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We describe and analyze observations by the Solar Dynamics Observatory of theemergence of a small, bipolar active region within an area of unipolar magneticflux that was surrounded by a circular, quiescent filament. Within only eighthours of the start of the emergence, a partial splitting of the filament andtwo consecutive coronal mass ejections took place. We argue that all threedynamic events occurred as a result of particular magnetic-reconnectionepisodes between the emerging bipole and the pre-existing coronal magneticfield. In order to substantiate our interpretation, we considerthree-dimensional magnetohydrodynamic simulations that model the emergence ofmagnetic flux in the vicinity of a large-scale coronal flux rope. Thesimulations qualitatively reproduce most of the reconnection episodes suggestedby the observations; as well as the filament-splitting, the first eruption, andthe formation of sheared/twisted fields that may have played a role in thesecond eruption. Our results suggest that the position of emerging flux withrespect to the background magnetic configuration is a crucial factor for theresulting evolution, while previous results suggest that parameters such as theorientation or the amount of emerging flux are important as well. This poses achallenge for predicting the onset of eruptions that are triggered by fluxemergence, and it calls for a detailed survey of the relevant parameter spaceby means of numerical simulations.

Sequential eruptions triggered by flux emergence - observations and modeling