Assessment of the Mesosiderite-Diogenite Connection and an Impact Model for the Genesis of Mesosiderites
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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. -
Warren and Taylor-2014-In Tog-The Moon-'Author's Personal Copy'.Pdf
This article was originally published in Treatise on Geochemistry, Second Edition published by Elsevier, and the attached copy is provided by Elsevier for the author's benefit and for the benefit of the author's institution, for non- commercial research and educational use including without limitation use in instruction at your institution, sending it to specific colleagues who you know, and providing a copy to your institution’s administrator. All other uses, reproduction and distribution, including without limitation commercial reprints, selling or licensing copies or access, or posting on open internet sites, your personal or institution’s website or repository, are prohibited. For exceptions, permission may be sought for such use through Elsevier's permissions site at: http://www.elsevier.com/locate/permissionusematerial Warren P.H., and Taylor G.J. (2014) The Moon. In: Holland H.D. and Turekian K.K. (eds.) Treatise on Geochemistry, Second Edition, vol. 2, pp. 213-250. Oxford: Elsevier. © 2014 Elsevier Ltd. All rights reserved. Author's personal copy 2.9 The Moon PH Warren, University of California, Los Angeles, CA, USA GJ Taylor, University of Hawai‘i, Honolulu, HI, USA ã 2014 Elsevier Ltd. All rights reserved. This article is a revision of the previous edition article by P. H. Warren, volume 1, pp. 559–599, © 2003, Elsevier Ltd. 2.9.1 Introduction: The Lunar Context 213 2.9.2 The Lunar Geochemical Database 214 2.9.2.1 Artificially Acquired Samples 214 2.9.2.2 Lunar Meteorites 214 2.9.2.3 Remote-Sensing Data 215 2.9.3 Mare Volcanism -
Validity of the Apatite/Merrillite Relationship in Evaluating the Water Content in the Martian Mantle: Implications from Shergottite Northwest Africa (NWA) 2975
Originally published as: Słaby, E., Förster, H.‐J., Wirth, R., Giera, A., Birski, Ł., Moszumańska, I. (2017): Validity of the Apatite/Merrillite Relationship in Evaluating the Water Content in the Martian Mantle: Implications from Shergottite Northwest Africa (NWA) 2975. ‐ Geosciences, 7, 4. DOI: http://doi.org/10.3390/geosciences7040099 geosciences Article Validity of the Apatite/Merrillite Relationship in Evaluating the Water Content in the Martian Mantle: Implications from Shergottite Northwest Africa (NWA) 2975 Ewa Słaby 1,*, Hans-Jürgen Förster 2, Richard Wirth 2, Alicja Wudarska 1,2, Łukasz Birski 1 and Izabela Moszuma ´nska 1 1 Institute of Geological Sciences, Polish Academy of Sciences, Research Centre in Warsaw, Twarda 51/55, 00-818 Warsaw, Poland; [email protected] (A.W.); [email protected] (Ł.B.); [email protected] (I.M.) 2 Helmholtz-Zentrum Potsdam Deutsches GeoForschungsZentrum GFZ, Telegrafenberg, 14473 Potsdam, Germany; [email protected] (H.-J.F.); [email protected] (R.W.) * Correspondence: [email protected] Received: 17 July 2017; Accepted: 26 September 2017; Published: 4 October 2017 Abstract: Phosphates from the Martian shergottite NWA 2975 were used to obtain insights into the source and subsequence differentiation of the melt/melts. The crystallization of two generations of fluorapatite (F > Cl~OH and F-rich), chlorapatite and ferromerrillite-merrillite were reconstructed from TEM (Transmission Electron Microscopy) and geochemical analyses. The research results indicated that the recognized volatiles budget of the two generations of fluorapatite was related to their magmatic origin. The apatite crystals crystallized from an evolved magma during its final differentiation and degassing stage. -
8. Projectile ˜˜˜
