Estimations and Scaling Laws for Stellar Magnetic Fields

In rapidly rotating turbulence (Rossby number much less than unity), the standard mixing length theory for turbulent convection breaks and Coriolis force enters balance such that magnetic field eventually depends on rotation. By simplifying self-sustained magnetohydrodynamics dynamo equations of electrically conducting fluid motion, with aid isotropic non-rotating or anisotropic driven by thermal convection, we make estimations derive scaling laws stellar fields slow fast Our are in good agreement observations.