The First 3D Simulations of Carbon Burning in a Massive Star

Cristini, A.; Meakin, C.; Hirschi, R.; Arnett, D.; Georgy, C.; Viallet, M.

Abstract

We present the first detailed three-dimensional hydrodynamic implicit large eddy simulations of turbulent convection for carbon burning. The simulations start with an initial radial profile mapped from a carbon burning shell within a 15 M⊙ stellar evolution model. We considered 4 resolutions from 1283 to 10243 zones. These simulations confirm that convective boundary mixing (CBM) occurs via turbulent entrainment as in the case of oxygen burning. The expansion of the boundary into the surrounding stable region and the entrainment rate are smaller at the bottom boundary because it is stiffer than the upper boundary. The results of this and similar studies call for improved CBM prescriptions in 1D stellar evolution models.

Citation

Cristini, A., Meakin, C., Hirschi, R., Arnett, D., Georgy, C., & Viallet, M. (2016). The First 3D Simulations of Carbon Burning in a Massive Star. . https://doi.org/10.1017/s1743921317003441

• Conference Name: Symposium S329: The Lives and Death-Throes of Massive Stars
• Online Publication Date: Jul 28, 2017
• Publication Date: 2016-11
• Deposit Date: Jun 16, 2023
• Publisher: Cambridge University Press
• Volume: 12
• Pages: 237-241
• Series Title: Proceedings of the International Astronomical Union
• DOI: https://doi.org/10.1017/s1743921317003441
• Keywords: Astronomy and Astrophysics; Space and Planetary Science