Stellar evolution through the Red Supergiant phase
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arXiv
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| Format: | Preprint |
| Published: |
2025
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| _version_ | 1866909698403336192 |
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| author | Ekström, Sylvia Georgy, Cyril |
| author_facet | Ekström, Sylvia Georgy, Cyril |
| contents | Massive stars less massive than ~30 Msol evolve into a red supergiant after the main sequence. Given a standard IMF, this means about 80% of all single massive stars will experience this phase. RSGs are dominated by convection, with a radius that may extend up to thousands of solar radii. Their low temperature and gravity make them prone to lose large amounts of masses, either through a pulsationally-driven wind or through mass-loss outburst. RSGs are the progenitors of the most common core-collapse supernovae, the type II. In the present review, we give an overview of our theoretical understanding about this spectacular phase of massive stars evolution. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_15960 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Stellar evolution through the Red Supergiant phase Ekström, Sylvia Georgy, Cyril Solar and Stellar Astrophysics Massive stars less massive than ~30 Msol evolve into a red supergiant after the main sequence. Given a standard IMF, this means about 80% of all single massive stars will experience this phase. RSGs are dominated by convection, with a radius that may extend up to thousands of solar radii. Their low temperature and gravity make them prone to lose large amounts of masses, either through a pulsationally-driven wind or through mass-loss outburst. RSGs are the progenitors of the most common core-collapse supernovae, the type II. In the present review, we give an overview of our theoretical understanding about this spectacular phase of massive stars evolution. |
| title | Stellar evolution through the Red Supergiant phase |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.15960 |