Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02
To explore overshoot mixing and rotational mixing beyond the convective core during the core He-burning phase in massive stars, we computed a grid of stellar models, both rotating and nonrotating, with the k − ω model at Z = 0.02, covering a mass range of 25–120 M _⊙ . The rotating models start with...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/aced88 |
| _version_ | 1827805862222102528 |
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| author | Zhi Li Yan Li |
| author_facet | Zhi Li Yan Li |
| author_sort | Zhi Li |
| collection | DOAJ |
| description | To explore overshoot mixing and rotational mixing beyond the convective core during the core He-burning phase in massive stars, we computed a grid of stellar models, both rotating and nonrotating, with the k − ω model at Z = 0.02, covering a mass range of 25–120 M _⊙ . The rotating models start with a rotation rate of v _ini / v _crit = 0.4 at the zero-age main sequence, and the evolution is computed until the end of the central carbon-burning phase. Models with the k − ω model provide larger convective cores and a broadening of the main-sequence width. The diffusive-overshoot models with f _ov = 0.027 are, on average, closer to the k − ω models for massive stars at Z = 0.02, particularly for the stars with masses greater than 40 M _⊙ . The final masses of the Wolf–Rayet (WR) stars range from 9.5–17.5 M _⊙ and 10–23 M _⊙ for the rotating and nonrotating models, respectively. In the rotating models, the C/N ratio decreases slowly below 0.1 outside the convective core, resulting in a flatter element transition region. In addition, the lifetimes of the WNC phase are 1–4 × 10 ^4 yr, which is about 1 order of magnitude longer than that in the nonrotating models. The masses of the WNC stars are dominated by internal mixing processes and the maximum masses of the He-burning convective cores during the core He-burning phase are in the range of 15–35 M _⊙ . The expected WNC/WR ratios are 0.059 and 0.004 for the rotating and nonrotating models, respectively. |
| first_indexed | 2024-03-11T21:32:11Z |
| format | Article |
| id | doaj.art-d175289b4ad34572b58de09138f07eb8 |
| institution | Directory Open Access Journal |
| issn | 0067-0049 |
| language | English |
| last_indexed | 2024-03-11T21:32:11Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj.art-d175289b4ad34572b58de09138f07eb82023-09-27T08:40:46ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492023-01-0126825110.3847/1538-4365/aced88Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02Zhi Li0https://orcid.org/0000-0003-0418-8461Yan Li1https://orcid.org/0000-0002-1424-3164Yunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; lizhi@ynao.ac.cn; Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , People’s Republic of China; University of Chinese Academy of Sciences , Shijingshan District, Beijing, 100049, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; lizhi@ynao.ac.cn; Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , People’s Republic of China; University of Chinese Academy of Sciences , Shijingshan District, Beijing, 100049, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , Beijing 100012, People’s Republic of ChinaTo explore overshoot mixing and rotational mixing beyond the convective core during the core He-burning phase in massive stars, we computed a grid of stellar models, both rotating and nonrotating, with the k − ω model at Z = 0.02, covering a mass range of 25–120 M _⊙ . The rotating models start with a rotation rate of v _ini / v _crit = 0.4 at the zero-age main sequence, and the evolution is computed until the end of the central carbon-burning phase. Models with the k − ω model provide larger convective cores and a broadening of the main-sequence width. The diffusive-overshoot models with f _ov = 0.027 are, on average, closer to the k − ω models for massive stars at Z = 0.02, particularly for the stars with masses greater than 40 M _⊙ . The final masses of the Wolf–Rayet (WR) stars range from 9.5–17.5 M _⊙ and 10–23 M _⊙ for the rotating and nonrotating models, respectively. In the rotating models, the C/N ratio decreases slowly below 0.1 outside the convective core, resulting in a flatter element transition region. In addition, the lifetimes of the WNC phase are 1–4 × 10 ^4 yr, which is about 1 order of magnitude longer than that in the nonrotating models. The masses of the WNC stars are dominated by internal mixing processes and the maximum masses of the He-burning convective cores during the core He-burning phase are in the range of 15–35 M _⊙ . The expected WNC/WR ratios are 0.059 and 0.004 for the rotating and nonrotating models, respectively.https://doi.org/10.3847/1538-4365/aced88Stellar evolutionMassive starsStellar convective zonesStellar rotationStellar structures |
| spellingShingle | Zhi Li Yan Li Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 The Astrophysical Journal Supplement Series Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures |
| title | Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 |
| title_full | Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 |
| title_fullStr | Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 |
| title_full_unstemmed | Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 |
| title_short | Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 |
| title_sort | grids of wolf rayet stars using mesa with the k ω model from 25 to 120 m ⊙ at z 0 02 |
| topic | Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures |
| url | https://doi.org/10.3847/1538-4365/aced88 |
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