Diffusion Kinetics of Cr in Olivine and Mn
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(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 . -
EPSC2010-345, 2010 European Planetary Science Congress 2010 C Author(S) 2010
EPSC Abstracts Vol. 5, EPSC2010-345, 2010 European Planetary Science Congress 2010 c Author(s) 2010 Study of non-equivalent Fe positions in some extraterrestrial minerals using Mössbauer spectroscopy with a high velocity resolution M.I. Oshtrakh (1), V.I. Grokhovsky (1), M.Yu. Larionov (1), D.G. Patrusheva (1), E.V. Petrova (1), V.A. Semionkin (1,2) (1) Faculty of Physical Techniques and Devices for Quality Control and (2) Faculty of Experimental Physics, Ural State Technical University – UPI, Ekaterinburg, 620002, Russian Federation. E-mail: [email protected]. Abstract phosphides extracted from iron meteorite. Study of extraterrestrial minerals with non-equivalent 2. Materials and Methods Fe positions such as the M1 and M2 sites in olivine and pyroxenes in ordinary chondrites, the M1 and Samples of Saratov L4, Mount Tazerzait L5, Tsarev L5, M2 sites in olivines from pallasites and the M1, M2 Farmington L5, Mbale L5/6, Kunashak L6, Zubkovsky and M3 sites in iron nickel phosphides from iron L6, Ochansk H4, Richardton H5, Vengerovo H5, meteorites was performed using Mössbauer Zvonkov H6 were prepared as powders for Mössbauer measurements with effective thickness of about 10 mg spectroscopy with a high velocity resolution. 2 Obtained differences were analyzed in order to Fe/cm . Samples of olivine extracted from Omolon PMG and Seymchan PMG were prepared as powders characterize these minerals. with effective thickness of about 6 mg Fe/cm2. Samples of schreibersite and rhabdites extracted from Sikhote- 1. Introduction Alin IIAB iron meteorite mechanically and electrochemically, respectively, were prepared with A number of extraterrestrial iron bearing minerals effective thickness of about 5–6 mg Fe/cm2. -
General Assembly Distr.: General 7 January 2005
United Nations A/AC.105/839 General Assembly Distr.: General 7 January 2005 Original: English Committee on the Peaceful Uses of Outer Space Scientific and Technical Subcommittee Forty-second session Vienna, 21 February-4 March 2004 Item 10 of the provisional agenda∗ Near-Earth objects Information on research in the field of near-Earth objects carried out by international organizations and other entities Note by the Secretariat Contents Page I. Introduction ................................................................... 2 II. Replies received from international organizations and other entities ..................... 2 European Space Agency ......................................................... 2 The Spaceguard Foundation ...................................................... 17 __________________ ∗ A/AC.105/C.1/L.277. V.05-80067 (E) 010205 020205 *0580067* A/AC.105/839 I. Introduction In accordance with the agreement reached at the forty-first session of the Scientific and Technical Subcommittee (A/AC.105/823, annex II, para. 18) and endorsed by the Committee on the Peaceful Uses of Outer Space at its forty-seventh session (A/59/20, para. 140), the Secretariat invited international organizations, regional bodies and other entities active in the field of near-Earth object (NEO) research to submit reports on their activities relating to near-Earth object research for consideration by the Subcommittee. The present document contains reports received by 17 December 2004. II. Replies received from international organizations and other entities European Space Agency Overview of activities of the European Space Agency in the field of near-Earth object research: hazard mitigation Summary 1. Near-Earth objects (NEOs) pose a global threat. There exists overwhelming evidence showing that impacts of large objects with dimensions in the order of kilometres (km) have had catastrophic consequences in the past. -
