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dc.contributor.authorReid, Jack
dc.contributor.authorCargill, Peter
dc.contributor.authorJohnston, Craig David
dc.contributor.authorHood, Alan William
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 .
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.otherWOS: 000671481700072
dc.identifier.otherScopus: 85128565131
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--1015m−3 for a coronal loop length of 80Mm⁠. 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.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (, which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.en
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleLinking computational models to follow the evolution of heated coronal plasmaen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Research Councilen
dc.contributor.sponsorEuropean Research Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.description.statusPeer revieweden

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