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.
Centre for Fusion, Space and Astrophysics; Department of Physics, University of Warwick, Coventry CV4 7AL, United Kingdom. k.kiyani@warwick.ac.uk
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