Modeling the initiation of the 2006 December 13 coronal mass ejection in AR 10930: the structure and dynamics of the erupting flux rope
Yuhong Fan

TL;DR
This study uses 3D MHD simulations to model the 2006 CME initiation in AR 10930, revealing the role of a twisted flux rope and its dynamics, including rotation and magnetic field configuration, in the eruption process.
Contribution
It presents a detailed 3D MHD simulation of CME initiation that incorporates a wider domain and explains observed magnetic field behaviors and potential for subsequent eruptions.
Findings
CME results from emergence of a twisted flux rope
Flux rope accelerates beyond 1500 km/s and rotates 180 degrees
Reformation of flux rope suggests potential for multiple eruptions
Abstract
We carry out a three-dimensional magneto-hydrodynamic (MHD) simulation to model the initiation of the coronal mass ejection (CME) on 13 December 2006 in the emerging {\delta}-sunspot active region NOAA 10930. The setup of the simulation is similar to a previous simulation by Fan (2011), but with a significantly widened simulation domain to accommodate the wide CME. The simulation shows that the CME can result from the emergence of a east-west oriented twisted flux rope whose positive, following emerging pole corresponds to the observed positive rotating sunspot emerging against the southern edge of the dominant pre-existing negative sunspot. The erupting flux rope in the simulation accelerates to a terminal speed that exceeds 1500 km/s and undergoes a counter-clockwise rotation of nearly 180 degrees such that its front and flanks all exhibit southward directed magnetic fields,…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