List of Meteorites in the Collections of the Central Siberian Geological Museum at the V.S.Sobolev Institute of Geology and Mineralogy SB RAS (SIGM)
List of meteorites in the collections of the Central Siberian Geological Museum at the V.S.Sobolev Institute of Geology and Mineralogy SB RAS (SIGM). Year Mass in Pieces in Main mass in Indication Meteorite Country Type found SIGM SIGM SIGM in MB Novosibirsk Russia 1978 H5/6 9.628 kg 2 yes 59 Markovka Russia 1967 H4 7.9584 kg 5 yes 48 Ochansk Russia 1887 H4 407 g 1 Kunashak Russia 1949 L6 268 g 1 6 Saratov Russia 1918 L4 183.4 g 1 Elenovka Ukraine 1951 L5 148.7 g 2 6 Zhovtnevyi Ukraine 1938 H6 88.5 g 1 Nikolskoe Russia 1954 L4 39.5 g 1 6 Krymka Ukraine 1946 LL3.2 11.1 g 1 Yurtuk Ukraine 1936 Howardite 5.3 g 1 Pervomaisky Russia 1933 L6 595 g 1 Ivanovka Russia 1983 H5 904 g 1 63 Tsarev Russia 1968 H5 1.91972 kg 3 59 Norton County USA 1948 Aubrite 144 g 1 Stannern Cz. Republic 1808 18.1 g 1 Eucrite-mmict Poland 1868 H5 63.02 g 1 Pultusk Chelyabinsk Russia 2013 LL5 1.55083 kg 28 102 Yaratkulova Russia 2016 H5 25.71 g 1 105 Tobychan Russia 1971 Iron, IIE 41.4998 kg 2 yes 51 Elga Russia 1959 Iron, IIE 10.5 kg 1 16 Sikhote-Alin Russia 1947 Iron, IIAB 37.1626 kg 12 Chebankol Russia 1938 Iron, IAB-sHL 87.1 g 1 Chinga (Chinge) Russia 1912 Iron, ungrouped 5.902 kg 3 13 Kaalijarv (Kaali) Estonia 1937 2.88 g a lot of Iron, IAB-MG Boguslavka Russia 1916 Iron, IIAB 55.57 g 1 Bilibino Russia 1981 Iron, IIAB 570.94 g 1 60 Anyujskij Russia 1981 Iron, IIAB 435.4 g 1 60 Sychevka Russia 1988 Iron, IIIAB 1.581 kg 1 70 Darjinskoe Kazakhstan 1984 Iron, IIC 6 kg 1 yes 78 Maslyanino Russia 1992 Iron, IAB complex 58 kg 2 yes 78 Onello Russia 1998 Iron, ungrouped -
Michael W. Busch Updated June 27, 2019 Contact Information
Curriculum Vitae: Michael W. Busch Updated June 27, 2019 Contact Information Email: [email protected] Telephone: 1-612-269-9998 Mailing Address: SETI Institute 189 Bernardo Ave, Suite 200 Mountain View, CA 94043 USA Academic & Employment History BS Physics & Astrophysics, University of Minnesota, awarded May 2005. PhD Planetary Science, Caltech, defended April 5, 2010. JPL Planetary Science Summer School, July 2006. Hertz Foundation Graduate Fellow, September 2007 to June 2010. Postdoctoral Researcher, University of California Los Angeles, August 2010 – August 2011. Jansky Fellow, National Radio Astronomy Observatory, August 2011 – August 2014. Visiting Scholar, University of Colorado Boulder, July – August 2012. Research Scientist, SETI Institute, August 2013 – present. Current Funding Sources: NASA Near Earth Object Observations. Research Interests: • Shapes, spin states, trajectories, internal structures, and histories of asteroids. • Identifying and characterizing targets for both robotic and human spacecraft missions. • Ruling out potential future asteroid-Earth impacts. • Radio and radar astronomy techniques. Selected Recent Papers: Marshall, S.E., and 24 colleagues, including Busch, M.W., 2019. Shape modeling of potentially hazardous asteroid (85989) 1999 JD6 from radar and lightcurve data, Icarus submitted. Reddy, V., and 69 colleagues, including Busch, M.W., 2019. Near-Earth asteroid 2012 TC4 campaign: results from global planetary defense exercise, Icarus 326, 133-150. Brozović, M., and 16 colleagues, including Busch, M.W., 2018. Goldstone and Arecibo radar observations of (99942) Apophis in 2012-2013, Icarus 300, 115-128. Brozović, M., and 19 colleagues, including Busch, M.W., 2017. Goldstone radar evidence for short-axis mode non-principal axis rotation of near-Earth asteroid (214869) 2007 PA8. Icarus 286, 314-329. -
MHMP 2014 UPDATE PART 3 I D Natural Geological Hazards
