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dc.contributor.authorReale, F.
dc.contributor.authorOrlando, S.
dc.contributor.authorGuarrasi, M.
dc.contributor.authorMignone, A.
dc.contributor.authorPeres, G.
dc.contributor.authorHood, A. W.
dc.contributor.authorPriest, E. R.
dc.date.accessioned2016-09-12T11:30:16Z
dc.date.available2016-09-12T11:30:16Z
dc.date.issued2016-10-10
dc.identifier.citationReale , F , Orlando , S , Guarrasi , M , Mignone , A , Peres , G , Hood , A W & Priest , E R 2016 , ' 3D MHD modeling of twisted coronal loops ' , Astrophysical Journal , vol. 830 , no. 1 , 21 . https://doi.org/10.3847/0004-637X/830/1/21en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 244719298
dc.identifier.otherPURE UUID: dec53ba3-c574-4b80-8591-17fa36b5917a
dc.identifier.otherBibCode: 2016arXiv160705500R
dc.identifier.otherScopus: 84991010696
dc.identifier.otherORCID: /0000-0003-2620-2068/work/58055121
dc.identifier.otherWOS: 000385633900004
dc.identifier.otherORCID: /0000-0003-3621-6690/work/74117708
dc.identifier.urihttp://hdl.handle.net/10023/9475
dc.description.abstractWe perform MHD modeling of a single bright coronal loop to include the interaction with a non-uniform magnetic field. The field is stressed by random footpoint rotation in the central region and its energy is dissipated into heating by growing currents through anomalous magnetic diffusivity that switches on in the corona above a current density threshold. We model an entire single magnetic flux tube, in the solar atmosphere extending from the high-beta chromosphere to the low-betacorona through the steep transition region. The magnetic field expands from the chromosphere to the corona. The maximum resolution is ~30 km. We obtain an overall evolution typical of loop models and realistic loop emission in the EUV and X-ray bands. The plasma confined in the fluxtube is heated to active region temperatures (~3 MK) after ~2/3 hr. Upflows from the chromosphere up to ~100 km/s fill the core of the fluxtube to densities above 109 cm-3. More heating is released in the low corona than the high corona and is finely structured both in space and time.
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.103847/0004-637X/830/1/21en
dc.subjectSun: coronaen
dc.subjectSun: activityen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.title3D MHD modeling of twisted coronal loopsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/0004-637X/830/1/21
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2016arXiv160705500Ren


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