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Photochemistry is expected to change the chemical composition of the upperatmospheres of irradiated exoplanets through the dissociation of species, suchas methane and ammonia, and the association of others, such as hydrogencyanide. Although primarily the high altitude day side should be affected byphotochemistry, it is still unclear how dynamical processes transportphotochemical species throughout the atmosphere, and how these chemicaldisequilibrium effects scale with different parameters. In this work weinvestigate the influence of photochemistry in a two-dimensional context, bysynthesizing a grid of photochemical models across a large range oftemperatures. We find that photochemistry can strongly change the atmosphericcomposition, even up to depths of several bar in cool exoplanets. We furtheridentify a sweet spot for the photochemical production of hydrogen cyanide andacetylene, two important haze precursors, between effective temperatures of 800and 1400 K. The night sides of most cool planets (effective temperature < 1800K) are shown to host photochemistry products, transported from the day side byhorizontal advection. Synthetic transmission spectra are only marginallyaffected by photochemistry, but we suggest that observational studies probinghigher altitudes, such as high-resolution spectroscopy, take photochemistryinto account.

Grid of pseudo-2D chemistry models for tidally locked exoplanets -- II. The role of photochemistry