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Ofe3+[Sirrorol: a New Rock-Forming Silicate Mineral of the Osumilite

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American Mineralogist, Volume 74, pages 1368-1373, 1989 Chayesite,K(Mg,Fe2+)oFe3+[SirrOrol: A new rock-formingsilicate mineral of the osumilite group from the Moon Canyon (Utah) lamproite DlNrpr.r-nVnr-on Laboratoire de P6trologieMin6ralogique, Universit6 P. et M. Curie (UA 0736 du CNRS), 4, PlaceJussieu, F-75252 Paris Cedex 05, France Orar MnoBNn.l,cH Institut liir Mineralogie, Ruhr-Universitat, Postfach 102148, D-4630 Bochum l, West Germany CnnrsrrlNn WAGNER Laboratoire de PdtrologieMin6ralogique, Universit6 P. et M. Curie (UA 0736 du CNRS), 4, PlaceJussieu, F-75252 Paris Cedex 05, France WnnNrn Scnnpvnn Institut fiir Mineralogie, Ruhr-Universitat, Postfach 102148, D-4630 Bochum 1, West Germany Ansrn-q,cr Microprobe analyses(mean of l0 grains)of chayesitegave SiO, :69.19, TiO, : 0.25, AlrO,:0.20, Fe'O,:4.88, FeO: 6.60,MnO :0.29, MgO : 12.71,Na'O:0.31, KrO :5.17, total: 99.60wto/o,leading to the formula (basedon O: 30, with Fe valences partitionedto give Si + Al + Fe2++ Fe3++ Mg + Mn + Ti : 17) (K, ,oNao,o)", ,o(Mg, ,nFefrjrMno.oo)*.oo(Fe3.toFet.lnAlo ooTio03)>1 ooSir2 ooO30 oo. The idealizedend-member is K(Mg,Fe'?+)oFe3*[Si,rOro],which (with Mg:Fe'z+'Fe3+: 3.32:0.99:0.69)requires SiOr 69.l5, FerOr 5.28,FeO 6.82,MgO 12.83,KrO 5.92,total 100.00wto/0. X-ray powder data prove chayesiteto be a member of the osumilite group. It is related to roedderite,(Na,K)r(Mg,Fe)r[Si,rOro], by the substitutionFe3+ + tr : Fe2++ (Na,K). The strongestpowder lines are 7.14 (st) 002, 5.08 (vst) I 10, 3.75 (vst) 202,3.24 (vst) l2l, 2.782 (st) 204. Chayesite is hexagonal,probably P6/mcc (by analogy with the osumilite group)wirh a : 10.153(4)A, c : 14.388(6)A, V : 1284.4L', Z: 2. Chayesiteoccurs microscopically as a late-crystallizing phase in a lamproite at Moon Canyon, Utah, U.S.A. The crystalsare deep blue, transparent,and tabular; their streak is white, and their luster is vitreous. They show no cleavage.D^":2.68 g/cm3.Uniaxial positivewith <o: 1.575(l) (O, sky blue) and e : 1.578(l) (E, colorless).There is probably a secondoccunence in a lamproite from Cancarix, Spain. The name is for Dr. Felix Chayes,Geophysical Laboratory, Washington, D.C., U.S.A. Type material is deposited in the Institut fiir Mineralogie, Ruhr-Universitiit Bochum, F.R.G., and in the National Museum of Natural History (Smithsonian Institution), Wash- ington,D.C., U.S.A.,number NMNH 165807. INrnooucrroN AND occuRRENCE the common elementsNa, K, Mg, Fe2+,Fe3*, and Al mostly present in members of the osumilite group, the The osumilite-$oup minerals form a constantly grow- milarite-type minerals as a whole may also contain other ing family of double-ring silicates with a milarite-type elementsuch as Li, Be,B, Ba, Sn, andZr, aswell aswater. structure. Six-membered double rings are linked by R,+ The present publication deals with the description of octahedra and by distorted tetrahedra. A review of mi- chayesite,a new member of the osumilite-group that has larite-type minerals was publishedby Forbeset al. (1972), been found as a rock-forming mineral in a lamproite who gave their generalformula as from Utah and probably also in a lamproite from Canca- rix, Spain. It has the idealized formula K(Mg,Fe'z+)o- 2tcrel8216lArr4lT(2)3 rrElDrr [r41T(I )' rOro]. Fe3*[Si,rOro] and is related to roedderite, (Na,K)r- (Mg,Fe'?