrestrial planets. THE STELLAR CAULDRON Earth’s mineralogical evolution KEYWORDS: mineral evolution, meteorites, asteroids, metamorphism, began not in the heat of an early differentiation, shock molten planet but in the blast furnace of stars that predated our FRAGMENTS FROM THE BEGINNING solar system. More than 4.6 billion years ago, presolar As Earth evolved over the last 4.5 billion years, its miner- grains formed when temperatures in the expanding enve- alogy changed.
    [Show full text]
  • Mineralogy of Silicate-Natrophosphate Immiscible † Inclusion in Elga IIE Iron Meteorite
    minerals Article Mineralogy of Silicate-Natrophosphate Immiscible y Inclusion in Elga IIE Iron Meteorite Victor V. Sharygin 1,2 1 V.S. Sobolev Institute of Geology and Mineralogy, Siberian Branch of the RAS, 3 Acad. Koptyuga pr., 630090 Novosibirsk, Russia; [email protected] 2 ExtraTerra Consortium, Institute of Physics and Technology, Ural Federal University, 19 Mira str., 620002 Ekaterinburg, Russia The paper was presented at the 81st Annual Meeting of the Meteoritical Society in Moscow, Russia, y 22–27 July 2018. Received: 7 April 2020; Accepted: 11 May 2020; Published: 13 May 2020 Abstract: Rare type of silicate inclusions found in the Elga iron meteorite (group IIE) has a very specific mineral composition and shows silicate ( 90%)–natrophosphate ( 10%) liquid ≈ ≈ immiscibility due to meniscus-like isolation of Na-Ca-Mg-Fe phosphates. The 3 mm wide immiscible inclusion has been first studied in detail using optical microscopy, scanning electron microscopy, electron microprobe analysis and Raman spectroscopy. The silicate part of the inclusion contains fine-grained quartz-feldspar aggregate and mafic minerals. The relationships of feldspars indicate solid decay of initially homogenous K-Na-feldspar into albite and K-feldspar with decreasing of temperature. Some mafic minerals in the silicate part are exotic in composition: the dominant phase is an obertiite-subgroup oxyamphibole (amphibole supergroup), varying from ferri-obertiite 3+ 2+ NaNa2Mg3Fe Ti[Si8O22]O2 to hypothetical NaNa2Mg3Fe 0.5Ti1.5[Si8O22]O2; minor phases are the aenigmatite-subgroup mineral (sapphirine supergroup) with composition close to median value 2+ of the Na2Fe 5TiSi6O18O2-Na2Mg5TiSi6O18O2 join, orthopyroxene (enstatite), clinopyroxene of the diopside Ca(Mg,Fe)Si2O6–kosmochlor NaCrSi2O6-Na(Mg,Fe)0.5Ti0.5Si2O6 series and chromite.
    [Show full text]
  • Trace Element Inventory of Meteoritic Ca-Phosphates
    Trace element inventory of meteoritic Ca-phosphates Dustin Ward1, Addi Bischoff1, Julia Roszjar2, Jasper Berndt3 and Martin J. Whitehouse4 1Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany 2Department of Mineralogy and Petrography, Natural History Museum Vienna, Burgring 7, 1010 Vienna, Austria 3Institut für Mineralogie, Westfälische Wilhelms-Universität Münster, Corrensstraße 24, 48149 Münster, Germany 4Department of Geosciences, Swedish Museum of Natural History, Box 50007, 10405 Stockholm, Sweden Abstract Most extraterrestrial samples feature the two accessory Ca-phosphates - apatite-group minerals and merrillite, which are the dominating carrier phases of the rare earth elements (REE). The trace element concentrations (REE, Sc, Ti, V, Cr, Mn, Co, As, Rb, Sr, Y, Zr, Nb, Ba, Hf, Ta, Pb, Th and U) of selected grains were analyzed by LA-ICP-MS and/or SIMS (REE only). This systematic investigation includes 99 apatite and 149 merrillite analyses from meteorites deriving from various asteroidal bodies including one carbonaceous chondrite, eight ordinary chondrites, three acapulcoites, one winonaite, two eucrites, five shergottites, one ureilitic trachyandesite, two mesosiderites and one silicated IAB iron meteorite. Although Ca-phosphates predominantly form in metamorphic and/or metasomatic reactions, some are of igneous origin. As late-stage phases that often incorporate a vast majority of their host’s bulk REE budget, the investigated Ca-phosphates have REE enrichments of up to two orders of magnitude compared to the host rocks bulk concentrations. Within a single sample, each phosphate species displays a uniform REE-pattern, and variations are mainly restricted to their enrichment, therefore indicating similar formation conditions. Exceptions are brecciated samples, i.e., the Adzhi- Bogdo (LL3-6) ordinary chondrite.
