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We present two-dimensional resistive magnetohydrodynamic simulations ofline-tied asymmetric magnetic reconnection in the context of solar flare andcoronal mass ejection current sheets. The reconnection process is madeasymmetric along the inflow direction by allowing the initial upstream magneticfield strengths and densities to differ, and along the outflow direction byplacing the initial perturbation near a conducting wall boundary thatrepresents the photosphere. When the upstream magnetic fields are asymmetric,the post-flare loop structure is distorted into a characteristic skewed candleflame shape. The simulations can thus be used to provide constraints on thereconnection asymmetry in post-flare loops. More hard X-ray emission isexpected to occur at the footpoint on the weak magnetic field side becauseenergetic particles are more likely to escape the magnetic mirror there than atthe strong magnetic field footpoint. The footpoint on the weak magnetic fieldside is predicted to move more quickly because of the requirement in twodimensions that equal amounts of flux must be reconnected from each upstreamregion. The X-line drifts away from the conducting wall in all simulations withasymmetric outflow and into the strong magnetic field region during most of thesimulations with asymmetric inflow. There is net plasma flow across the X-linefor both the inflow and outflow directions. The reconnection exhaust directedaway from the obstructing wall is significantly faster than the exhaustdirected towards it. The asymmetric inflow condition allows net vorticity inthe rising outflow plasmoid which would appear as rolling motions about theflux rope axis.

Asymmetric Magnetic Reconnection in Solar Flare and Coronal Mass Ejection Current Sheets