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dc.contributor.authorWiegelmann, Thomas
dc.contributor.authorNeukirch, Thomas
dc.contributor.authorNickeler, Dieter
dc.contributor.authorSolanki, Sami
dc.contributor.authorMartinez Pillet, Valentin
dc.contributor.authorBorrero, Juan Manule
dc.date.accessioned2015-12-04T10:40:06Z
dc.date.available2015-12-04T10:40:06Z
dc.date.issued2015-12
dc.identifier.citationWiegelmann , T , Neukirch , T , Nickeler , D , Solanki , S , Martinez Pillet , V & Borrero , J M 2015 , ' Magneto-static modeling of the mixed plasma Beta solar atmosphere based on SUNRISE/IMaX data ' , Astrophysical Journal , vol. 815 , no. 1 , 10 . https://doi.org/10.1088/0004-637X/815/1/10en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 225956812
dc.identifier.otherPURE UUID: 58575b73-dc00-4078-960b-025c395060cc
dc.identifier.otherScopus: 84951269153
dc.identifier.otherORCID: /0000-0002-7597-4980/work/34032281
dc.identifier.otherWOS: 000367105000010
dc.identifier.urihttp://hdl.handle.net/10023/7887
dc.descriptionTN acknowledges support by the U.K.’s Science and Technology Facilities Council and would like to thank the MPS for its hospitality during a visit in December 2014.en
dc.description.abstractOur aim is to model the 3D magnetic field structure of the upper solar atmosphere, including regions of non-negligible plasma beta. We use high-resolution photospheric magnetic field measurements from SUNRISE/IMaX as boundary condition for a magneto-static magnetic field model. The high resolution of IMaX allows us to resolve the interface region between photosphere and corona, but modelling this region is challenging for the following reasons. While the coronal magnetic field is thought to be force-free (the Lorentz-force vanishes), this is not the case in the mixed plasma β environment in the photosphere and lower chromosphere. In our model, pressure gradients and gravity forces are taken self-consistently into account and compensate the non-vanishing Lorentz-force. Above a certain height (about 2 Mm) the non-magnetic forces become very weak and consequently the magnetic field becomes almost force-free. Here we apply a linear approach, where the electric current density consists of a superposition of a field-line parallel current and a current perpendicular to the Sun’s gravity field. We illustrate the prospects and limitations of this approach and give an outlook for an extension towards a non-linear model.
dc.format.extent6
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2015, Publisher / the Author(s). This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at iopscience.iop.org / https://dx.doi.org/10.1088/0004-637X/815/1/10en
dc.subjectMethods: numericalen
dc.subjectSun: chromosphereen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: photosphereen
dc.subjectQB Astronomyen
dc.subjectQA Mathematicsen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQAen
dc.subject.lccQCen
dc.titleMagneto-static modeling of the mixed plasma Beta solar atmosphere based on SUNRISE/IMaX dataen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews.School of Mathematics and Statisticsen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/815/1/10
dc.description.statusPeer revieweden


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