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dc.contributor.authorSyntelis, P.
dc.contributor.authorAntolin, P.
dc.date.accessioned2019-10-21T15:30:02Z
dc.date.available2019-10-21T15:30:02Z
dc.date.issued2019-10-10
dc.identifier.citationSyntelis , P & Antolin , P 2019 , ' Kelvin–Helmholtz instability and Alfvénic vortex shedding in solar eruptions ' , Astrophysical Journal Letters , vol. 884 , no. 1 , L4 , pp. 1-7 . https://doi.org/10.3847/2041-8213/ab44aben
dc.identifier.issn2041-8205
dc.identifier.otherPURE: 262150619
dc.identifier.otherPURE UUID: 8272071a-b196-4b7d-8e55-8e526b0389bf
dc.identifier.otherBibCode: 2019ApJ...884L...4S
dc.identifier.otherScopus: 85074186783
dc.identifier.otherWOS: 000504269900002
dc.identifier.otherORCID: /0000-0002-6377-0243/work/77131795
dc.identifier.urihttp://hdl.handle.net/10023/18726
dc.descriptionFunding: UK STFC Ernest Rutherford Fellowship (No. ST/R004285/1) (P.A.). ERC synergy grant “The Whole Sun” (P.S.).en
dc.description.abstractWe report on a three-dimensional MHD numerical experiment of a small-scale coronal mass ejection (CME)-like eruption propagating though a nonmagnetized solar atmosphere. We find that the Kelvin–Helmholtz instability (KHI) develops at various but specific locations at the boundary layer between the erupting field and the background atmosphere, depending on the relative angle between the velocity and magnetic field. KHI develops at the front and at two of the four sides of the eruption. KHI is suppressed at the other two sides of the eruption. We also find the development of Alfvénic vortex shedding flows at the wake of the developing CME due to the 3D geometry of the field. Forward modeling reveals that the observational detectability of the KHI in solar eruptions is confined to a narrow ≈10° range when observing off-limb, and therefore its occurrence could be underestimated due to projection effects. The new findings can have significant implications for observations, for heating, and for particle acceleration by turbulence from flow-driven instabilities associated with solar eruptions of all scales.
dc.format.extent7
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Lettersen
dc.rightsCopyright © 2019 American Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.3847/2041-8213/ab44aben
dc.subjectMagnetohydrodynamicsen
dc.subjectSolar activityen
dc.subjectSolar active regionsen
dc.subjectSolar atmosphereen
dc.subjectSolar atmospheric motionsen
dc.subjectSolar coronaen
dc.subjectSolar coronal mass ejectionsen
dc.subjectSolar magnetic flux emergenceen
dc.subjectSolar magnetic fieldsen
dc.subjectMagnetohydrodynamical simulationsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleKelvin–Helmholtz instability and Alfvénic vortex shedding in solar eruptionsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Mathematics and Statisticsen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/2041-8213/ab44ab
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2019ApJ...884L...4Sen


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