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dc.contributor.authorJess, David
dc.contributor.authorReznikova, V
dc.contributor.authorVan Doorsselaere, Tom
dc.contributor.authorMackay, Duncan Hendry
dc.contributor.authorKeys, Peter
dc.date.accessioned2014-08-14T11:31:03Z
dc.date.available2014-08-14T11:31:03Z
dc.date.issued2013-12-03
dc.identifier.citationJess , D , Reznikova , V , Van Doorsselaere , T , Mackay , D H & Keys , P 2013 , ' The influence of the magnetic field on running penumbral waves in the solar chromosphere ' , Astrophysical Journal , vol. 779 , no. 2 , 168 . https://doi.org/10.1088/0004-637X/779/2/168en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 102317173
dc.identifier.otherPURE UUID: 5e2de3c0-de35-4ce3-94ec-7715eb804553
dc.identifier.otherScopus: 84889771957
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055449
dc.identifier.urihttps://hdl.handle.net/10023/5155
dc.descriptionD.B.J. acknowledges the European Commission and the Fonds Wetenschappelijk Onderzoek (FWO) for the award of a Marie Curie Pegasus Fellowship during which this work was initiated, in addition to the UK Science and Technology Facilities Council (STFC) for the award of an Ernest Rutherford Fellowship which allowed the completion of this project. The research carried out by V.E.R. is partly supported by grant MC FP7-PEOPLE-2011-IRSES-295272. T.V.D. acknowledges funding from the Odysseus Programme of the FWO Vlaanderen and from the EU's 7th Framework Programme as an ERG with grant number 276808. P.H.K. and D.H.M. are grateful to STFC for research support. This research has been funded by the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office (IAP P7/08 CHARM).en
dc.description.abstractWe use images of high spatial and temporal resolution, obtained using both ground- and space-based instrumentation, to investigate the role magnetic field inclination angles play in the propagation characteristics of running penumbral waves in the solar chromosphere. Analysis of a near-circular sunspot, close to the center of the solar disk, reveals a smooth rise in oscillatory period as a function of distance from the umbral barycenter. However, in one directional quadrant, corresponding to the north direction, a pronounced kink in the period-distance diagram is found. Utilizing a combination of the inversion of magnetic Stokes vectors and force-free field extrapolations, we attribute this behavior to the cut-off frequency imposed by the magnetic field geometry in this location. A rapid, localized inclination of the magnetic field lines in the north direction results in a faster increase in the dominant periodicity due to an accelerated reduction in the cut-off frequency. For the first time, we reveal how the spatial distribution of dominant wave periods, obtained with one of the highest resolution solar instruments currently available, directly reflects the magnetic geometry of the underlying sunspot, thus opening up a wealth of possibilities in future magnetohydrodynamic seismology studies. In addition, the intrinsic relationships we find between the underlying magnetic field geometries connecting the photosphere to the chromosphere, and the characteristics of running penumbral waves observed in the upper chromosphere, directly supports the interpretation that running penumbral wave phenomena are the chromospheric signature of upwardly propagating magneto-acoustic waves generated in the photosphere.
dc.format.extent11
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2013. The American Astronomical Society. All rights reserved.en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectMethods: numericalen
dc.subjectSun: atmosphereen
dc.subjectSun: chromosphereen
dc.subjectSun: oscillationsen
dc.subjectSun: photosphereen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleThe influence of the magnetic field on running penumbral waves in the solar chromosphereen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/779/2/168
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/K000950/1en


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