Abstract
The physical mechanisms for forming current sheets are reviewed. In a two-dimensional magnetic field, sheets may form near X-type neutral points or separatrices in response to footpoint motions (converging or shearing) or to magnetic instability. In three-dimensions they may develop near separators or separatrix surfaces, but also more generally near any potential singular line in a sheared field. They may also be created in an MHD turbulent state as magnetic energy cascades to small scales. It is suggested that the closed magnetic regions of stellar coronae are filled with many small current sheets that are continually forming, filamenting and dissipating. Also a new self-consistent theory for heating by MHD turbulence is presented in which both the macroscopic state and the turbulent diffusivities depend on each other and the resulting heating depends only on the boundary motions and the geometry.
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