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We present the first numerical simulations of the solar interior to exhibit atachocline consistent with the Gough and McIntyre (1998) model. We findnonlinear, axisymmetric, steady-state numerical solutions in which: (1) alarge-scale primordial field is confined within the radiation zone bydownwelling meridional flows that are gyroscopically pumped in the convectionzone (2) the radiation zone is in almost-uniform rotation, with a rotation rateconsistent with observations (3) the bulk of the tachocline is magnetic free,in thermal-wind balance and in thermal equilibrium and (4) the interactionbetween the field and the flows takes place within a very thin magneticboundary layer, the tachopause, located at the bottom of the tachocline. Weshow that the thickness of the tachocline scales with the amplitude of themeridional flows exactly as predicted by Gough and McIntyre. We also determinethe parameter conditions under which such solutions can be obtained, andprovide a simple explanation for the failure of previous numerical attempts atreproducing the Gough and McIntyre model. Finally, we discuss the implicationsof our findings for future numerical models of the solar interior, and forfuture observations of the Sun and other stars.

Dynamics of the solar tachocline III: Numerical solutions of the Gough and McIntyre model