Table 1
Planet radii for various planetary masses and cooling timescales.
| Mass [M⊕] | tcore [Gyr] | Radius [R⊕] | ||
|---|---|---|---|---|
| at 1 Gyr | at 5 Gyr | at 10 Gyr | ||
| 3 | std | 1.76 | 1.71 | 1.7 |
| 3 | 0.1 | 1.82 | 1.71 | 1.7 |
| 3 | 1 | 2.13 | 1.76 | 1.71 |
| 3 | 10 | 1.91 | 1.87 | 1.82 |
| 5 | std | 2.81 | 2.6 | 2.57 |
| 5 | 0.1 | 2.91 | 2.6 | 2.57 |
| 5 | 1 | 3.45 | 2.76 | 2.6 |
| 5 | 10 | 3.1 | 2.98 | 2.86 |
| 10 | std | 3.47 | 3.28 | 3.23 |
| 10 | 0.1 | 3.55 | 3.29 | 3.23 |
| 10 | 1 | 4.04 | 3.47 | 3.28 |
| 10 | 10 | 3.7 | 3.64 | 3.53 |
| 5 (1%) | std | 1.96 | 1.88 | 1.85 |
| 5 (1%) | 1 | 2.28 | 1.95 | 1.85 |
| 10 (10%) | std | 3.2 | 3.04 | 3.03 |
| 10 (10%) | 1 | 3.69 | 3.21 | 3.04 |
Notes. The std tcool is for the standard approximation of core cooling on the rate of the envelope. The initial energy content for all cases presented is taken as 20% of the binding energy. No irradiation by the star is included. The bottom section of the table is for different envelope fractions (in parenthesis) than in the models above.
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