I. Natural Hazards D. Geological Hazards The following outline summarizes the significant geological hazards covered in this section: 1. Ground Movement a. Earthquakes b. Subsidence 2. Celestial Impacts Although some states recognize “landslides” as an additional hazard, Michigan’s geology and history tends to make it more prone to land subsidence instead. Michigan’s two main vulnerabilities to ground movement are therefore identified in the sections on earthquakes and subsidence hazards. Erosion is not in itself typically considered an emergency event, except in cases involving encroachment into shoreline developments near a river or lake, and these have been dealt with in the Hydrological Hazards section of this plan. A new section of this plan, celestial impacts, deals not only with the impact of physical objects on property, but also with the effects of solar storms on our modern infrastructure. It will be seen that the systemic technological impacts of this hazard involve greater expected risks than the more well-known impacts of a meteoritic type. Although meteorite impacts are quite easy to understand and visualize, and do have a small potential to be catastrophic, it is the seemingly abstract and mostly invisible effect of “space weather” that has the greatest probability of causing widespread disruption and harm in the near future. Overlap Between Geological Hazards and Other Sections of the Hazard Analysis The most serious Michigan earthquakes would be expected to damage some of the utilities infrastructure in the southern part of the state, and could contribute to the occurrence of an energy emergency. Some flooding could result from broken water mains. -
Download Version of Record (PDF / 6MB)
Open Research Online The Open University’s repository of research publications and other research outputs An Isotopic Investigation Of Early Planetesimal Differentiation Processes Thesis How to cite: Windmill, Richard Joseph (2021). An Isotopic Investigation Of Early Planetesimal Differentiation Processes. PhD thesis The Open University. For guidance on citations see FAQs. c 2020 Richard Joseph Windmill https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.21954/ou.ro.00012472 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk AN ISOTOPIC INVESTIGATION OF EARLY PLANETESIMAL DIFFERENTIATION PROCESSES Richard J. Windmill Supervisors: Dr. I. A. Franchi Professor M. Anand Dr. R. C. Greenwood Submitted to the School of Physical Sciences at The Open University in accordance with the requirements for the degree of Doctor of Philosophy June 2020 School of Physical Sciences Robert Hooke Building The Open University Walton Hall Milton Keynes MK7 6AA United Kingdom Abstract The differentiation and early evolution of planetesimals is relatively poorly understood. The Main- Group pallasites (PMGs) and IIIAB irons are differentiated meteorite groups from deep planetesimal interiors. They provide a window into the early evolution of rocky planets because of the abundance of samples from these groups and because a common planetary provenance has been proposed. Oxygen isotope analyses are crucial in understanding these relationships. -
Fersman Mineralogical Museum of the Russian Academy of Sciences (FMM)
Table 1. The list of meteorites in the collections of the Fersman Mineralogical Museum of the Russian Academy of Sciences (FMM). Leninskiy prospect 18 korpus 2, Moscow, Russia, 119071. Pieces Year Mass in Indication Meteorite Country Type in found FMM in MB FMM Seymchan Russia 1967 Pallasite, PMG 500 kg 9 43 Kunya-Urgench Turkmenistan 1998 H5 402 g 2 83 Sikhote-Alin Russia 1947 Iron, IIAB 1370 g 2 Sayh Al Uhaymir 067 Oman 2000 L5-6 S1-2,W2 63 g 1 85 Ozernoe Russia 1983 L6 75 g 1 66 Gujba Nigeria 1984 Cba 2..8 g 1 85 Dar al Gani 400 Libya 1998 Lunar (anorth) 0.37 g 1 82 Dhofar 935 Oman 2002 H5S3W3 96 g 1 88 Dhofar 007 Oman 1999 Eucrite-cm 31.5 g 1 84 Muonionalusta Sweden 1906 Iron, IVA 561 g 3 Omolon Russia 1967 Pallasite, PMG 1,2 g 1 72 Peekskill USA 1992 