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

A. Cristini, C. Meakin, R. Hirschi, W David Arnett, C. Georgy, M. Viallet

Research output: Contribution to journalArticle

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.

Original languageEnglish (US)
Pages (from-to)237-241
Number of pages5
JournalProceedings of the International Astronomical Union
Volume12
Issue numberS329
DOIs
StatePublished - Nov 1 2016

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massive stars
carbon
stellar evolution
simulation
entrainment
large eddy simulation
convection
hydrodynamics
shell
oxygen
expansion
profiles

Keywords

  • Convection
  • hydrodynamics
  • methods: numerical
  • stars: interiors
  • turbulence

ASJC Scopus subject areas

  • Astronomy and Astrophysics

Cite this

The First 3D Simulations of Carbon Burning in a Massive Star. / Cristini, A.; Meakin, C.; Hirschi, R.; Arnett, W David; Georgy, C.; Viallet, M.

In: Proceedings of the International Astronomical Union, Vol. 12, No. S329, 01.11.2016, p. 237-241.

Research output: Contribution to journalArticle

Cristini, A. ; Meakin, C. ; Hirschi, R. ; Arnett, W David ; Georgy, C. ; Viallet, M. / The First 3D Simulations of Carbon Burning in a Massive Star. In: Proceedings of the International Astronomical Union. 2016 ; Vol. 12, No. S329. pp. 237-241.
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