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    Ultraviolet Observations of Coronal Mass Ejection Impact on Comet 67P/Churyumov–Gerasimenko by Alice

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    Noonan_2018_AJ_156_16.pdf
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    Author
    Noonan, John W.
    Stern, S. Alan
    Feldman, Paul D.
    Broiles, Thomas
    Wedlund, Cyril Simon
    Edberg, Niklas J. T.
    Schindhelm, Eric
    Parker, Joel Wm.
    Keeney, Brian A.
    Vervack Jr, Ronald J.
    Steffl, Andrew J.
    Knight, Matthew M.
    Weaver, Harold A.
    Feaga, Lori M.
    A’Hearn, Michael
    Bertaux, Jean-Loup
    Show allShow less
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2018-07
    Keywords
    comets: individual (67P/C-G)
    Sun: coronal mass ejections (CMEs)
    ultraviolet: planetary systems
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    John W. Noonan et al 2018 AJ 156 16
    Journal
    ASTRONOMICAL JOURNAL
    Rights
    © 2018. The American Astronomical Society.
    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
    The Alice ultraviolet spectrograph on the European Space Agency Rosetta spacecraft observed comet 67P/Churyumov-Gerasimenko in its orbit around the Sun for just over two years. Alice observations taken in 2015 October, two months after perihelion, show large increases in the comet's Ly beta, OI 1304, OI 1356, and CI 1657 angstrom atomic emission that initially appeared to indicate gaseous outbursts. However, the Rosetta Plasma Consortium instruments showed a coronal mass ejection (CME) impact at the comet coincident with the emission increases, suggesting that the CME impact may have been the cause of the increased emission. The presence of the semi-forbidden OI 1356 angstrom emission multiplet is indicative of a substantial increase in dissociative electron impact emission from the coma, suggesting a change in the electron population during the CME impact. The increase in dissociative electron impact could be a result of the interaction between the CME and the coma of 67P or an outburst coincident with the arrival of the CME. The observed dissociative electron impact emission during this period is used to characterize the O-2 content of the coma at two peaks during the CME arrival. The mechanism that could cause the relationship between the CME and UV emission brightness is not well constrained, but we present several hypotheses to explain the correlation.
    ISSN
    1538-3881
    DOI
    10.3847/1538-3881/aac432
    Version
    Final published version
    Sponsors
    NASA's Jet Propulsion Laboratory [1336850]; Research Council of Norway [240000]
    Additional Links
    http://stacks.iop.org/1538-3881/156/i=1/a=16?key=crossref.7ab6f5c0bcb948cd0272f9f37b15bd18
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-3881/aac432
    Scopus Count
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