+)r[Si,rOro],by the substitutionFe3* + E : Fe2+ This crystal-chemical formula allows for the incorpo- + (Na,K). Thus it contains only one alkali atom per for- ration ofcations with very different sizesand leads to an mula unit like osumilite itself, which has a composition enormous chemical variability and complexity. Besides nearK(Mg,Fe'z+ )2A13 [A12Si]oo3ol. 0003-004x/89/l r l 2-1368$02.00 r368 VELDE ET AL.: CHAYESITE l 369 Within the osumilite group, a chemical distinction is made by Bunch and Fuchs (1969) betweenthe Al-rich Choyesite,Moon Conyon osumilite-yagiite subgroup and the Al-poor merrihueite- Choyesrte,Concorix roedderitesubgroup, the latter being definedby an atomic Roedderite,Eifel Mountoins ratio Si/Al > 7. Chayesite thus belongs to the merri- hueite-roedderitesubgroup. = Chayesitehas been found in lamproite specimenMC7, o- originallydescribed from Moon Canyon,east of Francis, Summit County,Utah, by Bestet al. (1968).It is present d in all thin sections cut from this specimen but has not o beenfound in other samplescollected from the sameout- tl. crop. Unlike roedderite, which in terrestrial occurrencesis restricted to melt-coated cavities in gneiss xenoliths in volcanic rocks (Hentschelet al., 1980),chayesite is part of the igneous mineral assemblageand apparently crys- tallized as a late phasefrom the lamproite liquid. A min- eralogicaldescription of the Moon Canyon lamproite al- (K*No) p.f.u. .j::L* ready mentioning the new phase was given by Wagner and Velde (1986,p. 27-28). Fig.1. Plotofcalculated Fe3+ contents ofchayesite (this study) andselected roedderite from theliterature versus alkali contents The name hasbeen given in honor or Dr. Felix Chayes, analyzed.For methodofcalculation, see text. Solid line indicates a petrologist formerly on the staffof the GeophysicalLab- the substitutionfrom ideal chayesiteto ideal roedderiteend- oratory of the Carnegie Institution of Washington and members.Dashed line separatesthe chayesiteand roedderite past-presidentof the Mineralogical Society of America. solidsolution fields as defined by the alkali values. Dr. Chayes showed deep interest in the mineralogy of alkaline rocks before creating a new discipline, statistical petrology. The name and mineral have beenapproved by ring silicate.If the method of calculatingthe Fe2+/Fe3+ the InternationalMineralogical Association. ratios as outlined above is used,however, the Si values Type material has been deposited in the collections of per formula unit of Table I show only a small scatter the Institut fiir Mineralogie, Ruhr-Universitdt, Bochum, around 12.00.For valuesbelow 12.00.some Al can be F.R.G., as well as in the Museum of Natural History used to complete the tetrahedral T(l) sites to the ideal (Smithsonian Institution), Washington, D.C., U.S.A., occupancy(analyses l-3 of Table l). Only analysis4 shows numberNMNH 165807. a somewhatlarger deviation from the theoretical Si max- imum of 12.00.The generallyexcellent fit of the tetra- Crrnlrrc,c.L coMposrrroN hedral and octahedral occupanciesis consideredindirect Table I gives selected electron-microprobe analyses support for the calculationsas well as for the presenceof covering the range of chemical composition of chayesite a considerableamount of Fe3+.The presenceof Fe3+is from the Moon Canyon sample,together with some