of mineral clouds are determined by local thermodynamic properties which are the result of 3D dynamic atmosphere simulations. Horizontal transport can affect both the cloud formation and the cloud properties. Figure 4 in [@Lee2015] shows for the gas giant HD189733b (orbiting a similar host star to that of WASP-43b but at a larger orbital distance of 0.0314 AU) that the (vertical) settling of the cloud particles occurs at time scales longer then a typical (horizontal) advection time scale on the nightside but that the settling and advection are of comparable magnitudes on the dayside. Cloud particle properties such as particle size or particle composition should be smeared out in longitude compared to the results shown here. We note that comparing @Lee2015 (without horizontal advection) and  @Lee2016 (including horizontal advection), the non-coupled problem is both more computationally feasible, easier to interpret and provides reasonable first order insights into the expected mean cloud particle size and composition, cloud distribution and gas phase depletion in exoplanet atmospheres. The situation is somewhat different for photochemically triggered cloud formation. Photochemical hydrocarbon-haze production, for example, is determined by the external radiation field. A certain smearing out of the hydrocarbon haze properties should also be expected for 