How Turbulent is the Magnetically Closed Corona?
arXiv:2105.12212 · doi:10.3389/fspas.2021.662861
Abstract
We argue that the magnetically closed corona evolves primarily quasi-statically, punctuated by many localized bursts of activity associated with magnetic reconnection at a myriad of small current sheets. The sheets form by various processes that do not involve a traditional turbulent cascade whereby energy flows losslessly through a continuum of spatial scales starting from the large scale of the photospheric driving. If such an inertial range is a defining characteristic of turbulence, then the magnetically closed corona is not a turbulent system. It nonetheless has a complex structure that bears no direct relationship to the pattern of driving.
arXiv commentaccepted by Frontiers in Astronomy and Space Sciences - Space Physics
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