anal- also in ag.reementwith the deep blue color of chayesite, ysesofterrestrial roedderite from the literature. Analyses becauseGoldman and Rossman(1978) have alreadyin- wereperformed with an automatedcAMEBAX electron mi- terpreted the very similar blue color of most osumilites croprobe at the Laboratoire de P6trologieMin6ralogique, as being due to Fe2+-Fe3+charge transfer. Paris. Experimental conditions were the following: accel- It can also be seen from the empirical chayesite for- eration voltage, l5 kV; current intensity, l0 nA; counting mulae of Table I that the excessof the alkali sums (K + time, 30 s; standardswere oxides or natural minerals. No Na) over 1.00-that is, over that of the idealizedchay- elementswith atomic number >9, other than thoselist- esite formula K(Mg,Fe'z*)oFe3+[Si,rOro] -is charge-bal- ed, were detected.An ion-microprobe analysis showed a anced by a numerically similar deficiencyof Fe3+against very small amount of Li, but not enoughto be considered 1.0. The data are plotted for a total of l0 chayesiteanal- a significant constituent of the mineral. The Fe3+/Fe2+ ysesin Figure I and provide good evidenceforthe cation ratios were calculatedby assumingfull occupancyfor all substitution Fe3+ + [ : Fe2+ * (Na,K), which relates tetrahedraland octahedralsites, bringing this cation sum the idealized chayesiteend-member given above to roed- without the alkaliesto ) : 17.0 and charge-balancingthe derite,(Na,K)r(Mg,Fe,*)r[Si,rOro]. Analysis A of Table I total cations including the alkalies against 30 oxygens. and Figure I representsa terrestrial exampleofroedderite It should be emphasized here that a recalculation of (Hentschelet al., 1980) recalculatedaccording to the the structural formulae of chayesitewith the assumption method used in the presentpaper. that all Fe is present as FeO leads to impossibly high Si The substitutionalmechanism Fe3+ + E : Fe2+* Na+, values per formula unit (up to 12.18) and to sums of which leaves a vacancy in one of the alkali sites, has tetrahedralplus octahedralcations far above 17.00,which alreadybeen suspected by Hentschelet al. (1980)as well cannot be accommodated in the structure of a double- as bv Abraham et al. (1983)in analvticalstudies ofblue t370 VELDE ET AL.: CHAYESITE c o Choyesrte, Moon Conyon ", A Choyesite,Concqrix + O Roedderite,Eifel Mountoins o) ^\t + -a 02 Fig. 4. Idealized sketch of chayesite morphology (compare LL oc Fie. 3). o0 -o LL oA o2 04 UO No/(No*11) It is interesting to note in this connection that the sub- stitution Fe3+ * ! : Fe2+ + Na* linking chayesiteand Fig. 2. Fe,.,/(Fe.",+ Mg + Mn) versusNa/(Na + K) plot roedderite was also shown to occur in osumilite itself, showingnegative correlation for the chayesiteand roedderite for alkali deficienciesbelow 1.00 analysesofFig. 1. where it is responsible per formula unit (Schreyeret al., 1983). As the new mineral chayesitecontains Fe3+ as an es- sential component, minimum amounts of Fe are present roedderite crystals from the Eifel, Germany, in order to in the solid-solution seriesfrom roedderite to chayesite, explain their observed alkali deficiencies. The micro- increasingfrom zero for pure roedderite to one Fe3+per probe analysesof thesecrystals are also included in Table formula unit for the chayesiteend-member (seeFig.
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    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.
