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dc.contributor.authorFoullon, Claire
dc.contributor.authorVerwichte, E.
dc.contributor.authorNakariakov, V.M.
dc.date.accessioned2013-08-21T12:14:55Z
dc.date.issued2004-10-25
dc.description.abstractWe report the first detection of long-period (8-27 h) oscillatory intensity variations in a coronal filament. The filament is observed continuously as it crosses the solar disk in a 12-min-cadence SoHO/EIT 195 Å uninterrupted data set. Cyclic intensity variations are found to be correlated along the filament, while the most pronounced oscillations are detected at its southern end for nearly 6 days. The dominant period of these oscillations is 12.1 h and the amplitude of the intensity variations reaches approximately 10% of the background intensity. The ultra-long-period oscillations may be interpreted in terms of slow string MHD modes or may be connected with thermal over-stability associated with peculiarities of the cooling/heating function and with the effect of neutrals. These theoretical predictions however do not explain the spatial structure of the oscillations along the filament.en_GB
dc.identifier.citationVol. 427 (1), pp. L5 - L8en_GB
dc.identifier.doi10.1051/0004-6361:200400083
dc.identifier.urihttp://hdl.handle.net/10871/12661
dc.language.isoenen_GB
dc.publisherEDP Sciencesen_GB
dc.subjectSun: prominencesen_GB
dc.subjectfilamentsen_GB
dc.subjectoscillationsen_GB
dc.subjectUV radiationen_GB
dc.titleDetection of ultra-long-period oscillations in an EUV filamenten_GB
dc.typeArticleen_GB
dc.date.available2013-08-21T12:14:55Z
dc.identifier.issn0004-6361
dc.descriptionCopyright © 2004 ESO / EDP Sciencesen_GB
dc.identifier.eissn1432-0746
dc.identifier.journalAstronomy and Astrophysicsen_GB


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