LOCCI, DanieleDanieleLOCCIARESU, GiambattistaGiambattistaARESUPETRALIA, AntoninoAntoninoPETRALIAMICELA, GiuseppinaGiuseppinaMICELAMAGGIO, AntonioAntonioMAGGIOCECCHI-PESTELLINI, CesareCesareCECCHI-PESTELLINI2025-04-032025-04-0320242632-3338http://hdl.handle.net/20.500.12386/37033High-energy radiation from stars impacts planetary atmospheres, deeply affecting their chemistry and providing departures from chemical equilibrium. While the upper atmospheric layers are dominated by ionizations induced by extreme-ultraviolet radiation, deeper into the atmosphere, molecular abundances are controlled by a characteristic X-ray-dominated chemistry, mainly driven by an energetic secondary electron cascade. In this work, we aim at identifying molecular photochemically induced fingerprints in the transmission spectra of a giant planet atmosphere. We have developed a numerical code capable of synthesizing transmission spectra with arbitrary spectral resolution, exploiting updated infrared photoabsorption cross sections. Chemical mixing ratios are computed using a photochemical model tailored to investigate high-energy ionization processes. We find that in the case of high levels of stellar activity, synthetic spectra in both low and high resolutions show significant, potentially observable out-of-equilibrium signatures arising mainly from CO, CH4, C2H2, and HCN.ELETTRONICOenArticle10.3847/PSJ/ad24e42-s2.0-85186716369https://iopscience.iop.org/article/10.3847/PSJ/ad24e4FIS/05 - ASTRONOMIA E ASTROFISICA