How Turbulent is the Magnetically Closed Corona?
Solar and Stellar Astrophysics
2021-05-27 v1
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.
Keywords
Cite
@article{arxiv.2105.12212,
title = {How Turbulent is the Magnetically Closed Corona?},
author = {James A. Klimchuk and Spiro K. Antiochos},
journal= {arXiv preprint arXiv:2105.12212},
year = {2021}
}
Comments
accepted by Frontiers in Astronomy and Space Sciences - Space Physics