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A long established goal of solar physics is to build understanding of solar eruptions and develop flare and CME forecasting models. In this paper, we continue our investigation of non-linear forces free field (NLFFF) models by comparing topological properties of the solutions to the evolution of the flare ribbons. In particular, we show that data constrained NLFFF models of three erupting sigmoid regions (SOL2010-0408, SOL2010-08-07, and SOL2012-05-12) built to reproduce the active region magnetic field in the pre-flare state can be rendered unstable and the subsequent sequence of unstable solutions produce quasi-separatrix layers (QSLs) that match the flare ribbon evolution as observed by SDO/AIA. We begin with a best-fit equilibrium model for the pre-flare active region; we than add axial flux to the flux rope in the model to move it across the stability boundary; at this point the magnetofrictional code no longer converges to an equilibrium solution, the flux rope rises as the solutions are iterated. We interpret the sequence of magnetofrictional steps as an evolution of the active region as the flare/CME begins. The magnetic field solutions at different steps are compared with the flare ribbons. The results are fully consistent with the 3D extension of the standard flare/CME model. Our ability to capture essential topological features of flaring active regions with a non-dynamic magneto-frictional code strongly suggests that the pre-flare, large scale topological structures are preserved as the flux rope becomes unstable and lifts off. Subject headings: Sun:magnetic fields — Sun: sigmoid — Sun: flares — Sun: X-rays

THE RELATION BETWEEN SOLAR ERUPTION TOPOLOGIES AND OBSERVED FLARE FEATURES. II. DYNAMICAL EVOLUTION