A Two-dimensional Magnetohydrodynamic Simulation of Chromospheric Evaporation in a Solar Flare Based on a Magnetic Reconnection Model

Perhaps an optimally wrong cartoon, in the sense that it represents about the best one could do with a 2D numerical simulation. A necessary step, but this approach explicitly cannot embrace the basic physical truth of conservation of energy (globally, since it's 2D; of course the simulation conserves energy locally). Thus it may or may not have much predictive power. In this excellent example one can see several of the features that one can imagine in the observations, notably a possibly observable termination shock in the reconnection outflow.