8. Projectile ˜˜˜ Meteoritic remnants of the impacting asteroid that produced Barringer Crater littered the landscape when exploration began ~115 years ago. As described in Chapter 1, meteoritic irons are what initially captured Foote’s interest and spurred Barringer’s interest in a possibly rich natural source of native metal. After Foote’s description was published, samples were collected by F. W. Volz at a nearby trading post and sold widely. Gilbert (1896) estimated that 10 tons of meteoritic debris had already been recovered by the time of his visit. Similarly, Barringer (1905) estimated that 10 to 15 tons of it were circulating around the world by the time his exploration work began. Fortunately, he tried to document the geographic and mass distribution of that debris in a detailed map, which is reproduced in Fig. 8.1. The map indicates that meteoritic irons were recovered from distances approaching 10 km. Gilbert (1896) apparently recovered a sample nearly 13 km beyond the crater rim. A lot of the meteoritic material was oxidized. It is sometimes simply called oxidized iron, but large masses are also called shale balls. A concentrated deposit of small oxidized iron fragments was found northeast of the crater, although those types of fragments are distributed in all directions around the crater. The current estimate of the recovered meteoritic iron mass is 30 tons (Nininger, 1949; Grady, 2000), although this is a highly uncertain number. Specimens were transported in pre-historical times and have been found scattered throughout Arizona (see, for example, Wasson, 1968). Specimens have also been illicitly removed in recent times, without any documentation of the locations or masses recovered. -
MARTIAN METEORITES: GEOCHEMISTRY and SUCH 6:00 P.M
Lunar and Planetary Science XLVIII (2017) sess333.pdf Tuesday, March 21, 2017 [T333] POSTER SESSION I: MARTIAN METEORITES: GEOCHEMISTRY AND SUCH 6:00 p.m. Town Center Exhibit Area Irving A. J. Kuehner S. M. Lapen T. J. Righter M. Busemann H. et al. POSTER LOCATION #466 Keeping Up with the Martian Meteorites and Constraining the Number of Separate Launch Sites on Mars [#2068] Petrologic, chemical, and cosmogenic nuclide criteria suggest that the 101 unpaired martian meteorites may come from as few as 20 launch sites on Mars. Habermann M. Agee C. Spilde M. POSTER LOCATION #467 Multi-Layered Clast in Martian Breccia Northwest Africa 10922 [#2743] We performed chemical analyses of an unusual, concentrically-layered clast within the martian breccia NWA 10922. Santos A. R. Lewis J. A. Agee C. B. Humayun M. McCubbin F. M. et al. POSTER LOCATION #468 Feldspar Variability in Northwest Africa 7034 [#2349] Northwest Africa 7034 contains feldspar of different grain size, texture, and composition, some of which suggest modification by secondary alteration. Cao T. He Qi. POSTER LOCATION #469 Petrology and Mineral Chemistry of the Eniched Basaltic Shergottite Northwest Africa 8656 [#1384] The characterization of primary petrography and mineralogy of Northwest Africa 8656, basalt shergottite, are described in this abstract. Jacobs G. M. Abernethey F. J. Anand M. Franchi I. A. Grady M. M. POSTER LOCATION #470 Understanding the Early Martian Environment Through the Inventory of Breccia Clasts in Northwest Africa 7034 [#2139] The clasts and matrices of Northwest Africa 7034 and its breccia clasts reveal the meteorite aggregates material from multiple sources with distinct histories. -
(M = Ca, Mg, Fe2+), a Structural Base of Ca3mg3(PO4)4 Phosphors
crystals Article Crystal Chemistry of Stanfieldite, Ca7M2Mg9(PO4)12 (M = Ca, Mg, Fe2+), a Structural Base of Ca3Mg3(PO4)4 Phosphors Sergey N. Britvin 1,2,* , Maria G. Krzhizhanovskaya 1, Vladimir N. Bocharov 3 and Edita V. Obolonskaya 4 1 Department of Crystallography, Institute of Earth Sciences, St. Petersburg State University, Universitetskaya Nab. 7/9, 199034 St. Petersburg, Russia; [email protected] 2 Nanomaterials Research Center, Kola Science Center of Russian Academy of Sciences, Fersman Str. 14, 184209 Apatity, Russia 3 Centre for Geo-Environmental Research and Modelling, Saint-Petersburg State University, Ulyanovskaya ul. 1, 198504 St. Petersburg, Russia; [email protected] 