The Development of Structure in Coronal Magnetic Fields

  • Mitchell A. Berger
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 143)


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.


Boundary Motion Coronal Magnetic Field Flux Element Coronal Field Stellar Activity 
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Copyright information

© Kluwer Academic Publishers 1988

Authors and Affiliations

  • Mitchell A. Berger
    • 1
  1. 1.Department of Mathematical SciencesUniversity of St AndrewsFifeScotland

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