  We present the first application of a bin-scheme microphysical and vertical
transport model to determine the size distribution of titanium and silicate
cloud particles in the atmospheres of hot Jupiters. We predict particle size
distributions from first principles for a grid of planets at four
representative equatorial longitudes, and investigate how observed cloud
properties depend on the atmospheric thermal structure and vertical mixing. The
predicted size distributions are frequently bimodal and irregular in shape.
There is a negative correlation between total cloud mass and equilibrium
temperature as well as a positive correlation between total cloud mass and
atmospheric mixing. The cloud properties on the east and west limbs show
distinct differences that increase with increasing equilibrium temperature.
Cloud opacities are roughly constant across a broad wavelength range with the
exception of features in the mid-infrared. Forward scattering is found to be
important across the same wavelength range. Using the fully resolved size
distribution of cloud particles as opposed to a mean particle size has a
distinct impact on the resultant cloud opacities. The particle size that
contributes the most to the cloud opacity depends strongly on the cloud
particle size distribution. We predict that it is unlikely that silicate or
titanium clouds are responsible for the optical Rayleigh scattering slope seen
in many hot Jupiters. We suggest that cloud opacities in emission may serve as
sensitive tracers of the thermal state of a planet's deep interior through the
existence or lack of a cold trap in the deep atmosphere.
