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dc.contributor.authorHowson, Thomas Alexander
dc.contributor.authorDe Moortel, Ineke
dc.contributor.authorReid, Jack
dc.identifier.citationHowson , T A , De Moortel , I & Reid , J 2020 , ' Phase mixing and wave heating in a complex coronal plasma ' , Astronomy & Astrophysics , vol. 636 , A40 .
dc.identifier.otherPURE: 266759823
dc.identifier.otherPURE UUID: 1d0c1084-cd80-410f-b8cc-7c1f271a22d3
dc.identifier.otherWOS: 000526887200002
dc.identifier.otherORCID: /0000-0002-1452-9330/work/77131127
dc.identifier.otherORCID: /0000-0002-4895-6277/work/77131755
dc.identifier.otherScopus: 85083375587
dc.descriptionFunding: UK Science and Technology Facilities Council (consolidated grants ST/N000609/1 and ST/S000402/1); European Union Horizon 2020 research and innovation programme (grant agreement No. 647214); Research Council of Norway through its Centres of Excellence scheme, project number 262622 (IDM); Carnegie Trust for the Universities of Scotland (JR).en
dc.description.abstractAims. We investigate the formation of small scales and the related dissipation of magnetohydronamic (MHD) wave energy through non-linear interactions of counter-propagating, phase-mixed Alfvénic waves in a complex magnetic field. Methods. We conducted fully three-dimensional, non-ideal MHD simulations of transverse waves in complex magnetic field configurations. Continuous wave drivers were imposed on the foot points of magnetic field lines and the system was evolved for several Alfvén travel times. Phase-mixed waves were allowed to reflect off the upper boundary and the interactions between the resultant counter-streaming wave packets were analysed. Results. The complex nature of the background magnetic field encourages the development of phase mixing throughout the numerical domain, leading to a growth in alternating currents and vorticities. Counter-propagating phase-mixed MHD wave modes induce a cascade of energy to small scales and result in more efficient wave energy dissipation. This effect is enhanced in simulations with more complex background fields. High-frequency drivers excite localised field line resonances and produce efficient wave heating. However, this relies on the formation of large amplitude oscillations on resonant field lines. Drivers with smaller frequencies than the fundamental frequencies of field lines are not able to excite resonances and thus do not inject sufficient Poynting flux to power coronal heating. Even in the case of high-frequency oscillations, the rate of dissipation is likely too slow to balance coronal energy losses, even within the quiet Sun. Conclusions. For the case of the generalised phase-mixing presented here, complex background field structures enhance the rate of wave energy dissipation. However, it remains difficult for realistic wave drivers to inject sufficient Poynting flux to heat the corona. Indeed, significant heating only occurs in cases which exhibit oscillation amplitudes that are much larger than those currently observed in the solar atmosphere.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © 2020 ESO. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: oscillationsen
dc.subjectMagnetohydrodyanmics (MHD)en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titlePhase mixing and wave heating in a complex coronal plasmaen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Research Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorThe Royal Societyen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.description.statusPeer revieweden

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