4 The Mining Museum, Saint Petersburg Mining University, 2, 21st Line, 199106 St. Petersburg, Russia; [email protected] * Correspondence: [email protected] Received: 1 May 2020; Accepted: 25 May 2020; Published: 1 June 2020 Abstract: Stanfieldite, natural Ca-Mg-phosphate, is a typical constituent of phosphate-phosphide assemblages in pallasite and mesosiderite meteorites. The synthetic analogue of stanfieldite is used as a crystal matrix of luminophores and frequently encountered in phosphate bioceramics. However, the crystal structure of natural stanfieldite has never been reported in detail, and the data available so far relate to its synthetic counterpart. We herein provide the results of a study of stanfieldite from the Brahin meteorite (main group pallasite). The empirical formula of the mineral is Ca8.04Mg9.25Fe0.72Mn0.07P11.97O48. Its crystal structure has been solved and refined to R1 = 0.034. Stanfieldite from Brahin is monoclinic, C2/c, a 22.7973(4), b 9.9833(2), c 17.0522(3) Å, β 99.954(2)◦, 3 V 3822.5(1)Å . -
Moon Minerals a Visual Guide
Moon Minerals a visual guide A.G. Tindle and M. Anand Preliminaries Section 1 Preface Virtual microscope work at the Open University began in 1993 meteorites, Martian meteorites and most recently over 500 virtual and has culminated in the on-line collection of over 1000 microscopes of Apollo samples. samples available via the virtual microscope website (here). Early days were spent using LEGO robots to automate a rotating microscope stage thanks to the efforts of our colleague Peter Whalley (now deceased). This automation speeded up image capture and allowed us to take the thousands of photographs needed to make sizeable (Earth-based) virtual microscope collections. Virtual microscope methods are ideal for bringing rare and often unique samples to a wide audience so we were not surprised when 10 years ago we were approached by the UK Science and Technology Facilities Council who asked us to prepare a virtual collection of the 12 Moon rocks they loaned out to schools and universities. This would turn out to be one of many collections built using extra-terrestrial material. The major part of our extra-terrestrial work is web-based and we The authors - Mahesh Anand (left) and Andy Tindle (middle) with colleague have build collections of Europlanet meteorites, UK and Irish Peter Whalley (right). Thank you Peter for your pioneering contribution to the Virtual Microscope project. We could not have produced this book without your earlier efforts. 2 Moon Minerals is our latest output. We see it as a companion volume to Moon Rocks. Members of staff -
Meteorite Dunite Breccia Mil 03443: a Probable Crustal Cumulate Closely Related to Diogenites from the Hed Parent Asteroid
METEORITE DUNITE BRECCIA MIL 03443: A PROBABLE CRUSTAL CUMULATE CLOSELY RELATED TO DIOGENITES FROM THE HED PARENT ASTEROID. David W Mittlefehldt, Astromateri- als Research Office, NASA/Johnson Space Center, Houston, Texas, USA, ([email protected]). Introduction: There are numerous types of differ- Metal is very rare, and occurs as grains a few microns entiated meteorites, but most represent either the crusts in size associated with troilite. or cores of their parent asteroids. Ureilites, olivine- pyroxene-graphite rocks, are exceptions; they are man- tle restites [1]. Dunite is expected to be a common mantle lithology in differentiated asteroids. In particu- lar, models of the eucrite parent asteroid contain large volumes of dunite mantle [2-4]. Yet dunites are very rare among meteorites, and none are known associated with the howardite, eucrite, diogenite (HED) suite. Spectroscopic measurements of 4 Vesta, the probable HED parent asteroid, show one region with an olivine signature [5] although the surface is dominated by ba- saltic and orthopyroxenitic material equated with eucrites and diogenites [6]. One might expect that a small number of dunitic or olivine-rich meteorites might be delivered along with the HED suite. The 46 gram meteoritic dunite MIL 03443 (Fig. 1) Figure 2. BSE image of MIL 03443 showing its gen- was recovered from the Miller Range ice field of Ant- eral fragmental breccia texture, and primary texture arctica. This meteorite was tentatively classified as a between olivine, orthopyroxene and chromite. mesosiderite because large, dunitic clasts are found in this type of meteorite, but it was noted that MIL 03443 could represent a dunite sample of the HED suite [7]. -
