Context : Having a short orbital period and being tidally locked makes WASP-43b an ideal candidate for JWST phase curve measurements .
Phase curve observations of an entire orbit will enable the mapping of the atmospheric structure across the planet , with different wavelengths of observation allowing different atmospheric depths to be seen .

Aims : We provide insight into the details of the clouds that may form on WASP-43b , and their impact on the remaining gas phase , in order to prepare the forthcoming interpretation of the JWST and follow-up data .

Methods : We follow a hierarchical modelling strategy .
We utilize 3D GCM results as input for a kinetic , non-equilibrium model for mineral cloud particles , and for a kinetic model to study a photochemicaly-driven hydrocarbon haze component .

Results : Mineral condensation seeds form throughout the atmosphere of WASP-43b .
This is in stark contrast to the ultra-hot Jupiters , like WASP-18b and HAT-P-7b .
The dayside is not cloud free but is loaded with few but large mineral cloud particles in addition to hydrocarbon haze particles of comparable abundance .
Photochemically driven hydrocarbon haze appears on the dayside , but does not contribute to the cloud formation on the nightside .
The geometrical cloud extension differs across the globe due to the changing thermodynamic conditions .
Day and night differ by 6000km in pressure scale height .
As reported for other planets , the C/O is not constant throughout the atmosphere and varies between 0.74 and 0.3 .
The mean molecular weight is approximately constant in a \ce H2-dominated WASP-43b atmosphere because of the moderate day/night-temperature differences compared to the super-hot Jupiters .

Conclusions : WASP-43b is expected to be fully covered in clouds which are not homogeneously distributed throughout the atmosphere .
The dayside and the terminator clouds will be a combination of mineral particles of locally varying size and composition , and of hydrocarbon hazes .
The optical depth of hydrocarbon hazes is considerably lower than that of mineral cloud particles such that a wavelength-dependent radius measurement of WASP-43b would be determined by the mineral cloud particles but not by hazes .