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An Observationally-Constrained Model of a Flux Rope that Formed in the Solar Corona View all abstracts by submitter

Alexander James   Submitted: 2018-02-27 09:22

Coronal mass ejections (CMEs) are large-scale eruptions of plasma from the coronae of stars. Understanding the plasma processes involved in CME initiation has applications to space weather forecasting and laboratory plasma experiments. James et al. (Sol. Phys. 292, 71, 2017) used EUV observations to conclude that a magnetic flux rope formed in the solar corona above NOAA Active Region 11504 before it erupted on 14 June 2012 (SOL2012-06-14). In this work, we use data from the Solar Dynamics Observatory to model the coronal magnetic field of the active region one hour prior to eruption using a nonlinear force-free field extrapolation, and find a flux rope reaching a maximum height of 150 Mm above the photosphere. Estimations of the average twist of the strongly asymmetric extrapolated flux rope are between 1.35 and 1.88 turns, depending on the choice of axis, although the erupting structure was not observed to kink. The decay index near the apex of the axis of the extrapolated flux rope is comparable to typical critical values required for the onset of the torus instability, so we suggest that the torus instability drove the eruption.

Authors: James, A. W., Valori, G., Green, L. M., Liu, Y., Cheung, M. C. M., Guo, Y., van Driel-Gesztelyi, L.
Projects: SDO-AIA,SDO-HMI

Publication Status: Accepted in ApJL
Last Modified: 2018-02-28 14:01
Go to main E-Print page  Successive X-class flares and coronal mass ejections driven by shearing motion and sunspot rotation in active region NOAA 12673  The Duration of Energy Deposition on Unresolved Flaring Loops in the Solar Corona  Edit Entry  Download Preprint  Delete Entry 

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