Self-similar signature of the active solar corona within the inertial range of solar-wind turbulence.
We quantify the scaling of magnetic energy density in the inertial range of solar-wind turbulence seen in situ at 1 AU 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 minimum, 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 coronal heating of the solar wind.
Kiyani
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Centre for Fusion, Space and Astrophysics; Department of Physics, University of Warwick, Coventry CV4 7AL, United Kingdom. k.kiyani@warwick.ac.uk
Chapman
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