In the context of astrophysical dynamos we illustrate that the no-cosines flow , with zero mean helicity , can drive fast dynamo action and study the dynamo ’ s mode of operation during both the linear and non-linear saturation regime : It turns out that in addition to a high growth rate in the linear regime , the dynamo saturates at a level significantly higher than normal turbulent dynamos , namely at exact equipartition when the magnetic Prandtl number Pr _ { m } \sim 1 .
Visualization of the magnetic and velocity fields at saturation will help us to understand some of the aspects of the non-linear dynamo problem .