Modelling Time-dependent Convective Penetration in 1D Stellar Evolution

One-dimensional stellar evolution calculations produce uncertain predictions for quantities like the age, core mass, core compactness, and nucleosynthetic yields; a key source of uncertainty is the modeling of interfaces between regions that are convectively stable and those that are not. Theoretica...
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Autor*in:	Cole Johnston [verfasserIn] Mathias Michielsen [verfasserIn] Evan H. Anders [verfasserIn] Mathieu Renzo [verfasserIn] Matteo Cantiello [verfasserIn] P. Marchant [verfasserIn] Jared A. Goldberg [verfasserIn] Richard H. D. Townsend [verfasserIn] Gautham Sabhahit [verfasserIn] Adam S. Jermyn [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Stellar evolution Stellar convective zones Stellar structures Stellar interiors

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 964(2024), 2, p 170
Übergeordnetes Werk:	volume:964 ; year:2024 ; number:2, p 170

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad2343

Katalog-ID:	DOAJ09866588X

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source	In The Astrophysical Journal 964(2024), 2, p 170 volume:964 year:2024 number:2, p 170
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author	Cole Johnston
spellingShingle	Cole Johnston misc QB460-466 misc Stellar evolution misc Stellar convective zones misc Stellar structures misc Stellar interiors misc Astrophysics Modelling Time-dependent Convective Penetration in 1D Stellar Evolution
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topic_title	QB460-466 Modelling Time-dependent Convective Penetration in 1D Stellar Evolution Stellar evolution Stellar convective zones Stellar structures Stellar interiors
topic	misc QB460-466 misc Stellar evolution misc Stellar convective zones misc Stellar structures misc Stellar interiors misc Astrophysics
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title	Modelling Time-dependent Convective Penetration in 1D Stellar Evolution
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title_auth	Modelling Time-dependent Convective Penetration in 1D Stellar Evolution
abstract	One-dimensional stellar evolution calculations produce uncertain predictions for quantities like the age, core mass, core compactness, and nucleosynthetic yields; a key source of uncertainty is the modeling of interfaces between regions that are convectively stable and those that are not. Theoretical and numerical work has demonstrated that there should be numerous processes adjacent to the convective boundary that induce chemical and angular momentum transport, as well as modify the thermal structure of the star. One such process is called convective penetration, wherein vigorous convection extends beyond the nominal convective boundary and alters both the composition and thermal structure. In this work, we incorporate the process of convective penetration in stellar evolution calculations using the stellar evolution software instrument mesa . We implement convective penetration according to the description presented by Anders et al. to to calculate a grid of models from the pre-main sequence to helium core depletion. The extent of the convective penetration zone is self-consistently calculated at each time step without introducing new free parameters. We find both a substantial penetration zone in all models with a convective core and observable differences to global stellar properties such as the luminosity and radius. We present how the predicted radial extent of the penetration zone scales with the total stellar mass, age, and metallicity of the star. We discuss our results in the context of existing numerical and observational studies.
abstractGer	One-dimensional stellar evolution calculations produce uncertain predictions for quantities like the age, core mass, core compactness, and nucleosynthetic yields; a key source of uncertainty is the modeling of interfaces between regions that are convectively stable and those that are not. Theoretical and numerical work has demonstrated that there should be numerous processes adjacent to the convective boundary that induce chemical and angular momentum transport, as well as modify the thermal structure of the star. One such process is called convective penetration, wherein vigorous convection extends beyond the nominal convective boundary and alters both the composition and thermal structure. In this work, we incorporate the process of convective penetration in stellar evolution calculations using the stellar evolution software instrument mesa . We implement convective penetration according to the description presented by Anders et al. to to calculate a grid of models from the pre-main sequence to helium core depletion. The extent of the convective penetration zone is self-consistently calculated at each time step without introducing new free parameters. We find both a substantial penetration zone in all models with a convective core and observable differences to global stellar properties such as the luminosity and radius. We present how the predicted radial extent of the penetration zone scales with the total stellar mass, age, and metallicity of the star. We discuss our results in the context of existing numerical and observational studies.
abstract_unstemmed	One-dimensional stellar evolution calculations produce uncertain predictions for quantities like the age, core mass, core compactness, and nucleosynthetic yields; a key source of uncertainty is the modeling of interfaces between regions that are convectively stable and those that are not. Theoretical and numerical work has demonstrated that there should be numerous processes adjacent to the convective boundary that induce chemical and angular momentum transport, as well as modify the thermal structure of the star. One such process is called convective penetration, wherein vigorous convection extends beyond the nominal convective boundary and alters both the composition and thermal structure. In this work, we incorporate the process of convective penetration in stellar evolution calculations using the stellar evolution software instrument mesa . We implement convective penetration according to the description presented by Anders et al. to to calculate a grid of models from the pre-main sequence to helium core depletion. The extent of the convective penetration zone is self-consistently calculated at each time step without introducing new free parameters. We find both a substantial penetration zone in all models with a convective core and observable differences to global stellar properties such as the luminosity and radius. We present how the predicted radial extent of the penetration zone scales with the total stellar mass, age, and metallicity of the star. We discuss our results in the context of existing numerical and observational studies.
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title_short	Modelling Time-dependent Convective Penetration in 1D Stellar Evolution
url	https://doi.org/10.3847/1538-4357/ad2343 https://doaj.org/article/ce66b8e98b7a468c94b2a6bde2678dd3 https://doaj.org/toc/1538-4357
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Modelling Time-dependent Convective Penetration in 1D Stellar Evolution

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