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Coronal MHD transport theory and phenomenology

dc.contributor.authorMilano, L. J.
dc.contributor.authorMatthaeus, William H.
dc.contributor.authorDmitruk, Pablo
dc.contributor.authorOughton, Sean
dc.coverage.spatialConference held at Pisa, Italyen_NZ
dc.date.accessioned2014-04-04T02:54:38Z
dc.date.available2014-04-04T02:54:38Z
dc.date.issued2003
dc.identifier.citationMilano, L. J., Matthaeus, W. H., Dmitruk, P., & Oughton, S. (2003). Coronal MHD transport theory and phenomenology. In M. Velli, R. Bruno, & F. Malara, Proceedings of the Tenth International Solar Wind Coference (pp. 34-346).en_NZ
dc.identifier.urihttps://hdl.handle.net/10289/8634
dc.description.abstractIn the presence of a weakly inhomogeneous background, magnetohydrodynamic fluctuations are transported, reflected and at small scales, dissipated. In contrast to orderings appropriate to outer solar wind conditions, here we explore transport in a regime relevant for solar coronal heating and solar wind acceleration, in which effects of the order of the Alfvén speed are retained while disregarding the solar wind velocity. We consider the general properties of the transport equations as well as some solutions of interest.en_NZ
dc.format.mimetypeapplication/pdf
dc.language.isoenen_NZ
dc.publisherAmerican Institute of Physicsen_NZ
dc.rights© 2003 American Institute of Physics.en_NZ
dc.source10th International Solar Wind Conferenceen_NZ
dc.subjectmagnetohydrodynamics (MHD)en_NZ
dc.titleCoronal MHD transport theory and phenomenologyen_NZ
dc.identifier.doi10.1063/1.1618609en_NZ
dc.relation.isPartOfSolar Wind Ten: Proc 10th International Solar Wind Conferenceen_NZ
pubs.begin-page343en_NZ
pubs.elements-id12644
pubs.end-page346en_NZ
pubs.finish-date2003-06-21en_NZ
pubs.place-of-publicationMelville, New Yorken_NZ
pubs.start-date2003-06-17en_NZ
pubs.volumeAIP Conference Proceedings 679en_NZ


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