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

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

doi:10.1017/S1743921317003441

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

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

Steward Observatory

Research output: Contribution to journal › Article › peer-review

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 language	English (US)
Pages (from-to)	237-241
Number of pages	5
Journal	Proceedings of the International Astronomical Union
Volume	12
Issue number	S329
DOIs	https://doi.org/10.1017/S1743921317003441
State	Published - Nov 1 2016

Keywords

Convection
hydrodynamics
methods: numerical
stars: interiors
turbulence

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1017/S1743921317003441

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title = "The First 3D Simulations of Carbon Burning in a Massive Star",

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.",

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author = "A. Cristini and C. Meakin and R. Hirschi and D. Arnett and C. Georgy and M. Viallet",

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T1 - The First 3D Simulations of Carbon Burning in a Massive Star

AU - Cristini, A.

AU - Meakin, C.

AU - Hirschi, R.

AU - Arnett, D.

AU - Georgy, C.

AU - Viallet, M.

PY - 2016/11/1

Y1 - 2016/11/1

N2 - 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.

AB - 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.

KW - Convection

KW - hydrodynamics

KW - methods: numerical

KW - stars: interiors

KW - turbulence

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

Abstract

Keywords

ASJC Scopus subject areas

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