  Rotational scaling relationships are examined for the degree of equipartition
between magnetic and kinetic energies in stellar convection zones. These
scaling relationships are approached from two paradigms, with first a glance at
scaling relationship built upon an energy-balance argument and second a look at
a force-based scaling. The latter implies a transition between a
nearly-constant inertial scaling when in the asymptotic limit of minimal
diffusion and magnetostrophy, whereas the former implies a weaker scaling with
convective Rossby number. Both scaling relationships are then compared to a
suite of 3D convective dynamo simulations with a wide variety of domain
geometries, stratifications, and range of convective Rossby numbers.
