A stellar convection zone is a region where buoyant fluid motion transports a significant part of the stellar heat flux. Rising and sinking parcels carry enthalpy, so heat transport is not entirely radiative. The Sun's outer convection zone extends from near to the surface and overlies its radiative interior. The tachocline lies near this transition, and the convection helps power the solar dynamo.
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The convection zone is a layer within a star, such as the Sun, where energy is transported primarily through the process of convection. In this zone, hot plasma rises toward the surface, cools down, and then sinks back down to be reheated. This cycle creates convective currents, much like boiling water where hot water rises and cooler water descends.