Table 1. Open in new tab Initial mass...

Isotope

Norm. pop.^a

Int. pop.^b

Extr. pop.^c

¹H

0.748 815

0.674 238

0.614 576

³He

6.554 11 × 10⁻⁵

3.277 06 × 10⁻⁵

6.554 16 × 10⁻⁶

⁴He

0.250 000

0.324 641

0.384 353

⁷Li

1.045 86 × 10⁻⁹

5.232 63 × 10⁻¹⁰

1.051 87 × 10⁻¹⁰

¹²C

9.501 77 × 10⁻⁵

5.779 48 × 10⁻⁵

2.801 65 × 10⁻⁵

¹³C

1.153 10 × 10⁻⁶

3.509 72 × 10⁻⁶

5.395 01 × 10⁻⁶

¹⁴N

2.805 40 × 10⁻⁵

3.529 88 × 10⁻⁴

6.129 36 × 10⁻⁴

¹⁵N

1.105 07 × 10⁻⁷

6.435 48 × 10⁻⁸

2.743 31 × 10⁻⁸

¹⁶O

6.554 65 × 10⁻⁴

3.312 00 × 10⁻⁴

7.178 76 × 10⁻⁵

¹⁷O

1.033 84 × 10⁻⁷

5.946 62 × 10⁻⁸

2.433 19 × 10⁻⁸

¹⁸O

5.886 41 × 10⁻⁷

2.943 23 × 10⁻⁷

5.886 87 × 10⁻⁸

¹⁹F

1.387 44 × 10⁻⁸

6.941 44 × 10⁻⁹

1.395 06 × 10⁻⁹

²⁰Ne

1.357 40 × 10⁻⁴

1.313 17 × 10⁻⁴

1.277 79 × 10⁻⁴

²¹Ne

1.360 18 × 10⁻⁷

6.964 19 × 10⁻⁸

1.654 12 × 10⁻⁸

²²Ne

4.370 84 × 10⁻⁶

2.213 63 × 10⁻⁶

4.878 57 × 10⁻⁷

²³Na

1.161 95 × 10⁻⁶

4.760 80 × 10⁻⁶

7.639 88 × 10⁻⁶

²⁴Mg

4.377 80 × 10⁻⁵

2.349 66 × 10⁻⁵

7.271 60 × 10⁻⁶

²⁵Mg

5.774 73 × 10⁻⁶

3.703 20 × 10⁻⁶

2.045 97 × 10⁻⁶

²⁶Mg

6.607 31 × 10⁻⁶

1.364 72 × 10⁻⁵

1.927 91 × 10⁻⁵

²⁷Al

2.017 55 × 10⁻⁶

2.256 30 × 10⁻⁵

3.899 94 × 10⁻⁵

²⁸Si

5.694 95 × 10⁻⁵

5.867 96 × 10⁻⁵

6.006 38 × 10⁻⁵

⁵⁶Fe

3.928 93 × 10⁻⁵

⁵⁸Ni

4.334 57 × 10⁻⁵

[(C + N + O)/H]

−1.24

−1.19

−1.15

Table 1.

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Initial mass fractions of isotopes used in our calculations.

Isotope	Norm. pop.^a	Int. pop.^b	Extr. pop.^c
¹H	0.748 815	0.674 238	0.614 576
³He	6.554 11 × 10⁻⁵	3.277 06 × 10⁻⁵	6.554 16 × 10⁻⁶
⁴He	0.250 000	0.324 641	0.384 353
⁷Li	1.045 86 × 10⁻⁹	5.232 63 × 10⁻¹⁰	1.051 87 × 10⁻¹⁰
¹²C	9.501 77 × 10⁻⁵	5.779 48 × 10⁻⁵	2.801 65 × 10⁻⁵
¹³C	1.153 10 × 10⁻⁶	3.509 72 × 10⁻⁶	5.395 01 × 10⁻⁶
¹⁴N	2.805 40 × 10⁻⁵	3.529 88 × 10⁻⁴	6.129 36 × 10⁻⁴
¹⁵N	1.105 07 × 10⁻⁷	6.435 48 × 10⁻⁸	2.743 31 × 10⁻⁸
¹⁶O	6.554 65 × 10⁻⁴	3.312 00 × 10⁻⁴	7.178 76 × 10⁻⁵
¹⁷O	1.033 84 × 10⁻⁷	5.946 62 × 10⁻⁸	2.433 19 × 10⁻⁸
¹⁸O	5.886 41 × 10⁻⁷	2.943 23 × 10⁻⁷	5.886 87 × 10⁻⁸
¹⁹F	1.387 44 × 10⁻⁸	6.941 44 × 10⁻⁹	1.395 06 × 10⁻⁹
²⁰Ne	1.357 40 × 10⁻⁴	1.313 17 × 10⁻⁴	1.277 79 × 10⁻⁴
²¹Ne	1.360 18 × 10⁻⁷	6.964 19 × 10⁻⁸	1.654 12 × 10⁻⁸
²²Ne	4.370 84 × 10⁻⁶	2.213 63 × 10⁻⁶	4.878 57 × 10⁻⁷
²³Na	1.161 95 × 10⁻⁶	4.760 80 × 10⁻⁶	7.639 88 × 10⁻⁶
²⁴Mg	4.377 80 × 10⁻⁵	2.349 66 × 10⁻⁵	7.271 60 × 10⁻⁶
²⁵Mg	5.774 73 × 10⁻⁶	3.703 20 × 10⁻⁶	2.045 97 × 10⁻⁶
²⁶Mg	6.607 31 × 10⁻⁶	1.364 72 × 10⁻⁵	1.927 91 × 10⁻⁵
²⁷Al	2.017 55 × 10⁻⁶	2.256 30 × 10⁻⁵	3.899 94 × 10⁻⁵
²⁸Si	5.694 95 × 10⁻⁵	5.867 96 × 10⁻⁵	6.006 38 × 10⁻⁵
⁵⁶Fe	3.928 93 × 10⁻⁵	3.928 93 × 10⁻⁵	3.928 93 × 10⁻⁵
⁵⁸Ni	4.334 57 × 10⁻⁵	4.334 57 × 10⁻⁵	4.334 57 × 10⁻⁵
[(C + N + O)/H]	−1.24	−1.19	−1.15

