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dc.contributor.authorKarampelas, K.
dc.contributor.authorVan Doorsselaere, T.
dc.contributor.authorAntolin, P.
dc.date.accessioned2017-06-30T11:30:07Z
dc.date.available2017-06-30T11:30:07Z
dc.date.issued2017-08-25
dc.identifier.citationKarampelas , K , Van Doorsselaere , T & Antolin , P 2017 , ' Heating by transverse waves in simulated coronal loops ' Astronomy & Astrophysics , vol. 604 , A130 . https://doi.org/10.1051/0004-6361/201730598en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 250308889
dc.identifier.otherPURE UUID: 1b5b05b8-51c0-4a2f-9972-72617ca298a1
dc.identifier.otherBibCode: 2017arXiv170602640K
dc.identifier.otherScopus: 85028603914
dc.identifier.urihttp://hdl.handle.net/10023/11122
dc.descriptionK.K. was funded by GOA-2015-014 (KU Leuven). T.V.D was supported by the IAP P7/08 CHARM (Belspo) and the GOA-2015-014 (KU Leuven). P.A. acknowledges 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.abstractContext.  Recent numerical studies of oscillating flux tubes have established the significance of resonant absorption in the damping of propagating transverse oscillations in coronal loops. The nonlinear nature of the mechanism has been examined alongside the Kelvin-Helmholtz instability,which is expected to manifest in the resonant layers at the edges of the flux tubes. While these two processes have been hypothesized to heat coronal loops through the dissipation of wave energy into smaller scales, the occurring mixing with the hotter surroundings can potentially hide this effect. Aims.  We aim to study the effects of wave heating from driven and standing kink waves in a coronal loop. Methods.  Using the MPI-AMRVAC code, we perform ideal, three dimensional magnetohydrodynamic (MHD) simulations of both (a) footpoint driven and (b) free standing oscillations in a straight coronal flux tube, in the presence of numerical resistivity. Results.  We have observed the development of Kelvin-Helmholtz eddies at the loop boundary layer of all three models considered here, as well as an increase of the volume averaged temperature inside the loop. The main heating mechanism in our setups was Ohmic dissipation, as indicated by the higher values for the temperatures and current densities located near the footpoints. The introduction of a temperature gradient between the inner tube and the surrounding plasma, suggests that the mixing of the two regions, in the case of hotter environment, greatly increases the temperature of the tube at the site of the strongest turbulence, beyond the contribution of the aforementioned wave heating mechanism.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2017, ESO . This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at www.aanda.org / https://doi.org/https://doi.org/10.1051/0004-6361/201730598en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: coronaen
dc.subjectSun: oscillationsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleHeating by transverse waves in simulated coronal loopsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201730598
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017arXiv170602640K


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