Fig. 9
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Relative difference in transit radius between the model of Jin et al. (2014) and model D of Parmentier & Guillot (2014) used in BICEPS, as a function of planetary equilibrium temperature. The relative difference was calculated as in Eq. (50) for three different planetary volatile mass fractions of 10−2 (dark blue), 10−3 (blue) and 10−5 (light blue) and two exoplanet masses: 5 mE (solid) and 10 mE (dashed).
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