this challenge in due time.

A theoretical analysis of kinetically forming, mineral clouds on WASP-43b {#s:clouds}
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In this section, we discuss the principle results for mineral cloud formation in the hot Jupiter WASP-43b to enable a detailed insight into the cloud properties that will shape the JWST spectrum of WASP-43b. In Sect. \[s:ncheq\], we show in how far photochemical hydrocarbon haze formation does complete this picture of cloud formation in the atmosphere of WASP-43b leading to the idea of the possible presence of two chemically distinct cloud ensembles if photochemical processes affect the chemical carbon reservoir of the atmosphere (Sect. \[s:twocloud\]).

[*Firstly,*]{} we observe that nucleation seeds form for all the 1D profiles used here to probe cloud formation in the 3D atmosphere of WASP-43b (Fig. \[TpNuc\], right, top). This is in stark contrast to the ultra-hot Jupiters, like WASP-18b and HAT-P7b, but in line with other hot Jupiters like HD189733b and HD209458b. [*Secondly,*]{} the rate of seed formation differs strongly between the day and the nightside because of the different thermodynamic conditions. The seed formation is more efficient on the nightside where SiO seeds dominate in the low-pressure part of the atmosphere. Once SiO\[s\] surface growth kicks in 