Abstract
A review is presented on the physics of the convective zone and the implications at the coronal level. Solar magnetic fields are created in the convective layer from the kinetic energy of the dense plasma. At the coronal level, the magnetic field controls the plasma and is forced to evolve according to the time-dependent boundary conditions given at the photospheric level by the convective zone. The coronal field cannot find a smooth equilibrium when its topology is complex and current sheets are formed. These are the preferred regions where reconnection can occur. Present development of 3D reconnection is reviewed, and we show how observed flare kernels are related to the magnetic field topology. Then we describe how our present theoretical understanding of flares can help us to understand both large and small scale coronal events.KeywordsField LineCurrent SheetCoronal Mass EjectionSolar PhysConvective ZoneThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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