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dc.contributor.authorMatthaeus, William H.
dc.contributor.authorZank, Gary P.
dc.contributor.authorOughton, Sean
dc.contributor.authorMullan, D. J.
dc.contributor.authorDmitruk, Pablo
dc.date.accessioned2014-04-03T04:09:14Z
dc.date.available2014-04-03T04:09:14Z
dc.date.copyright1999-09-20
dc.date.issued1999
dc.identifier.citationMatthaeus, W. H., Zank, G. P., Oughton, S., Mullan, D. J., & Dmitruk, P. (1999). Coronal heating by magnetohydrodynamic turbulence driven by reflected low-frequency waves. The Astrophysical Journal, 523(1), L93-L96.en_NZ
dc.identifier.urihttps://hdl.handle.net/10289/8610
dc.description.abstractA candidate mechanism for the heating of the solar corona in open field line regions is described. The interaction of Alfvén waves, generated in the photosphere or chromosphere, with their reflections and the subsequent driving of quasi-two-dimensional MHD turbulence is considered. A nonlinear cascade drives fluctuations toward short wavelengths which are transverse to the mean field, thereby heating at rates insensitive to restrictive Alfvén timescales. A phenomenology is presented, providing estimates of achievable heating efficiency that are most favorable.en_NZ
dc.format.mimetypeapplication/pdf
dc.language.isoenen_NZ
dc.publisherIOP PUBLISHING LTDen_NZ
dc.relation.ispartofThe Astrophysical Journal
dc.rights©1999 the American Astronomical Societyen_NZ
dc.subjectMHDen_NZ
dc.subjectSunen_NZ
dc.subjectcoronaen_NZ
dc.subjectturbulenceen_NZ
dc.titleCoronal heating by magnetohydrodynamic turbulence driven by reflected low-frequency wavesen_NZ
dc.typeJournal Articleen_NZ
dc.identifier.doi10.1086/312259en_NZ
dc.relation.isPartOfASTROPHYSICAL JOURNALen_NZ
pubs.begin-pageL93en_NZ
pubs.elements-id28188
pubs.end-pageL96en_NZ
pubs.issue1en_NZ
pubs.volume523en_NZ


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