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Table 2

Model that reproduces abundances calculated via recombination lines plus correction for dust depletion. In Col. 3, “W” is for well mixed wind prescription.

Model Mup Wind Mgas t O/Ha log (C/O) log (N/O) log (Ne/O) log (S/O) log (Cl/O) log (Ar/O) log (Fe/O)
(M) (108 M) (Gyr)

M1R 80 W 2.08 13.50 8.41 –0.24 –0.75 –0.91 –1.74 –3.89 -2.56 –1.29
12.90 8.34 –0.24 –0.74 –0.91 –1.74 –3.90 –2.56 –1.29
7.50 8.05 –0.27 –0.63 –0.89 –1.74 –3.93 –2.55 –1.30

Observational constraints
H ii regionsc, A stars 1.98b  ±  0.20 13.50 8.42  ±  0.06 –0.31  ±  0.13 –1.37  ±  0.17 –0.79  ±  0.09 –1.62  ±  0.09 –3.71  ±  0.10 –2.36  ±  0.08 –1.41d  ±  0.20
PN young 12.90  ±  0.50 8.41  ±  0.10 –0.77  ±  0.14 –1.80  ±  0.20 –2.26  ±  0.16
PN old 7.50  ±  3.00 8.02  ±  0.10 –0.74  ±  0.16 –1.62  ±  0.20 –2.26  ±  0.16

Notes. 

(a)

Abundances in units of 12 + log (O/H).

(b)

CCP06.

(c)

Peimbert et al. (2005).

(e)

Fe/H from A-stars by Venn et al. (2001) and RL O/H from H ii regions.

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