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Fig. 6.12. Planetary mass-radius diagram (from Gillon et al. 2007a) comparing the position of Solar System planets, transiting hot Jupiters (diamonds), and GJ 436 b. The lines indicate the position of the Fortney et al. (2007) models for different compositions: pure iron, pure silicate, pure water ice (with thermal profiles from Solar System planets), and models for irradiated planets at 0.1 au from a Solar-type star with a fraction of 10%, 50% and 100% of Hydrogen/Helium. The dotted lines show the models for a cold (a = 10 au) and very hot (a = 0.02 au) pure H/He gas giant.

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Fig. 6.12. Planetary mass-radius diagram (from Gillon et al. 2007a) comparing the position of Solar System planets, transiting hot Jupiters (diamonds), and GJ 436 b. The lines indicate the position of the Fortney et al. (2007) models for different compositions: pure iron, pure silicate, pure water ice (with thermal profiles from Solar System planets), and models for irradiated planets at 0.1 au from a Solar-type star with a fraction of 10%, 50% and 100% of Hydrogen/Helium. The dotted lines show the models for a cold (a = 10 au) and very hot (a = 0.02 au) pure H/He gas giant.

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