Solar flares and coronal mass ejections are powered by the sudden release of magnetic energy stored in the Sun’s low corona. Understanding these explosive events requires tracking how magnetic fields evolve—not only during, but also before the eruptions. Yet, direct measurements of the 3D coronal magnetic field remain a major challenge. In this talk, I will overview what we currently know about the structure of the pre-eruption magnetic field and the physical mechanisms that trigger eruptions. I will present recent results from both statistical analyses of Solar Dynamics Observatory observations and data-driven MHD simulations of eruptive flares. Using novel diagnostics, including L-maps, I will illustrate how observed features such as flare ribbons and coronal dimmings can be used to trace the dynamic evolution of magnetic fields throughout the eruption process. I will conclude by looking ahead to the exciting future of solar physics, as new generation observatories — DKIST, Solar Orbiter, and the upcoming Vigil mission — will provide key empirical constraints on the physics of the solar flares in the decade to come.
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