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Observations have shown a clear association of filament/prominence eruptionswith the emergence of magnetic flux in or near filament channels.Magnetohydrodynamic (MHD) simulations have been employed to systematicallystudy the conditions under which such eruptions occur. These simulations todate have modeled filament channels as two-dimensional (2D) flux ropes or 3Duniformly sheared arcades. Here we present MHD simulations of flux emergenceinto a more realistic configuration consisting of a bipolar active regioncontaining a line-tied 3D flux rope. We use the coronal flux-rope model ofTitov et al. (2014) as the initial condition and drive our simulations byimposing boundary conditions extracted from a flux-emergence simulation byLeake et al. (2013). We identify three mechanisms that determine the evolutionof the system: (i) reconnection displacing foot points of field lines overlyingthe coronal flux rope, (ii) changes of the ambient field due to the intrusionof new flux at the boundary, and (iii) interaction of the (axial) electriccurrents in the pre-existing and newly emerging flux systems. The relativecontributions and effects of these mechanisms depend on the properties of thepre-existing and emerging flux systems. Here we focus on the location andorientation of the emerging flux relative to the coronal flux rope. Varyingthese parameters, we investigate under which conditions an eruption of thelatter is triggered.

Solar Eruptions Triggered by Flux Emergence Below or Near a Coronal Flux Rope