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    The abundances of F, Cl, and H2O in eucrites: Implications for the origin of volatile depletion in the asteroid 4 Vesta

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    Name:
    McCubbin et al 2021 GCA.pdf
    Embargo:
    2023-08-27
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    Description:
    Final Accepted Manuscript
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    Author
    McCubbin, Francis M.
    Lewis, Jonathan A.
    Barnes, Jessica J.
    Elardo, Stephen M.
    Boyce, Jeremy W.
    Affiliation
    Lunar and Planetary Laboratory, University of Arizona
    Issue Date
    2021-12
    Keywords
    Achondrites
    Apatite
    Chlorine isotopes
    Magma ocean
    Meteorites
    Water
    
    Metadata
    Show full item record
    Publisher
    Elsevier BV
    Citation
    McCubbin, F. M., Lewis, J. A., Barnes, J. J., Elardo, S. M., & Boyce, J. W. (2021). The abundances of F, Cl, and H2O in eucrites: Implications for the origin of volatile depletion in the asteroid 4 Vesta. Geochimica et Cosmochimica Acta.
    Journal
    Geochimica et Cosmochimica Acta
    Rights
    Copyright © Elsevier Ltd.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    We conducted a petrologic study of apatite within eight unbrecciated, non-cumulate eucrites and two monomict, non-cumulate eucrites. These data were combined with previously published data to quantify the abundances of F, Cl, and H2O in the bulk silicate portion of asteroid 4 Vesta (BSV). Using a combination of apatite-based melt hygrometry/chlorometry and appropriately paired volatile/refractory element ratios, we determined that BSV has 3.0–7.2 ppm F, 0.39–1.8 ppm Cl, and 3.6–22 ppm H2O. The abundances of F and H2O are depleted in BSV relative to CI chondrites to a similar degree as F and H2O in the bulk silicate portion of the Moon. This degree of volatile depletion in BSV is similar to what has been determined previously for many moderately volatile elements in 4 Vesta (e.g., Na, K, Zn, Rb, Cs, and Pb). In contrast, Cl is depleted in 4 Vesta by a greater degree than what is recorded in samples from Earth or the Moon. Based on the Cl-isotopic compositions of eucrites and the bulk rock Cl/F ratios determined in this study, the eucrites likely formed through serial magmatism of a mantle with heterogeneous δ37Cl and Cl/F, not as extracts from a partially crystallized global magma ocean. Furthermore, the volatile depletion and Cl-isotopic heterogeneity recorded in eucrites is likely inherited, at least in part, from the precursor materials that accreted to form 4 Vesta and is unlikely to have resulted solely from degassing of a global magma ocean, magmatic degassing of eucrite melts, and/or volatile loss during thermal metamorphism. Although our results can be reconciled with the past presence of wide-scale melting on 4 Vesta (i.e., a partial magma ocean), any future models for eucrite petrogenesis involving a global magma ocean would need to account for the preservation of a heterogeneous eucrite source with respect to Cl/F ratios and Cl isotopes.
    Note
    24 month embargo; available online 27 August 2021
    ISSN
    0016-7037
    DOI
    10.1016/j.gca.2021.08.021
    Version
    Final accepted manuscript
    Sponsors
    NASA
    ae974a485f413a2113503eed53cd6c53
    10.1016/j.gca.2021.08.021
    Scopus Count
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    UA Faculty Publications

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