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dc.contributor.authorVerwichte, E.
dc.contributor.authorMarsh, M.
dc.contributor.authorFoullon, Claire
dc.contributor.authorVan Doorsselaere, T.
dc.contributor.authorDe Moortel, I.
dc.contributor.authorHood, A.W.
dc.contributor.authorNakariakov, V.M.
dc.date.accessioned2013-08-22T09:25:48Z
dc.date.issued2010-11-10
dc.description.abstractRecent spectral observations of upward moving quasi-periodic intensity perturbations in solar coronal structures have shown evidence of periodic line asymmetries near their footpoints. These observations challenge the established interpretation of the intensity perturbations in terms of propagating slow magnetoacoustic waves. We show that slow waves inherently have a bias toward enhancement of emission in the blue wing of the emission line due to in-phase behavior of velocity and density perturbations. We demonstrate that slow waves cause line asymmetries when the emission line is averaged over an oscillation period or when a quasi-static plasma component in the line of sight is included. Therefore, we conclude that slow magnetoacoustic waves remain a valid explanation for the observed quasi-periodic intensity perturbations.en_GB
dc.identifier.citationVol. 724 (2), pp. L194 - L198en_GB
dc.identifier.doi10.1088/2041-8205/724/2/L194
dc.identifier.urihttp://hdl.handle.net/10871/12824
dc.language.isoenen_GB
dc.publisherAmerican Astronomical Society / IOP Publishingen_GB
dc.subjectline: formationen_GB
dc.subjectmagnetohydrodynamics (MHD)en_GB
dc.subjectSun: coronaen_GB
dc.subjectSun: oscillationsen_GB
dc.titlePeriodic spectral line asymmetries in solar coronal structures from slow magnetoacoustic wavesen_GB
dc.typeArticleen_GB
dc.date.available2013-08-22T09:25:48Z
dc.identifier.issn2041-8205
dc.description© 2010 American Astronomical Society / IOP Publishingen_GB
dc.identifier.eissn2041-8213
dc.identifier.journalAstrophysical Journal Lettersen_GB


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