individual nucleation rates, $J_{\rm s}$ \[cm$^{-3}$ s$^{-1}$\], for s=, SiO, KCl, C on four selected (longitude, latitude) 1D profiles from the 3D GCM (@Parmentier2018) for WASP-43b. [**Top:**]{} dayside, [**Bottom:**]{} nightside. []{data-label="fig:NucRateDayNight"}](images/43b_NucNight.pdf "fig:"){width="1.0\linewidth"}

![Drift velocity for all 1D trajectories of WASP-43b. The nighside profiles are shown in blue, the dayside profiles in orange, the terminator profiles in grey.[]{data-label="fig:vdr"}](images/vdrift_Type2.pdf){width="\linewidth"}

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![image](images/5line_matvolfrac_-9000.pdf){width="0.45\linewidth"} ![image](images/5line_matvolfrac_9000.pdf){width="0.45\linewidth"}\
![image](images/5line_matvolfrac_0000.pdf){width="0.45\linewidth"} ![image](images/5line_matvolfrac_-18000.pdf){width="0.45\linewidth"}

The lower boundary of the seed formation region (see Fig. \[TpNuc\], right) does not coincide with the lower boundary of the cloud (compare Fig. \[fig:DusttoGas\], left) because the particles grow and fall (gravitational settle) through the atmosphere into deeper, warmer atmospheric regions of increasing pressure. The growth in these warm regions is supported by the increasing gas pressure which increases the collision rates. The higher pressures further stabilises materials that already formed at high temperatures. The inner cloud boundary is set by the thermal stability of the particles of a particular size; big particles survive longer as they have more material to evaporate.

Figure \[fig:DusttoGas\] (left) demonstrates that the cloud particles sizes are not homogeneous but change for all 1D profiles probed in our study. Figure \[fig:DusttoGas\] 