Table 2
Stellar parameters and carbon abundances of our 3D CEMP model atmospheres.
| Teff K | log(g) dex | [Fe/H] dex | [C/Fe] dex | A(C) dex | Resolution Nx × Ny × Nz | Size Mm |
|---|---|---|---|---|---|---|
| 5750 | 4.5 | −6 | 4 | 6.56 | 2402 × 120 | 5.2 |
| 5750 | 4.5 | −5 | 3 | 6.56 | 2402 × 120 | 5.2 |
| 5750 | 4.5 | −4 | 2 | 6.56 | 2402 × 120 | 5.1 |
| 5750 | 4.5 | −3 | 1 | 6.56 | 2402 × 120 | 5.2 |
| 5750 | 4.5 | −2 | 1 | 7.56 | 2402 × 120 | 5.4 |
| 5250 | 3.0 | −6 | 4 | 6.56 | 2402 × 120 | 140 |
| 5250 | 3.0 | −5 | 3 | 6.56 | 2402 × 120 | 140 |
| 5250 | 3.0 | −4 | 2 | 6.56 | 2402 × 120 | 140 |
| 5250 | 3.0 | −3 | 1 | 6.56 | 2402 × 120 | 150 |
| 5250 | 3.0 | −2 | 1 | 7.56 | 2402 × 120 | 160 |
Notes. The level of C-enhancement varies from [C/Fe] = 1 (at [Fe/H] = −3) to [C/Fe] = 4(at [Fe/H] = −6). Here, Ni corresponds to the number of grid points in dimension i. In the last column, we provide the horizontal extend of the corresponding model atmosphere. Note that the vertical extend is half that number. For every CEMP model listed here, we generated a scaled-solar ([C/Fe] = 0) counterpart. For each model, convergence was achieved in less than 3500 CPU-h.
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