Fig. 3: Metallicity impacts on the atmosphere.
From: Metal-rich stars are less suitable for the evolution of life on their planets
a–c The change of surface UV-C (202 to 230 nm, W/m2) with [Fe/H] for O2 levels of 2% (light blue), 1% (magenta), 0.2% (blue) and 0.02% (red). The dashed lines indicate the UV-C levels of 5 × 10−5 and 10−3 W/m2. d–f Impact of O2 content and [Fe/H] on CH4 lifetime. g–l Dependencies of O3 column density (g–i DU) and surface UV-B (j–l W/m2) on O2 content and stellar metallicity [Fe/H]. m–o The same as j-l but for an O2 content less than 5%. a–o The calculations were performed for stellar Teff of 6300 K (left), 5800 K (center) and 5300 K (right). The grey and white curves (j–o) represent surface UV-B of 0.82 W/m2 (220 DU, ozone hole definition) and 1.65 W/m2 (80 DU, extreme in ozone hole), respectively. Source data are provided as a Source Data file.
