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dc.contributor.authorGunar, Stanislav
dc.contributor.authorMackay, Duncan Hendry
dc.contributor.authorAnzer, U
dc.contributor.authorHeinzel, Petr
dc.date.accessioned2014-09-23T12:01:04Z
dc.date.available2014-09-23T12:01:04Z
dc.date.issued2013-03
dc.identifier.citationGunar , S , Mackay , D H , Anzer , U & Heinzel , P 2013 , ' Non-linear force-free magnetic dip models of quiescent prominence fine structures ' , Astronomy & Astrophysics , vol. 551 , A3 . https://doi.org/10.1051/0004-6361/201220597en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 102600518
dc.identifier.otherPURE UUID: edd8de1d-89c0-4003-aac2-cd1552ca5e00
dc.identifier.otherScopus: 84873690674
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055422
dc.identifier.urihttp://hdl.handle.net/10023/5476
dc.descriptionS.G. and P.H. acknowledge the support from grant 209/12/0906 of the Grant Agency of the Czech Republic. P.H. acknowledges the support from grant P209/10/1680 of the Grant Agency of the Czech Republic. S.G. and P.H. acknowledge the support from the MPA Garching; U.A. thanks for support from the Ondřejov Observatory. S.G. acknowledges the support from St Andrews University. Work of S.G. and P.H. was supported by the project RVO: 67985815. DHM acknowledges financial support from the STFC and the Leverhulme Trust. In addition research leading to these results has received funding from the European Commission’s Seventh Framework Programme (FP7/2007-2013) under the grant agreement SWIFF (project N° 263340, http://www.swiff.eu).en
dc.description.abstractAims. We use 3D non-linear force-free magnetic field modeling of prominence/filament magnetic fields to develop the first 2D models of individual prominence fine structures based on the 3D configuration of the magnetic field of the whole prominence. Methods. We use an iterative technique to fill the magnetic dips produced by the 3D modeling with realistic prominence plasma in hydrostatic equilibrium and with a temperature structure that contains the prominence-corona transition region. With this well-defined plasma structure the radiative transfer can be treated in detail in 2D and the resulting synthetic emission can be compared with prominence/filament observations. Results. Newly developed non-linear force-free magnetic dip models are able to produce synthetic hydrogen Lyman spectra in a qualitative agreement with a range of quiescent prominence observations. Moreover, the plasma structure of these models agrees with the gravity induced prominence fine structure models which have already been shown to produce synthetic spectra in good qualitative agreement with several observed prominences. Conclusions. We describe in detail the iterative technique which can be used to produce realistic plasma models of prominence fine structures located in prominence magnetic field configurations containing dips, obtained using any kind of magnetic field modeling.
dc.format.extent9
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2013. Reproduced with permission from Astronomy & Astrophysics, © ESOen
dc.subjectSun: filaments, prominencesen
dc.subjectMagnetic fieldsen
dc.subjectRadiative transferen
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleNon-linear force-free magnetic dip models of quiescent prominence fine structuresen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201220597
dc.description.statusPeer revieweden


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