Table 2.
List of parameters adopted in the simulations of metal and dust evolution described in Sect. 3.2.
| Theoretical metal yields | ||
|---|---|---|
| Stellar source | Data set and Denomination | Mass range in M⊙ |
| Type II SNe | Limongi & Chieffi (2018), Prantzos et al. (2018) – LC18 | [13, 120] |
| AGB stars | Cristallo et al. (2015) – C15 | [1, 7] |
| Pop III stars | Heger & Woosley (2010) | [10, 100] |
| Type Ia SNe | Iwamoto et al. (1999) | – |
| Systematic calculations | ||
| τ [Myr] | 500 | |
| IMF | Chabrier (2003) | |
| IMF (Top-Heavy) | ∝M−ξ, ξ = 1.8 | |
| M*, fin [M⊙] | 1 | |
| MGas, ini [M⊙] | (2 − 6)×Mstar, fin | |
| ηout | 0–3 | |
| ηin | 0–10 | |
| Mswept [M⊙] | 1535 ![$ n_{\mathrm{SNe}}^{-0.202}[(Z/Z_{\odot}) + 0.039]^{-0.289} $](/articles/aa/full_html/2025/02/aa51542-24/aa51542-24-eq5.gif){kind=small} |
|
| ϵSNe | 0.1, 0.5, 1.0 | |
| SNe condensation fraction | fkey, py = 0.05, fkey, ol = 0, fkey, car = 0.05 (fcond = 5%) | |
| fkey, py = 0.10, fkey, ol = 0, fkey, car = 0.10 (fcond = 10%) | ||
| fkey, py = 0.25, fkey, ol = 0, fkey, car = 0.25 (fcond = 25%) | ||
| fkey, py = 0.5, fkey, ol = 0, fkey, car = 0.5 (fcond = 50%) | ||
| fkey, py = 0.75, fkey, ol = 0, fkey, car = 0.5 (fcond = 75%) | ||
| fkey, py = 1, fkey, ol = 0, fkey, car = 0.5 (fcond = 100%) | ||
| AGB condensation fraction | fpy = 0.3, fol = 0.3, fir = 0.01, fcar = 0.5 | |
| Dust growth efficiency in the ISM | 0.0, 0.5, 1 | |
Notes. First tests are run in order to select the reference parameters adopted to run systematic calculations. The stellar mass produced by the end of the simulation is always normalized to 1 M⊙. The chemical species are abbreviated as olivine: ol, pyroxene: py, and carbon: car. fcond is the condensation fraction.
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