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dc.contributor.authorDe Moortel, I.
dc.contributor.authorAntolin, Patrick
dc.contributor.authorVan Doorsselaere, T.
dc.identifier.citationDe Moortel , I , Antolin , P & Van Doorsselaere , T 2015 , ' Observational signatures of waves and flows in the solar corona ' , Solar Physics , vol. 290 , no. 2 , pp. 399-421 .
dc.identifier.otherPURE: 163380759
dc.identifier.otherPURE UUID: dbd5a945-2d95-4756-88d8-828e58b023d2
dc.identifier.otherBibtex: urn:951357990a72a9ca5965737cb3861d3b
dc.identifier.otherWOS: 000346644000008
dc.identifier.otherScopus: 84927662989
dc.identifier.otherORCID: /0000-0002-1452-9330/work/39526491
dc.descriptionDM acknowledges support of a Royal Society University Research Fellowship and a KU Leuven Research Council senior research fellowship (SF/12/008). The research leading to these results has also received funding from the European Commission Seventh Framework Programme (FP7/2007-2013) under the grant agreement SOLSPANET (project No. 269299, ). TVD has been sponsored by an Odysseus grant of the FWO Vlaanderen. The research was performed in the context of the IAP P7/08 CHARM (Belspo) and the GOA-2015-014 (KU Leuven). TVD acknowledges the funding from the FP7 ERG grant with number 276808.en
dc.description.abstractPropagating perturbations have been observed in extended coronal loop structures for a number of years, but the interpretation in terms of slow (propagating) magneto-acoustic waves and/or as quasi-periodic upflows remains unresolved. We used forward-modelling to construct observational signatures associated with a simple slow magneto-acoustic wave or periodic flow model. Observational signatures were computed for the 171 Å Fe ix and the 193 Å Fe xii spectral lines. Although there are many differences between the flow and wave models, we did not find any clear, robust observational characteristics that can be used in isolation (i.e. that do not rely on a comparison between the models). For the waves model, a relatively rapid change of the average line widths as a function of (shallow) line-of-sight angles was found, whereas the ratio of the line width amplitudes to the Doppler velocity amplitudes is relatively high for the flow model. The most robust observational signature found is that the ratio of the mean to the amplitudes of the Doppler velocity is always higher than one for the flow model. This ratio is substantially higher for flows than for waves, and for the flows model used in the study is exactly the same in the 171 Å Fe ix and the 193 Å Fe xii spectral lines. However, these potential observational signatures need to be treated cautiously because they are likely to be model-dependent.
dc.relation.ispartofSolar Physicsen
dc.rightsCopyright © 2015, Springer Science+Business Media Dordrecht. This work is 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
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: coronaen
dc.subjectQA Mathematicsen
dc.subjectQC Physicsen
dc.titleObservational signatures of waves and flows in the solar coronaen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Commissionen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews. School of Managementen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.description.statusPeer revieweden

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