Fig. 1: Atmospheric He fractions, pressures and optical radii.
From: Earth-mass planets with He atmospheres in the habitable zone of Sun-like stars
a, Atmospheric He fraction at the end of the evolution simulations as a function of planetary mass and considering the solar-like host star as a slow-, moderate- or fast-rotating young G-type star. Planets in the dotted part of the lines subsequently lose their remaining primordial atmospheres in a geologically short timescale. Planets in the solid parts keep remnants of their thermally stable primordial atmospheres. The vertical black dashed lines show the critical planetary mass above which thermally stable atmospheres remain. b, The total and partial pressures for planets with thermally stable atmospheres. c, The final broadband photospheric radii rph (in the optical) of the planets with thermally stable atmospheres.
