Show simple item record

Files in this item

Thumbnail

Item metadata

dc.contributor.authorWright, Andrew Nicholas
dc.contributor.authorElsden, Thomas William
dc.date.accessioned2016-11-18T15:30:14Z
dc.date.available2016-11-18T15:30:14Z
dc.date.issued2016-12-20
dc.identifier.citationWright , A N & Elsden , T W 2016 , ' Theoretical foundation of 3D Alfvén resonances : normal modes ' , Astrophysical Journal , vol. 833 , no. 2 , 230 , pp. 1-10 . https://doi.org/10.3847/1538-4357/833/2/230en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 247759218
dc.identifier.otherPURE UUID: ea440d27-fbeb-4cc9-8eb9-0edc1d6d99c9
dc.identifier.otherScopus: 85007605894
dc.identifier.otherORCID: /0000-0002-9877-1457/work/58055380
dc.identifier.otherORCID: /0000-0002-1910-2010/work/60196732
dc.identifier.otherWOS: 000391169600105
dc.identifier.urihttps://hdl.handle.net/10023/9847
dc.description.abstractWe consider the resonant coupling of fast and Alfvén magnetohydrodynamic (MHD) waves in a 3D equilibrium. Numerical solutions to normal modes (∝ exp(−iωt)) are presented, along with a theoretical framework to interpret them. The solutions we find are fundamentally different from those in 1D and 2D. In 3D there exists an infinite number of possible resonant solutions within a “Resonant Zone," and we show how boundary conditions and locally 2D regions can favor particular solutions. A unique feature of the resonance in 3D is switching between different permissible solutions when the boundary of the Resonant Zone is encountered. The theoretical foundation that we develop relies upon recognizing that in 3D the orientation of the resonant surface will not align in a simple fashion with an equilibrium coordinate. We present a method for generating the Alfvén wave natural frequencies for an arbitrarily oriented Alfvén wave, which requires a careful treatment of scale factors describing the background magnetic field geometry.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at http://dx.doi.org/10.3847/1538-4357/833/2/230en
dc.subjectMagnetohydrodynamicsen
dc.subjectPlanets and satellites: magnetic fieldsen
dc.subjectSun: magnetic fieldsen
dc.subjectWavesen
dc.subjectQA Mathematicsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subjectBDCen
dc.subjectR2Cen
dc.subject.lccQAen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleTheoretical foundation of 3D Alfvén resonances : normal modesen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorThe Leverhulme Trusten
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/833/2/230
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/K000950/1en
dc.identifier.grantnumberST/N000609/1en
dc.identifier.grantnumberRPG-2016-071en


This item appears in the following Collection(s)

Show simple item record