  Many hot and ultra-hot Jupiters have inflated radii, implying that their
interiors retain significant entropy from formation. These hot interiors lead
to an enhanced internal heat flux that impinges upon the atmosphere from below.
In this work, we study the effect of this hot interior on the atmospheric
circulation and thermal structure of hot and ultra-hot Jupiters. To do so, we
incorporate the population-level predictions from evolutionary models of hot
and ultra-hot Jupiters as input for a suite of General Circulation Models
(GCMs) of their atmospheric circulation with varying semi-major axis and
surface gravity. We conduct simulations with and without a hot interior, and
find that there are significant local differences in temperature of up to
hundreds of Kelvin and in wind speeds of hundreds of m s$^{-1}$ or more across
the observable atmosphere. These differences persist throughout the parameter
regime studied, and are dependent on surface gravity through the impact on
photosphere pressure. These results imply that the internal evolution and
atmospheric thermal structure and dynamics of hot and ultra-hot Jupiters are
coupled. As a result, a joint approach including both evolutionary models and
GCMs may be required to make robust predictions for the atmospheric circulation
of hot and ultra-hot Jupiters.
