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Table 1.

Core masses and total masses of the most abundant isotopes at the onset of core collapse for stars stripped in binaries and single stars with the same initial masses.

Minit MCC MHe core MCO core MSi core MFe core M1H M4He M12C M14N M16O M20Ne M24Mg M28Si M32S M36Ar M40Ca MFe
[M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙] [M⊙]
Binary stripped stars
11.0 3.11 3.11 1.88 1.43 1.32 0.00018 1.13 0.062 0.0060 0.20 0.05 0.05 0.11 0.05 0.008 0.0074 0.54
12.1 3.52 3.52 2.09 1.49 1.33 0.00046 1.21 0.095 0.0045 0.27 0.11 0.07 0.10 0.06 0.013 0.0129 0.62
13.0 3.87 3.87 2.46 1.42 1.32 0.00034 1.25 0.104 0.0064 0.49 0.18 0.1 0.20 0.103 0.019 0.0137 0.46
14.0 4.23 4.23 2.57 1.38 1.27 0.00020 1.28 0.128 0.0064 0.49 0.33 0.08 0.26 0.201 0.044 0.0479 0.46
14.6 4.48 4.48 2.99 1.47 1.37 0.00020 1.29 0.14 0.0044 0.73 0.33 0.16 0.19 0.103 0.021 0.0191 0.55
15.0 4.61 4.61 2.44 1.47 1.36 0.00026 1.28 0.167 0.0033 0.72 0.47 0.09 0.2 0.137 0.029 0.0247 0.55
16.0 4.97 4.97 3.42 1.47 1.33 0.00027 1.28 0.175 0.0052 1.04 0.27 0.19 0.35 0.154 0.026 0.0222 0.55
17.0 5.31 5.31 3.73 1.71 1.47 0.00063 1.29 0.193 0.0063 1.34 0.36 0.27 0.23 0.051 0.009 0.0069 0.67
18.0 5.61 5.61 2.49 1.65 1.46 0.00058 1.25 0.226 0.0051 1.56 0.35 0.32 0.24 0.059 0.014 0.0134 0.70
20.0 6.28 6.28 4.60 1.80 1.52 0.00064 1.16 0.345 0.0032 1.68 0.82 0.26 0.17 0.08 0.016 0.0134 0.82
21.0 6.62 6.62 4.07 1.82 1.54 0.00085 1.07 0.430 0.0007 1.98 0.68 0.34 0.27 0.125 0.027 0.023 0.72
Single stars
11.0 9.32 3.78 2.31 1.44 1.32 3.79 2.95 0.113 0.0211 0.42 0.11 0.09 0.25 0.127 0.021 0.0173 0.49
12.1 9.73 4.33 2.81 1.31 1.26 3.68 3.01 0.121 0.0185 0.57 0.12 0.07 0.37 0.273 0.06 0.0596 0.44
13.0 9.97 4.79 3.19 1.53 1.41 3.52 3.04 0.123 0.0167 1.01 0.29 0.20 0.14 0.047 0.011 0.0114 0.58
14.0 10.12 5.28 3.60 1.67 1.47 3.27 3.03 0.137 0.0145 1.23 0.42 0.23 0.14 0.037 0.008 0.0066 0.71
14.6 10.15 5.63 3.90 1.70 1.51 3.03 2.98 0.169 0.0147 1.36 0.50 0.24 0.11 0.035 0.008 0.0071 0.8
15.0 10.16 5.82 4.07 1.69 1.44 2.9 2.96 0.158 0.014 1.61 0.37 0.29 0.20 0.046 0.011 0.0113 0.62
16.0 10.05 6.34 4.47 1.71 1.5 2.44 2.84 0.147 0.0124 1.68 0.74 0.31 0.13 0.061 0.016 0.0162 0.75
17.0 9.88 6.87 4.97 1.85 1.58 1.94 2.72 0.188 0.0106 1.82 0.6 0.22 0.31 0.234 0.081 0.0607 0.77
18.0 10.13 7.32 5.42 1.89 1.62 1.78 2.71 0.178 0.0102 2.10 0.78 0.33 0.23 0.154 0.042 0.0492 0.81
19.0 10.58 7.42 5.49 1.97 1.65 1.84 3.04 0.209 0.0143 2.04 0.72 0.14 0.35 0.262 0.086 0.048 0.83
20.0 11.66 7.59 5.67 1.96 1.63 2.50 3.26 0.204 0.0148 2.06 0.67 0.23 0.41 0.308 0.089 0.0617 0.84
21.0 10.40 8.21 6.20 1.54 1.40 1.00 3.00 0.228 0.0146 2.31 0.72 0.07 0.65 0.547 0.142 0.1503 0.58

Notes. These models are for solar metallicity (Z = 0.014). We define the core boundaries as the mass coordinate where the mass fraction of the depleted element (for example, 1H in the case of the helium core) decreases below 0.01 and the mass fraction of the most abundant element (for example, 4He) increases above 0.1. In the case of the CO core, we calculate the maximum between the values of the 12C and 12O core boundary values. For the mass of iron (MFe), we have added the mass of 52Fe, 53Fe, 54Fe, 55Fe, 56Fe, 57Fe, and 58Fe. Of these isotopes, 54Fe, 56Fe, and 58Fe dominate and contribute with similar amounts.

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