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dc.contributor.authorWiegelmann, Thomas
dc.contributor.authorNeukirch, Thomas
dc.contributor.authorNickeler, Dieter
dc.contributor.authorChifu, Iulia
dc.date.accessioned2020-11-10T17:30:10Z
dc.date.available2020-11-10T17:30:10Z
dc.date.issued2020-10-29
dc.identifier.citationWiegelmann , T , Neukirch , T , Nickeler , D & Chifu , I 2020 , ' An optimization principle for computing stationary MHD equilibria with solar wind flow ' , Solar Physics , vol. 295 , 145 . https://doi.org/10.1007/s11207-020-01719-8en
dc.identifier.issn0038-0938
dc.identifier.otherPURE: 270518517
dc.identifier.otherPURE UUID: 9a53bddf-2f4a-4466-b86f-faec1751e3fe
dc.identifier.otherORCID: /0000-0002-7597-4980/work/83481718
dc.identifier.otherScopus: 85094652525
dc.identifier.urihttp://hdl.handle.net/10023/20942
dc.descriptionTW acknowledges financial support by DLR-grant 50 OC 1701 and DFG-grant WI 3211/5-1. TN acknowledges financial support by the UK’s Science and Technology Facilities Council (STFC) via Consolidated Grant ST/S000402/1. The Astronomical Institute of the Czech Academy of Sciences is supported by the project RVO:67985815. IC acknowledges funding by DFG-grant WI 3211/5-1.en
dc.description.abstractIn this work we describe a numerical optimization method for computing stationary MHD-equilibria. The newly developed code is based on a nonlinearforce-free optimization principle. We apply our code to model the solar corona using synoptic vector magnetograms as boundary condition. Below about two solar radii the plasma β and Alfvén Mach number MA are small and the magnetic field configuration of stationary MHD is basically identical to a nonlinear force-free field, whereas higher up in the corona (where β and MA are above unity) plasma and flow effects become important and stationary MHD and force-free configuration deviate significantly. The new method allows the reconstruction of the coronal magnetic field further outwards than with potential field, nonlinear force-free or magneto-static models. This way the model might help to provide the magnetic connectivity for joint observations of remote sensing and in-situ instruments on Solar Orbiter and Parker Solar Probe.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofSolar Physicsen
dc.rightsCopyright © The Author(s) 2020. This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.en
dc.subjectMagnetic fields, coronaen
dc.subjectMagnetic fields, modelsen
dc.subjectMagnetohydrodynamicsen
dc.subjectVelocity fields, solar winden
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleAn optimization principle for computing stationary MHD equilibria with solar wind flowen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1007/s11207-020-01719-8
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2010.02945en


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