a scale factor to the particle sedimentation.

For radiative calculations, Lunine et al. (1989) assume all particles in the frozen-in and dust-like clouds are 1 and 10 $\mu$m in radius, respectively.

Marley et al. (1999)
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The Marley et al. (1999) model of water and silicate clouds in extrasolar giant planets represents a variation on the Lewis (1969) model. As in the Lewis model, the calculation of vapor pressure (or equivalently, $q_{\rm v}$) assumes that any supersaturation is quenched locally by condensation (Equation \[lewis\_qv\]). However, the calculation of the condensate mole fraction ($q_{\rm c}$) represents a departure: instead of calculating it from the vapor pressure in the underlying layer from Equation \[lewis\_qc\], Marley et al. scale it to the local saturation vapor pressure with the following assumption: $$q_{\rm c}(z) = \cases{0 & if $q_{\rm v}(z-\Delta z) < q_{\rm s}(z)$ \cr
                f_{\rm s} q_{\rm s}(z) & otherwise \cr }$$ The parameter $f_{\rm s}$ corresponds to the potential supersaturation prior to condensation. Marley et al. (1999) treat $f_{\rm s}$ as an adjustable parameter, ranging from a baseline value of 0.01 to an extreme value of 1. The baseline model as applied to the Jovian ammonia cloud is shown in Figure 1. The 