THE SUN'S MERIDIONAL CIRCULATION AND INTERIOR MAGNETIC FIELD

摘要: To date, no self-consistent numerical simulation of the solar interior has succeeded in reproducing observed thinness tachocline and persistence uniform rotation beneath it. Although it is known that can be explained by presence a global-scale confined magnetic field, simulations have thus far failed to produce any solution where such field remains against outward diffusion. We argue problem lies choice parameters for which these been performed. construct simple analytical magnetohydrodynamic model identify several distinct parameter regimes. For realistic values, our results are broad agreement with Gough & McIntyre. In this regime, meridional flows driven at base convection zone sufficient amplitude hold back values used existing simulations, on other hand, we find significantly weaker and, argue, unable confine field. propose method selecting future models.