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dc.contributor.authorKarampelas, Konstantinos
dc.contributor.authorVan Doorsselaere, Tom
dc.contributor.authorPascoe, David J.
dc.contributor.authorGuo, Mingzhe
dc.contributor.authorAntolin, Patrick
dc.identifier.citationKarampelas , K , Van Doorsselaere , T , Pascoe , D J , Guo , M & Antolin , P 2019 , ' Amplitudes and energy fluxes of simulated decayless kink oscillations ' , Frontiers in Astronomy and Space Sciences , vol. 6 , 38 .
dc.identifier.otherPURE: 259062054
dc.identifier.otherPURE UUID: 160fd78d-ed54-4c20-8e3e-5bf38a5ef8c3
dc.identifier.otherRIS: urn:6135D6445543E04E25C3F20452671B1B
dc.identifier.otherWOS: 000468498900001
dc.identifier.otherScopus: 85075276328
dc.descriptionKK, TVD, and DP and were funded by GOA-2015-014 (KU Leuven). MG is supported by the China Scholarship Council (CSC) and the National Natural Science Foundation of China (41674172). PA acknowledges funding from his STFC Ernest Rutherford Fellowship (No. ST/R004285/1). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 724326).en
dc.description.abstractRecent observations with the Atmospheric Imaging Assembly (AIA) instrument on the SDO spacecraft have revealed the existence of decayless coronal kink oscillations. These transverse oscillations are not connected to any external phenomena like flares or coronal mass ejections, and show significantly lower amplitudes than the externally excited decaying oscillations. Numerical studies have managed to reproduce such decayless oscillations in the form of footpoint driven standing waves in coronal loops, and to treat them as a possible mechanism for wave heating of the solar corona. Our aim is to investigate the correlation between the observed amplitudes of the oscillations and input the energy flux from different drivers. We perform 3D MHD simulations in single, straight, density-enhanced coronal flux tubes for different drivers, in the presence of gravity. Synthetic images at different spectral lines are constructed with the use of the FoMo code. The development of the Kelvin-Helmholtz instability leads to mixing of plasma between the flux tube and the hot corona. Once the KHI is fully developed, the amplitudes of the decayless oscillations show only a weak correlation with the driver strength. We find that low amplitude decayless kink oscillations may correspond to significant energy fluxes of the order of the radiative losses for the Quiet Sun. A clear correlation between the input energy flux and the observed amplitudes from our synthetic imaging data cannot be established. Stronger drivers lead to higher vales of the line width estimated energy fluxes. Finally, estimations of the energy fluxes by spectroscopic data are affected by the LOS angle, favoring combined analysis of imaging and spectroscopic data for single oscillating loops.
dc.relation.ispartofFrontiers in Astronomy and Space Sciencesen
dc.rightsCopyright © 2019 Karampelas, Van Doorsselaere, Pascoe, Guo and Antolin. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.en
dc.subjectSolar coronaen
dc.subjectForward modelingen
dc.subjectCorona loopsen
dc.subjectDecayless oscillationsen
dc.subjectQB Astronomyen
dc.titleAmplitudes and energy fluxes of simulated decayless kink oscillationsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.description.statusPeer revieweden

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