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dc.contributor.authorvan Ballegooijen, A. A.
dc.contributor.authorAsgari-Targhi, M.
dc.contributor.authorVoss, A.
dc.date.accessioned2017-12-05T17:30:06Z
dc.date.available2017-12-05T17:30:06Z
dc.date.issued2017-10-30
dc.identifier.citationvan Ballegooijen , A A , Asgari-Targhi , M & Voss , A 2017 , ' The heating of solar coronal loops by Alfvèn wave turbulence ' Astrophysical Journal , vol. 849 , no. 1 , 46 . https://doi.org/10.3847/1538-4357/aa9118en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 251423842
dc.identifier.otherPURE UUID: 3fea4901-473d-445b-9b4b-94db670c6aec
dc.identifier.otherORCID: /0000-0002-8053-2175/work/38124084
dc.identifier.urihttp://hdl.handle.net/10023/12261
dc.descriptionThis project was supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and contract SP02H1701R from Lockheed Martin Space and Astrophysics Laboratory (LMSAL) to SAO.en
dc.description.abstractIn this paper we further develop a model for the heating of coronal loops by Alfvèn wave turbulence (AWT). The Alfvèn waves are assumed to be launched from a collection of kilogauss flux tubes in the photosphere at the two ends of the loop. Using a three-dimensional magneto-hydrodynamic (MHD) model for an active-region loop, we investigate how the waves from neighboring flux tubes interact in the chromosphere and corona. For a particular combination of model parameters we find that AWT can produce enough heat to maintain a peak temperature of about 2.5 MK, somewhat lower than the temperatures of 3 – 4 MK observed in the cores of active regions. The heating rates vary strongly in space and time, but the simulated heating events have durations less than 1 minute and are unlikely to reproduce the observed broad Differential Emission Measure distributions of active regions. The simulated spectral line non-thermal widths are predicted to be about 27 km s−1, which is high compared to the observed values. Therefore, the present AWT model does not satisfy the observational constraints. An alternative “magnetic braiding” model is considered in which the coronal field lines are subject to slow random footpoint motions, but we find that such long period motions produce much less heating than the shorter period waves launched within the flux tubes. We discuss several possibilities for resolving the problem of producing sufficiently hot loops in active regions.
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2017 The 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 may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-4357/aa9118en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectTurbulenceen
dc.subjectWavesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe heating of solar coronal loops by Alfvèn wave turbulenceen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Computer Scienceen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aa9118
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1710.05074


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