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dc.contributor.authorHansteen, V. H.
dc.contributor.authorArchontis, V.
dc.contributor.authorPereira, T. M. D.
dc.contributor.authorCarlsson, M.
dc.contributor.authorRouppe van der Voort, L.
dc.contributor.authorLeenaarts, J.
dc.date.accessioned2017-05-10T13:30:09Z
dc.date.available2017-05-10T13:30:09Z
dc.date.issued2017-04-10
dc.identifier.citationHansteen , V H , Archontis , V , Pereira , T M D , Carlsson , M , Rouppe van der Voort , L & Leenaarts , J 2017 , ' Bombs and flares at the surface and lower atmosphere of the Sun ' , Astrophysical Journal , vol. 839 , no. 1 , 22 . https://doi.org/10.3847/1538-4357/aa6844en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 249965413
dc.identifier.otherPURE UUID: 8f02a2bd-5721-4adc-97a5-402d60fcfb2e
dc.identifier.otherScopus: 85018516621
dc.identifier.otherWOS: 000399251000007
dc.identifier.otherORCID: /0000-0002-6926-8676/work/73700854
dc.identifier.urihttps://hdl.handle.net/10023/10741
dc.descriptionThis research was supported by the Research Council of Norway and by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007–2013)/ERC Grant agreement no. 291058.en
dc.description.abstractA spectacular manifestation of solar activity is the appearance of transient brightenings in the far wings of the Hα line, known as Ellerman bombs (EBs). Recent observations obtained by the Interface Region Imaging Spectrograph have revealed another type of plasma "bombs" (UV bursts) with high temperatures of perhaps up to 8 × 104 K within the cooler lower solar atmosphere. Realistic numerical modeling showing such events is needed to explain their nature. Here, we report on 3D radiative magnetohydrodynamic simulations of magnetic flux emergence in the solar atmosphere. We find that ubiquitous reconnection between emerging bipolar magnetic fields can trigger EBs in the photosphere, UV bursts in the mid/low chromosphere and small (nano-/micro-) flares (106 K) in the upper chromosphere. These results provide new insights into the emergence and build up of the coronal magnetic field and the dynamics and heating of the solar surface and lower atmosphere.
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2017. 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/10.3847/1538-4357/aa6844en
dc.subjectSun: activityen
dc.subjectSun: atmosphereen
dc.subjectSun: chromosphereen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: photosphereen
dc.subjectSun: UV radiationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectAstronomy and Astrophysicsen
dc.subjectNDASen
dc.subjectBDCen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleBombs and flares at the surface and lower atmosphere of the Sunen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aa6844
dc.description.statusPeer revieweden


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