in clouds, a finding similar to HD189733b and HD209458b, and hazes that mainly occur on the dayside and in the terminator regions. We suggest that spectra and phase-curves of irradiated exoplanets, and giant gas planet like WASP-43b in particular, may be confused by the co-existence of hydrocarbon haze particles and mineral seed particles in the upper most atmosphere that is accessible by transmission spectroscopy. These are atmospheric regions of low gas density where photochemical processes enable the formation of hydrocarbon haze particles but where surface growth processes are still far too inefficient to cause a substantial growth of the mineral particles (in fact, of any particle).

Section \[s:ap\] summarises our approach and provides necessary details to allow a comparison to our previous modelling method. Section \[s:Tp\] gives an account of the temperature structure which is a major driver of the cloud formation. Sect. \[s:clouds\] presents our analysis of the kinetically forming mineral clouds in WASP-43b. Section \[s:cheq\] summarises our general findings for the gas-phase composition assuming chemical equilibrium. Here we discuss the validity of assuming a constant mean molecular weight, the carbon-to-oxygen ratio and the degree of ionsation. Section \[s:ncheq\] addresses the effect of mixing processes on the abundance of 