\rangle$ the mean particle size as defined in Eq. \[eq:amean2\]. Figure \[fig:&lt;&lt;a&gt;&gt;\_Parm\] very clearly shows the anti-correlation between the nucleation rate (top) and the mean cloud particle size (middle) also in these column integrated values: The dayside (orange) shows a distinctly lower column integrated seed formation rate than the nightside which corresponds to distinctly larger average mean particle sizes on the dayside compared to the nightside. The terminator profiles are not included in Fig. \[fig:&lt;&lt;a&gt;&gt;\_Parm\].

Figure \[fig:&lt;&lt;a&gt;&gt;\_Parm\] (bottom) shows the column integrated values for the material composition ($\int_{\rm zmin}^{\rm zmax} (V_{\rm s}(z)/V_{\rm tot}(z))\,dz$) for the substellar and the anti-stellar point, and the two equatorial terminator points. These values demonstrate the contribution of the individual material groups to the composition of the whole cloud at this longitudes and latitudes. It suggests that the mineral clouds that form on WASP-43b are mainly made of silicates, metal oxides and high-temperature condensates. Salts like KCl\[s\] play a less important role in the frame of the model used here.

These integrated values do, however, not provide much insight into cloud formation in particular pressure regimes like for example the low-pressure regime that is tested by transmission spectroscopy.

Gas phase composition in chemical equilibrium {#s:cheq}
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