Exploring the deep atmospheres of HD 209458b and WASP-43b using a non-gray general circulation model

Simulations with a 3D general circulation model (GCM) suggest that one potential driver behind the observed radius inflation in hot Jupiters may be downward advection of energy from highly irradiated photosphere into deeper layers. Here, we compare dynamical heat transport within non-inflated Jupiter WASP-43b and canonical inflated HD 209458b, similar effective temperatures. We investigate to what extent radiatively driven heating cooling (at pressures smaller than 1 bar) influence temperature profile between 700 bar). Our simulations new non-gray radiation-hydrodynamical expeRT/MITgcm show deep is associated relatively cold adiabat. The layers however, do not converge remain nearly unchanged regardless whether or initial state used. Furthermore, different flow structures atmospheric arise. There, find exhibits equatorial jet, by fast tidally locked rotation this planet (0.81 days), as compared 209458b (3.47 days). However, comparing periods, resulting only marginally evolution atmosphere, which almost completely dominated radiative cooling. can structure WASP-43b. Thus, dayside emission spectra shed more light onto processes occurring at greater depths.