Effect of vapor abundances at the lower boundary of atmosphere on the solid, vapor, nuclei profile, particle size, and cloud composition. (a) 10×-Z hot Jupiter model; (b) C/O=0.9 hot Jupiter model; (c) C/O=0.9 hot Jupiter model, similar to (b), but with injection of larger nuclei deeper in the atmosphere, mimicking nucleation featuring high particle surface tension. The thick solid, dashed, and dotted lines indicate total cloud, vapor, and nuclei mixing ratios, respectively. The purple solid line shows the particle size. The right subpanel in each panel shows the composition of the cloud particles in mass. Compared to the default model (Figure 3) the upper cloud layers of the 10×-[Z] run become devoid in Mg (SiO₂ dominates) while in the C/O=0.9 run Fe-bearing cloud particles make it into the upper regions.