Table 1
DARWIN models with outflows driven by the scattering of stellar photons on olivine-type silicate grains.
| Model | nd ∕nH | ΔuP | fL | ΔMbol | Ṁ | uext | fSi | fMg | fFe | agr | Fe/Mg |
|---|---|---|---|---|---|---|---|---|---|---|---|
| name | (km s−1) | (mag) | (M⊙ yr−1) | (km s−1) | (μm) | ||||||
| An115u3 / oli | 1.0 × 10−15 | 3.0 | 2.0 | 0.54 | 1 × 10−7 | 4 | 0.18 | 0.32 | 0.014 | 0.48 | 0.037 |
| An315u3 / oli | 3.0 × 10−15 | 3.0 | 2.0 | 0.54 | 3 × 10−7 | 7 | 0.21 | 0.37 | 0.016 | 0.35 | 0.036 |
| An114u3 / oli | 1.0 × 10−14 | 3.0 | 2.0 | 0.54 | 3 × 10−7 | 8 | 0.28 | 0.50 | 0.026 | 0.26 | 0.043 |
| An314u3 / oli | 3.0 × 10−14 | 3.0 | 2.0 | 0.54 | 4 × 10−7 | 8 | 0.40 | 0.71 | 0.044 | 0.20 | 0.052 |
| An115u4 / oli | 1.0 × 10−15 | 4.0 | 2.0 | 0.73 | 3 × 10−7 | 4 | 0.17 | 0.30 | 0.017 | 0.47 | 0.048 |
| An315u4 / oli | 3.0 × 10−15 | 4.0 | 2.0 | 0.73 | 4 × 10−7 | 6 | 0.20 | 0.36 | 0.017 | 0.34 | 0.040 |
| An114u4 / oli | 1.0 × 10−14 | 4.0 | 2.0 | 0.73 | 5 × 10−7 | 9 | 0.28 | 0.50 | 0.026 | 0.26 | 0.043 |
| An314u4 / oli | 3.0 × 10−14 | 4.0 | 2.0 | 0.73 | 4 × 10−7 | 8 | 0.39 | 0.69 | 0.043 | 0.20 | 0.052 |
| Bn316u3 / oli | 3.0 × 10−16 | 3.0 | 2.0 | 0.53 | 3 × 10−7 | 3 | 0.14 | 0.24 | 0.012 | 0.65 | 0.041 |
| Bn115u3 / oli | 1.0 × 10−15 | 3.0 | 2.0 | 0.53 | 5 × 10−7 | 6 | 0.14 | 0.24 | 0.015 | 0.44 | 0.052 |
| Bn315u3 / oli | 3.0 × 10−15 | 3.0 | 2.0 | 0.53 | 7 × 10−7 | 8 | 0.18 | 0.32 | 0.019 | 0.33 | 0.050 |
| Bn114u3 / oli | 1.0 × 10−14 | 3.0 | 2.0 | 0.53 | 7 × 10−7 | 10 | 0.25 | 0.45 | 0.031 | 0.25 | 0.058 |
| Bn314u3 / oli | 3.0 × 10−14 | 3.0 | 2.0 | 0.53 | 7 × 10−7 | 10 | 0.36 | 0.64 | 0.051 | 0.20 | 0.067 |
| Bn316u4 / oli | 3.0 × 10−16 | 4.0 | 2.0 | 0.71 | 3 × 10−7 | 3 | 0.13 | 0.22 | 0.013 | 0.64 | 0.049 |
| Bn115u4 / oli | 1.0 × 10−15 | 4.0 | 2.0 | 0.71 | 5 × 10−7 | 5 | 0.14 | 0.24 | 0.014 | 0.44 | 0.048 |
| Bn315u4 / oli | 3.0 × 10−15 | 4.0 | 2.0 | 0.71 | 7 × 10−7 | 8 | 0.18 | 0.32 | 0.019 | 0.33 | 0.050 |
| Bn114u4 / oli | 1.0 × 10−14 | 4.0 | 2.0 | 0.71 | 8 × 10−7 | 10 | 0.25 | 0.45 | 0.031 | 0.25 | 0.058 |
| Bn314u4 / oli | 3.0 × 10−14 | 4.0 | 2.0 | 0.71 | 7 × 10−7 | 10 | 0.36 | 0.64 | 0.051 | 0.20 | 0.067 |
| M2n115u6 / oli | 1.0 × 10−15 | 6.0 | 1.5 | 0.95 | 1 × 10−6 | 6 | 0.20 | 0.36 | 0.019 | 0.49 | 0.045 |
| M2n315u6 / oli | 3.0 × 10−15 | 6.0 | 1.5 | 0.95 | 2 × 10−6 | 11 | 0.24 | 0.43 | 0.026 | 0.37 | 0.051 |
| M2n114u6 / oli | 1.0 × 10−14 | 6.0 | 1.5 | 0.95 | 2 × 10−6 | 16 | 0.35 | 0.62 | 0.044 | 0.28 | 0.060 |
Notes. This table gives an overview of input parameters and resulting properties of the models: nd ∕nH is the seed particle abundance, and ΔuP is the velocity amplitude at the inner boundary. This amplitude, in combination with the parameter fL (see Paper I, Appendix B), determines the luminosity amplitude and the corresponding bolometric amplitude ΔMbol. 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, the fraction of Fe condensed into grains fFe, the grain radius agr, and the ratio of Mg and Fe in the grains, all taken at the outer boundary of the models (located at about 20–30 stellar radii). The model names are constructed in the following way: A, B, or M2 represents a combination of stellar parameters (see Sect. 3), the letter n followed by a 3-digit number stands for the seed particle abundance (i.e., n315 for nd ∕nH = 3 × 10−15, n114 for nd ∕nH = 1 × 10−14, etc.) and the letter u followed by a number (3, 4, 6) represents the velocity amplitude at the inner boundary (km s−1). We note that the parameter ΔuP is the half-amplitude of the sinusoidal velocity variation (see Paper I, Appendix B), while ΔMbol listed in this table represents the full bolometric amplitude (minimum to maximum).
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