Heating experiments relevant to the depletion of Na,K and Mn in the Earth and other planetary bodies |
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| Institution: | 1. Institut für Geowissenschaften, Universität Kiel, Germany;2. Forschungsinstitut und Naturmuseum Senckenberg, Frankfurt/Main, Germany;1. School of Ocean, Earth Science and Technology, Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, USA;2. Geoscience Institute/Mineralogy, Goethe University Frankfurt, Germany;3. Centre for Star and Planet Formation, University of Copenhagen, Denmark;4. Institute of Meteoritics, University of New Mexico, USA;5. Division of Geological and Planetary Sciences, California Institute of Technology, USA;6. Department of Geology, School of Earth and Environment, Rowan University, USA;7. Department of the Geophysical Sciences, The University of Chicago, USA;8. Enrico Fermi Institute, The University of Chicago, USA;9. Chicago Center for Cosmochemistry, USA;1. Dept 5.1, Federal Institute for Materials, Research and Testing (BAM), Unter den Eichen 87, 12205 Berlin, Germany;2. Institut für Geowissenschaften (IGW), Friedrich-Schiller-Universität Jena (FSU), Germany;1. Planetary Geosciences Institute, Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA;2. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA;1. Natural History Sciences, Hokkaido University, Sapporo 060-0810, Japan;2. Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo 001-0021, Japan;3. UTokyo Organization for Planetary and Space Science (UTOPS), University of Tokyo, Tokyo 113-0033, Japan;4. ISAS/JAXA, Sagamihara, Kanagawa 252-210, Japan;1. UCL/Birkbeck Centre for Planetary Sciences, University College London, Gower St, London, WC1E 6BT, UK;2. Dept. of Earth Sciences, Natural History Museum, Cromwell Rd, London, SW7 5BD, UK;3. Dept. of Earth and Planetary Sciences, Birkbeck University of London, Malet St., London, WC1E 7HX, UK;4. Lunar and Planetary Institute/USRA, 3600 Bay Area Blvd, Houston, TX 77058, USA;5. Earth Observatory of Singapore & Facility for Analysis, Characterisation, Testing, and Simulation, Nanyang Technological University, 639798, Singapore;6. Astromaterials Research Office, NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX 77058, USA;7. Department of Earth, Ocean and Atmospheric, Science & National High Magnetic Field Laboratory, Florida State University, 1800 E. Paul Dirac Drive, Tallahassee, FL 32310, USA |
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| Abstract: | We have studied the evaporation of Na, K and Mn from Al-Na-K- and Mn-rich silicates at various conditions. Total alkali oxide contents ranged from 5 to 20%. The evaporation rate of Na increases with temperature and decreasing oxygen fugacity and decreases with duration of heating. The loss of K is in all cases less pronounced than for Na. Heating in an evacuated vacuum furnace is more effective in removing Na and K from melt droplets than in furnaces with one atm gas flow of air or gas mixtures controlling the oxygen fugacity. The strong pumping required to keep the vacuum removes Na and K atoms very effectively. In all experiments, the rate of evaporation is determined by quasi-equilibrium between a thin layer of Na and K rich gas above the molten silicates. The results of the experiments are in agreement with several other studies.In experiments with more than one sample in the furnace, equilibration of Na- and K-rich samples with Na- and K-poor samples occurred rapidly, mediated by the ambient gas phase.The results of experiments with Mn in starting compositions showed much stronger losses of Na than Mn under a variety of conditions.Thus the nearly chondritic Mn/Na ratios in the Earth cannot be the result of evaporation of Na and Mn in Earth-making materials, as the Mn/Na ratios in evaporation residues would be much higher than chondritic ratios. Such evaporation processes may have occurred in the parent material of Moon, Vesta and Mars.The data suggest, in agreement with earlier hypotheses, that the high and variable contents of Na and K in chondrules require a gas phase high in Na and K equilibrating with chondrule melts. The volume of nebular gas parental to a certain type of chondrites was heated and Na and K were lost from the chondrule precursors to the gas phase. Subsequently the nebular parcel was compressed leading to higher partial pressures of Na and K. Flash heating then produced chondrule melts which incorporated some of the gaseous Na and K and then cooled rapidly. The large range of Na and K contents in chondrule melts reflects very local enrichments of Na and K in the gas phase. Despite these variations bulk chondritic meteorites have well defined bulk Na and K contents, implying a closed system during formation of chondrules and matrix. |
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| Keywords: | Alkali evaporation Heating experiments Depletion of volatile elements Chondrule formation |
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