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dc.contributor.authorGibb, Gordon Peter Samuel
dc.contributor.authorMackay, Duncan Hendry
dc.contributor.authorGreen, Lucie
dc.contributor.authorMeyer, Karen Alison
dc.identifier.citationGibb , G P S , Mackay , D H , Green , L & Meyer , K A 2014 , ' Simulating the formation of a sigmoidal flux rope in AR10977 from SOHO /MDI magnetograms ' , Astrophysical Journal , vol. 782 , no. 2 , 71 .
dc.identifier.otherPURE: 102315531
dc.identifier.otherPURE UUID: bf49b0c7-b828-40fe-8834-c11872d3a2b7
dc.identifier.otherScopus: 84893582446
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055434
dc.identifier.otherWOS: 000334584700013
dc.descriptionG.P.S.G. acknowledges STFC for financial support. D.H.M. acknowledges the STFC, the Leverhulme Trust, and the EU FP7 funded project "SWIFF" (263340) for financial support. L.M.G. acknowledges to the Royal Society for a University Research Fellowship. K.A.M. acknowledges the Leverhulme Trust for financial support. Simulations were carried out on a STFC/SRIF funded UKMHD cluster at St Andrews.en
dc.description.abstractThe modeling technique of Mackay et al. is applied to simulate the coronal magnetic field of NOAA active region AR10977 over a seven day period (2007 December 2-10). The simulation is driven with a sequence of line-of-sight component magnetograms from SOHO/MDI and evolves the coronal magnetic field though a continuous series of non-linear force-free states. Upon comparison with Hinode/XRT observations, results show that the simulation reproduces many features of the active region's evolution. In particular, it describes the formation of a flux rope across the polarity inversion line during flux cancellation. The flux rope forms at the same location as an observed X-ray sigmoid. After five days of evolution, the free magnetic energy contained within the flux rope was found to be 3.9 × 1030 erg. This value is more than sufficient to account for the B1.4 GOES flare observed from the active region on 2007 December 7. At the time of the observed eruption, the flux rope was found to contain 20% of the active region flux. We conclude that the modeling technique proposed in Mackay et al.—which directly uses observed magnetograms to energize the coronal field—is a viable method to simulate the evolution of the coronal magnetic field.
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectSun: coronaen
dc.subjectSun: coronal mass ejections (CMEs)en
dc.subjectSun: flaresen
dc.subjectSun: X-rays, gamma raysen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleSimulating the formation of a sigmoidal flux rope in AR10977 from SOHO/MDI magnetogramsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorThe Leverhulme Trusten
dc.contributor.sponsorEuropean Commissionen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.description.statusPeer revieweden

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