taken into account. For the simulation of the sub-stellar point, we ignore the diurnal variation factor of 1/2 in the expression of the photodissociation rate [see @2018ApJ...853....7K Eq. (3)], which we adopt for the terminator points, and for that of the anti-stellar point, we ignore photochemistry. Finally, as for the zenith angle of the stellar irradiation, which should be $0.0^{\circ}$ for the sub-stellar point while the value somewhat smaller than $90.0^{\circ}$ for the terminator if the host star is spatially resolved, we use the globally-averaged value of $57.3^{\circ}$ [@2012ApJ...761..166H] for all the points for simplicity.

The warm atmosphere of WASP-43b {#s:Tp}
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Figure \[TpNuc\] (left) visualises the thermodynamic input that we utilize for our following study of cloud and haze formation and the gas-phase composition in the atmosphere of WASP-43b. WASP-43b is a hot Jupiter that is assumed to be tidally locked with its host star which results in a dayside that is hotter than the nightside. The resulting gas temperature difference of $\approx 700$K at a gas pressure of $\approx 10^{-4}$ bar drives a global circulation from the day to the nightside (@Parmentier2018 [@2018AJ....155..150M]). A smaller temperature difference is suggested between the substellar and anti-stellar point (top left) and 