photochemical simulations to derive the steady-state distribution of gaseous species. Then, assuming the production rate of haze monomers at each altitude as the sum of the photodissociation rates of the major hydrocarbons in our photochemical model, $\mathrm{CH_4}$, $\mathrm{HCN}$, and $\mathrm{C_2H_2}$, we derive the steady-state distribution of haze particles by the particle growth simulations. In the particle growth simulation, distribution of haze particles is derived considering coagulation of homo-disperse monomers, gravitational sedimentation, and diffusion. Neither evaporation nor condensation is considered. Thermal decomposition such as considered in [@2017ApJ...847...32L] can be important in such a hot atmosphere of WASP-43b, but is ignored due to the uncertainty of the thermal stability of haze. We adopt the haze monomer radius of 1 nm and its density of 1 $\mathrm{g}$ $\mathrm{cm^{-3}}$. The haze formation feedback on the atmospheric chemistry such as the elemental depletion is not considered due to the high computational cost. For the details of the photochemical and particle growth models, see [@2018ApJ...853....7K].

We choose four representative points along the equator ($\theta = 0\degree$) to perform the haze formation simulations because of the high computational cost; sub-stellar point ($\phi = 0\degree$), evening terminator ($\phi = 90\degree$), anti-stellar point ($\phi = 180\degree$), and morning terminator 