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Torsional oscillations represent bands of fast and slow zonal flows aroundthe Sun, which extend deep into the convection zone and migrate during solarcycles towards the equator following the sunspot butterfly diagram. Analysis ofhelioseismology data obtained in 1996-2018 for almost two solar cycles revealszones of deceleration of the torsional oscillations inside the Sun due todynamo-generated magnetic field. The zonal deceleration originates near thebottom of the convection zone at high latitudes, and migrates to the surfacerevealing patterns of magnetic dynamo waves predicted by the Parker's dynamotheory. The analysis reveals that the primary seat of the solar dynamo islocated in a high-latitude zone of the tachocline. It suggests a dynamoscenario that can explain 'extended solar cycles' previously observed in theevolving shape of the solar corona. The results show a substantial decrease ofthe zonal acceleration in the current solar cycle and indicate further declineof activity in the next solar cycle. Although the relationship between themagnitude of zonal deceleration and the amount of emerged toroidal field thatleads to formation of sunspots is not yet established, the results open a newperspective for solar cycle modeling and prediction using helioseismology data.

Dynamo Wave Patterns Inside the Sun Revealed by Torsional Oscillations