Table 3.
Mass fractions of stable isotopes or elements of interest from the solar distribution (Asplund et al. 2009), the W7 type Ia SN model (Nomoto et al. 1984), the N100DDT type Ia SN model (Seitenzahl et al. 2013a), and the G14a ONe deflagration simulation (Jones et al. 2016a), with and without weak reaction rates by Nabi & Klapdor-Kleingrothaus (2004) included in the nucleosynthesis post-processing.
| Isotope/element | ⊙ | W7 | N100DDT | G14a | G14aNKK | J07aNKK | W13 |
|---|---|---|---|---|---|---|---|
| Zn | 1.85e-06 | 2.06e-05 | 2.22e-06 | 4.83e-03 | 6.80e-03 | 8.33e-03 | 9.97e-02 |
| Se | 1.34e-07 | 0.00e+00 | 0.00e+00 | 4.51e-05 | 4.80e-04 | 7.60e-04 | 6.87e-03 |
| Kr | 1.16e-07 | 0.00e+00 | 0.00e+00 | 4.41e-05 | 3.95e-04 | 5.86e-04 | 1.04e-02 |
| 48Ca | 1.53e-07 | 1.90e-09 | 5.60e-15 | 1.32e-03 | 2.13e-03 | 2.64e-03 | 2.04e-03 |
| 50Ti | 1.79e-07 | 7.82e-05 | 1.86e-07 | 4.46e-03 | 3.91e-03 | 4.37e-03 | 1.65e-04 |
| 54Cr | 4.33e-07 | 6.75e-04 | 7.92e-06 | 9.48e-03 | 8.64e-03 | 9.56e-03 | 3.97e-04 |
Notes. The higher-density model J07 is also included (see Table 2). The last column is the cECSN yields from Wanajo et al. (2013a,b), where the total ejecta mass was 1.14 × 10−2 M⊙. The simulation results are all decayed yields, i.e. they are for the ejecta only. The N100DDT model was decayed to 2 Gyr and the G14 and J07 models to 1016 s enough time for all radioactive nuclides produced to decay – see half lives in Table 4.
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