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dc.contributor.authorDe Moortel, Ineke
dc.contributor.authorPascoe, David James
dc.date.accessioned2014-05-09T10:01:00Z
dc.date.available2014-05-09T10:01:00Z
dc.date.issued2014-03-11
dc.identifier.citationDe Moortel , I & Pascoe , D J 2014 , ' Standing kink modes in three-dimensional coronal loops ' , Astrophysical Journal , vol. 784 , 101 . https://doi.org/10.1088/0004-637X/784/2/101en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 102821455
dc.identifier.otherPURE UUID: 462e9489-3e7a-46ba-b2e7-0080002dc008
dc.identifier.otherScopus: 84896507354
dc.identifier.otherORCID: /0000-0002-1452-9330/work/39526482
dc.identifier.otherWOS: 000335519400016
dc.identifier.urihttps://hdl.handle.net/10023/4745
dc.descriptionI.D.M. acknowledges support from a Royal Society University Research Fellowship. The computational work for this paper was carried out at the joint STFC and SFC (SRIF)-fundedclusterattheUniversityofStAndrews(UK). The research leading to these results has also received funding from the European Commissions Seventh Framework Programme (FP7/2007-2013) under the grant agreement SOLSPANET (project No. 269299;www.solspanet.eu/solspanet).en
dc.description.abstractSo far, the straight flux tube model proposed by Edwin & Roberts is the most commonly used tool in practical coronal seismology, in particular, to infer values of the (coronal) magnetic field from observed, standing kink mode oscillations. In this paper, we compare the period predicted by this basic model with three-dimensional (3D) numerical simulations of standing kink mode oscillations, as the period is a crucial parameter in the seismological inversion to determine the magnetic field. We perform numerical simulations of standing kink modes in both straight and curved 3D coronal loops and consider excitation by internal and external drivers. The period of oscillation for the displacement of dense coronal loops is determined by the loop length and the kink speed, in agreement with the estimate based on analytical theory for straight flux tubes. For curved coronal loops embedded in a magnetic arcade and excited by an external driver, a secondary mode with a period determined by the loop length and external Alfvén speed is also present. When a low number of oscillations is considered, these two periods can result in a single, non-resolved (broad) peak in the power spectrum, particularly for low values of the density contrast for which the two periods will be relatively similar. In that case (and for this particular geometry), the presence of this additional mode would lead to ambiguous seismological estimates of the magnetic field strength.
dc.format.extent7
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: atmosphereen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: oscillationsen
dc.subjectWavesen
dc.subjectQC Physicsen
dc.subject.lccQCen
dc.titleStanding kink modes in three-dimensional coronal loopsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/784/2/101
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/K000950/1en
dc.identifier.grantnumberST/L005522/1en


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