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MHD turbulence and heating of the open field-line solar corona
Nonlinear Processes in Geophysics
This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static magnetohydrodynamic fluctuations. Reflection from coronal inhomogeneities plays an important role in sustaining the cascade. Physical and observational constraints are discussed. Kinetic processes that convert cascaded energy into heat must occur in regions of turbulent small-scale reconnection, anddoi:10.5194/npg-10-93-2003 fatcat:25isips7bjahfgsex76r4434ia