Fig. 11
Mass-radius relationship for pure-water planets in an isothermal model. The surface temperature and pressure are indicated in the figure and compared to the result of Seager et al. (2007) over the entire range of planets currently detected (panel a); for planets with mass less than 10 MEarth (panel b). Isothermal models for pure silicates (MgSiO3) and iron (Fe) (Bouchet et al. 2013; Mazevet et al. 2015) are also displayed.
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