Table 2.
Stellar yields of nitrogen and oxygen for different Pop III and very metal-poor stellar models.
Mini | MCO | Mrem | Final | 14N | 16O |
---|---|---|---|---|---|
[M⊙] | [M⊙] | [M⊙] | fate | [M⊙] | [M⊙] |
Z = 0 | |||||
υini = 0 | |||||
9 | 0.718 | 0.718 | WD | 2.52E−08 | 0.109 |
20 | 4.047 | 1.517 | NS | 1.39E−03 | 1.719 |
60 | 22.575 | 26.575 | BH | 1.01E−04 | 4.42E−07 |
85 | 31.768 | 35.768 | BH | 2.26E−05 | 0.008 |
120 | 52.887 | 34.640 | PPISN | 9.02E−06 | 15.969 |
υini = 0.2 υcrit | |||||
9 | 0.940 | 0.940 | WD | 2.89E−05 | 0.173 |
12 | 1.385 | 1.385 | WD | 1.27E−04 | 0.173 |
15 | 2.180 | 1.400 | NS | 2.88E−04 | 0.814 |
20 ( * ) | 19.99 | 19.99 | BH | 0.0 | 0.0 |
υini = 0.4 υcrit | |||||
9 | 0.895 | 0.895 | WD | 0.0011 | 0.304 |
20 | 3.981 | 1.785 | NS | 2.26E−07 | 2.006 |
60 ( * ) | 19.373 | 23.373 | BH | 8.54E−07 | 1.06E−08 |
85 ( * ) | 30.465 | 34.465 | BH | 7.15E−06 | 2.07E−06 |
120 ( * ) | 56.397 | 30.550 | PPISN | 0.0007 | 16.540 |
υini = 0.7 υcrit | |||||
9 | 1.389 | 1.389 | WD | 0.004 | 0.551 |
20 | 8.679 | 12.679 | BH | 0.207 | 0.213 |
60 | 14.442 | 18.442 | BH | 3.760 | 0.914 |
85 | 33.07 | 37.070 | BH | 0.706 | 3.068 |
120 ( * ) | 61.645 | 0.0 | PISN | 0.318 | 26.707 |
Z = 10−5 | |||||
υini = 0 | |||||
9 | 1.009 | 1.009 | WD | 1.91E−05 | 0.123 |
20 | 3.748 | 7.748 | BH | 3.79E−05 | −8.67E−05 |
60 | 20.925 | 24.925 | BH | 1.70E−04 | −9.96E−05 |
85 | 31.622 | 35.622 | BH | 2.51E−04 | 0.001 |
120 | 47.977 | 41.620 | PPISN | 2.66E−04 | 6.292 |
υini = 0.4 υcrit | |||||
9 | 1.119 | 1.119 | WD | 0.008 | 0.529 |
20 | 2.980 | 6.980 | BH | 0.171 | 0.216 |
60 | 13.419 | 17.419 | BH | 2.902 | 1.750 |
85 | 37.358 | 41.358 | BH | 0.051 | 0.652 |
120 | 59.437 | 0.0 | PISN | 0.012 | 53.17 |
Notes. The asterisk after the initial mass indicates that the model is still in the core He-burning phase. The Pop III models with υini/υcrit = 0, 0.2, and 0.4 are from Murphy et al. (2021a) and the models with Z = 10−5 are from Sibony et al. (in prep.).
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