Isotope	Norm. pop.^a	Int. pop.^b	Extr. pop.^c
¹H	0.748 815	0.674 238	0.614 576
³He	6.554 11 × 10⁻⁵	3.277 06 × 10⁻⁵	6.554 16 × 10⁻⁶
⁴He	0.250 000	0.324 641	0.384 353
⁷Li	1.045 86 × 10⁻⁹	5.232 63 × 10⁻¹⁰	1.051 87 × 10⁻¹⁰
¹²C	9.501 77 × 10⁻⁵	5.779 48 × 10⁻⁵	2.801 65 × 10⁻⁵
¹³C	1.153 10 × 10⁻⁶	3.509 72 × 10⁻⁶	5.395 01 × 10⁻⁶
¹⁴N	2.805 40 × 10⁻⁵	3.529 88 × 10⁻⁴	6.129 36 × 10⁻⁴
¹⁵N	1.105 07 × 10⁻⁷	6.435 48 × 10⁻⁸	2.743 31 × 10⁻⁸
¹⁶O	6.554 65 × 10⁻⁴	3.312 00 × 10⁻⁴	7.178 76 × 10⁻⁵
¹⁷O	1.033 84 × 10⁻⁷	5.946 62 × 10⁻⁸	2.433 19 × 10⁻⁸
¹⁸O	5.886 41 × 10⁻⁷	2.943 23 × 10⁻⁷	5.886 87 × 10⁻⁸
¹⁹F	1.387 44 × 10⁻⁸	6.941 44 × 10⁻⁹	1.395 06 × 10⁻⁹
²⁰Ne	1.357 40 × 10⁻⁴	1.313 17 × 10⁻⁴	1.277 79 × 10⁻⁴
²¹Ne	1.360 18 × 10⁻⁷	6.964 19 × 10⁻⁸	1.654 12 × 10⁻⁸
²²Ne	4.370 84 × 10⁻⁶	2.213 63 × 10⁻⁶	4.878 57 × 10⁻⁷
²³Na	1.161 95 × 10⁻⁶	4.760 80 × 10⁻⁶	7.639 88 × 10⁻⁶
²⁴Mg	4.377 80 × 10⁻⁵	2.349 66 × 10⁻⁵	7.271 60 × 10⁻⁶
²⁵Mg	5.774 73 × 10⁻⁶	3.703 20 × 10⁻⁶	2.045 97 × 10⁻⁶
²⁶Mg	6.607 31 × 10⁻⁶	1.364 72 × 10⁻⁵	1.927 91 × 10⁻⁵
²⁷Al	2.017 55 × 10⁻⁶	2.256 30 × 10⁻⁵	3.899 94 × 10⁻⁵
²⁸Si	5.694 95 × 10⁻⁵	5.867 96 × 10⁻⁵	6.006 38 × 10⁻⁵
⁵⁶Fe	3.928 93 × 10⁻⁵	3.928 93 × 10⁻⁵	3.928 93 × 10⁻⁵
⁵⁸Ni	4.334 57 × 10⁻⁵	4.334 57 × 10⁻⁵	4.334 57 × 10⁻⁵
[(C + N + O)/H]	−1.24	−1.19	−1.15

Notes.^a The heavy-element mass fraction for this and the other two mixtures is Z ≈ 0.0011.

^bFor the intermediate population, we assume a mixture of 50 per cent of the abundances from the normal population with 50 per cent of the abundances from our 6 × 10⁴ M_⊙ MS star model when its He abundance has increased to Y = 0.40.

^cFor the extreme population, we assume a mixture of 10 per cent of the abundances from the normal population with 90 per cent of the abundances from our 6 × 10⁴ M_⊙ MS star model when its He abundance has increased to Y = 0.40.

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