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We calculated an atmospheric grid for hot mini-Neptune and giant exoplanets,that links astrophysical observable parameters- orbital distance and stellartype- with the chemical atmospheric species expected. The grid can be appliedto current and future observations to characterize exoplanet atmospheres andserves as a reference to interpret atmospheric retrieval analysis results. Tobuild the grid, we developed a 1D code for calculating the atmospheric thermalstructure and link it to a photochemical model that includes disequilibriumchemistry (molecular diffusion, vertical mixing and photochemistry). We comparethermal profiles and atmospheric composition of planets at different semimajoraxis (0.01$\leq$a$\leq$0.1AU) orbiting F, G, K and M stars. Temperature and UVflux affect chemical species in the atmosphere. We explore which effects aredue to temperature and which due to stellar characteristics, showing thespecies most affected in each case. CH$_4$ and H$_2$O are the most sensitive toUV flux, H displaces H$_2$ as the most abundant gas in the upper atmosphere forplanets receiving a high UV flux. CH$_4$ is more abundant for cooler planets.We explore vertical mixing, to inform degeneracies on our models and in theresulting spectral observables. For lower pressures observable species likeH$_2$O or CO$_2$ can indicate the efficiency of vertical mixing, with largermixing ratios for a stronger mixing. By establishing the grid, testing thesensitivity of the results and comparing our model to published results, ourpaper provides a tool to estimate what observations could yield. We apply ourmodel to WASP-12b, CoRoT-2b, XO-1b, HD189733b and HD97658b.

astrophysical journal/the astrophysical journal

Exploring atmospheres of hot mini-Neptunes and extrasolar giant planets  orbiting different stars with application to HD 97658b, WASP-12b, CoRoT-2b,  XO-1b and HD 189733b