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Numerical MHD simulations of 3D reconnection events in the solar corona haveimproved enormously over the last few years, not only in resolution, but alsoin their complexity, enabling more and more realistic modeling. Various ways toobtain the initial magnetic field, different forms of solar atmospheric modelsas well as diverse driving speeds and patterns have been employed. This studyconsiders differences between simulations with stratified and non-stratifiedsolar atmospheres, addresses the influence of the driving speed on the plasmaflow and energetics, and provides quantitative formulas for mapping electricfields and dissipation levels obtained in numerical simulations to thecorresponding solar quantities. The simulations start out from a potentialmagnetic field containing a null-point, obtained from a Solar and HeliosphericObservatory (SOHO) magnetogram extrapolation approximately 8 hours before aC-class flare was observed. The magnetic field is stressed with a boundarymotion pattern similar to - although simpler than - horizontal motions observedby SOHO during the period preceding the flare. The general behavior is nearlyindependent of the driving speed, and is also very similar in stratified andnon-stratified models, provided only that the boundary motions are slow enough.The boundary motions cause a build-up of current sheets, mainly in thefan-plane of the magnetic null-point, but do not result in a flare-like energyrelease. The additional free energy required for the flare could have beenpartly present in non-potential form in the initial state, with subsequentadditions from magnetic flux emergence or from components of the boundarymotion that were not represented by the idealized driving pattern.

3D Solar Null Point Reconnection MHD Simulations