Table 1.
Presupernova models for blue supergiants.
| Model | RpSN |  |
 |
MpSN | MZAMS | Ysurf | Zsurf | Rot. | Ref. |
|---|---|---|---|---|---|---|---|---|---|
| (R⊙) | (M⊙) | (10−2) | |||||||
| W16 | 28.8 | 2.57 | 6.55 | 15.36 | 16 | 0.521 | 0.50 | Yes | 1 |
| W18r | 41.9 | 2.67 | 6.65 | 17.09 | 18 | 0.453 | 0.50 | Yes | – |
| W18x | 30.4 | 2.12 | 5.13 | 17.56 | 18 | 0.281 | 0.60 | Yes | 1 |
| B15 | 56.1 | 1.64 | 4.05 | 15.02 | 15.02 | 0.230 | 0.34 | No | 2 |
| W18 | 46.8 | 3.06 | 7.40 | 16.92 | 18.0 | 0.515 | 0.50 | Yes | 1 |
| W20 | 64.2 | 2.33 | 5.79 | 19.38 | 20.10 | 0.256 | 0.56 | No | 3 |
| N20 | 47.9 | 3.75 | 5.98 | 16.27 | ∼20.0 | 0.435 | 0.50 | No | 4 |
Notes. The columns list the name of the pre-SN model; its radius, RpSN; the CO-core mass, 
; the helium-core mass, 
; the pre-SN mass, MpSN; the progenitor mass, MZAMS; and the mass fraction of helium, Ysurf, and heavy elements, Zsurf, in the hydrogen-rich envelope at the stage of core collapse. The last two columns note whether the progenitor was rotating or not, and the corresponding reference is listed. The lower four initial models were previously used in Utrobin et al. (2015).
References. (1) Sukhbold et al. (2016); (2) Woosley et al. (1988); (3) Woosley et al. (1997); (4) Shigeyama & Nomoto (1990).
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