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dc.contributor.authorTenerani, Anna
dc.contributor.authorVelli, Marco
dc.contributor.authorMatteini, Lorenzo
dc.contributor.authorRéville, Victor
dc.contributor.authorShi, Chen
dc.contributor.authorBale, Stuart D.
dc.contributor.authorKasper, Justin C.
dc.contributor.authorBonnell, John W.
dc.contributor.authorCase, Anthony W.
dc.contributor.authorDudok de Wit, Thierry
dc.contributor.authorGoetz, Keith
dc.contributor.authorHarvey, Peter R.
dc.contributor.authorKlein, Kristopher G.
dc.contributor.authorKorreck, Kelly
dc.contributor.authorLarson, Davin
dc.contributor.authorLivi, Roberto
dc.contributor.authorMacDowall, Robert J.
dc.contributor.authorMalaspina, David M.
dc.contributor.authorPulupa, Marc
dc.contributor.authorStevens, Michael
dc.contributor.authorWhittlesey, Phyllis
dc.date.accessioned2020-12-03T21:52:43Z
dc.date.available2020-12-03T21:52:43Z
dc.date.issued2020-02-03
dc.identifier.citationTenerani, 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.en_US
dc.identifier.issn0067-0049
dc.identifier.doi10.3847/1538-4365/ab53e1
dc.identifier.urihttp://hdl.handle.net/10150/649211
dc.description.abstractParker 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.en_US
dc.description.sponsorshipNational Aeronautics and Space Administrationen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rights© 2020. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.titleMagnetic Field Kinks and Folds in the Solar Winden_US
dc.typeArticleen_US
dc.identifier.eissn1538-4365
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben_US
dc.contributor.departmentUniv Arizona, Dept Planetary Scien_US
dc.identifier.journalASTROPHYSICAL JOURNAL SUPPLEMENT SERIESen_US
dc.description.collectioninformationThis 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.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal Supplement Series
dc.source.volume246
dc.source.issue2
dc.source.beginpage32
refterms.dateFOA2020-12-03T21:52:56Z


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