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dc.contributor.authorOkamoto, Takenori J.
dc.contributor.authorAntolin, Patrick
dc.contributor.authorDe Pontieu, Bart
dc.contributor.authorUitenbroek, Han
dc.contributor.authorVan Doorsselaere, Tom
dc.contributor.authorYokoyama, Takaaki
dc.date.accessioned2017-02-14T12:30:13Z
dc.date.available2017-02-14T12:30:13Z
dc.date.issued2015-08-11
dc.identifier.citationOkamoto , T J , Antolin , P , De Pontieu , B , Uitenbroek , H , Van Doorsselaere , T & Yokoyama , T 2015 , ' Resonant absorption of transverse oscillations and associated heating in a solar prominence. I. Observational aspects ' , Astrophysical Journal , vol. 809 , no. 1 , 71 . https://doi.org/10.1088/0004-637X/809/1/71en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 248969371
dc.identifier.otherPURE UUID: 5cfc859f-0395-40fa-8d6d-efb736a560ad
dc.identifier.otherBibCode: 2015ApJ...809...71O
dc.identifier.otherScopus: 84945268671
dc.identifier.urihttp://hdl.handle.net/10023/10294
dc.description.abstractTransverse magnetohydrodynamic waves have been shown to be ubiquitous in the solar atmosphere and can, in principle, carry sufficient energy to generate and maintain the Sun's million-degree outer atmosphere or corona. However, direct evidence of the dissipation process of these waves and subsequent heating has not yet been directly observed. Here we report on high spatial, temporal, and spectral resolution observations of a solar prominence that show a compelling signature of so-called resonant absorption, a long hypothesized mechanism to efficiently convert and dissipate transverse wave energy into heat. Aside from coherence in the transverse direction, our observations show telltale phase differences around 180° between transverse motions in the plane-of-sky and line-of-sight velocities of the oscillating fine structures or threads, and also suggest significant heating from chromospheric to higher temperatures. Comparison with advanced numerical simulations support a scenario in which transverse oscillations trigger a Kelvin–Helmholtz instability (KHI) at the boundaries of oscillating threads via resonant absorption. This instability leads to numerous thin current sheets in which wave energy is dissipated and plasma is heated. Our results provide direct evidence for wave-related heating in action, one of the candidate coronal heating mechanisms.
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2015 The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1088/0004-637X/809/1/71en
dc.subjectSun: chromosphereen
dc.subjectSun: transition regionen
dc.subjectWavesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleResonant absorption of transverse oscillations and associated heating in a solar prominence. I. Observational aspectsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/809/1/71
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2015ApJ...809...71Oen


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