The standard flare model in three dimensions - I. Strong-to-weak shear transition in post-flare loops

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Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, background): “There are ongoing attempts to generalise the standard model of a flare accounting for 3D effects (see, e.g. Aulanier et al. 2012).”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, background): “These loops become cooler and cooler as they shrink (Forbes et al., 1989; Forbes and Acton, 1996; Aulanier et al., 2012).”
ELECTRIC CURRENTS IN FLARE RIBBONS: OBSERVATIONS AND THREE-DIMENSIONAL STANDARD MODEL (2014, methodology): “…of these scenarios involves a torus-unstable flux rope (Bateman 1978; Lin et al. 1998; Kliem & Török 2006), and numerical simulations of such an evolution have been able to reproduce many of the eruptive flare characteristics (e.g., Aulanier et al. 2012; Janvier et al. 2013; Dudı́k et al. 2014).”
The standard flare model in three dimensions II: upper limit on solar flare energy (2012, methodology): “The simulation settings are thoroughly described in Aulanier et al. (2010, 2012).”