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dc.contributor.authorMatthaeus, William H.
dc.contributor.authorMullan, D. J.
dc.contributor.authorDmitruk, Pablo
dc.contributor.authorMilano, L. J.
dc.contributor.authorOughton, Sean
dc.coverage.spatialTromso, NORWAYen_NZ
dc.date.accessioned2014-04-04T02:14:10Z
dc.date.available2014-04-04T02:14:10Z
dc.date.copyright2003
dc.date.issued2003
dc.identifier.citationMatthaeus, W. H., Mullan, D. J., Dmitruk, P., Milano, L., & Oughton, S. (2003). MHD turbulence and heating of the open field-line solar corona. Nonlin. Processes Geophys., 10(1/2), 93-100.en_NZ
dc.identifier.urihttps://hdl.handle.net/10289/8627
dc.description.abstractThis 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.en_NZ
dc.format.mimetypeapplication/pdf
dc.language.isoenen_NZ
dc.publisherEuropean Geoscience Unionen_NZ
dc.relation.ispartofNonlinear Processes in Geophysics
dc.rights© Author(s) 2003. This work is licensed under the Creative Commons Attribution-NonCommercial-ShareAlike 2.5 License.en_NZ
dc.subjectmagnetohydrodynamics (MHD)en_NZ
dc.titleMHD turbulence and heating of the open field-line solar coronaen_NZ
dc.typeJournal Articleen_NZ
dc.identifier.doi10.5194/npg-10-93-2003en_NZ
dc.relation.isPartOfNon-Linear Processes in Geophysicsen_NZ
pubs.begin-page93en_NZ
pubs.elements-id28206
pubs.end-page100en_NZ
pubs.issue1-2en_NZ
pubs.volume10en_NZ


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