  We present a reanalysis (using the Minnaert limb-darkening approximation) of
visible/near-infrared (0.3 - 2.5 micron) observations of Uranus and Neptune
made by several instruments. We find a common model of the vertical aerosol
distribution that is consistent with the observed reflectivity spectra of both
planets, consisting of: 1) a deep aerosol layer with a base pressure > 5-7 bar,
assumed to be composed of a mixture of H2S ice and photochemical haze; 2) a
layer of photochemical haze/ice, coincident with a layer of high static
stability at the methane condensation level at 1-2 bar; and 3) an extended
layer of photochemical haze, likely mostly of the same composition as the
1-2-bar layer, extending from this level up through to the stratosphere, where
the photochemical haze particles are thought to be produced. For Neptune, we
find that we also need to add a thin layer of micron-sized methane ice
particles at ~0.2 bar to explain the enhanced reflection at longer
methane-absorbing wavelengths. We suggest that methane condensing onto the haze
particles at the base of the 1-2-bar aerosol layer forms ice/haze particles
that grow very quickly to large size and immediately 'snow out' (as predicted
by Carlson et al. 1988), re-evaporating at deeper levels to release their core
haze particles to act as condensation nuclei for H2S ice formation. In
addition, we find that the spectral characteristics of 'dark spots', such as
the Voyager-2/ISS Great Dark Spot and the HST/WFC3 NDS-2018, are well modelled
by a darkening or possibly clearing of the deep aerosol layer only.
