FIG. 13.
A selection of M and K dwarf super-Earths that could have detectable O2 atmospheres if they formed with abundant surface water; as before, the dashed lines represent the RG and MG limits. Calculations were performed assuming a mass of 5 M⊕, an initial water content of 10 TO, and diffusion-limited escape. Contours correspond to the equivalent O2 atmospheric pressure in bar at the end of the runaway phase, assuming all the O2 remains in the atmosphere. Of the planets shown here, only Kepler-62f does not build up any oxygen.