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Solar flares are energetic events taking place in the Sun's atmosphere, andtheir effects can greatly impact the environment of the surrounding planets. Inparticular, eruptive flares, as opposed to confined flares, launch coronal massejections into the interplanetary medium, and as such, are one of the maindrivers of space weather. After briefly reviewing the main characteristics ofsolar flares, we summarize the processes that can account for the build up andrelease of energy during their evolution. In particular, we focus on thedevelopment of recent 3D numerical simulations that explain many of theobserved flare features. These simulations can also provide predictions of thedynamical evolution of coronal and photospheric magnetic field. Here we presenta few observational examples that, together with numerical modelling, point tothe underlying physical mechanisms of the eruptions.

From coronal observations to MHD simulations, the building blocks for 3D models of solar flares