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dc.contributor.authorGuo, Mingzhe
dc.contributor.authorVan Doorsselaere, Tom
dc.contributor.authorKarampelas, Kostas
dc.contributor.authorLi, Bo
dc.contributor.authorAntolin, Patrick
dc.contributor.authorDe Moortel, Ineke
dc.date.accessioned2018-11-19T15:30:15Z
dc.date.available2018-11-19T15:30:15Z
dc.date.issued2019-01-10
dc.identifier.citationGuo , M , Van Doorsselaere , T , Karampelas , K , Li , B , Antolin , P & De Moortel , I 2019 , ' Heating effects from driven transverse and Alfvén waves in coronal loops ' , Astrophysical Journal , vol. 870 , no. 2 , 55 . https://doi.org/10.3847/1538-4357/aaf1d0en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 256614421
dc.identifier.otherPURE UUID: 05dcf698-b008-414a-a903-56120ad37bac
dc.identifier.otherORCID: /0000-0002-1452-9330/work/52888674
dc.identifier.otherScopus: 85060229452
dc.identifier.otherWOS: 000455820100001
dc.identifier.urihttp://hdl.handle.net/10023/16502
dc.descriptionFunding: 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 and No.647214) (IDM). P.A. acknowledges funding from his STFC Ernest Rutherford Fellowship (No. ST/R004285/1).en
dc.description.abstractRecent numerical studies revealed that transverse motions of coronal loops can induce the Kelvin-Helmholtz Instability (KHI). This process could be important in coronal heating because it leads to dissipation of energy at small spatial-scale plasma interactions. Meanwhile, small amplitude decayless oscillations in coronal loops have been discovered recently in observations of SDO/AIA. We model such oscillations in coronal loops and study wave heating effects, considering a kink and Alfvén driver separately and a mixed driver at the bottom of flux tubes. Both the transverse and Alfvén oscillations can lead to the KHI. Meanwhile, the Alfvén oscillations established in loops will experience phase mixing. Both processes will generate small spatial-scale structures, which can help the dissipation of wave energy. Indeed, we observe the increase of internal energy and temperature in loop regions. The heating is more pronounced for the simulation containing the mixed kink and Alfvén driver. This means that the mixed wavemodes can lead to a more efficient energy dissipation in the turbulent state of the plasma and that the KHI eddies act as an agent to dissipate energy in other wave modes. Furthermore, we also obtained forward modelling results using the FoMo code. We obtained forward models which are very similar to the observations of decayless oscillations. Due to the limited resolution of instruments, neither Alfvén modes nor the fine structures are observable. Therefore, this numerical study shows that Alfvén modes probably can co-exist with kink modes, leading to enhanced heating.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2018, American Astronomical Society. 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 as such may differ slightly from the final published version. The final published version of this work is available at http://iopscience.iop.org/journal/0004-637Xen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectWavesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleHeating effects from driven transverse and Alfvén waves in coronal loopsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aaf1d0
dc.description.statusPeer revieweden


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