Stellar Evolution Through the Red Supergiant Phase
Massive stars less massive than ∼30 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>M</mi><mo>⊙</mo></msub></semantics></math></inline-formula> evolve in...
| Published in: | Galaxies |
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| Main Authors: | , |
| Format: | Article |
| Language: | English |
| Published: |
MDPI AG
2025-07-01
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| Subjects: | |
| Online Access: | https://www.mdpi.com/2075-4434/13/4/81 |
| _version_ | 1849360775686127616 |
|---|---|
| author | Sylvia Ekström Cyril Georgy |
| author_facet | Sylvia Ekström Cyril Georgy |
| author_sort | Sylvia Ekström |
| collection | DOAJ |
| container_title | Galaxies |
| description | Massive stars less massive than ∼30 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>M</mi><mo>⊙</mo></msub></semantics></math></inline-formula> 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 losing large amounts of mass, either through pulsationally driven wind or through mass-loss outburst. RSGs are the progenitors of the most common core-collapse supernovae, type II. In the present review, we give an overview of our theoretical understanding about this spectacular phase of massive star evolution. |
| format | Article |
| id | doaj-art-a723c0c677754bff9bb0c848bb3684fb |
| institution | Directory of Open Access Journals |
| issn | 2075-4434 |
| language | English |
| publishDate | 2025-07-01 |
| publisher | MDPI AG |
| record_format | Article |
| spelling | doaj-art-a723c0c677754bff9bb0c848bb3684fb2025-08-27T14:30:59ZengMDPI AGGalaxies2075-44342025-07-011348110.3390/galaxies13040081Stellar Evolution Through the Red Supergiant PhaseSylvia Ekström0Cyril Georgy1Department of Astronomy, University of Geneva, Chemin Pegasi 51, 1290 Versoix, SwitzerlandDepartment of Astronomy, University of Geneva, Chemin Pegasi 51, 1290 Versoix, SwitzerlandMassive stars less massive than ∼30 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>M</mi><mo>⊙</mo></msub></semantics></math></inline-formula> 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 losing large amounts of mass, either through pulsationally driven wind or through mass-loss outburst. RSGs are the progenitors of the most common core-collapse supernovae, type II. In the present review, we give an overview of our theoretical understanding about this spectacular phase of massive star evolution.https://www.mdpi.com/2075-4434/13/4/81stars: massivestars: supergiantsstars: evolutionstars: mass loss |
| spellingShingle | Sylvia Ekström Cyril Georgy Stellar Evolution Through the Red Supergiant Phase stars: massive stars: supergiants stars: evolution stars: mass loss |
| title | Stellar Evolution Through the Red Supergiant Phase |
| title_full | Stellar Evolution Through the Red Supergiant Phase |
| title_fullStr | Stellar Evolution Through the Red Supergiant Phase |
| title_full_unstemmed | Stellar Evolution Through the Red Supergiant Phase |
| title_short | Stellar Evolution Through the Red Supergiant Phase |
| title_sort | stellar evolution through the red supergiant phase |
| topic | stars: massive stars: supergiants stars: evolution stars: mass loss |
| url | https://www.mdpi.com/2075-4434/13/4/81 |
| work_keys_str_mv | AT sylviaekstrom stellarevolutionthroughtheredsupergiantphase AT cyrilgeorgy stellarevolutionthroughtheredsupergiantphase |