Table 1
DARWIN models with outflows driven by scattering of stellar photons on Fe-free silicate grains.
| Model | nd/nH | ΔuP | Ṁ | u ext | f Si | f Mg | a gr | f Al | f Al | f Al |
| name | [km s-1] | [M⊙/yr] | [km s-1] | [μm] | Talu = Tsil | high k | low k | |||
|
|
||||||||||
| An115u3 | 1.0 × 10-15 | 3.0 | 1 × 10-7 | 2 | 0.17 | 0.32 | 0.47 | 0.29 | 0.04 | 0.95 |
| An315u3 | 3.0 × 10-15 | 3.0 | 3 × 10-7 | 5 | 0.20 | 0.37 | 0.34 | 0.41 | 0.07 | 1.00 |
| An114u3 | 1.0 × 10-14 | 3.0 | 4 × 10-7 | 7 | 0.27 | 0.50 | 0.25 | 0.60 | 0.14 | 1.00 |
| An314u3 | 3.0 × 10-14 | 3.0 | 4 × 10-7 | 7 | 0.38 | 0.71 | 0.20 | 0.86 | 0.36 | 1.00 |
| An115u4 | 1.0 × 10-15 | 4.0 | 3 × 10-7 | 3 | 0.17 | 0.32 | 0.47 | 0.55 | 0.19 | 0.98 |
| An315u4 | 3.0 × 10-15 | 4.0 | 5 × 10-7 | 6 | 0.20 | 0.37 | 0.34 | 0.78 | 0.44 | 1.00 |
| An114u4 | 1.0 × 10-14 | 4.0 | 6 × 10-7 | 9 | 0.27 | 0.50 | 0.25 | 0.84 | 0.59 | 1.00 |
| An314u4 | 3.0 × 10-14 | 4.0 | 5 × 10-7 | 8 | 0.37 | 0.69 | 0.20 | 0.96 | 0.82 | 1.00 |
| Bn316u3 | 3.0 × 10-16 | 3.0 | 3 × 10-7 | 2 | 0.13 | 0.24 | 0.64 | 0.98 | 0.77 | 1.00 |
| Bn115u3 | 1.0 × 10-15 | 3.0 | 5 × 10-7 | 5 | 0.14 | 0.26 | 0.44 | 0.99 | 0.94 | 1.00 |
| Bn315u3 | 3.0 × 10-15 | 3.0 | 7 × 10-7 | 7 | 0.17 | 0.32 | 0.33 | 1.00 | 0.99 | 1.00 |
| Bn114u3 | 1.0 × 10-14 | 3.0 | 8 × 10-7 | 8 | 0.24 | 0.45 | 0.24 | 1.00 | 1.00 | 1.00 |
| Bn314u3 | 3.0 × 10-14 | 3.0 | 8 × 10-7 | 8 | 0.35 | 0.65 | 0.19 | 1.00 | 1.00 | 1.00 |
| Bn316u4 | 3.0 × 10-16 | 4.0 | 3 × 10-7 | 2 | 0.13 | 0.24 | 0.64 | 0.99 | 0.62 | 1.00 |
| Bn115u4 | 1.0 × 10-15 | 4.0 | 5 × 10-7 | 4 | 0.13 | 0.24 | 0.43 | 1.00 | 0.86 | 1.00 |
| Bn315u4 | 3.0 × 10-15 | 4.0 | 7 × 10-7 | 6 | 0.17 | 0.32 | 0.33 | 1.00 | 0.97 | 1.00 |
| Bn114u4 | 1.0 × 10-14 | 4.0 | 8 × 10-7 | 8 | 0.24 | 0.45 | 0.24 | 1.00 | 0.99 | 1.00 |
| Bn314u4 | 3.0 × 10-14 | 4.0 | 8 × 10-7 | 8 | 0.34 | 0.64 | 0.19 | 1.00 | 1.00 | 1.00 |
Notes. The letters A and B denote 2 different combinations of stellar parameters (see Table 2), nd/nH the seed particle abundance, and ΔuP the velocity amplitude at the inner boundary. The resulting wind and dust properties listed here are temporal means of the mass loss rate Ṁ, the wind velocity uext, the fraction of Si condensed into grains fSi, the fraction of Mg condensed into grains fMg, and the grain radius agr at the outer boundary. In this set of models Al2O3 is included as a separate, passive dust species (ignoring its feedback on the atmosphere and wind). Condensation fractions of Al, denoted by fAl, are given for 3 different cases of radiative heating, discussed in Sect. 3.2. Talu and Tsil are the grain temperatures of Al2O3 and Mg2SiO4, respectively. The model names are constructed in the following way: the capital letter (A, B) represents a combination of stellar parameters (see Table 2), the letter n followed by a 3-digit number stands for the seed particle abundance (i.e., n316 for nd/nH = 3 × 10-16, n115 for nd/nH = 1 × 10-15, etc.) and the letter u followed by 3 or 4 represents the pulsation amplitude (km s-1).
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