H6 1,1 g 1 75 Gibeon Namibia 1836 Iron, IVA 120 g 2 36 Potter USA 1941 L6 103.8g 1 Jiddat Al Harrasis 020 Oman 2000 L6 598 gr 2 85 Canyon Diablo USA 1891 Iron, IAB-MG 329 gr 1 33 Gold Basin USA 1995 LA 101 g 1 82 Campo del Cielo Argentina 1576 Iron, IAB-MG 2550 g 4 36 Dronino Russia 2000 Iron, ungrouped 22 g 1 88 Morasko Poland 1914 Iron, IAB-MG 164 g 1 Jiddat al Harasis 055 Oman 2004 L4-5 132 g 1 88 Tamdakht Morocco 2008 H5 18 gr 1 Holbrook USA 1912 L/LL5 2,9g 1 El Hammami Mauritani 1997 H5 19,8g 1 82 Gao-Guenie Burkina Faso 1960 H5 18.7 g 1 83 Sulagiri India 2008 LL6 2.9g 1 96 Gebel Kamil Egypt 2009 Iron ungrouped 95 g 2 98 Uruacu Brazil 1992 Iron, IAB-MG 330g 1 86 NWA 859 (Taza) NWA 2001 Iron ungrouped 18,9g 1 86 Dhofar 224 Oman 2001 H4 33g 1 86 Kharabali Russia 2001 H5 85g 2 102 Chelyabinsk -
A R T O F R E S I L I E N
Art of Resilience NEO _Aster_2090-2092___2019-04-10-00-53-37-75 TITLE NEO_2034_2019-04-10-00-55-51-305 (NEO: Near Earth Object) APPROACH Visualizations of Big Data - data art as an emerging form of science communication: Superforecasting: The Art and Science of Prediction; visualizing the risk posed by potential Earth impacts. WHAT Photographic 3D render from an artscience datavisualization dealing with the prediction of potential asteroid impacts on Earth. TECHNIQUE Custom predictive software and code made in openFrameworks in C++ (see addendum) to generate an accurate datavisualization and predictions of bolide events based on data from NASA and KAGGLE. The computation of Earth impact probabilities for near- Earth objects is a complex process requiring sophisticated mathematical techniques. PROCESS The datavisualizations resulted in svg. and obj. files which allows 3D model export, 3D printing and lasercutting techniques. For the Art of Resilience a photographic 3D render was selected by the artist for this exhibition. ART OF RESILIENCE On the 18th of december 2018 an asteroid some ten metres across detonated with an explosive energy ten times greater than the bomb dropped on Hiroshima. The shock wave shattered windows of almost 7200 buildings. Nearly 1500 people were injured. Although astronomers have managed to locate 93% of the extremely dangerous asteroids, nobody saw it coming. Can art contribute to save the Earth from future threats the means of super forecasting and increase our resilience in regards to potential future asteroid impacts? ARTISTIC STATEMENT Artists often channel the future; seeing patterns before they form and putting them in their work, so that later, in hindsight, the work explodes like a time bomb. -
Mineralogy of Olivine-Hosted Inclusions from the Omolon Pallasite
Lunar and Planetary Science XXXVII (2006) 1235.pdf MINERALOGY OF OLIVINE-HOSTED INCLUSIONS FROM THE OMOLON PALLASITE. V. V. Shary- gin1, S. V. Kovyazin1 and N. M. Podgornykh2, 1Institute of Mineralogy and Petrography, Koptyuga prospect 3, 630090 Novosibirsk, Russia ([email protected]), 2Siberian Geological Museum of UIGGM SD RAS, Kop- tyuga prospect 3, 630090 Novosibirsk, Russia. Introduction: The Omolon meteorite (250 kg) was Metal-sulfide and fluid inclusions are most common. found in 1982 (it fell in 1981) near the Omolon river Typical phase composition of large metal-sulfide blebs (Magadan district, Russia). This meteorite belongs to is troilite + kamacite. Nickelphosphide, taenite, the main group of the pallasite family. It contains stanfieldite, and chromite are minor. Whitlockite, rounded olivine grains (about 60 vol. %, sizes – up to eskolaite and unidentified Si-O-rich phase occur very 3 cm, Fa content – 12.3 mole %) in nickeloan iron rarely. Fluid inclusions contain low-density fluid and matrix consisting of kamacite, taenite and plessite [1- sometimes metal-sulfide isolations (Fig. 1 C). Color- 2]. In addition, troilite, chromite, schreibersite, nikel- less transparent phase (phosphate?) rarely occurs in phosphide (former rhabdite) and stanfieldite were large fluid inclusions (>100 µm). Some mineral asso- found in the meteorite [1-3]. The irradiation time of ciations from the arrays resemble the silicate melt in- this meteorite was determined to at 78±7 Ma (by noble clusions; however, microprobe analysis has demon- gases); the K-Ar age for olivine crystallization was strated, that they are assemblages of stanfieldite, assessed as 4.6 Ga, i.e., close to the starting time for metal-sulfide bleb, and gas bubble (Fig. -
