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Large-scale magnetic fields in stars and galaxies are thought to arise bymean-field dynamo action due to the combined influence of both helicalturbulence and shear. Those systems are also highly conducting and theturbulence therein leads to a fluctuation (or small-scale) dynamo which morerapidly amplifies magnetic field fluctuations on the eddy scales and smaller.Will this then interfere with and suppress the mean (or large-scale) fieldgrowth? Using direct numerical simulations of helical turbulence (with andwithout shear), we identify a novel quasi-kinematic large-scale dynamo whichoperates as the small-scale dynamo saturates. Thus both dynamos operateefficiently, one after the other, and lead to the generation of significantlarge-scale fields.

Efficient quasi-kinematic large-scale dynamo as the small-scale dynamo saturates