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We present axisymmetric numerical simulations of the solar interior,including the convection zone and an extended radiative interior. We find thatdifferential rotation in the convection zone induces a toroidal field from aninitially purely poloidal field. This toroidal field becomes unstable to theaxisymmetric Tayler instability and undergoes equatorward propagating toroidalfield reversals. These reversals occur in the absence of a dynamo and withoutaccompanying poloidal field reversals. The nature and presence of suchreversals depends sensitively on the initial poloidal field strength imposed,with north-south symmetric reversals only seen at a particular initial fieldstrength. Coupled with a dynamo mechanism which regenerates the poloidal fieldthis could be one ingredient in the sunspot cycle.

Toroidal Field Reversals and the Axisymmetric Tayler Instability