Self-similar signature of the active solar corona within the inertial range of solar wind turbulence

Abstract

We quantify the scaling of magnetic energy density in the inertial range of solar wind turbulence seen in-situ at 1AU with respect to solar activity. At solar maximum, when the coronal magnetic field is dynamic and topologically complex, we find self-similar scaling in the solar wind, whereas at solar mimimum, when the coronal fields are more ordered, we find multifractality. This quantifies the solar wind signature that is of direct coronal origin, and distinguishes it from that of local MHD turbulence, with quantitative implications for our understanding of coronal heating of the solar wind.

5 pages, 7 figures, accepted in Phys. Rev. Lett

References in corpus (3)

• Solar Flares as Cascades of Reconnecting Magnetic Loops
• Intermittency, scaling and the Fokker-Planck approach to fluctuations of the solar wind bulk plasma parameters as seen by the WIND spacecraft
• A method for extracting the scaling exponents of a self-affine, non-Gaussian process from a finite length timeseries

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