Table 2
Approximate timescales (in Myr) needed for the modelled planets to evolve out of the boil-off regime, following the analysis described in Sect. 4.
| Star | Mpl | Teq | Λ i | Λ f | Timescale |
| M⊕ | K | Myr | |||
|
|
|||||
| G2 | 5 | 500 | 17 | 34 | 14 600 |
| G2 | 5 | 1000 | 16 | 29 | 48 |
| G2 | 10 | 500 | 22 | 38 | 72 500 |
| G2 | 10 | 1000 | 15 | 24 | 22 700 |
|
|
|||||
| K2 | 5 | 500 | 17 | 29 | 14 600 |
| K2 | 5 | 1000 | 8 | 21 | 495 |
| K2 | 10 | 500 | 19 | 30 | 102 200 |
| K2 | 10 | 1000 | 10 | 18 | 8200 |
|
|
|||||
| M2 | 5 | 500 | 20 | 29 | 28 000 |
| M2 | 5 | 1000 | 16 | 21 | 3 |
| M2 | 10 | 500 | 19 | 25 | 24 800 |
| M2 | 10 | 1000 | 20 | 24 | 167 |
Notes. Timescales larger than 1 Gyr have been rounded to the nearest 100 Myr. The fourth and fifth columns indicate the initial and final Λ values of the planets used to calculate the timescales.
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