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dc.contributor.authorJohnston, C. D.
dc.contributor.authorHood, A. W.
dc.contributor.authorCargill, P. J.
dc.contributor.authorDe Moortel, I.
dc.identifier.citationJohnston , C D , Hood , A W , Cargill , P J & De Moortel , I 2017 , ' A new approach for modelling chromospheric evaporation in response to enhanced coronal heating : II. Non-uniform heating ' , Astronomy & Astrophysics , vol. 605 , A8 , pp. 1-14 .
dc.identifier.otherPURE: 249911293
dc.identifier.otherPURE UUID: c135c90f-fd98-4e5f-8486-8d4c60014bce
dc.identifier.otherBibCode: 2017arXiv170504054J
dc.identifier.otherBibCode: 2017arXiv170504054J
dc.identifier.otherBibCode: 2017A&A...605A...8J
dc.identifier.otherWOS: 000412231200097
dc.identifier.otherScopus: 85028598924
dc.identifier.otherORCID: /0000-0002-1452-9330/work/39526509
dc.identifier.otherORCID: /0000-0003-4023-9887/work/36874707
dc.identifier.otherORCID: /0000-0003-2620-2068/work/58055204
dc.descriptionThis project has received funding from the Science and Technology Facilities Council (UK) through the consolidated grant ST/N000609/1 and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No 647214).en
dc.description.abstractWe proposed that the use of an approximate “jump condition” at the solar transition region permits fast and accurate numerical solutions of the one dimensional hydrodynamic equations when the corona undergoes impulsive heating. In particular, it eliminates the need for the very short timesteps imposed by a highly resolved numerical grid. This paper presents further examples of the applicability of the method for cases of non-uniform heating, in particular, nanoflare trains (uniform in space but non-uniform in time) and spatially localised impulsive heating, including at the loop apex and base of the transition region. In all cases the overall behaviour of the coronal density and temperature shows good agreement with a fully resolved one dimensional model and is significantly better than the equivalent results from a 1D code run without using the jump condition but with the same coarse grid. A detailed assessment of the errors introduced by the jump condition is presented showing that the causes of discrepancy with the fully resolved code are (i) the neglect of the terms corresponding to the rate of change of total energy in the unresolved atmosphere; (ii) mass motions at the base of the transition region and (iii) for some cases with footpoint heating, an over-estimation of the radiative losses in the transition region.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2017, ESO. This work has been 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 /
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: chromosphereen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleA new approach for modelling chromospheric evaporation in response to enhanced coronal heating : II. Non-uniform heatingen
dc.typeJournal articleen
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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