Volatile Abundances of Coexisting Merrillite and Apatite in the Martian 4 Meteorite Shergotty: Implications for Merrillite in Hydrous Magmas 5 6 Francis M
1 Revision 1 2 3 Volatile abundances of coexisting merrillite and apatite in the martian 4 meteorite Shergotty: Implications for merrillite in hydrous magmas 5 6 Francis M. McCubbin1, Charles K. Shearer1, Paul V. Burger1, Erik H. Hauri2, Jianhua Wang2, 7 Stephen M. Elardo1, and James J. Papike1 8 9 1Institute of Meteoritics, Department of Earth & Planetary Sciences, University of New Mexico, Albuquerque, NM 10 87131, USA 11 12 2Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Rd., N.W, 13 Washington, DC 20015, USA 14 15 16 Abstract 17 18 Whitlockite and merrillite are two Ca-phosphate minerals found in terrestrial and 19 planetary igneous rocks, sometimes coexisting with apatite. Whitlockite has essential structural 20 hydrogen, and merrillite is devoid of hydrogen. Whitlockite components have yet to be 21 discovered in samples of extraterrestrial merrillite, despite evidence for whitlockite-merrillite 22 solid solution in terrestrial systems. The observation of merrillite in meteoritic and lunar samples 23 has led many to conclude that the magmas from which the merrillite formed were “very dry”. 24 However, the Shergotty martian meteorite has been reported to contain both apatite and 25 merrillite, and recently the apatite has been shown to contain substantial OH abundances, up to 26 the equivalent of 8600 ppm H2O. In the present study, we determined the abundances of F, Cl, 27 H2O, and S in merrillite from Shergotty using secondary ion mass spectrometry (SIMS). We 28 determined that the merrillite in Shergotty was properly identified (i.e., no discernible 29 whitlockite component), and it coexists with OH-rich apatite. -
Howardite-Eucrite-Diogenite) Title PARENT BODY -PARTIAL MELT EXPERIMENTS on DIFFERENTIATION PROCESSES-( Dissertation 全文 )
EVOLUTION OF THE HED (Howardite-Eucrite-Diogenite) Title PARENT BODY -PARTIAL MELT EXPERIMENTS ON DIFFERENTIATION PROCESSES-( Dissertation_全文 ) Author(s) Isobe, Hiroshi Citation Kyoto University (京都大学) Issue Date 1991-03-23 URL http://dx.doi.org/10.11501/3053044 Right Type Thesis or Dissertation Textversion author Kyoto University 学位 申請論文 磯部博志 EVOLUTION OF THE HED (howardite-eucrite-diogenite) PARENT BODY -PARTIAL MELT EXPERIMENTS ON DIFFERENTIATION PROCESSES- Hiroshi ISOBE Department of Environmental Safety Research Japan Atomic Energy Research Institute Tokai, Ibaraki, 319-11, JAPAN CONTENTS Abstract 1 Introduction1 2 Experiments —starting materials and procedures13 2-1 Composition of the starting materials13 2-2 Experimental procedures19 3 Results and interpretation25 3-1 Mineral assemblages of the run products25 3-2 Composition of the melts and minerals34 4 Discussion60 4-1 Melting relations on the 'pseudo-liquidus' diagrams 60 4-2 Fractionation sequence71 4-3 Physical conditions of the solid-liquid separations 78 4-4 Summary of the present evolution model of HEDP-PB96 Acknowledgments98 References99 Appendix 1 Chemistry of HED and pallasite meteorites106 Appendix 2 Tables of compositions of run products116 Abstract Three series of melting experiments with a chondritic material, a eucrite-diogenite mixture, and a eucritic material were carried out using a one atmosphere gas mixing furnace to illustrate liquidus phase relation and chemical compositions of the phases. Locations of an olivine control line, olivine-pyroxene phase boundary -
