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dc.contributor.authorHowson, T. A.
dc.contributor.authorDe Moortel, I.
dc.contributor.authorAntolin, P.
dc.date.accessioned2017-03-10T16:30:09Z
dc.date.available2017-03-10T16:30:09Z
dc.date.issued2017-06-16
dc.identifier249348122
dc.identifierd498b0a0-28ff-420d-91cc-1ff91c8a26df
dc.identifier85020855609
dc.identifier000404648300090
dc.identifier.citationHowson , T A , De Moortel , I & Antolin , P 2017 , ' The effects of resistivity and viscosity on the Kelvin-Helmholtz instability in oscillating coronal loops ' , Astronomy & Astrophysics , vol. 602 , A74 . https://doi.org/10.1051/0004-6361/201630259en
dc.identifier.issn0004-6361
dc.identifier.otherBibCode: 2017A&A...602A..74H
dc.identifier.otherBibCode: 2017A&A...602A..74H
dc.identifier.otherORCID: /0000-0002-1452-9330/work/39526493
dc.identifier.otherORCID: /0000-0002-4895-6277/work/66070057
dc.identifier.urihttps://hdl.handle.net/10023/10450
dc.descriptionThe research leading to these results has received funding from the UK Science and Technology Facilities Council and the European Union Horizon 2020 research and innovation programme (grant agreement No. 647214).en
dc.description.abstractAims. Investigate the effects of resistivity and viscosity on the onset and growth of the Kelvin-Helmholtz instability (KHI) in an oscillating coronal loop. Methods. We modelled a standing kink wave in a density-enhanced loop with the three dimensional (3-D), resistive magnetohydrodynamics code, Lare3d. We conducted a parameter study on the viscosity and resistivity coefficients to examine the effects of dissipation on the KHI. Results. Enhancing the viscosity (ν) and resistivity (η) acts to suppress the KHI. Larger values of ν and η delay the formation of the instability and, in some cases, prevent the onset completely. This leads to the earlier onset of heating for smaller values of the transport coefficients. We note that viscosity has a greater effect on the development of the KHI than resistivity. Furthermore, when using anomalous resistivity, the Ohmic heating rate associated with the KHI may be greater than that associated with the phase mixing that occurs in an instability-suppressed regime (using uniform resistivity). Conclusions. From our study, it is clear that the heating rate crucially depends on the formation of small length scales (influenced by the numerical resolution) as well as the values of resistivity and viscosity. As larger values of the transport coefficients suppress the KHI, the onset of heating is delayed but the heating rate is larger. As increased numerical resolution allows smaller length scales to develop, the heating rate will be higher even for the same values of η and ν.
dc.format.extent12
dc.format.extent3377611
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fielden
dc.subjectSun: oscillationsen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe effects of resistivity and viscosity on the Kelvin-Helmholtz instability in oscillating coronal loopsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEuropean Research Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201630259
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017A%26A...602A..74Hen
dc.identifier.grantnumberST/K000950/1en
dc.identifier.grantnumber647214en
dc.identifier.grantnumberST/N000609/1en
dc.identifier.grantnumberN/Aen


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