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We present results from 3D radiative-hydrodynamical simulations of HD 209458bwith a fully coupled treatment of clouds using the EddySed code, critically,including cloud radiative feedback via absorption and scattering. Wedemonstrate that the thermal and optical structure of the simulated atmosphereis markedly different, for the majority of our simulations, when includingcloud radiative effects, suggesting this important mechanism can not beneglected. Additionally, we further demonstrate that the cloud structure issensitive to not only the cloud sedimentation efficiency (termed$f_{\textrm{sed}}$ in EddySed), but also the temperature-pressure profile ofthe deeper atmosphere. We briefly discuss the large difference between theresolved cloud structures of this work, adopting a phase-equilibrium andparameterised cloud model, and our previous work incorporating a cloudmicrophysical model, although a fairer comparison where, for example, the samelist of constituent condensates is included in both treatments, is reserved fora future work. Our results underline the importance of further study into thepotential condensate size distributions and vertical structures, as bothstrongly influence the radiative impact of clouds on the atmosphere. Finally,we present synthetic observations from our simulations reporting an improvedmatch, over our previous cloud-free simulations, to the observed transmission,HST WFC3 emission and 4.5 $\mu$m Spitzer phase curve of HD 209458b.Additionally, we find all our cloudy simulations have an apparent albedoconsistent with observations.

monthly notices of the royal astronomical society

Overcast on Osiris: 3D radiative-hydrodynamical simulations of a cloudy  hot Jupiter using the parameterised, phase-equilibrium cloud formation code  EddySed