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A cancellation nanoflare model for solar chromospheric and coronal heating

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dc.contributor.authorPriest, E. R.
dc.contributor.authorChitta, L. P.
dc.contributor.authorSyntelis, P.
dc.date.accessioned2018-08-15T15:30:13Z
dc.date.available2018-08-15T15:30:13Z
dc.date.issued2018-08-01
dc.identifier.citationPriest , E R , Chitta , L P & Syntelis , P 2018 , ' A cancellation nanoflare model for solar chromospheric and coronal heating ' , Astrophysical Journal Letters , vol. 862 , no. 2 , L24 . https://doi.org/10.3847/2041-8213/aad4fcen
dc.identifier.issn2041-8205
dc.identifier.otherPURE: 255392376
dc.identifier.otherPURE UUID: 214dbde2-6c88-48a4-8f04-305c73d38c7e
dc.identifier.otherBibCode: 2018ApJ...862L..24P
dc.identifier.otherScopus: 85051544518
dc.identifier.otherWOS: 000440575200004
dc.identifier.otherORCID: /0000-0003-3621-6690/work/74117761
dc.identifier.otherORCID: /0000-0002-6377-0243/work/77131791
dc.identifier.urihttps://hdl.handle.net/10023/15826
dc.descriptionL.P.C. received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 707837. The German contribution to SUNRISE and its reflight was funded by the Max Planck Foundation, the Strategic Innovations Fund of the President of the Max Planck Society (MPG), DLR, and private donations by supporting members of the Max Planck Society. The Spanish contribution was funded by the Ministerio de Economía y Competitividad under Projects ESP2013-47349-C6 and ESP2014-56169-C6, partially using European FEDER funds.en
dc.description.abstractNanoflare models for heating the solar corona usually assume magnetic braiding and reconnection as the source of the energy. However, recent observations at record spatial resolution from the SUNRISE balloon mission suggest that photospheric magnetic flux cancellation is much more common than previously realized. We therefore examine the possibility of three-dimensional reconnection driven by flux cancellation as a cause of chromospheric and coronal heating. In particular, we estimate how the heights and amount of energy release produced by flux cancellation depend on flux size, flux cancellation speed, and overlying field strength.
dc.format.extent7
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Lettersen
dc.rights© 2018. 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://doi.org/10.3847/2041-8213/aad4fcen
dc.subjectMagnetohydrodynamics: MHDen
dc.subjectMagnetic reconnectionen
dc.subjectSun: atmosphereen
dc.subjectSun: chromosphereen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleA cancellation nanoflare model for solar chromospheric and coronal heatingen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/2041-8213/aad4fc
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1807.08161en


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