Differential rotation profiles in the solar interior, taken from Markiel & Thomas (1999) (see Fig. 6) but corrected at high latitudes in order to reproduce more closely the original data from Schou et al. (1998), according to which close to the poles the tachocline is not confined to a thin layer below the convection zone, but it extends towards the surface. This profile has been constructed so that at θ = 55° the tachocline extends over a fraction of the sub-adiabatic layer and expands towards the whole convection zone at θ ~ 30°.