The radiative-convective equilibrium models of Appleby and Hogan (1984) used K and 95.0 K for the effective IR temperatures of Jupiter and Saturn. The radiative-convective boundary is expected to occur at the point where the atmospheric temperature lapse rate first decreases from the convectively unstable adiabatic rate to a sub-adiabatic value. The atmospheric level at which this transition occurs delineates the boundary between the well-mixed troposphere and the overlying stably stratified stratosphere. The radiative-convective boundary thus marks the true dynamical boundary between the tropopause and stratosphere, although it occurs slightly deeper than the temperature inversion (which occurs at mbar in Jupiter).