Wednesday

Coronal jets are observed above minority polarity intrusions throughout the solar corona. Some of the most energetic occur on the periphery of active regions where the magnetic field is strongly inclined. These jets exhibit a non-radial propagation in the low corona as they follow the inclined field, and often have a broad, helical shape. We present a three-dimensional magnetohydrodynamic simulation of such an active region periphery helical jet. Free energy is injected into an initially potential field, creating a sigmoidal flux rope which eventually erupts to produce the helical jet. We find that the eruption results from a combination of magnetic breakout and an ideal kinking of the erupting flux rope. We discuss how the two mechanisms are coupled, and contrast our results with our previous simulations of coronal-hole jets.