Table 1
Numerical models.
| Model | M⋆ (M⊙) | v⋆ (km s−1) | Evolution history |
|---|---|---|---|
| Run-20-MHD-20-SNR | 20 | 20 | MS → RSG → SN |
| Run-20-MHD-40-SNR | 20 | 40 | MS → RSG → SN |
| Run-35-MHD-20-SNR(a) | 35 | 20 | MS → RSG → WR → SN |
| Run-35-MHD-40-SNR(a) | 35 | 40 | MS → RSG → WR → SN |
Notes. All simulations assume a rotating massive progenitor of a ZAMS mass, M⋆ (in M⊙), at solar metallicity and moving with velocity, v⋆, through the warm phase of the Galactic plane. The table indicates the stellar evolution history in each model from the MS (main sequence) phase to the final SN (supernova) explosion and ultimately to the pulsar wind nebula (PWN) through the red supergiant (RSG) and WR (Wolf–Rayet) stages.
References.(a)Meyer et al. (2023)
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