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dc.contributor.authorPascoe, David James
dc.contributor.authorWright, Andrew Nicholas
dc.contributor.authorDe Moortel, Ineke
dc.contributor.authorHood, Alan William
dc.identifier.citationPascoe , D J , Wright , A N , De Moortel , I & Hood , A W 2015 , ' Excitation and damping of broadband kink waves in the solar corona ' , Astronomy & Astrophysics , vol. 578 , A99 .
dc.identifier.otherPURE: 195851477
dc.identifier.otherPURE UUID: c8c30a91-d801-419d-9285-faa69565acc4
dc.identifier.otherScopus: 84934961393
dc.identifier.otherORCID: /0000-0002-1452-9330/work/39526510
dc.identifier.otherORCID: /0000-0003-2620-2068/work/58055222
dc.identifier.otherORCID: /0000-0002-9877-1457/work/58055406
dc.identifier.otherWOS: 000357502600111
dc.descriptionD.J.P. acknowledges financial support from STFC. I.D.M. acknowledges support of a Royal Society University Research Fellowship. The research leading to these results has also received funding from the European Commission Seventh Framework Programme (FP7/ 2007−2013) under the grant agreement SOLSPANET (project No. 269299,
dc.description.abstractContext. Observations such as those by the Coronal Multi-Channel Polarimeter (CoMP) have revealed that broadband kink oscillations are ubiquitous in the solar corona. Aims. We consider footpoint-driven kink waves propagating in a low β coronal plasma with a cylindrical density structure. We investigate the excitation and damping of propagating kink waves by a broadband driver, including the effects of different spatial profiles for the driver. Methods. We employ a general spatial damping profile in which the initial stage of the damping envelope is approximated by a Gaussian profile and the asymptotic state by an exponential one. We develop a method of accounting for the presence of these different damping regimes and test it using data from numerical simulations. Results. Strongly damped oscillations in low density coronal loops are more accurately described by a Gaussian spatial damping profile than an exponential profile. The consequences for coronal seismology are investigated and applied to observational data for the ubiquitous broadband waves observed by CoMP. Current data cannot distinguish between the exponential and Gaussian profiles because of the levels of noise. We demonstrate the importance of the spatial profile of the driver on the resulting damping profile. Furthermore, we show that a small-scale turbulent driver is inefficient at exciting propagating kink waves
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2015. Reproduced with permission from Astronomy & Astrophysics, © ESO.en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: atmosphereen
dc.subjectSun: coronaen
dc.subjectSun: magnetic topologyen
dc.subjectSun: oscillationsen
dc.subjectQC Physicsen
dc.subjectQA Mathematicsen
dc.titleExcitation and damping of broadband kink waves in the solar coronaen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEuropean Commissionen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.description.statusPeer revieweden

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