The Enhancement of Proton Stochastic Heating in the Near-Sun Solar Wind
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Martinović_2020_ApJS_246_30.pdf
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Final Published Version
Author
Martinović, Mihailo M.Klein, Kristopher G.
Kasper, Justin C.
Case, Anthony W.
Korreck, Kelly E.
Larson, Davin
Livi, Roberto
Stevens, Michael
Whittlesey, Phyllis
Chandran, Benjamin D. G.
Alterman, Ben L.
Huang, Jia
Chen, Christopher H. K.
Bale, Stuart D.
Pulupa, Marc
Malaspina, David M.
Bonnell, John W.
Harvey, Peter R.
Goetz, Keith
Dudok de Wit, Thierry
MacDowall, Robert J.
Affiliation
Univ Arizona, Lunar & Planetary LabIssue Date
2020-02-03
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IOP PUBLISHING LTDCitation
Martinović, M. M., Klein, K. G., Kasper, J. C., Case, A. W., Korreck, K. E., Larson, D., ... & MacDowall, R. J. (2020). The Enhancement of Proton Stochastic Heating in the Near-Sun Solar Wind. The Astrophysical Journal Supplement Series, 246(2), 30.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
Stochastic heating (SH) is a nonlinear heating mechanism driven by the violation of magnetic moment invariance due to large-amplitude turbulent fluctuations producing diffusion of ions toward higher kinetic energies in the direction perpendicular to the magnetic field. It is frequently invoked as a mechanism responsible for the heating of ions in the solar wind. Here, we quantify for the first time the proton SH rate Q(perpendicular to) at radial distances from the Sun as close as 0.16 au, using measurements from the first two Parker Solar Probe encounters. Our results for both the amplitude and radial trend of the heating rate, Q(perpendicular to) proportional to r(-2.5), agree with previous results based on the Helios data set at heliocentric distances from 0.3 to 0.9 au. Also in agreement with previous results, Q(perpendicular to) is significantly larger in the fast solar wind than in the slow solar wind. We identify the tendency in fast solar wind for cuts of the core proton velocity distribution transverse to the magnetic field to exhibit a flattop shape. The observed distribution agrees with previous theoretical predictions for fast solar wind where SH is the dominant heating mechanism.ISSN
0067-0049EISSN
1538-4365Version
Final published versionSponsors
National Aeronautics and Space Administrationae974a485f413a2113503eed53cd6c53
10.3847/1538-4365/ab527f