Table 2
Dust and wind properties.
| Model | nd / nH | Ṁ (M⊙ yr−1) | fMg | aɡr (µm) |
|---|---|---|---|---|
| st28gm06n052 | 3 × 10−16 | 5 × 10−6 | 0.5 | 0.8 |
| st28gm05n033 | 3 × 10−15 | 5 × 10−8 | 0.15 | 0.2 |
Notes. Listed here are the assumed seed particle abundance nd/nH, and the resulting temporal means of the mass-loss rate Ṁ, the fraction of Mg condensed into grains fMg, and the grain radius agr at the outer boundary. When forming Mg2SiO4 grains in a gas of solar composition, the abundance of Mg is the limiting factor, since that element will be used up first. In the models described here, however, fMg is well below its maximum value of 1.
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