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Solar active regions, produced by the emergence of tubes of strong magneticfield in the photosphere, are restricted to within 35 degrees of the solarequator. The nature of the dynamo processes that create and renew these fields,and are therefore responsible for solar magnetic phenomena, are not wellunderstood. We analyze the magneto-rotational stability of the solar tachoclinefor general field geometry. This thin region of strong radial and latitudinaldifferential rotation, between the radiative and convective zones, is unstableat latitudes above 37 degrees, yet is stable closer to the equator. We proposethat small-scale magneto-rotational turbulence prevents coherent magneticdynamo action in the tachocline except in the vicinity of the equator, thusexplaining the latitudinal restriction of active regions. Tying the magneticdynamo to the tachocline elucidates the physical conditions and processesrelevant to solar magnetism.

The Origin of Solar Activity in the Tachocline