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Rotational scaling relationships are examined for the degree of equipartitionbetween magnetic and kinetic energies in stellar convection zones. Thesescaling relationships are approached from two paradigms, with first a glance atscaling relationship built upon an energy-balance argument and second a look ata force-based scaling. The latter implies a transition between anearly-constant inertial scaling when in the asymptotic limit of minimaldiffusion and magnetostrophy, whereas the former implies a weaker scaling withconvective Rossby number. Both scaling relationships are then compared to asuite of 3D convective dynamo simulations with a wide variety of domaingeometries, stratifications, and range of convective Rossby numbers.

Rossby and Magnetic Prandtl Number Scaling of Stellar Dynamos