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dc.contributor.authorGunar, Stanislav
dc.contributor.authorMackay, Duncan Hendry
dc.date.accessioned2016-07-25T11:30:08Z
dc.date.available2016-07-25T11:30:08Z
dc.date.issued2016-08
dc.identifier.citationGunar , S & Mackay , D H 2016 , ' Properties of the prominence magnetic field and plasma distributions as obtained from 3D whole-prominence fine structure modeling ' , Astronomy & Astrophysics , vol. 592 , A60 . https://doi.org/10.1051/0004-6361/201527704en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 243133761
dc.identifier.otherPURE UUID: 4b24954f-69c0-4551-b194-4bcf24948335
dc.identifier.otherScopus: 84979992237
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055447
dc.identifier.otherWOS: 000384722600053
dc.identifier.urihttp://hdl.handle.net/10023/9203
dc.description.abstractAims. We analyze distributions of the magnetic field strength and prominence plasma (temperature, pressure, plasma beta, and mass) using the 3D whole-prominence fine structure model. Methods. The model combines a 3D magnetic field configuration of an entire prominence, obtained from non-linear force-free field simulations, with a detailed semi-empirically derived description of the prominence plasma. The plasma is located in magnetic dips in hydrostatic equilibrium and is distributed along multiple fine structures within the 3D magnetic model. Results. We show that in the modeled prominence, the variations of the magnetic field strength and its orientation are insignificant on scales comparable to the smallest dimensions of the observed prominence fine structures. We also show the ability of the 3D whole-prominence fine structure model to reveal the distribution of the prominence plasma, with respect to its temperature within the prominence volume. This provides new insights into the composition of the prominence-corona transition region. We further demonstrate that the values of the plasma beta are small throughout the majority of the modeled prominence when realistic photospheric magnetic flux distributions and prominence plasma parameters are assumed. While this is generally true, we also find that in the region with the deepest magnetic dips, the plasma beta may increase towards unity. Finally, we show that the mass of the modeled prominence plasma is in good agreement with the mass of observed non-eruptive prominences.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2016, ESO. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at www.aanda.org / https://dx.doi.org/10.1051/0004-6361/201527704en
dc.subjectSun: filaments, prominencesen
dc.subjectSun: magnetic fieldsen
dc.subjectPlasmasen
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleProperties of the prominence magnetic field and plasma distributions as obtained from 3D whole-prominence fine structure modelingen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201527704
dc.description.statusPeer revieweden
dc.date.embargoedUntil2017-06-25


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