Show simple item record

Files in this item


Item metadata

dc.contributor.authorAntolin, Patrick
dc.contributor.authorPagano, Paolo
dc.contributor.authorDe Moortel, Ineke
dc.contributor.authorNakariakov, Valery M.
dc.identifier.citationAntolin , P , Pagano , P , De Moortel , I & Nakariakov , V M 2018 , ' In situ generation of transverse magnetohydrodynamic waves from colliding flows in the solar corona ' , Astrophysical Journal Letters , vol. 861 , no. 2 , L15 .
dc.identifier.otherPURE: 253603983
dc.identifier.otherPURE UUID: 8437de60-b623-4f3b-8fc5-70d3d63e1d1c
dc.identifier.otherBibCode: 2018arXiv180700395A
dc.identifier.otherScopus: 85049958899
dc.identifier.otherORCID: /0000-0002-1452-9330/work/46362063
dc.identifier.otherWOS: 000438213900002
dc.descriptionThis research has received funding from the UK Science and Technology Facilities Council (Consolidated Grant ST/K000950/1) and the European Union Horizon 2020 Research and Innovation Programme (grant agreement No. 647214). V.M.N. acknowledges the support of the BK21 plus program through the National Research Foundation funded by the Ministry of Education of Korea.en
dc.description.abstractTransverse magnetohydrodynamic (MHD) waves permeate the solar atmosphere and are a candidate for coronal heating. However, the origin of these waves is still unclear. In this Letter, we analyze coordinated observations from Hinode/Solar Optical Telescope (SOT) and Interface Region Imaging Spectrograph (IRIS) of a prominence/coronal rain loop-like structure at the limb of the Sun. Cool and dense downflows and upflows are observed along the structure. A collision between a downward and an upward flow with an estimated energy flux of 107–108 erg cm−2 s−1 is observed to generate oscillatory transverse perturbations of the strands with an estimated ≈40 km s−1 total amplitude, and a short-lived brightening event with the plasma temperature increasing to at least 105 K. We interpret this response as sausage and kink transverse MHD waves based on 2D MHD simulations of plasma flow collision. The lengths, density, and velocity differences between the colliding clumps and the strength of the magnetic field are major parameters defining the response to the collision. The presence of asymmetry between the clumps (angle of impact surface and/or offset of flowing axis) is crucial for generating a kink mode. Using the observed values, we successfully reproduce the observed transverse perturbations and brightening, and show adiabatic heating to coronal temperatures. The numerical modeling indicates that the plasma β in this loop-like structure is confined between 0.09 and 0.36. These results suggest that such collisions from counter-streaming flows can be a source of in situ transverse MHD waves, and that for cool and dense prominence conditions such waves could have significant amplitudes.
dc.relation.ispartofAstrophysical Journal Lettersen
dc.rights© 2018. 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:
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: activityen
dc.subjectSun: filaments, prominencesen
dc.subjectSun: oscillationsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleIn situ generation of transverse magnetohydrodynamic waves from colliding flows in the solar coronaen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEuropean Research Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.description.statusPeer revieweden

This item appears in the following Collection(s)

Show simple item record