When Magnetic Field Lines Stretch, Snap, and Expand: A New Look at Solar Flares with L-maps

Abstract Understanding the three-dimensional evolution of coronal magnetic fields during solar flares remains challenging due to the lack of direct coronal field measurements. Here, we combine data-driven MHD simulations of NOAA AR 11158 with flare-ribbon and coronal-dimming observations to investigate realistic coronal magnetic-field evolution during an X-class flare. We introduce L-maps —maps of natural logarithm of magnetic field-line lengths—as a diagnostic tool to track the dynamics of simulated coronal magnetic structures. Variations in L-maps identify flare ribbons through field-line shortening and coronal dimmings through field-line lengthening. Comparison with Solar Dynamics Observatory/Atmospheric Imaging Assembly observations demonstrates strong morphological and temporal agreement, validating the simulated field evolution. Applying K-means clustering to the L-map temporal profiles, we distinguish three stages of coronal evolution: (1) slow preflare rise phase, (2) flare reconnection accompanied by coronal mass ejection (CME) rise, and (3) post-reconnection CME expansion. We detect a slow preflare rise phase of magnetic field lines routed in ribbon footpoints and identify reconnection dimming —an area of rapid expansion of active-region core magnetic field lines during the flare impulsive phase due to reconnection. Our results show that L-maps provide a powerful and physically intuitive framework for bridging simulations and observations and for tracking the full three-dimensional evolution of coronal magnetic fields during flares.