Carbonaceous Chondrite-Rich Howardites; the Potential for Hydrous Lithologies on the Hed Parent
CARBONACEOUS CHONDRITE-RICH HOWARDITES; THE POTENTIAL FOR HYDROUS LITHOLOGIES ON THE HED PARENT. J. S. Herrin 1,2 , M. E. Zolensky 2, J. A. Cartwright 3, D. W. Mittle- fehldt 2, and D. K. Ross 1,2 . 1ESCG Astromaterials Research Group, Houston, Texas, USA ( [email protected] ), 2NASA Johnson Space Center, Houston, Texas, USA, 3Max Planck Institut für Chemie, Mainz, Germany. Introduction: Howardites, eucrites, and dioge- clasts texturally resembling CM2 up to 7mm occupy- nites, collectively referred to as the “HED’s”, are a ing nearly half of the sample area accompanied 1-5 clan of meteorites thought to represent three different mm subangular impact melt clasts containing relict lithologies from a common parent body. Collectively eucritic fragments. The remaining medium and fine they are the most abundant type of achondrites in terre- fraction of the specimen consists of mm-to-sub-mm strial collections [1]. Eucrites are crustal basalts and angular-to-subrounded eucritic, diogenitic, carbona- gabbros, diogenites are mostly orthopyroxenites and ceous chondrite clasts set in a medium-to-coarse angu- are taken to represent lower crust or upper mantle ma- lar matrix of same materials. The eucrite/diogenite terials, and howardites are mixed breccias containing ratio of identifiable clasts is approximately 50/50. The both lithologies and are generally regarded as derived total modal abundance of visible carbonaceous chon- from the regolith or near-surface. drite fragments is ~60%. The presence of exogenous chondritic material in PRA 04402 is a howardite breccia consisting of howardite breccias has long been recognized [2,3]. As mm-to-sub-mm subrounded-to-subangular diogenite a group, howardites exhibit divergence in bulk chemi- and eucritic clasts in roughly equal proportions set in a stry from what would be produced by mixing of dioge- medium-to-coarse matrix. -
Aqueous Alteration in Martian Meteorites: Comparing Mineral Relations in Igneous-Rock Weathering of Martian Meteorites and in the Sedimentary Cycle of Mars
AQUEOUS ALTERATION IN MARTIAN METEORITES: COMPARING MINERAL RELATIONS IN IGNEOUS-ROCK WEATHERING OF MARTIAN METEORITES AND IN THE SEDIMENTARY CYCLE OF MARS MICHAEL A. VELBEL Department of Geological Sciences, 206 Natural Science Building, Michigan State University, East Lansing, Michigan 48824-1115 USA e-mail: [email protected] ABSTRACT: Many of the minerals observed or inferred to occur in the sediments and sedimentary rocks of Mars, from a variety of Mars-mission spacecraft data, also occur in Martian meteorites. Even Martian meteorites recovered after some exposure to terrestrial weathering can preserve preterrestrial evaporite minerals and useful information about aqueous alteration on Mars, but the textures and textural contexts of such minerals must be examined carefully to distinguish preterrestrial evaporite minerals from occurrences of similar minerals redistributed or formed by terrestrial processes. Textural analysis using terrestrial microscopy provides strong and compelling evidence for preterrestrial aqueous alteration products in a numberof Martian meteorites. Occurrences of corroded primary rock-forming minerals and alteration products in meteorites from Mars cover a range of ages of mineral–water interaction, from ca. 3.9 Ga (approximately mid-Noachian), through one or more episodes after ca. 1.3 Ga (approximately mid–late Amazonian), through the last half billion years (late Amazonian alteration in young shergottites), to quite recent. These occurrences record broadly similar aqueous corrosion processes and formation of soluble weathering products over a broad range of times in the paleoenvironmental history of the surface of Mars. Many of the same minerals (smectite-group clay minerals, Ca-sulfates, Mg-sulfates, and the K-Fe–sulfate jarosite) have been identified both in the Martian meteorites and from remote sensing of the Martian surface.