Influence of various M-dwarf SEDs on the temperature profile (K) of an Earth-like planet. The stellar spectra of Fig. 1 are scaled to reproduce a surface temperature of 288.15 K (see Table 2). Each coloured line represents the temperature profile of the modelled hypothetical planet orbiting a different host star. Weak UV emission of M dwarfs leads to low O₃ heating inthe middle atmosphere and therefore to a reduced or missing temperature inversion. Enhanced CH₄ heating increases the temperature in the middle atmosphere of Earth-like planets around late-type M dwarfs by up to 60 K.