Grids of Wolf–Rayet Stars Using MESA with the k ? ω Model: From 25 to 120 M ⊙ at Z = 0.02
文献类型：期刊论文
| 作者 | Li,Zhi2,3,4; Li,Yan1,2,3,4; Li Y(李焱) ; Li Z(李志)
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| 刊名 | The Astrophysical Journal Supplement Series
 |
| 出版日期 | 2023-09-27 |
| 卷号 | 268期号:2 |
| ISSN号 | 0067-0049 |
| DOI | 10.3847/1538-4365/aced88 |
| 通讯作者 | Li,Zhi() |
| 英文摘要 | Abstract 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 × 104 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. |
| 语种 | 英语 |
| 出版者 | The American Astronomical Society |
| WOS记录号 | IOP:APJS_268_2_51 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/26346]  |
| 专题 | 云南天文台_恒星物理研究组 云南天文台_中国科学院天体结构与演化重点实验室 |
| 通讯作者 | Li,Zhi; Li Z(李志) |
| 作者单位 | 1.Center for Astronomical Mega-Science, Chinese Academy of Sciences, Beijing 100012, People’s Republic of China 2.University of Chinese Academy of Sciences, Shijingshan District, Beijing, 100049, People’s Republic of China 3.Key Laboratory for Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, People’s Republic of China 4.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People’s Republic of China; lizhi@ynao.ac.cn |
| 推荐引用方式 GB/T 7714 | Li,Zhi,Li,Yan,Li Y,et al. Grids of Wolf–Rayet Stars Using MESA with the k ? ω Model: From 25 to 120 M ⊙ at Z = 0.02[J]. The Astrophysical Journal Supplement Series,2023,268(2). |
| APA | Li,Zhi,Li,Yan,Li Y,&Li Z.(2023).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,268(2). |
| MLA | Li,Zhi,et al."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 268.2(2023). |
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来源：云南天文台
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