Helicity and Celestial Magnetism rspa.royalsocietypublishing.org H. K. Moffatt1 1 Research Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Article submitted to journal Wilberforce Road, Cambridge CB3 0WA, UK This informal article discusses the central role of Subject Areas: magnetic and kinetic helicity in relation to the geophysics, astrophysics, dynamo evolution of magnetic fields in geophysical and theory astrophysical contexts. It is argued that the very existence of magnetic fields of the intensity and Keywords: scale observed is attributable in large part to the magnetic fields, chirality, chirality of the background turbulence or random- magnetostrophic, magnetic relaxation wave field of flow, the simplest measure of this chirality being non-vanishing helicity. Such flows are responsible for the generation of large-scale Author for correspondence: magnetic fields which themselves exhibit magnetic Insert corresponding author name helicity. In the geophysical context, the turbulence e-mail:
[email protected] has a ‘magnetostrophic’ character in which the force balance is primarily that between buoyancy forces, Coriolis forces and Lorentz forces associated with the dynamo-generated magnetic field; the dominant nonlinearity here arises from the convective transport of buoyant elements erupting from the ‘mushy zone’ at the inner core boundary. At the opposite extreme, in a highly conducting low-density plasma, the near-invariance of magnetic field topology (and of associated helicity) presents the challenging problem of ‘magnetic relaxation under topological constraints’, of central importance both in astrophysical contexts and in controlled-fusion plasma dynamics. These problems are reviewed and open issues, particularly concerning saturation mechanisms, are reconsidered.