  • Chance and Necessity in the Mineral Diversity of Terrestrial Planets

    Chance and Necessity in the Mineral Diversity of Terrestrial Planets

    295 The Canadian Mineralogist Vol. 53, pp. 295-324 (2015) DOI: 10.3749/canmin.1400086 MINERAL ECOLOGY: CHANCE AND NECESSITY IN THE MINERAL DIVERSITY OF TERRESTRIAL PLANETS § ROBERT M. HAZEN Geophysical Laboratory, Carnegie Institution of Washington, 5251 Broad Branch Road NW, Washington, DC 20015, U.S.A. EDWARD S. GREW School of Earth and Climate Sciences, University of Maine, Orono, Maine 04469, U.S.A. ROBERT T. DOWNS AND JOSHUA GOLDEN Department of Geosciences, University of Arizona, 1040 E. 4th Street, Tucson, Arizona 85721-0077, U.S.A. GRETHE HYSTAD Department of Mathematics, University of Arizona, 617 N. Santa Rita Ave., Tucson, Arizona 85721-0089, U.S.A. ABSTRACT Four factors contribute to the roles played by chance and necessity in determining mineral distribution and diversity at or near the surfaces of terrestrial planets: (1) crystal chemical characteristics; (2) mineral stability ranges; (3) the probability of occurrence for rare minerals; and (4) stellar and planetary stoichiometries in extrasolar systems. The most abundant elements generally have the largest numbers of mineral species, as modeled by relationships for Earth’s upper continental crust (E) and the Moon (M), respectively: 2 LogðNEÞ¼0:22 LogðCEÞþ1:70 ðR ¼ 0:34Þð4861 minerals; 72 elementsÞ 2 LogðNMÞ¼0:19 LogðCMÞþ0:23 ðR ¼ 0:68Þð63 minerals; 24 elementsÞ; where C is an element’s abundance in ppm and N is the number of mineral species in which that element is essential. Several elements that plot significantly below the trend for Earth’s upper continental crust (e.g., Ga, Hf, and Rb) mimic other more abundant elements and thus are less likely to form their own species.
  • New Mineral Names*,†

    New Mineral Names*,†

    American Mineralogist, Volume 98, pages 2201–2204, 2013 New Mineral Names*,† DMITRIY BELAKOVSKIY Fersman Mineralogical Museum, Russian Academy of Sciences, Moscow, Russia IN THIS ISSUE This New Mineral Names has entries for five new minerals, including christofschäferite-(Ce), kasatkinite, osumilite-(Mg), steklite, and vigrishinite. These new minerals have been published in Zapiski Rossiyskogo Mineralogicheskogo Obshchestva (Proceedings of the Russian Mineralogical Society) and in Novye dannye o mineralakh (New data on minerals). CHRISTOFSCHÄFERITE‑(CE)* chemical analyses (WDS, valency of Mn by XANES data, N.V. Chukanov, S.M. Aksenov, R.K. Rastsvetaeva, D.I. Bela- wt%) is: CaO 2.61 (2.24–2.98), La2O3 19.60 (19.20–19.83), kovskiy, J. Göttlicher, S.N. Britvin, and S. Möckel (2012) Ce2O3 22.95 (22.84–23.06), Pr2O3 0.56 (0.43–0.68), Nd2O3 2.28 2+ 3+ 3+ (2.01–2.50), MgO 0.08 (0–0.20), MnO 4.39 (4.27–4.51), total Christofschäferite-(Ce), (Ce,La,Ca)4Mn (Ti,Fe )3(Fe , 2+ Fe as FeO 6.98 (6.74–7.26) (apportioned in the proportions Fe ,Ti) (Si2O7)2O8, a new chevkinite-group mineral from 2+ 3+ the Eifel area, Germany. Novye dannye o mineralakh, 47, Fe :Fe = 3:2, by structural data: FeO 4.18, Fe2O3 3.11), Al2O3 33–42 (in English). 0.08 (0–0.19), TiO2 19.02 (18.64–19.39), Nb2O5 0.96 (0.83–1.11), SiO2 19.38 (19.16–19.52), total 99.20. The empirical formula 2+ 2+ A new mineral, christofschäferite-(Ce), was discovered at based on 22 O is (Ce1.72La1.48Nd0.17Pr0.04Ca0.57)Σ3.98Mn 0.76Fe 0.72 3+ the famous outcrop Wingertsbergwand (Wingertsberg Mt.) Mg0.02Ti2.935Fe 0.48Al0.02Nb0.09Si3.98O22.