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Table 2.

Parameters adopted in the simulations of metal and dust evolution described in Sect. 3.

First tests
τ [Myrs] 83, 300
Mstars [M] 1
Mgas [M] (2, 10, 20, 100) × Mstar
Mbar [M] Mgas + Mev
Mswept [M] 1000, 6800
ML (0, 0.5, 0.6, 0.65, 0.8)×Mgas
I/O 0, 0.2, 0.5
IMF Chabrier
∝ Mα, α = −1, −1.35, −1.5
SN condensation fraction fpy = 1, fol = 0, fir = 1, fcar = 0.5
fpy = 0.5, fol = 0, fir = 0.5, fcar = 0.5
fpy = 0.25, fol = 0, fir = 0.25, fcar = 0.25
fpy = 0.10, fol = 0, fir = 0.10, fcar = 0.10
TP-AGB condensation fraction fpy = 0.3, fol = 0.3, fir = 0.01, fcar = 0.5
Dust growth in the ISM YES, NO

Theoretical metal yields
Stellar source Data set and denomination Mass range in M

Type II SNe Kobayashi et al. (2006) – K06 [13–40]
Nomoto et al. (2013) – N13 [13–40]
Limongi & Chieffi (2018) – LC18 [13–120]
Ritter et al. (2018) – R18 [12–25]
TP-AGB Cristallo et al. (2015) – C15 [1–7]
Karakas (2010) – K10 [1–6]
Ritter et al. (2018) – R18 [1–7]
Pop III stars Heger & Woosley (2010) [10–100]
Nomoto et al. (2013) [13–300]
Type Ia SN Iwamoto et al. (1999)

Systematic calculations

τ [Myrs] 83, 300
Mstars [M] 1
Mgas [M] [10, 100] × Mstar, spacing 10
Mbar [M] Mgas + Mev
Mswept [M] 1000, 6800
ML [0, 0.95] × Mgas, spacing 0.05
I/O 0
IMF ∝ Mα, α = −1, −1.35, −1.5
SN condensation fraction fpy = 0.25, fol = 0, fir = 0.25, fcar = 0.25
fpy = 0.5, fol = 0, fir = 0.5, fcar = 0.5
fpy = 1, fol = 0, fir = 1, fcar = 0.5
AGB condensation fraction fpy = 0.3, fol = 0.3, fir = 0.01, fcar = 0.5
Dust growth in the ISM NO

Notes. First tests are run in order to select the reference parameters adopted to run systematic calculations. The stellar mass produced after 13 Gyr is always normalised to 1 M. Different theoretical metal yields are tested in Sect. 5.2.6.

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