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Three dimensional magnetohydrodynamic simulations of the injection of poloidal magnetic flux bundles into a vertically stratifed atmosphere have been performed. As the flux emerges into the corona, a strongly twisted bundle of poloidal flux starts to move rapidly upward, carrying chromospheric plasma with it. Typical coronal vertical speeds are between $100$ and $200$ km/s, while the photosphere remains relatively undisturbed. This mechanism can be viewed as an efficient way of transmitting magnetic energy from the bottom of the photosphere into the corona. One possible application of these results is to the blue-shifted line profiles observed during flares by SMM and YOHKOH.
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