    [Show full text]
  • Part 1. Meteorites
    Part 1. Meteorites GEOLOGICAL SURViTf PROFESSIONAL PAPER Data of Geochemistry Sixth Edition MICHAEL FLEISCHER, Technical Editor Chapter B. Cosmochemistry Part 1. Meteorites By BRIAN MASON GEOLOGICAL SURVEY PROFESSIONAL PAPER 440-B-l Tabulation and discussion of elemental abundances in the different classes of stony and iron meteorites, and in their constituent minerals UNITED STATES GOVERNMENT PRINTING OFFICE, WASHINGTON : 1979 UNITED STATES DEPARTMENT OF THE INTERIOR CECIL D. ANDRUS, Secretary GEOLOGICAL SURVEY H. William Menard, Director Library of Congress catalog-card No. 79-64561 For sale by the Superintendent of Documents, U.S. Government Printing Office Washington, D.C. 20402 Stock Number 024-001-031621 DATA OF GEOCHEMISTRY, SIXTH EDITION Michael Fleischer, Technical Editor The first edition of the Data of Geochemistry, by F. W. Clarke, was published in 1908 as U.S. Geological Survey Bulletin 330. Later editions, also by Clarke, were published in 1911, 1916, 1920, and 1924 as Bulletins 491, 616, 695, and 770. This, the sixth edition, has been written by several scientists in the Geological Survey and in other institutions in the United States and abroad, each preparing a chapter on his special field. The current edition is being published in individual chapters, titles of which are listed below. Chapters already published are indicated by boldface. CHAPTER A. The chemical elements B. Cosmochemistry Part 1, Meteorites by Brian Mason] Part 2, Cosmochemistry. C. Internal structure and composition of the earth. D. Composition of the earth's crust, by R. L. Parker E. Chemistry of the atmosphere F. Chemical composition of subsurface waters, by Donald E. White, John D.
    [Show full text]
  • Supplement Abstracts.Fm
    Abstracts for the 61st Annual Meeting of the Meteoritical Society Item Type Article; text Citation Abstracts for the 61st Annual Meeting of the Meteoritical Society. Meteoritics & Planetary Science, 43(S7), 15-178 (2008). DOI 10.1111/j.1945-5100.2008.tb00711.x Publisher The Meteoritical Society Journal Meteoritics & Planetary Science Rights Copyright © The Meteoritical Society Download date 28/09/2021 00:01:36 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/656517 Meteoritics & Planetary Science 43, Nr 7, Supplement, A15–A178 (2008) http://meteoritics.org Abstracts 5316 5030 ROSETTA FLYBY TARGET ASTEROID (2867) STEINS: AN VARIETIES OF CARBON MINERALS IN ANTARCTIC ENSTATITE ACHONDRITE ANALOGUE CARBONACEOUS CHONDRITES BY TEM AND THEIR P. A. Abell 1, 2, P. R. Weissman3, M. D. Hicks3, Y. J. Choi3, and S. C. Lowry3. IMPLICATIONS 1Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson, AZ Junji Akai1, Takayuki Aoki2, and Hikaru Ohtani1. 1Department of Geology, 85719, USA. E-mail: [email protected]. 2NASA Johnson Space Center, Fac. Sci., Niigata University, Niigata, Japan. 2Asahi Carbon Co., Niigata, Houston, TX 77058, USA. 3Jet Propulsion Laboratory, 4800 Oak Grove Japan. Drive, Pasadena, CA 91109, USA. A variety of fine-grained carbonaceous materials are contained in Introduction: On September 5, 2008, the European Space Agency’s carbonaceous chondrite (CC) matrix. However, Antarctic meteorites have not Rosetta spacecraft will fly by the main-belt asteroid
    [Show full text]