MHD turbulence and heating of the open field-line solar corona

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 su...

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Bibliographic Details
Published in:Nonlinear Processes in Geophysics
Main Authors: Matthaeus, William H., Mullan, D. J., Dmitruk, Pablo, Milano, L. J., Oughton, Sean
Format: Article in Journal/Newspaper
Language:English
Published: European Geoscience Union 2003
Subjects:
magnetohydrodynamics (MHD)
Norway
Tromso
Online Access:https://hdl.handle.net/10289/8627
https://doi.org/10.5194/npg-10-93-2003
Description
Summary: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, and may be similar in some respects to ion heating due to intense electron beams observed in the aurora.

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