A Dynamo in the Radiative Interior
Magnetic fields can be created in the stably stratified layers below the convection zone of the Sun. A magnetic instability in the toroidal field (wound up by differential rotation) replaces the role of convection in closing the field amplification loop. Several different instabilities can play this role in principle, but Tayler instability is likely to be the most relevant one. A dynamo model is developed from these ingredients, and applied to the problem of angular momentum transport in the solar interior. It produces a predominantly horizontal field. This dynamo process is found to be much more effective in transporting angular momentum than the known hydrodynamic mechanisms, operating already at very low gradients in rotation rate. It might account for the observed pattern of rotation in the solar core.
KeywordsRayleigh Number Rotation Rate Convection Zone Tayler Instability Radial Gradient
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