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

Published online by Cambridge University Press:  28 July 2017


A. Cristini
Affiliation:
Astrophysics Group, Keele University, Lennard-Jones Laboratories, Keele, ST5 5BG, UK
C. Meakin
Affiliation:
Karagozian & Case, Inc., 700 N. Brand Blvd. Suite 700, Glendale, CA, 91203, USA Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
R. Hirschi
Affiliation:
Astrophysics Group, Keele University, Lennard-Jones Laboratories, Keele, ST5 5BG, UK Kavli IPMU (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
D. Arnett
Affiliation:
Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
C. Georgy
Affiliation:
Astrophysics Group, Keele University, Lennard-Jones Laboratories, Keele, ST5 5BG, UK Geneva Observatory, University of Geneva, Maillettes 51, 1290 Versoix, Switzerland
M. Viallet
Affiliation:
Max-Planck-Institut für Astrophysik, Karl Schwarzschild Strasse 1, Garching, D-85741, Germany
Corresponding
E-mail address:

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.


Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

References

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