Table 1
Models in our study.
| Model | M★ (M⊙) | v★ (km s−1) | Mej (M⊙) | Evolution history |
|---|---|---|---|---|
| Pulsar wind nebula-20Mo-v20 kms | 20 | 20 | 7.28 | MS → RSG → SN → pulsarwindnebula |
| Pulsar wind nebula-20Mo-v40 kms (a) | 20 | 40 | 7.28 | MS → RSG → SN → pulsarwindnebula |
| Pulsar wind nebula-35Mo-v20 kms | 35 | 20 | 10.12 | MS → RSG → WR → SN → pulsarwindnebula |
| Pulsar wind nebula-35Mo-v40 kms | 35 | 40 | 10.12 | MS → RSG → WR → SN → pulsarwindnebula |
Notes. (a)Meyer & Meliani (2022). The simulations consider the evolution of a rotating massive star at solar metallicity of mass M★ (in M⊙), followed by its zero-age main-sequence time that is moving with velocity v★. The ejecta mass M★ (in ej) is also indicated. In each one of the models, the ambient medium is that of the warm phase of the Galactic plane nISM ≈ 0.79 cm−3. The different evolutionary phases of the stellar evolution are labelled as MS (main-sequence), RSG (red supergiant), WR (Wolf-Rayet), SN (supernova explosion), and pulsar-wind nebula (pulsar wind).
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