modelling step which is a kinetic cloud formation model consistently combined with equilibrium gas-chemistry calculations. We utilise 97 1D (T$_{\rm
  gas}$(z), p$_{\rm gas}$(z), v$_{\rm z}(x,y,z)$)-profiles for WASP-43b similar to our work on HAT-P-7b as visualised in Fig. 1: T$_{\rm gas}$(z) is the local gas temperature \[K\], p$_{\rm gas}$(z) is the local gas pressure \[bar\], and v$_{\rm z}$(x,y,z) is the local vertical velocity component \[cm s$^{-1}$\]. The same 1D profiles are used as input for our third modelling step, the kinetic haze simulation (@2018ApJ...853....7K [@2019ApJ...876L...5K; @2019ApJ...877..109K]). The same, height-dependent mixing coefficient $K_{\rm zz}$, which is assumed as $H v_{\rm z}$ with $H$ being the atmospheric scale height, is used in both the kinetic cloud formation and the kinetic haze formation model. We use the solar element abundances from for the undepleted element abundances.

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  ![image](images/Wasp43b.pdf){width="1.0\linewidth"}                ![image](images/NucRate_Type2.pdf){width="1.1\linewidth"}
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![Comparison of WASP-43b to the ultra-hot Jupiter WASP-18b (red) and [Drift-Phoenix]{} young planets / brown dwarf atmosphere structures for log(g)=3.0 and T$_{\rm eff}=1000\,\ldots\,3000$K [ by steps of 200K]{} (). []{data-label="TpDP"}](images/18b_43b_BD.pdf){width="0.9\linewidth"}

The hierarchical approach has the limitation of not explicitly taking into account the potential effect of horizontal winds on cloud formation. However, processes governing the formation 