Problems of Planetology, Cosmochemistry and Meteoritica
Problems of Planetology, Cosmochemistry and Meteoritica Problems of Planetology, Cosmochemistry and Meteoritica Alexeev V.A., Pavlova T.A., Kalinina G.K. sample. The submitted work presents the analysis Some features of the radiation history of results of the distribution of the cosmic-ray exposure ureilites ages and masses of ureilites in comparison with those for ordinary chondrites, as well as the analysis results Vernadsky Institute of Geochemistry and Analytical of Wilkening and Marti (1976) of the track studies of Chemistry RAS, Moscow ([email protected]) the Kanne ureilite. Abstract. The analysis of the distributions of the cosmic- ray exposure ages and masses of ureilites in comparison with those for ordinary chondrites, as well as the analysis of the track study results of the Kenna ureilite are presented. The characteristic features found in the distributions are most likely associated with the presence of a larger proportion of ureilites with the small cosmic-ray exposure ages among the ureilites with small sizes. This fact may be due to the faster delivery of small-sized meteoroids on the orbits crossing the Earth’s orbit, which in turn is associated with the more efficient transfer of the small bodies from the region of the asteroid belt in the resonances regions mainly in result of the action of "daily" component of the Yarkovsky effect. Keywords: ureilites, cosmic-ray exposure ages, particle tracks Introduction. Among the meteorites, the total number of which exceeded 70,000, the ureilites account are less than 0.8% - only 553 meteorites (https://www.lpi.usra.edu/meteor/metbull.php). The most of these meteorites (~55%) were found in the deserts of northwestern Africa. -
Near-Earth Object Resource
NEO Resource Near-Earth Object Resource Compiled and edited by James M. Thomas for the Museum Astronomical Resource Society http://marsastro.org and the NASA/JPL Solar System Ambassador Program http://www.jpl.nasa.gov/ambassador Updated July 15, 2006 Based upon material available through the NASA Near-Earth Object Program http://neo.jpl.nasa.gov/ 1 of 104 NEO Resource Table of Contents Section Page Introduction & Overview 5 Target Earth 6 • The Cretaceous/Tertiary (K-T) Extinction 9 • Chicxulub Crater 10 • Barringer Meteorite Crater 13 What Are Near-Earth Objects (NEOs)? 14 What Is The Purpose Of The Near-Earth Object Program? 14 How Many Near-Earth Objects Have Been Discovered So Far? 15 What Is A PHA? 16 What Are Asteroids And Comets? 17 What Are The Differences Between An Asteroid, Comet, Meteoroid, Meteor and 19 Meteorite? Why Study Asteroids? 21 Why Study Comets? 24 What Are Atens, Apollos and Amors? 27 NEO Groups 28 Near-Earth Objects And Life On Earth 29 Near-Earth Objects As Future Resources 31 Near-Earth Object Discovery Teams 32 2 of 104 NEO Resource • Lincoln Near-Earth Asteroid Research (LINEAR) 35 • Near-Earth Asteroid Tracking (NEAT) 37 • Spacewatch 39 • Lowell Observatory Near-Earth Object Search (LONEOS) 41 • Catalina Sky Surveys 42 • Japanese Spaceguard Association (JSGA) 44 • Asiago DLR Asteroid Survey (ADAS) 45 Spacecraft Missions to Comets and Asteroids 46 • Overview 46 • Mission Summaries 49 • Near-Earth Asteroid Rendezvous (NEAR) 49 • DEEP IMPACT 49 • DEEP SPACE 1 50 • STARDUST 50 • Hayabusa (MUSES-C) 51 • ROSETTA