All Tables

Table 1: Radius and central thermodynamic properties of a planet of mass $M_{\rm P}=20~{M}_\oplus$ at 1 Gyr with a total heavy element mass fraction $Z=(M_Z/M_{\rm P})=50\%$ . Results for different heavy element compositions (water = W, rock = R, iron = I) and EOS (aneos = a, sesame = s, SCVH = SC) and different heavy element distributions are given.
Table 2: Radius and central thermodynamic properties of a planet of mass $M_{\rm P}=1~M_{\rm J}$ at 1 Gyr for two heavy element mass fractions $Z=(M_Z/M_{\rm P})=50$ % and Z=20%. The labels are the same as in Table 1. As mentioned at the end of Sect. 4.2, for Z=50%, the solution with $~{M}_{\rm core}=0$ and $Z=~{Z}_{\rm env}$ is similar to a solution with $~{M}_{\rm core}\sim 10~{M}_\oplus$ and the rest of the heavy material distributed in the envelope.
Table 3: Radius of a 22.6 ${M}_\oplus$ planet at 2 Gyr with different water core masses, EOS and levels of irradiation, characterised by a stellar incident flux, $F_{\rm inc}$ . Two cases are considered: no irradiation ( $F_{\rm inc}=0$ ) and $F_{\rm inc}=6\times F_{\rm inc}$ of GJ 436b. Comparison is done with the pure water (ice) case of Seager et al. (2007). Results based on the assumption of a uniform core temperature of T=300 K are also given.
Table 4: Radii of planets (in $R_{\rm J}$ ) in the mass range 20 ${M}_\oplus$ -1 $M_{\rm J}$ for different levels of heavy element enrichment Z (see text, Sect. 7.2, for the choice of the heavy material distribution) and at different ages.
Table 5: Same as Table 4 for irradiated models by a Sun at 0.045 AU.