Energy deposition in Saturn’s equatorial upper atmosphere

We construct Saturn equatorial neutral temperature and density profiles of H, H$_2$, He, CH$_4$, between 10$^{-12}$ 1 bar using measurements from Cassini's Ion Neutral Mass Spectrometer (INMS) taken during the spacecraft's final plunge into Saturn's atmosphere on 15 September 2017, combined with previous deeper atmospheric Cassini Composite InfraRed (CIRS) UltraViolet Imaging Spectrograph (UVIS). These are fed an energy deposition model employing soft X-ray Extreme (EUV) solar fluxes at a range spectral resolutions ($\Delta\lambda=4\times10^{-3}$ nm to nm) assembled TIMED/SEE, SOHO/SUMER, Whole Heliosphere Interval (WHI) quiet Sun campaign. Our calculates ion production rate through photo-ionisation electron-impact ionisation processes, as well rates photo-dissociation CH$_4$. The reaction we determine important obtain accurate profiles, meanwhile methane is key initiate complex organic chemical processes. assess importance resolution in by high-resolution H$_2$ photo-absorption cross section, which has effect producing additional peaks near 800 km altitude. find that these still formed when low-resolution ($\Delta\lambda=1$ or mid-resolution ($\Delta\lambda=0.1$ spectra, long sections included model.