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Understanding the plasma and magnetic field evolution of a filament using observations and non-linear force-free field modelling : evolution of an intermediate filament

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Date
23/12/2019
Author
Yardley, Stephanie Louise
Savcheva, Antonia
Green, Lucie M.
van Driel-Gesztelyi, Lidia
Long, David
Williams, David R.
Mackay, Duncan Hendry
Keywords
Sun: activity
Sun: filaments, prominences
Sun: coronal mass ejections (CMEs)
Sun: evolution
Sun: magnetic fields
Sun; photosphere
QB Astronomy
QC Physics
3rd-DAS
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Abstract
We present observations and magnetic field models of an intermediate filament present on the Sun in August 2012, associated with a polarity inversion line that extends from AR 11541 in the east into the quiet sun at its western end. A combination of SDO/AIA, SDO/HMI, and GONG Hα data allow us to analyse the structure and evolution of the filament from 2012 August 4 23:00 UT to 2012 August 6 08:00 UT when the filament was in equilibrium. By applying the flux rope insertion method, nonlinear force-free field models of the filament are constructed using SDO/HMI line-of-sight magnetograms as the boundary condition at the two times given above. Guided by observed filament barbs, both modelled flux ropes are split into three sections each with a different value of axial flux to represent the non-uniform photospheric field distribution. The flux in the eastern section of the rope increases by 4x1020 Mx between the two models, which is in good agreement with the amount of flux cancelled along the internal PIL of AR 11541, calculated to be 3.2x1020 Mx. This suggests that flux cancellation builds flux into the filament's magnetic structure. Additionally, the number of field line dips increases between the two models in the locations where flux cancellation, the formation of new filament threads and growth of the filament is observed. This suggests that flux cancellation associated with magnetic reconnection forms concave-up magnetic field that lifts plasma into the filament. During this time, the free magnetic energy in the models increases by 0.2 x 1031 ergs.
Citation
Yardley , S L , Savcheva , A , Green , L M , van Driel-Gesztelyi , L , Long , D , Williams , D R & Mackay , D H 2019 , ' Understanding the plasma and magnetic field evolution of a filament using observations and non-linear force-free field modelling : evolution of an intermediate filament ' , Astrophysical Journal , vol. 887 , no. 2 , 240 . https://doi.org/10.3847/1538-4357/ab54d2
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-4357/ab54d2
ISSN
0004-637X
Type
Journal article
Rights
Copyright © 2019 American Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://iopscience.iop.org/journal/0004-637X
Description
Funding: UK STFC via PhD studentship and the Consolidated Grant SMC1/YST025 (S.L.Y.); STFC and Leverhulme trust (D.H.M.).
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/18852

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