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We present a 3D MHD simulation that qualitatively models the coronal mag-netic field evolution associated with the eruptive flare that occurred onDecember 13, 2006 in the emerging {\delta}-sunspot region NOAA 10930 observedby the Hinode satellite. The simulation is set up where we drive the emergenceof an east-west oriented magnetic flux rope at the lower boundary into apre-existing coronal field constructed from the SOHO/MDI full-disk magnetogramat 20:51:01 UT on December 12, 2006. The resulting coronal flux rope embeddedin the ambi- ent coronal magnetic field first settles into a stage ofquasi-static rise, and then undergoes a dynamic eruption, with the leading edgeof the flux rope cavity accel- erating to a steady speed of about 830 km/s. Thepre-eruption coronal magnetic field shows morphology that is in qualitativeagreement with that seen in the Hinode soft X-ray observation in both themagnetic connectivity as well as the development of an inverse-S shaped X-raysigmoid. We examine the properties of the erupting flux rope and the morphologyof the post-reconnection loops, and compare them with the observations.

An MHD Model of the December 13 2006 Eruptive Flare