Table 1.
Compositions of key species in our radiative transfer input model (in solar masses) at 160 s post explosion.
| Element | Mass [M⊙] |
|---|---|
| He | 2.64 × 10−1 |
| C | 6.56 × 10−2 |
| O | 2.13 × 10−1 |
| Ne | 2.01 × 10−2 |
| Na | 2.08 × 10−4 |
| Mg | 2.76 × 10−2 |
| Al | 1.18 × 10−3 |
| Si | 1.70 × 10−1 |
| S | 8.18 × 10−2 |
| Ar | 1.50 × 10−2 |
| Ca | 1.91 × 10−2 |
| Ti | 5.16 × 10−3 |
| Cr | 5.43 × 10−3 |
| Fe | 1.03 × 10−2 |
| Co | 1.06 × 10−3 |
| Ni | 9.08 × 10−3 |
| 48Cr | 4.97 × 10−3 |
| 52Fe | 4.42 × 10−3 |
| 56Ni | 7.46 × 10−3 |
Notes. Elemental masses are given in the upper part of table with the masses of radioisotopes whose decay chain energy deposition is tracked in the simulation included in the lower part of the table. When mapping the output of the explosion simulation to our radiative transfer input model we exclude the outermost ejecta (> 16 500 km s−1), which are very low density and thus will not contribute significant opacity. The yields listed here therefore show some differences to the yields that come directly from the nucleosynthesis post processing of the explosion simulation.
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