The Development of Structure in Coronal Magnetic Fields
Much of solar and stellar activity arises from the release of stored magnetic energy. This energy can often be associated with the existence of fieldline structures such as shear, twist, and braiding. At what rate does magnetic structure enter a coronal field? This paper discusses the growth of structure due to random photospheric motions. Helicity integrals are used to quantify the complexity of the magnetic field. As a concrete example, the braiding of two fieldlines due to random motions will be discussed.
KeywordsBoundary Motion Coronal Magnetic Field Flux Element Coronal Field Stellar Activity
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