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Sunspots and the plethora of other phenomena occuring in the course of the11-year cycle of solar activity are a consequence of the emergence of magneticflux at the solar surface. The observed orientations of bipolar sunspot groupsimply that they originate from toroidal (azimuthally orientated) magnetic fluxin the convective envelope of the Sun. We show that the net toroidal magneticflux generated by differential rotation within a hemisphere of the convectionzone is determined by the emerged magnetic flux at the solar surface and thuscan be calculated from the observed magnetic field distribution. The mainsource of the toroidal flux is the roughly dipolar surface magnetic field atthe polar caps, which peaks around the minima of the activity cycle.

The crucial role of surface magnetic fields for the solar dynamo