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In giant planet atmosphere modelling, the intrinsic temperature$T_\mathrm{int}$ and radiative-convective boundary (RCB) are important lowerboundary conditions. Often in one-dimensional radiative-convective models andin three-dimensional general circulation models it is assumed that$T_\mathrm{int}$ is similar to that of Jupiter itself, around 100 K, whichyields a RCB around 1 kbar for hot Jupiters. In this work, we show that theinflated radii, and hence high specific entropy interiors, of hot Jupiterssuggest much higher $T_\mathrm{int}$ values. Assuming the effect is primarilydue to current heating (rather than delayed cooling), we derive an equilibriumrelation between $T_\mathrm{eq}$ and $T_\mathrm{int}$, showing that the lattercan take values as high as 700 K. In response, the RCB moves upward in theatmosphere. Using one-dimensional radiative-convective atmosphere models, wefind RCBs of only a few bars, rather than the kilobar typically supposed. Thismuch shallower RCB has important implications for the atmospheric structure,vertical and horizontal circulation, interpretations of phase curves, and theeffect of deep cold traps on cloud formation.

The Intrinsic Temperature and Radiative-Convective Boundary Depth in the Atmospheres of Hot Jupiters