http://arxiv.org/abs/2112.15103
For rapidly rotating turbulence (Rossby number much less than unity), the standard mixing length theory for turbulent convection breaks but Coriolis force enters the force balance such that magnetic field eventually depends on rotation. By simplifying the self-sustained magnetohydrodynamics dynamo equations of electrically conducting fluid motion, with the aid of theory of isotropic non-rotating or anisotropic rotating turbulence driven by thermal convection, we make estimations and derive scaling laws for stellar magnetic fields for slow and fast rotation. Our scaling laws are in good agreement with the observations.
X. Wei
Mon, 3 Jan 22
29/49
Comments: N/A