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dc.contributor.authorReid, Jack
dc.contributor.authorCargill, Peter
dc.contributor.authorJohnston, Craig David
dc.contributor.authorHood, Alan William
dc.date.accessioned2021-05-28T15:30:16Z
dc.date.available2021-05-28T15:30:16Z
dc.date.issued2021-08
dc.identifier.citationReid , J , Cargill , P , Johnston , C D & Hood , A W 2021 , ' Linking computational models to follow the evolution of heated coronal plasma ' , Monthly Notices of the Royal Astronomical Society , vol. 505 , no. 3 , pp. 4141-4150 . https://doi.org/10.1093/mnras/stab1255en
dc.identifier.issn1365-2966
dc.identifier.otherPURE: 273991815
dc.identifier.otherPURE UUID: e4f7d7cb-bca9-4843-9d20-210f878d8cf5
dc.identifier.otherORCID: /0000-0003-2620-2068/work/96140927
dc.identifier.otherORCID: /0000-0003-4023-9887/work/96141422
dc.identifier.urihttp://hdl.handle.net/10023/23271
dc.descriptionFunding: JR acknowledges the support of the Carnegie Trust for the Universities of Scotland. JR and AWH acknowledge the financial support of STFC through the Consolidated grant, ST/S000402/1, to the University of St Andrews. AWH acknowledges support from ERC Synergy grant ‘The Whole Sun’ (810218). CDJ acknowledges funding from the European Research Council (ERC) under grant agreement No. 647214.en
dc.description.abstractA ‘proof of principle’ is presented, whereby the Ohmic and viscous heating determined by a three-dimensional (3D) MHD model of a coronal avalanche are used as the coronal heating input for a series of field-aligned, one-dimensional (1D) hydrodynamic models. Three-dimensional coronal MHD models require large computational resources. For current numerical parameters, it is difficult to model both the magnetic field evolution and the energy transport along field lines for coronal temperatures much hotter than 1MK, because of severe constraints on the time step from parallel thermal conduction. Using the 3D MHD heating derived from a simulation and evaluated on a single field line, the 1D models give coronal temperatures of 1MK and densities 1014–1015 m−3 for a coronal loop length of 80 Mm. While the temperatures and densities vary smoothly along the field lines, the heating function leads to strong asymmetries in the plasma flows. The magnitudes of the velocities in the 1D model are comparable with those seen in 3D reconnection jets in our earlier work. Advantages and drawbacks of this approach for coronal modelling are discussed.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2021 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/stab1255.en
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleLinking computational models to follow the evolution of heated coronal plasmaen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews.School of Mathematics and Statisticsen
dc.identifier.doihttps://doi.org/10.1093/mnras/stab1255
dc.description.statusPeer revieweden


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