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dc.contributor.authorCargill, Peter
dc.contributor.authorDe Moortel, Ineke
dc.contributor.authorKiddie, Greg
dc.identifier.citationCargill , P , De Moortel , I & Kiddie , G 2016 , ' Coronal density structure and its role in wave damping in loops ' , Astrophysical Journal , vol. 823 , no. 1 , 31 , pp. 1-10 .
dc.identifier.otherPURE: 241577622
dc.identifier.otherPURE UUID: e5553a39-7692-4405-9efc-e2d915e20725
dc.identifier.otherScopus: 84973366485
dc.identifier.otherORCID: /0000-0002-1452-9330/work/39526512
dc.identifier.otherWOS: 000377216300031
dc.descriptionThis project has received funding from the Science and Technology Facilities Council (UK) and the European Research Council (ERC) under the European Unionʼs Horizon 2020 research and innovation program (grant agreement No 647214). 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.abstractIt has long been established that gradients in the Alfvén speed, and in particular the plasma density, are an essential part of the damping of waves in the magnetically closed solar corona by mechanisms such as resonant absorption and phase mixing. While models of wave damping often assume a fixed density gradient, in this paper the self-consistency of such calculations is assessed by examining the temporal evolution of the coronal density. It is shown conceptually that for some coronal structures, density gradients can evolve in a way that the wave-damping processes are inhibited. For the case of phase mixing we argue that (a) wave heating cannot sustain the assumed density structure and (b) inclusion of feedback of the heating on the density gradient can lead to a highly structured density, although on long timescales. In addition, transport coefficients well in excess of classical are required to maintain the observed coronal density. Hence, the heating of closed coronal structures by global oscillations may face problems arising from the assumption of a fixed density gradient, and the rapid damping of oscillations may have to be accompanied by a separate (non-wave-based) heating mechanism to sustain the required density structuring.
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at:
dc.subjectSun: coronaen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleCoronal density structure and its role in wave damping in loopsen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Research Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEuropean Commissionen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.description.statusPeer revieweden

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