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In this work we study the effect of disequilibrium processes on mixing ratioprofiles of neutral species and on the simulated spectra of a hot Jupiterexoplanet that orbits stars of different spectral types. We also address theimpact of stellar activity that should be present to a different degree in allstars with convective envelopes. We used the VULCAN chemical kinetic code tocompute number densities of species. The temperature-pressure profile of theatmosphere was computed with the HELIOS code. We also utilized the $\tau$-ReXforward model to predict the spectra of planets in primary and secondaryeclipses. In order to account for the stellar activity we made use of theobserved solar XUV spectrum taken from Virtual Planetary Laboratory (VPL) as aproxy for an active sun-like star. We find large changes in mixing ratios ofmost chemical species in planets orbiting A-type stars that radiate strong XUVflux inducing a very effective photodissociation. For some species, thesechanges can propagate very deep into the planetary atmosphere to pressures ofaround 1 bar. To observe disequilibrium chemistry we favor hot Jupiters withtemperatures Teq=1000 K and ultra-hot Jupiters with Teq=3000$ K that also havetemperature inversion in their atmospheres. On the other hand, disequilibriumcalculations predict little changes in spectra of planets with intermediatetemperatures. We also show that stellar activity similar to the one of themodern Sun drives important changes in mixing ratio profiles of atmosphericspecies. However, these changes take place at very high atmospheric altitudesand thus do not affect predicted spectra. We estimate that the effect ofdisequilibrium chemistry in planets orbiting nearby bright stars could berobustly detected and studied with future missions with spectroscopiccapabilities in infrared such as, e.g., JWST and ARIEL.

Stellar impact on disequilibrium chemistry and on observed spectra of hot Jupiter atmospheres