then the size distributions.

Condensate Mass Profiles
------------------------

The eddy diffusion coefficient ($K$) for $q_{\rm t}$ is assumed to be the same as that for heat as derived for free convection (Gierasch and Conrath, 1985): $$\begin{aligned}
\label{K_equals}
K = \frac{H}{3} \left( \frac{L}{H} \right)^{4/3}
    \left( \frac{R F}{\mu \rho_{\rm a} c_{\rm p}} \right)^{1/3}\end{aligned}$$ where the atmospheric scale height is given by $H = R T / \mu g$ (for Jupiter we use $g$ = 25 m s$^{-2}$), $L$ is the turbulent mixing length, $R$ the universal gas constant, $\mu$ the atmospheric molecular weight (2.2 g mol$^{-1}$ assumed here), $\rho_{\rm a}$ the atmospheric density, and $c_{\rm p}$ the specific heat of the atmosphere at constant pressure (ideal gas assumed). Here we assume all the interior heat to be transported through the convective heat flux: $F = \sigma T_{\rm eff}^4$, where $\sigma$ is the Stefan-Boltzmann constant and the effective temperature for Jupiter is $T_{\rm eff}$ = 124 K. In the general case, a profile of $F$ is specified by an external model, which partitions the transport of interior heat between radiative and convective fluxes. The convective heat flux can be reduced further by other heat fluxes, such as para hydrogen conversion or latent heat 