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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Gespeichert in:

Autor*in:	Zhi Li [verfasserIn] Yan Li [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures

Übergeordnetes Werk:	In: The Astrophysical Journal Supplement Series - IOP Publishing, 2022, 268(2023), 2, p 51
Übergeordnetes Werk:	volume:268 ; year:2023 ; number:2, p 51

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4365/aced88

Katalog-ID:	DOAJ099508788

Internformat


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allfields	10.3847/1538-4365/aced88 doi (DE-627)DOAJ099508788 (DE-599)DOAJd175289b4ad34572b58de09138f07eb8 DE-627 ger DE-627 rakwb eng QB460-466 Zhi Li verfasserin aut Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures Astrophysics Yan Li verfasserin aut In The Astrophysical Journal Supplement Series IOP Publishing, 2022 268(2023), 2, p 51 (DE-627)312200196 (DE-600)2006860-8 15384365 nnns volume:268 year:2023 number:2, p 51 https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/article/d175289b4ad34572b58de09138f07eb8 kostenfrei https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/toc/0067-0049 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 268 2023 2, p 51
spelling	10.3847/1538-4365/aced88 doi (DE-627)DOAJ099508788 (DE-599)DOAJd175289b4ad34572b58de09138f07eb8 DE-627 ger DE-627 rakwb eng QB460-466 Zhi Li verfasserin aut Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures Astrophysics Yan Li verfasserin aut In The Astrophysical Journal Supplement Series IOP Publishing, 2022 268(2023), 2, p 51 (DE-627)312200196 (DE-600)2006860-8 15384365 nnns volume:268 year:2023 number:2, p 51 https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/article/d175289b4ad34572b58de09138f07eb8 kostenfrei https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/toc/0067-0049 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 268 2023 2, p 51
allfields_unstemmed	10.3847/1538-4365/aced88 doi (DE-627)DOAJ099508788 (DE-599)DOAJd175289b4ad34572b58de09138f07eb8 DE-627 ger DE-627 rakwb eng QB460-466 Zhi Li verfasserin aut Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures Astrophysics Yan Li verfasserin aut In The Astrophysical Journal Supplement Series IOP Publishing, 2022 268(2023), 2, p 51 (DE-627)312200196 (DE-600)2006860-8 15384365 nnns volume:268 year:2023 number:2, p 51 https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/article/d175289b4ad34572b58de09138f07eb8 kostenfrei https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/toc/0067-0049 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 268 2023 2, p 51
allfieldsGer	10.3847/1538-4365/aced88 doi (DE-627)DOAJ099508788 (DE-599)DOAJd175289b4ad34572b58de09138f07eb8 DE-627 ger DE-627 rakwb eng QB460-466 Zhi Li verfasserin aut Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures Astrophysics Yan Li verfasserin aut In The Astrophysical Journal Supplement Series IOP Publishing, 2022 268(2023), 2, p 51 (DE-627)312200196 (DE-600)2006860-8 15384365 nnns volume:268 year:2023 number:2, p 51 https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/article/d175289b4ad34572b58de09138f07eb8 kostenfrei https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/toc/0067-0049 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 268 2023 2, p 51
allfieldsSound	10.3847/1538-4365/aced88 doi (DE-627)DOAJ099508788 (DE-599)DOAJd175289b4ad34572b58de09138f07eb8 DE-627 ger DE-627 rakwb eng QB460-466 Zhi Li verfasserin aut Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures Astrophysics Yan Li verfasserin aut In The Astrophysical Journal Supplement Series IOP Publishing, 2022 268(2023), 2, p 51 (DE-627)312200196 (DE-600)2006860-8 15384365 nnns volume:268 year:2023 number:2, p 51 https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/article/d175289b4ad34572b58de09138f07eb8 kostenfrei https://doi.org/10.3847/1538-4365/aced88 kostenfrei https://doaj.org/toc/0067-0049 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 268 2023 2, p 51
language	English
source	In The Astrophysical Journal Supplement Series 268(2023), 2, p 51 volume:268 year:2023 number:2, p 51
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callnumber-first	Q - Science
author	Zhi Li
spellingShingle	Zhi Li misc QB460-466 misc Stellar evolution misc Massive stars misc Stellar convective zones misc Stellar rotation misc Stellar structures misc Astrophysics Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02
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topic_title	QB460-466 Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02 Stellar evolution Massive stars Stellar convective zones Stellar rotation Stellar structures
topic	misc QB460-466 misc Stellar evolution misc Massive stars misc Stellar convective zones misc Stellar rotation misc Stellar structures misc Astrophysics
topic_unstemmed	misc QB460-466 misc Stellar evolution misc Massive stars misc Stellar convective zones misc Stellar rotation misc Stellar structures misc Astrophysics
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title	Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02
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title_full	Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02
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title_sort	grids of wolf–rayet stars using mesa with the k − ω model: from 25 to 120 m ⊙ at z = 0.02
callnumber	QB460-466
title_auth	Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02
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 × 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.
abstractGer	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.
abstract_unstemmed	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.
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container_issue	2, p 51
title_short	Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02
url	https://doi.org/10.3847/1538-4365/aced88 https://doaj.org/article/d175289b4ad34572b58de09138f07eb8 https://doaj.org/toc/0067-0049
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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 _⊙ . 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Grids of Wolf–Rayet Stars Using MESA with the k − ω Model: From 25 to 120 M ⊙ at Z = 0.02

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