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dc.contributor.authorSyntelis, P.
dc.contributor.authorPriest, E. R.
dc.date.accessioned2020-03-20T13:30:01Z
dc.date.available2020-03-20T13:30:01Z
dc.date.issued2020-03-03
dc.identifier.citationSyntelis , P & Priest , E R 2020 , ' A cancellation nanoflare model for solar chromospheric and coronal heating. III. 3D simulations and atmospheric response ' , Astrophysical Journal , vol. 891 , no. 1 , 52 . https://doi.org/10.3847/1538-4357/ab6ffcen
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 266968518
dc.identifier.otherPURE UUID: a04adfd8-ec2f-4a33-88ad-26a7fe61d1d4
dc.identifier.otherWOS: 000519058200001
dc.identifier.otherORCID: /0000-0003-3621-6690/work/74117709
dc.identifier.otherScopus: 85083917825
dc.identifier.otherORCID: /0000-0002-6377-0243/work/77131781
dc.identifier.urihttp://hdl.handle.net/10023/19686
dc.descriptionThis research has made use of NASA's Astrophysics Data System. This work was supported by computational time granted from the Greek Research and Technology Network (GRNET) in the National HPC facility ARIS. P.S. acknowledges support by the ERC synergy grant "The Whole Sun."en
dc.description.abstractInspired by recent observations suggesting that photospheric magnetic flux cancellation occurs much more frequently than previously thought, we analytically estimated the energy released from reconnection driven by photospheric flux cancellation, and propose that it can act as a mechanism for chromospheric and coronal heating. Using two-dimensional simulations we validated the analytical estimates and studied the resulting atmospheric response. In the present work, we set up 3D resistive MHD simulations of two canceling polarities in a stratified atmosphere with a horizontal external field to further validate and improve upon the analytical estimates. The computational evaluation of the parameters associated with the energy release are in good qualitative agreement with the analytical estimates. The computational Poynting energy flux into the current sheet is in good qualitative agreement with the analytical estimates, after correcting the analytical expression to better account for the horizontal extent of the current sheet. The atmospheric response to the cancellation is the formation of hot ejections, cool ejections, or a combination of both hot and cool ejections, which can appear with a time difference and/or be spatially offset, depending on the properties of the canceling region and the resulting height of the reconnection. Therefore, during the cancellation, a wide spectrum of ejections can be formed, which can account for the variety of multi-thermal ejections associated with Ellerman bombs, UV bursts, and IRIS bombs, and also other ejections associated with small-scale canceling regions and spicules.
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rightsCopyright © 2020. The American Astronomical Society. All rights reserved. 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 final published version of the work, which was originally published at https://doi.org/10.3847/1538-4357/ab6ffcen
dc.subjectSolar coronal heatingen
dc.subjectMagnetohydrodynamicsen
dc.subjectSolar magnetic reconnectionen
dc.subjectSolar activityen
dc.subjectMagnetic fieldsen
dc.subjectMagnetohydrodynamical simulationsen
dc.subjectSolar coronal transientsen
dc.subjectQB Astronomyen
dc.subjectQA Mathematicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQAen
dc.titleA cancellation nanoflare model for solar chromospheric and coronal heating. III. 3D simulations and atmospheric responseen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ab6ffc
dc.description.statusPeer revieweden


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