  We present a new two-dimensional, bin-scheme microphysical model of cloud
formation in the atmospheres of hot Jupiters that includes the effects of
longitudinal gas and cloud transport. We predict cloud particle size
distributions as a function of planetary longitude and atmospheric height for a
grid of hot Jupiters with equilibrium temperatures ranging from 1000-2100 K.
The predicted 2D cloud distributions vary significantly from models that do not
consider horizontal cloud transport and we discuss the microphysical and
transport timescales that give rise to the differences in 2D versus 1D models.
We find that the horizontal advection of cloud particles increases the cloud
formation efficiency for nearly all cloud species and homogenizes cloud
distributions across the planets in our model grid. In 2D models, certain cloud
species are able to be transported and survive on the daysides of hot Jupiters
in cases where 1D models would not predict the existence of clouds. We
demonstrate that the depletion of condensible gas species varies as a function
of longitude and atmospheric height across the planet, which impacts the
resultant gas-phase chemistry. Finally, we discuss various model sensitivities
including the sensitivity of cloud properties to microphysical parameters,
which we find to be substantially less than the sensitivity to the atmospheric
thermal structure and horizontal and vertical transport of condensible
material.
