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dc.contributor.authorLiu, J.
dc.contributor.authorMcintosh, S.W.
dc.contributor.authorDe Moortel, I.
dc.contributor.authorThrelfall, J.
dc.contributor.authorBethge, C.
dc.date.accessioned2015-01-12T11:01:04Z
dc.date.available2015-01-12T11:01:04Z
dc.date.issued2014-12-10
dc.identifier.citationLiu , J , Mcintosh , S W , De Moortel , I , Threlfall , J & Bethge , C 2014 , ' Statistical evidence for the existence of Alfvénic turbulence in solar coronal loops ' , Astrophysical Journal , vol. 797 , no. 1 , 7 . https://doi.org/10.1088/0004-637X/797/1/7en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 160061857
dc.identifier.otherPURE UUID: bb6d6888-b7ee-45fa-9d8b-7b02edf8f5df
dc.identifier.otherScopus: 84914124826
dc.identifier.otherORCID: /0000-0002-1452-9330/work/39526505
dc.identifier.otherWOS: 000345915000007
dc.identifier.urihttp://hdl.handle.net/10023/5987
dc.descriptionThe authors acknowledge support from NASA contracts NNX08BA99G, NNX11AN98G, NNM12AB40P, NNG09FA40C (IRIS), and NNM07AA01C (Hinode). 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, www.solspanet.eu/solspanet).en
dc.description.abstractRecent observations have demonstrated that waves capable of carrying large amounts of energy are ubiquitous throughout the solar corona. However, the question of how this wave energy is dissipated (on which timescales and length scales) and released into the plasma remains largely unanswered. Both analytic and numerical models have previously shown that Alfvénic turbulence may play a key role not only in the generation of the fast solar wind, but in the heating of coronal loops. In an effort to bridge the gap between theory and observations, we expand on a recent study by analyzing 37 clearly isolated coronal loops using data from the Coronal Multi-channel Polarimeter instrument.We observe Alfvénic perturbations with phase speeds which range from 250 to 750 km s-1 and periods from 140 to 270 s for the chosen loops. While excesses of high-frequency wave power are observed near the apex of some loops (tentatively supporting the onset of Alfvénic turbulence), we show that this excess depends on loop length and the wavelength of the observed oscillations. In deriving a proportional relationship between the loop length/wavelength ratio and the enhanced wave power at the loop apex, and from the analysis of the line widths associated with these loops, our findings are supportive of the existence of Alfvénic turbulence in coronal loops.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserveden
dc.subjectSun: coronaen
dc.subjectWavesen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleStatistical evidence for the existence of Alfvénic turbulence in solar coronal loopsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Managementen
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/797/1/7
dc.description.statusPeer revieweden


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