The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere
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Author
Chen, C. H. K.Bale, S. D.

Bonnell, J. W.
Borovikov, D.
Bowen, T. A.
Burgess, D.
Case, A. W.
Chandran, B. D. G.
Dudok de Wit, T.
Goetz, K.
Harvey, P. R.
Kasper, J. C.
Klein, K. G.
Korreck, K. E.
Larson, D.
Livi, R.
MacDowall, R. J.
Malaspina, D. M.
Mallet, A.
McManus, M. D.
Moncuquet, M.
Pulupa, M.
Stevens, M. L.
Whittlesey, P.
Affiliation
Univ Arizona, Lunar & Planetary LabIssue Date
2020-02-03
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IOP PUBLISHING LTDCitation
Chen, C. H. K., Bale, S. D., Bonnell, J. W., Borovikov, D., Bowen, T. A., Burgess, D., ... & Whittlesey, P. (2020). The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere. The Astrophysical Journal Supplement Series, 246(2), 53.Rights
© 2020 The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.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 first two orbits of the Parker Solar Probe spacecraft have enabled the first in situ measurements of the solar wind down to a heliocentric distance of 0.17 au (or 36 R-circle dot). Here, we present an analysis of this data to study solar wind turbulence at 0.17 au and its evolution out to 1 au. While many features remain similar, key differences at 0.17 au include increased turbulence energy levels by more than an order of magnitude, a magnetic field spectral index of -3/2 matching that of the velocity and both Elsasser fields, a lower magnetic compressibility consistent with a smaller slow-mode kinetic energy fraction, and a much smaller outer scale that has had time for substantial nonlinear processing. There is also an overall increase in the dominance of outward-propagating Alfvenic fluctuations compared to inward-propagating ones, and the radial variation of the inward component is consistent with its generation by reflection from the large-scale gradient in Alfven speed. The energy flux in this turbulence at 0.17 au was found to be similar to 10% of that in the bulk solar wind kinetic energy, becoming similar to 40% when extrapolated to the Alfven point, and both the fraction and rate of increase of this flux toward the Sun are consistent with turbulence-driven models in which the solar wind is powered by this flux.Note
Open access articleISSN
0067-0049EISSN
1538-4365Version
Final published versionSponsors
Science and Technology Facilities Councilae974a485f413a2113503eed53cd6c53
10.3847/1538-4365/ab60a3
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Except where otherwise noted, this item's license is described as © 2020 The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.