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dc.contributor.authorArchontis, Vasilis
dc.contributor.authorHood, Alan William
dc.date.accessioned2014-01-16T11:01:01Z
dc.date.available2014-01-16T11:01:01Z
dc.date.issued2010-05
dc.identifier.citationArchontis , V & Hood , A W 2010 , ' Flux emergence and coronal eruption ' , Astronomy & Astrophysics , vol. 514 , A56 . https://doi.org/10.1051/0004-6361/200913502en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 481348
dc.identifier.otherPURE UUID: d04a9f7a-a5c7-47a7-902c-06b21bc0f9e3
dc.identifier.otherstandrews_research_output: 32667
dc.identifier.otherScopus: 77952665884
dc.identifier.otherORCID: /0000-0003-2620-2068/work/58055225
dc.identifier.otherORCID: /0000-0002-6926-8676/work/73700882
dc.identifier.urihttp://hdl.handle.net/10023/4376
dc.description.abstractAims. Our aim is to study the photospheric flux distribution of a twisted flux tube that emerges from the solar interior. We also report on the eruption of a new flux rope when the emerging tube rises into a pre-existing magnetic field in the corona. Methods. To study the evolution, we use 3D numerical simulations by solving the time-dependent and resistive MHD equations. We qualitatively compare our numerical results with MDI magnetograms of emerging flux at the solar surface. Results. We find that the photospheric magnetic flux distribution consists of two regions of opposite polarities and elongated magnetic tails on the two sides of the polarity inversion line (PIL), depending on the azimuthal nature of the emerging field lines and the initial field strength of the rising tube. Their shape is progressively deformed due to plasma motions towards the PIL. Our results are in qualitative agreement with observational studies of magnetic flux emergence in active regions (ARs). Moreover, if the initial twist of the emerging tube is small, the photospheric magnetic field develops an undulating shape and does not possess tails. In all cases, we find that a new flux rope is formed above the original axis of the emerging tube that may erupt into the corona, depending on the strength of the ambient field.
dc.format.extent4
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2010, ESO. A&A 514, A56 (2010). Reproduced with permission from the publishers.en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun activityen
dc.subjectCoronaen
dc.subjectMagnetic fieldsen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleFlux emergence and coronal eruptionen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews.School of Mathematics and Statisticsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/200913502
dc.description.statusPeer revieweden


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