Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase
Our understanding of stellar evolution and nucleosynthesis is limited by the uncertainties coming from the complex multi-dimensional processes in stellar interiors, such as convection and nuclear burning. Three-dimensional stellar models can improve this knowledge by studying multi-D processes, but...
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| Language: | English |
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MDPI AG
2024-12-01
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| Series: | Galaxies |
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| Online Access: | https://www.mdpi.com/2075-4434/12/6/87 |
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| author | Federico Rizzuti Raphael Hirschi Vishnu Varma William David Arnett Cyril Georgy Casey Meakin Miroslav Mocák Alexander StJ. Murphy Thomas Rauscher |
| author_facet | Federico Rizzuti Raphael Hirschi Vishnu Varma William David Arnett Cyril Georgy Casey Meakin Miroslav Mocák Alexander StJ. Murphy Thomas Rauscher |
| author_sort | Federico Rizzuti |
| collection | DOAJ |
| description | Our understanding of stellar evolution and nucleosynthesis is limited by the uncertainties coming from the complex multi-dimensional processes in stellar interiors, such as convection and nuclear burning. Three-dimensional stellar models can improve this knowledge by studying multi-D processes, but only for a short time range (minutes or hours). Recent advances in computing resources have enabled 3D stellar models to reproduce longer time scales and include nuclear reactions, making the simulations more accurate and allowing to study explicit nucleosynthesis. Here, we present results from 3D stellar simulations of a convective neon-burning shell from a 20 M<sub>⊙</sub> star, run with an explicit nuclear network from its early development to complete fuel exhaustion. We show that convection halts when fuel is exhausted, stopping its further growth after the entrainment of fresh material. These results, which highlight the differences and similarities between 1D and multi-D stellar models, have important implications for the evolution of convective regions in stars and their nucleosynthesis. |
| format | Article |
| id | doaj-art-ca1cdf8ae5f141a684ea57f1780f61d2 |
| institution | OA Journals |
| issn | 2075-4434 |
| language | English |
| publishDate | 2024-12-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Galaxies |
| spelling | doaj-art-ca1cdf8ae5f141a684ea57f1780f61d22025-08-20T02:00:38ZengMDPI AGGalaxies2075-44342024-12-011268710.3390/galaxies12060087Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning PhaseFederico Rizzuti0Raphael Hirschi1Vishnu Varma2William David Arnett3Cyril Georgy4Casey Meakin5Miroslav Mocák6Alexander StJ. Murphy7Thomas Rauscher8Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UKAstrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UKAstrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UKSteward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USAGeneva Observatory, Geneva University, CH-1290 Sauverny, SwitzerlandPasadena Consulting Group, 1075 N Mar Vista Ave, Pasadena, CA 91104, USAAstrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UKSchool of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3FD, UKDepartment of Physics, University of Basel, CH-4056 Basel, SwitzerlandOur understanding of stellar evolution and nucleosynthesis is limited by the uncertainties coming from the complex multi-dimensional processes in stellar interiors, such as convection and nuclear burning. Three-dimensional stellar models can improve this knowledge by studying multi-D processes, but only for a short time range (minutes or hours). Recent advances in computing resources have enabled 3D stellar models to reproduce longer time scales and include nuclear reactions, making the simulations more accurate and allowing to study explicit nucleosynthesis. Here, we present results from 3D stellar simulations of a convective neon-burning shell from a 20 M<sub>⊙</sub> star, run with an explicit nuclear network from its early development to complete fuel exhaustion. We show that convection halts when fuel is exhausted, stopping its further growth after the entrainment of fresh material. These results, which highlight the differences and similarities between 1D and multi-D stellar models, have important implications for the evolution of convective regions in stars and their nucleosynthesis.https://www.mdpi.com/2075-4434/12/6/87convectionhydrodynamicsnuclear reactions, nucleosynthesis, abundancesstars: evolutionstars: interiorsstars: massive |
| spellingShingle | Federico Rizzuti Raphael Hirschi Vishnu Varma William David Arnett Cyril Georgy Casey Meakin Miroslav Mocák Alexander StJ. Murphy Thomas Rauscher Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase Galaxies convection hydrodynamics nuclear reactions, nucleosynthesis, abundances stars: evolution stars: interiors stars: massive |
| title | Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase |
| title_full | Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase |
| title_fullStr | Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase |
| title_full_unstemmed | Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase |
| title_short | Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase |
| title_sort | stellar evolution and convection in 3d hydrodynamic simulations of a complete burning phase |
| topic | convection hydrodynamics nuclear reactions, nucleosynthesis, abundances stars: evolution stars: interiors stars: massive |
| url | https://www.mdpi.com/2075-4434/12/6/87 |
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