Abstract
This is a review of the physics of magnetic flares in the Sun. The details of the energy release processes in a solar flare are, at present, not clear and do not form a subject of this Chapter. Rather, we point out fundamental aspects of the conversion of kinetic into magnetic energy. We show the physical conditions required for magnetic flares to appear. Particular attention is paid to force free equilibria, energy storage, the amount of liberated energy, resistivity, and magnetic helicity. These findings are then applied to other stars, in particular to accretion disks around magnetic neutron stars.
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