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dc.contributor.authorGalsgaard, Klaus
dc.contributor.authorMadjarska, Maria
dc.contributor.authorMackay, Duncan H.
dc.contributor.authorMou, Chaozhou
dc.date.accessioned2019-02-07T14:30:04Z
dc.date.available2019-02-07T14:30:04Z
dc.date.issued2019-03
dc.identifier.citationGalsgaard , K , Madjarska , M , Mackay , D H & Mou , C 2019 , ' Eruptions from quiet Sun coronal bright points : II. Non-potential modelling ' Astronomy & Astrophysics , vol. 623 , A78 . https://doi.org/10.1051/0004-6361/201834329en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 257662497
dc.identifier.otherPURE UUID: 3404d334-844b-40a1-afe4-91ff25b4403e
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055426
dc.identifier.otherScopus: 85062711004
dc.identifier.urihttp://hdl.handle.net/10023/17015
dc.descriptionSupport for VAPOR is provided by the U.S. National Science Foundation (grants # 03-25934 and 09-06379, ACI-14-40412), and by the Korea Institute of Science and Technology Information. C. M. thanks the National Natural Science Foundation of China (41474150). The HMI data are provided courtesy of NASA/SDO and corresponding science teams. The HMI data have been retrieved using the Stanford University’s Joint Science Operations Centre/Science Data Processing Facility. M.M. and K.G. thank the ISSI Bern for the support to the team “Observation-Driven Modelling of Solar Phenomena”.en
dc.description.abstractContext. Our recent observational study shows that the majority of coronal bright points (CBPs) in the quiet Sun are sources of one or more eruptions during their lifetime. Aims. Here, we investigate the non-potential time-dependent structure of the magnetic field of the CBP regions with special emphasison the time-evolving magnetic structure at the spatial locations where the eruptions are initiated. Methods. The magnetic structure is evolved in time using a non-linear force-free field (NLFFF) relaxation approach based on a timeseries of helioseismic and magnetic imager (HMI) longitudinal magnetograms. This results in a continuous time series of NLFFFs.The time series is initiated with a potential field extrapolation based on a magnetogram taken well before the time of the eruptions. This initial field is then evolved in time in response to the observed changes in the magnetic field distribution at the photosphere. The local and global magnetic field structures from the time series of NLFFF field solutions are analysed in the vicinity of the eruption sites at the approximate times of the eruptions. Results. The analysis shows that many of the CBP eruptions reported in a recent publication contain twisted flux tube located atthe sites of eruptions. The presence of flux ropes at these locations provides in many cases a direct link between the magnetic field structure, their eruption, and the observation of mini coronal mass ejections (mini-CMEs). It is found that all repetitive eruptions are homologous. Conclusions. The NLFFF simulations show that twisted magnetic field structures are created at the locations hosting eruptions inCBPs. These twisted structures are produced by footpoint motions imposed by changes in the photospheric magnetic field observations.The true nature of the micro-flares remains unknown. Further 3D data-driven magnetohydrodynamic modelling is required to show how these twisted regions become unstable and erupt.
dc.format.extent16
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2019, ESO. This work has been 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/10.1051/0004-6361/201834329en
dc.subjectMethods: observational, numericalen
dc.subjectSun: eruptions, magnetic fieldsen
dc.subjectTechniques: NLFFF relaxationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleEruptions from quiet Sun coronal bright points : II. Non-potential modellingen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201834329
dc.description.statusPeer revieweden


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