Table 1
Summary of the properties of the magnetic models.
| 〈Bz〉 (G) | Dur (h) | Teff (K) | z⋆ (km) | lg τ⋆ | ∆ifr (%) | ID d3gt57g44… |
|---|---|---|---|---|---|---|
| 0 | 11.4 | 5750 | 360 | −2.37 | 0.0 | b000m592 |
| 50 | 9.5 | 5760 | 350 | −2.38 | 0.1 | b050m592 |
| 100 | 9.5 | 5775 | 342 | −2.39 | 0.2 | b100m592 |
| 200 | 9.5 | 5794 | 323 | −2.40 | 0.6 | b200m592 |
| 400 | 8.6 | 5825 | 292 | −2.40 | 1.5 | b400m592 |
| 800 | 8.6 | 5816 | 273 | −2.39 | 3.5 | b800m592 |
| 1200 | 10.1 | 5660 | 280 | −2.39 | 5.3 | b1200msc592 |
| 1600 | 9.5 | 5381 | 285 | −2.40 | 6.9 | b1600msc592 |
| 2400 | 6.7 | 4711 | 267 | −2.42 | – | b2400msc592 |
Notes. 〈Bz〉 is the horizontal average of the vertical component of the magnetic field of the run, which is imposed by the initial conditions. Dur (duration) is the length of the interval over which the model is run after it has reached a statistically steady state. Teff is the mean effective temperature of the model snapshots that were selected for subsequent spectral synthesis, z⋆ is the height of the stellar limb above optical depth unity, lg τ⋆ the logarithm of optical depth at z⋆. ∆ifr is an interferometric radius correction (see Sect. 3.3). ID is an internal model identifier. Uncertainties: σz⋆ ≤ 1.4km, σlg τ⋆ ≤ 0.002.
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