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We carry out a three-dimensional magneto-hydrodynamic (MHD) simulation tomodel the initiation of the coronal mass ejection (CME) on 13 December 2006 inthe emerging {\delta}-sunspot active region NOAA 10930. The setup of thesimulation is similar to a previous simulation by Fan (2011), but with asignificantly widened simulation domain to accommodate the wide CME. Thesimulation shows that the CME can result from the emergence of a east-westoriented twisted flux rope whose positive, following emerging pole correspondsto the observed positive rotating sunspot emerging against the southern edge ofthe dominant pre-existing negative sunspot. The erupting flux rope in thesimulation accelerates to a terminal speed that exceeds 1500 km/s and undergoesa counter-clockwise rotation of nearly 180 degrees such that its front andflanks all exhibit southward directed magnetic fields, explaining the observedsouthward magnetic field in the magnetic cloud impacting the Earth. Withcontinued driving of flux emergence, the source region coronal magnetic fieldalso shows the reformation of a coronal flux rope underlying the flare currentsheet of the erupting flux rope, ready for a second eruption. This may explainthe build up for another X-class eruptive flare that occurred the following dayfrom the same region.

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