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    Magnetic Field Kinks and Folds in the Solar Wind

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    Tenerani_2020_ApJS_246_32.pdf
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    Final Published Version
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    Author
    Tenerani, Anna
    Velli, Marco
    Matteini, Lorenzo
    Réville, Victor
    Shi, Chen
    Bale, Stuart D.
    Kasper, Justin C.
    Bonnell, John W.
    Case, Anthony W.
    Dudok de Wit, Thierry
    Goetz, Keith
    Harvey, Peter R.
    Klein, Kristopher G.
    Korreck, Kelly
    Larson, Davin
    Livi, Roberto
    MacDowall, Robert J.
    Malaspina, David M.
    Pulupa, Marc
    Stevens, Michael
    Whittlesey, Phyllis
    Show allShow less
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Univ Arizona, Dept Planetary Sci
    Issue Date
    2020-02-03
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Tenerani, A., Velli, M., Matteini, L., Réville, V., Shi, C., Bale, S. D., ... & Whittlesey, P. (2020). Magnetic field kinks and folds in the solar wind. The Astrophysical Journal Supplement Series, 246(2), 32.
    Journal
    ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
    Rights
    © 2020. The American Astronomical Society. All rights reserved.
    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
    Parker Solar Probe (PSP) observations during its first encounter at 35.7 R-circle dot have shown the presence of magnetic field lines that are strongly perturbed to the point that they produce local inversions of the radial magnetic field, known as switchbacks. Their counterparts in the solar wind velocity field are local enhancements in the radial speed, or jets, displaying (in all components) the velocity-magnetic field correlation typical of large amplitude Alfven waves propagating away from the Sun. Switchbacks and radial jets have previously been observed over a wide range of heliocentric distances by Helios, Wind, and Ulysses, although they were prevalent in significantly faster streams than seen at PSP. Here we study via numerical magnetohydrodynamics simulations the evolution of such large amplitude Alfvenic fluctuations by including, in agreement with observations, both a radial magnetic field inversion and an initially constant total magnetic pressure. Despite the extremely large excursion of magnetic and velocity fields, switchbacks are seen to persist for up to hundreds of Alfven crossing times before eventually decaying due to the parametric decay instability. Our results suggest that such switchback/jet configurations might indeed originate in the lower corona and survive out to PSP distances, provided the background solar wind is sufficiently calm, in the sense of not being pervaded by strong density fluctuations or other gradients, such as stream or magnetic field shears, that might destabilize or destroy them over shorter timescales.
    ISSN
    0067-0049
    EISSN
    1538-4365
    DOI
    10.3847/1538-4365/ab53e1
    Version
    Final published version
    Sponsors
    National Aeronautics and Space Administration
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4365/ab53e1
    Scopus Count
    Collections
    UA Faculty Publications

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