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dc.contributor.authorMadjarska, Maria
dc.contributor.authorGalsgaard, Klaus
dc.contributor.authorMackay, Duncan Hendry
dc.contributor.authorKoleva, Kostadinka
dc.contributor.authorDechev, Momchil
dc.date.accessioned2020-09-14T12:30:02Z
dc.date.available2020-09-14T12:30:02Z
dc.date.issued2020-11
dc.identifier.citationMadjarska , M , Galsgaard , K , Mackay , D H , Koleva , K & Dechev , M 2020 , ' Eruptions from coronal hole bright points : observations and non-potential modeling ' , Astronomy & Astrophysics , vol. 643 , A19 . https://doi.org/10.1051/0004-6361/202038287en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 267666027
dc.identifier.otherPURE UUID: 03add8c4-bd44-4262-b3bb-a27ebb7692c1
dc.identifier.otherORCID: /0000-0001-6065-8531/work/82788590
dc.identifier.otherScopus: 85095112073
dc.identifier.otherWOS: 000588070500019
dc.identifier.urihttp://hdl.handle.net/10023/20619
dc.descriptionFunding: DHM would like to thank the Science and Technology Facilities Council (UK) through the consolidated grant ST/N000609/1 and the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 647214).en
dc.description.abstractContext. We report on the third part of a series of studies on eruptions associated with small-scale loop complexes named coronal bright points (CBPs). Aims. A single case study of a CBP in an equatorial coronal hole with an exceptionally large size is investigated to extend our understanding of the formation of mini-filaments (MFs), their destabilisation and the origin of the eruption triggering the formation of jet-like features recorded in the extreme-ultraviolet (EUV) and X-ray emission. We aim to explore the nature of the so called micro-flares in CBPs associated with jets in coronal holes and mini coronal mass ejections in the quiet Sun. Methods. Co-observations from the Atmospheric Imaging Assembly (AIA) and Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO), and GONG Halpha images are used together with a Non-Linear Force Free Field (NLFFF) relaxation approach, where the latter is based on a time series of HMI line-of-sight magnetograms. Results. A mini-filament (MF) that formed beneath the CBP arcade around 3–4 h before the eruption is seen in the Halpha and EUV AIA images to lift up and erupt triggering the formation of an X-ray jet. No significant photospheric magnetic flux concentration displacement (convergence) is observed and neither is magnetic flux cancellation between the two main magnetic polarities forming the CBP in the time period leading to the MF liftoff. The CBP micro-flare is associated with three flare kernels that formed shortly after the MF liftoff. No observational signature is found for reconnection beneath the erupting MF. The applied NLFFF modeling successfully reproduces both the CBP loop complex as well as the magnetic flux rope that hosts the MF. Conclusions. The applied NLFFF modellng is able to clearly show that an initial potential field can be evolved into a non-potential magnetic field configuration that contains free magnetic energy in the region that observationally hosts the eruption. The comparison of the magnetic field structure shows that the magnetic NLFFF model contains many of the features that can explain the dfferent observational signatures found in the evolution and eruption of the CBP. In future it may eventually indicate the location of destabilisation that results in the eruptions of flux ropes.
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © M. S. Madjarska 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.subjectSun: chromosphereen
dc.subjectSun: coronaen
dc.subjectSun: activityen
dc.subjectSun: filamentsen
dc.subjectSun: magnetic fieldsen
dc.subjectMethods: observational, theoreticalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleEruptions from coronal hole bright points : observations and non-potential modelingen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202038287
dc.description.statusPeer revieweden


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