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Improving upon our purely dynamical work, we present three‐dimensional simulations of the atmospheric circulation on Earth‐like (exo)planets and hot Jupiters using the Geophysical Fluid Dynamics Laboratory (GFDL)‐Princeton  Flexible Modelling System  ( fms ). As the first steps away from the dynamical benchmarks of Heng, Menou &amp; Phillipps, we add dual‐band radiative transfer and dry convective adjustment schemes to our computational set‐up. Our treatment of radiative transfer assumes stellar irradiation to peak at a wavelength shorter than and distinct from that at which the exoplanet re‐emits radiation (‘shortwave’ versus ‘longwave’), and also uses a two‐stream approximation. Convection is mimicked by adjusting unstable lapse rates to the dry adiabat. The bottom of the atmosphere is bounded by a uniform slab with a finite thermal inertia. For our models of hot Jupiter, we include an analytical formalism for calculating temperature–pressure profiles, in radiative equilibrium, which accounts for the effect of collision‐induced absorption via a single parameter. We discuss our results within the context of the following: the predicted temperature–pressure profiles and the absence/presence of a temperature inversion; the possible maintenance, via atmospheric circulation, of the putative high‐altitude, shortwave absorber expected to produce these inversions; the angular/temporal offset of the hotspot from the substellar point, its robustness to our ignorance of hyperviscosity and hence its utility in distinguishing between different hot Jovian atmospheres; and various zonal‐mean flow quantities. Our work bridges the gap between three‐dimensional simulations which are purely dynamical and those which incorporate multiband radiative transfer, thus contributing to the construction of a required hierarchy of three‐dimensional theoretical models.

Atmospheric circulation of tidally locked exoplanets: II. Dual‐band radiative transfer and convective adjustment