Show simple item record

Files in this item


Item metadata

dc.contributor.authorYardley, Stephanie Louise
dc.contributor.authorSavcheva, Antonia
dc.contributor.authorGreen, Lucie M.
dc.contributor.authorvan Driel-Gesztelyi, Lidia
dc.contributor.authorLong, David
dc.contributor.authorWilliams, David R.
dc.contributor.authorMackay, Duncan Hendry
dc.identifier.citationYardley , 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 .
dc.identifier.otherORCID: /0000-0001-6065-8531/work/67525848
dc.descriptionFunding: UK STFC via PhD studentship and the Consolidated Grant SMC1/YST025 (S.L.Y.); STFC and Leverhulme trust (D.H.M.).en
dc.description.abstractWe 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.
dc.relation.ispartofAstrophysical Journalen
dc.subjectSun: activityen
dc.subjectSun: filaments, prominencesen
dc.subjectSun: coronal mass ejections (CMEs)en
dc.subjectSun: evolutionen
dc.subjectSun: magnetic fieldsen
dc.subjectSun; photosphereen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleUnderstanding the plasma and magnetic field evolution of a filament using observations and non-linear force-free field modelling : evolution of an intermediate filamenten
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.description.statusPeer revieweden

This item appears in the following Collection(s)

Show simple item record