All Outputs (3)

Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase (2024)
Journal Article
Rizzuti, F., Hirschi, R., Varma, V., Arnett, W. D., Georgy, C., Meakin, C., Mocák, M., Murphy, A. S., & Rauscher, T. (2024). Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase. Galaxies, 12(6), 87. https://doi.org/10.3390/galaxies12060087

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... Read More about Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase.

Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations (2024)
Journal Article
Rizzuti, F., Hirschi, R., Varma, V., Arnett, W. D., Georgy, C., Meakin, C., Mocák, M., Murphy, A. S., & Rauscher, T. (2024). Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations. Monthly Notices of the Royal Astronomical Society, 533(1), 687-704. https://doi.org/10.1093/mnras/stae1778

One-dimensional (1D) stellar evolution models are widely used across various astrophysical fields, however they are still dominated by important uncertainties that deeply affect their predictive power. Among those, the merging of independent convecti... Read More about Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations.

3D simulations of a neon burning convective shell in a massive star (2024)
Journal Article
Georgy, C., Rizzuti, F., Hirschi, R., Varma, V., Arnett, W. D., Meakin, C., Mocak, M., Murphy, A. S., & Rauscher, T. (2024). 3D simulations of a neon burning convective shell in a massive star. Monthly Notices of the Royal Astronomical Society, 531(4), 4293–4310. https://doi.org/10.1093/mnras/stae1381

The treatment of convection remains a major weakness in the modelling of stellar evolution with one-dimensional (1D) codes. The ever increasing computing power makes now possible to simulate in 3D part of a star for a fraction of its life, allowing u... Read More about 3D simulations of a neon burning convective shell in a massive star.