Radial Evolution of Magnetic Field Fluctuations in an Interplanetary Coronal Mass Ejection Sheath

Abstract

The sheaths of compressed solar wind that precede interplanetary coronal mass ejections (ICMEs) commonly display large-amplitude magnetic field fluctuations. As ICMEs propagate radially from the Sun, the properties of these fluctuations may evolve significantly. We have analyzed magnetic field fluctuations in an ICME sheath observed by MESSENGER at 0.47 au and subsequently by STEREO-B at 1.08 au while the spacecraft were close to radial alignment. Radial changes in fluctuation amplitude, compressibility, inertial-range spectral slope, permutation entropy, Jensen-Shannon complexity, and planar structuring are characterized. These changes are discussed in relation to the evolving turbulent properties of the upstream solar wind, the shock bounding the front of the sheath changing from a quasi-parallel to quasi-perpendicular geometry, and the development of complex structures in the sheath plasma.

13 pages, 5 figures

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• Cross Helicity of the November 2018 Magnetic Cloud Observed by the Parker Solar Probe
• Categorization of Coronal Mass Ejection Driven Sheath Regions: Characteristics of STEREO Events
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• Structure and fluctuations of a slow ICME sheath observed at 0.5 au by the Parker Solar Probe
• A coronal mass ejection encountered by four spacecraft within 1 au from the Sun: Ensemble modelling of propagation and magnetic structure
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• Complexity-entropy analysis of solar photospheric turbulence: Hinode images of magnetic and Poynting fluxes
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