and material composition, can change throughout a planetary atmosphere because the thermodynamic conditions change vertically and horizontally. This has been demonstrated for WASP-43b in the previous sections. The vertical structures have been shown to be very inhomogeneous such that not one value suffices to describe exoplanet clouds, and the same holds for the horizontal cloud distributions for which we have not only demonstrated a large day-night difference but our model suggests also a west-east change in cloud properties on the dayside of WASP-43b. Despite this complexity, column integrated mean values of selected cloud properties do recover our major findings from the previous, more detailed discussions as follows.

Figure \[fig:&lt;&lt;a&gt;&gt;\_Parm\] (top) shows the column integrated total nucleation rate $\int_{\rm zmin}^{\rm zmax} J_*(z) dz$ \[cm$^{-2}$ s$^{-1}$\] with $J_*=\sum_{\rm s} J_{\rm s}$ ($s=\,$, SiO, C, KCl), $z_{\rm min}$ and $z_{\rm max}$ spanning the geometric extension of the atmosphere at each of 18 (out of 97) selected (longitudes, latitude)-profiles. Figure \[fig:&lt;&lt;a&gt;&gt;\_Parm\] (middle) provides the height-averaged, number density weighted cloud mean particle size $\langle\langle a \rangle\rangle = (\int_{\rm zmin}^{\rm zmax} n_{\rm d}(z)\langle a(z) \rangle \,dz)/( \int_{\rm zmin}^{\rm zmax} n_{\rm d}(z) \,dz)$ \[$\mu$m\] with $n_{\rm d}(z)$ \[cm$^{-3}$\] the local cloud particle number density, and $\langle a(z) 