  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.
