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

By K. Kiyani, Sandra C. Chapman, B. Hnat and Ruth Mary Nicol


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

Topics: QC
Publisher: American Physical Society
Year: 2007
OAI identifier:

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