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dc.contributor.authorKaneko, T
dc.contributor.authorGoossens, Marcel
dc.contributor.authorSoler, Roberto
dc.contributor.authorTerradas, Jaume
dc.contributor.authorVan Doorsselaere, Tom
dc.contributor.authorYokoyama, T
dc.contributor.authorWright, Andrew Nicholas
dc.identifier.citationKaneko , T , Goossens , M , Soler , R , Terradas , J , Van Doorsselaere , T , Yokoyama , T & Wright , A N 2015 , ' Apparent cross-field superslow propagation of magnetohydrodynamic waves in solar plasmas ' , Astrophysical Journal , vol. 812 , no. 2 , 121 .
dc.identifier.otherPURE: 218619253
dc.identifier.otherPURE UUID: 8405768d-5476-4a65-8d7d-49225646dab5
dc.identifier.otherScopus: 84946099356
dc.identifier.otherORCID: /0000-0002-9877-1457/work/58055397
dc.identifier.otherWOS: 000365206600033
dc.descriptionTK was supported by the Program for Leading Graduate School, MEXT, Japan. This work was supported by JSPS KAKENHI Grant Number 15H03640. RS acknowledges support from MINECO through project AYA2014-54485-P and from FEDER funds. RS also acknowledges support from MINECO through a ‘Juan de la Cierva’ grant, from MECD through project CEF11-0012, and from the ‘Vicerectorat d’Investigació Postgrau’ of the UIB. JT acknowledges support from the Spanish Ministerio de Educación y Ciencia through a Ramón y Cajal grant. JT acknowledges support from MINECO through project AYA2014-54485-P and from FEDER funds. MG was supported by IAP P7/08 CHARM (Belspo) and the GOA-2015-014 (KU Leuven). TVD was supported by an Odysseus grant of the FWO Vlaanderen, the IAP P7/08 CHARM (Belspo) and the GOA-2015-014 (KU Leuven)en
dc.description.abstractIn this paper we show that the phase mixing of continuum Alfvén waves and/or continuum slow waves in magnetic structures of the solar atmosphere as, e.g., coronal arcades, can create the illusion of wave propagation across the magnetic eld. This phenomenon could be erroneously interpreted as fast mag- netosonic waves. The cross-field propagation due to phase mixing of continuum waves is apparent because there is no real propagation of energy across the magnetic surfaces. We investigate the continuous Alfvén and slow spectra in 2D Cartesian equilibrium models with a purely poloidal magnetic field. We show that apparent superslow propagation across the magnetic surfaces in solar coronal structures is a consequence of the existence of continuum Alfvén waves and continuum slow waves that naturally live on those structures and phase mix as time evolves. The apparent cross-field phase velocity is related to the spatial variation of the local Alfvén/slow frequency across the magnetic surfaces and is slower than the Alfvén/sound velocities for typical coronal conditions. Understanding the nature of the apparent cross-field propagation is important for the correct analysis of numerical simulations and the correct interpretation of observations.
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2015, Publisher / the Author(s). This work is 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 /
dc.subjectSun: coronaen
dc.subjectSun: filaments, prominencesen
dc.subjectSun: oscillationsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleApparent cross-field superslow propagation of magnetohydrodynamic waves in solar plasmasen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.description.statusPeer revieweden

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