further demonstrates that cloud particles are present thought almost the entire atmospheric volume sampled here, in particular also on both the day- and the nightside. The characteristic cloud properties, however, are different between the day- and the nightside. As consequence of the seed formation discussed with regard to Fig. \[TpNuc\] (right), the mean cloud particle sizes are larger over a larger pressure range on the easterly dayside ($\phi=0^o\rightarrow 90^o$) compared to the westerly dayside ($\phi=0^o\rightarrow 270^o$) and the nightside (Fig.\[fig:DusttoGas\], middle left). A similar but less pronounced asymmetry occurs for the terminator regions (Fig.\[fig:DusttoGas\], bottom left).

The cloud opacity is determined by the cloud particles sizes, their abundance and their material properties. The dust-to-gas ratio, $\rho_{\rm d}/\rho_{\rm gas}$ (Fig.\[fig:DusttoGas\], right) combines these properties and visualises where the highest cloud mass load occurs in an atmosphere. $\rho_{\rm d}/\rho_{\rm gas}$ shows that only the inner part of the WASP-43b atmosphere is cloud-free. The largest $\rho_{\rm d}/\rho_{\rm gas}$ occurs on the nightside and reaches well across the morning terminator at $\phi=270^o$. The dayside is not cloud free but has a considerable lower cloud load, hence, it might be mistakenly interpreted as cloud-free.

Simple time scale estimate shows that cloud particle of sizes $\langle 