Table 1
Input parameters for each simulation model.
| Model | λp | ρp | ρ* | fpress | Tsub | cs, sub | cc, anti |
|---|---|---|---|---|---|---|---|
| (g cm−3) | (g cm−3) | (%) | (K) | (km s−1) | (km s−1) | ||
| B1 | 3 | 6.92 × 10−15 | 4.64 × 10−15 | 100 | 14100 | 9.7 | 9.7 |
| B2 | 3 | 6.92 × 10−15 | 4.64 × 10−15 | 1 | 14100 | 9.7 | 1.0 |
| S1 | 9 | 5.38 × 10−13 | 4.64 × 10−15 | 100 | 4700 | 5.6 | 5.6 |
| S2 | 9 | 5.38 × 10−13 | 4.64 × 10−15 | 1 | 4700 | 5.6 | 0.6 |
| S3 | 9 | 5.38 × 10−13 | 2.09 × 10−14 | 1 | 4700 | 5.6 | 0.6 |
| S4 | 9 | 5.38 × 10−13 | 2.78 × 10−14 | 1 | 4700 | 5.6 | 0.6 |
Notes. We present two hot wind models (B) and four cold wind models (S). For each, λp is the hydrodynamic escape parameter, and fpress is the pressure fraction at the anti-stellar point relative to the substellar point. The table lists the planetary and stellar surface density (ρp and ρ*, respectively); the substellar temperature Tsub, calculated with μ = 1.25 (although this varies as a function of the outflow’s location); and the sound speed cs at both substellar (sub) and anti-stellar (anti) points on the planetary surface, which has a constant density ρp. Models S3 and S4 have a higher stellar mass-loss rate compared to model S2.
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