3D hydrodynamic simulations of carbon burning in massive stars

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

Research output: Contribution to journalArticle

19 Citations (Scopus)

Abstract

We present the first detailed 3D hydrodynamic implicit large eddy simulations of turbulent convection of carbon burning in massive stars. Simulations begin with radial profiles mapped from a carbon-burning shell within a 15M 1D stellar evolution model. We consider models with 1283, 2563, 5123, and 10243 zones. The turbulent flow properties of these carbon-burning simulations are very similar to the oxygen-burning case. We performed a mean field analysis of the kinetic energy budgets within the Reynolds-averaged Navier-Stokes framework. For the upper convective boundary region, we find that the numerical dissipation is insensitive to resolution for linear mesh resolutions above 512 grid points. For the stiffer, more stratified lower boundary, our highest resolution model still shows signs of decreasing sub-grid dissipation suggesting it is not yet numerically converged. We find that the widths of the upper and lower boundaries are roughly 30 per cent and 10 per cent of the local pressure scaleheights, respectively. The shape of the boundaries is significantly different from those used in stellar evolution models. As in past oxygen-shell-burning simulations, we observe entrainment at both boundaries in our carbon-shell-burning simulations. In the large Peclet number regime found in the advanced phases, the entrainment rate is roughly inversely proportional to the bulk Richardson number, RiB (∝RiB, 0.5 ≲ α ≲ 1.0).We thus suggest the use of RiB as a means to take into account the results of 3D hydrodynamics simulations in new 1D prescriptions of convective boundary mixing.

Original languageEnglish (US)
Pages (from-to)279-300
Number of pages22
JournalMonthly Notices of the Royal Astronomical Society
Volume471
Issue number1
DOIs
StatePublished - Jan 1 2017

Fingerprint

massive stars
hydrodynamics
carbon
simulation
stellar evolution
entrainment
shell
dissipation
grids
Richardson number
energy budgets
oxygen
Peclet number
large eddy simulation
energy budget
turbulent flow
kinetic energy
mesh
convection
high resolution

Keywords

  • Convection
  • Hydrodynamics
  • Stars: evolution
  • Stars: interiors
  • Stars: massive
  • Turbulence

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Cristini, A., Meakin, C., Hirschi, R., Arnett, W. D., Georgy, C., Viallet, M., & Walkington, I. (2017). 3D hydrodynamic simulations of carbon burning in massive stars. Monthly Notices of the Royal Astronomical Society, 471(1), 279-300. https://doi.org/10.1093/MNRAS/STX1535

3D hydrodynamic simulations of carbon burning in massive stars. / Cristini, A.; Meakin, C.; Hirschi, R.; Arnett, W David; Georgy, C.; Viallet, M.; Walkington, I.

In: Monthly Notices of the Royal Astronomical Society, Vol. 471, No. 1, 01.01.2017, p. 279-300.

Research output: Contribution to journalArticle

Cristini, A, Meakin, C, Hirschi, R, Arnett, WD, Georgy, C, Viallet, M & Walkington, I 2017, '3D hydrodynamic simulations of carbon burning in massive stars', Monthly Notices of the Royal Astronomical Society, vol. 471, no. 1, pp. 279-300. https://doi.org/10.1093/MNRAS/STX1535
Cristini, A. ; Meakin, C. ; Hirschi, R. ; Arnett, W David ; Georgy, C. ; Viallet, M. ; Walkington, I. / 3D hydrodynamic simulations of carbon burning in massive stars. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 471, No. 1. pp. 279-300.
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