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dc.contributor.authorChitta, L. P.
dc.contributor.authorPeter, H.
dc.contributor.authorPriest, E. R.
dc.contributor.authorSolanki, S. K.
dc.date.accessioned2021-01-06T13:30:02Z
dc.date.available2021-01-06T13:30:02Z
dc.date.issued2020-12
dc.identifier.citationChitta , L P , Peter , H , Priest , E R & Solanki , S K 2020 , ' Impulsive coronal heating during the interaction of surface magnetic fields in the lower solar atmosphere ' , Astronomy & Astrophysics , vol. 644 , A130 . https://doi.org/10.1051/0004-6361/202039099en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 272117097
dc.identifier.otherPURE UUID: da37dddc-b21e-40f9-bbb7-823f0a939061
dc.identifier.otherBibtex: ISI:000599930900001
dc.identifier.otherScopus: 85097879912
dc.identifier.otherORCID: /0000-0003-3621-6690/work/86537310
dc.identifier.otherWOS: 000599930900001
dc.identifier.urihttp://hdl.handle.net/10023/21226
dc.descriptionThis project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 695075) and has been supported by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea. Open Access funding provided by Max Planck Society.en
dc.description.abstractCoronal plasma in the cores of solar active regions is impulsively heated to more than 5 MK. The nature and location of the magnetic energy source responsible for such impulsive heating is poorly understood. Using observations of seven active regions from the Solar Dynamics Observatory, we found that a majority of coronal loops hosting hot plasma have at least one footpoint rooted in regions of interacting mixed magnetic polarity at the solar surface. In cases when co-temporal observations from the Interface Region Imaging Spectrograph space mission are available, we found spectroscopic evidence for magnetic reconnection at the base of the hot coronal loops. Our analysis suggests that interactions of magnetic patches of opposite polarity at the solar surface and the associated energy release during reconnection are key to impulsive coronal heating.
dc.format.extent29
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © L. P. Chitta et al. 2020. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.en
dc.subjectMagnetic reconnectionen
dc.subjectSun: chromosphereen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectSun: transition regionen
dc.subjectSun: flaresen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleImpulsive coronal heating during the interaction of surface magnetic fields in the lower solar atmosphereen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202039099
dc.description.statusPeer revieweden


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