Table 1.
Photospheric velocity, vph; total mass above photosphere; and the helium mass required above the photosphere. Lastly, given the ratio of MHe(> vph) to Mej(> vph) one can compute the implied helium mass fraction, XHe.
| Time | vph | Mej ( > vph) | MHe(> vph) | XHe |
|---|---|---|---|---|
| [days] | [c] | [10−2 M⊙] | [10−2 M⊙] | |
| 0.92 | ∼0.3 | 0.3 | ≲0.3 | ≲1.0 |
| 1.17 | ∼0.3 | 0.3 | 1.2 ± 0.4 | 4 ± 1 |
| 1.43 | 0.30 | 0.3 | 0.21 ± 0.06 | 0.8 ± 0.3 |
| 2.4 | 0.27 | 0.4 | 0.05 ± 0.01 | 0.13 ± 0.03 |
| 3.4 | 0.23 | 0.7 | 0.03 ± 0.01 | 0.05 ± 0.02 |
| 4.4 | 0.19 | 1.0 | 0.012 ± 0.005 | 0.012 ± 0.005 |
Notes. The photospheric velocity is ill-constrained at 0.92 and 1.17 day, as only the bluest absorption part of the 1 μm feature is within the covered spectral range. However, the line-forming region is not expected to be dramatically different between 0.92, 1.17, and 1.43 days, and the radius of the black body at these epochs supports a velocity of around 0.3c.
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