Journal articles
The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere
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 ${R}_{\odot }$). 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 Alfvénic 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 Alfvén speed. The energy flux in this turbulence at 0.17 au was found to be ~10% of that in the bulk solar wind kinetic energy, becoming ~40% when extrapolated to the Alfvén 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.
Cited literature [118 references]
https://hal-insu.archives-ouvertes.fr/insu-02937674
Contributor : Nathalie Pothier <>
Submitted on : Thursday, September 17, 2020 - 4:38:27 PM
Last modification on : Wednesday, October 14, 2020 - 4:10:16 AM
Contributor : Nathalie Pothier <>
Submitted on : Thursday, September 17, 2020 - 4:38:27 PM
Last modification on : Wednesday, October 14, 2020 - 4:10:16 AM
File
Chen_2020_ApJS_246_53.pdf
Publisher files allowed on an open archive
Licence
Distributed under a Creative Commons Attribution - NoDerivatives 4.0 International License