Show simple item record  

dc.contributor.authorOughton, Seanen_NZ
dc.contributor.authorMatthaeus, William H.en_NZ
dc.contributor.authorDmitruk, Pabloen_NZ
dc.date.accessioned2017-05-23T22:20:28Z
dc.date.available2017-04-10en_NZ
dc.date.available2017-05-23T22:20:28Z
dc.date.issued2017-04-10en_NZ
dc.identifier.citationOughton, S., Matthaeus, W. H., & Dmitruk, P. (2017). Reduced MHD in Astrophysical Applications: Two-dimensional or Three-dimensional? The Astrophysical Journal, 839(1). https://doi.org/10.3847/1538-4357/aa67e2en
dc.identifier.issn0004-637Xen_NZ
dc.identifier.urihttp://hdl.handle.net/10289/11075
dc.description.abstractOriginally proposed as an efficient approach to computation of nonlinear dynamics in tokamak fusion research devices, reduced magnetohydrodynamics (RMHD) has subsequently found application in studies of coronal heating, flux tube dynamics, charged particle transport, and, in general, as an approximation to describe plasma turbulence in space physics and astrophysics. Given the diverse set of derivations available in the literature, there has emerged some level of discussion and a lack of consensus regarding the completeness of RMHD as a turbulence model, and its applicability in contexts such as the solar wind. Some of the key issues in this discussion are examined here, emphasizing that RMHD is properly neither 2D nor fully 3D, being rather an incomplete representation that enforces at least one family of extraneous conservation laws.
dc.format.mimetypeapplication/pdf
dc.language.isoenen_NZ
dc.publisherAmerican Astronomical Societyen_NZ
dc.rightsThis is an author’s accepted version of an article published in the journal: The Astrophysical Journal. © 2017 The American Astronomical Society.
dc.subjectScience & Technologyen_NZ
dc.subjectPhysical Sciencesen_NZ
dc.subjectAstronomy & Astrophysicsen_NZ
dc.subjectmagnetohydrodynamics (MHD)en_NZ
dc.subjectmethods: numericalen_NZ
dc.subjectplasmasen_NZ
dc.subjectSun: coronaen_NZ
dc.subjectSun: magnetic fieldsen_NZ
dc.subjectturbulenceen_NZ
dc.subjectCOMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCEen_NZ
dc.subjectRESOLUTION HYBRID SIMULATIONSen_NZ
dc.subjectMAGNETIC-FIELD CORRELATIONen_NZ
dc.subjectALFVEN-WAVE TURBULENCEen_NZ
dc.subjectSOLAR-WINDen_NZ
dc.subjectINCOMPRESSIBLE FLUIDSen_NZ
dc.subjectVARIANCE ANISOTROPYen_NZ
dc.subjectSTRAUSS EQUATIONSen_NZ
dc.subjectINERTIAL RANGEen_NZ
dc.subjectCORONAen_NZ
dc.titleReduced MHD in Astrophysical Applications: Two-dimensional or Three-dimensional?en_NZ
dc.typeJournal Article
dc.identifier.doi10.3847/1538-4357/aa67e2en_NZ
dc.relation.isPartOfThe Astrophysical Journalen_NZ
pubs.elements-id194022
pubs.issue1en_NZ
pubs.organisational-group/Waikato
pubs.organisational-group/Waikato/2018 PBRF
pubs.organisational-group/Waikato/FCMS
pubs.organisational-group/Waikato/FCMS/2018 PBRF - FCMS
pubs.publication-statusPublisheden_NZ
pubs.volume839en_NZ
dc.identifier.eissn1538-4357en_NZ
uow.identifier.article-no2


Files in this item

This item appears in the following Collection(s)

Show simple item record