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 solar mass stellar evolution model. We considered 4 resolutions from 128^3 to 1024^3 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.
@article{arxiv.1712.06852,
title = {The First 3D Simulations of Carbon Burning in a Massive Star},
author = {Andrea Cristini and Casey Meakin and Raphael Hirschi and David Arnett and Cyril Georgy and Maxime Viallet},
journal= {arXiv preprint arXiv:1712.06852},
year = {2017}
}
Comments
5 pages, 3 figures. Published in IAUS 329 on 28/07/17