Abstract EANA2024-75

Exoplanets exist around most stellar types in systems different and far away from our solar system. Those various possibilities result in a large diversity of atmospheric climates and cloud structures on the exoplanets. This work focuses on tidally locked gaseous exoplanets with an equilibrium temperature between 1600 K to 2600 K which orbit an F- or G-type host star. There is a strong temperature contrast between the day- and night-sides of the planets, which leads to extreme climatic conditions including strong equatorial wind jets.  For modelling the atmospheric structure of the exoplanets, a hierarchical approach was used. The temperature and wind structure, which are calculated using the 3D climate model expeRT/MITgcm, are used to create a grid of one-dimensional temperature, pressure and wind profiles. These are then used for the detailed microphysical cloud formation model. To consider the effect of different elemental replenishment efficiencies, two mixing types were considered in the model: normal and scaled. The results show that the equilibrium temperature, the associated distance to the star, as well as the mixing type has a strong impact of the cloud structures. Exoplanets with a high equilibrium temperature only form clouds on the night-side and the morning terminator while exoplanets with a lower equilibrium temperature can form clouds globally. A less efficient element replenishment via scaled mixing leads to a lower dust-to-gas ratio and a smaller size of the cloud particles. The results presented in this study can support the physical interpretation of observations of exoplanets with e.g. JWST, CHEOPS and PLATO.