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Simulating the formation of a sigmoidal flux rope in AR10977 from SOHO/MDI magnetograms

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Date
20/02/2014
Author
Gibb, Gordon Peter Samuel
Mackay, Duncan Hendry
Green, Lucie
Meyer, Karen Alison
Funder
Science & Technology Facilities Council
The Leverhulme Trust
European Commission
Grant ID
ST/K000950/1
RPG-305
263340
Keywords
Sun: corona
Sun: coronal mass ejections (CMEs)
Sun: flares
Sun: X-rays, gamma rays
QB Astronomy
QC Physics
BDC
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Abstract
The 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.
Citation
Gibb , 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 . https://doi.org/10.1088/0004-637X/782/2/71
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.1088/0004-637X/782/2/71
ISSN
0004-637X
Type
Journal article
Rights
© 2014. The American Astronomical Society. All rights reserved.
Description
G.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.
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/5154

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