Turbulent diffusion in stars and the /C-12/C-13/ abundance ratio

Details Turbulent diffusion in stars and the /C-12/C-13/ abundance ratio Turbulent diffusion in stars and the /C-12/C-13/ abundance ratio

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....78..323g&link_type=abstract

Astronomy and Astrophysics, vol. 78, no. 3, Oct. 1979, p. 323-327.

Astronomy and Astrophysics

Astrophysics

25

Abundance, Carbon Isotopes, Giant Stars, Stellar Atmospheres, Stellar Models, Turbulent Diffusion, Carbon 12, Carbon 13, Mass Ratios, Thermonuclear Reactions

Scientific paper

Very mild turbulence drives slow transport of chemical elements by turbulent diffusion within stars. Due to the strong gradient of C-13 generated by thermo-nuclear reactions, a flow of C-13 penetrates the outer part of a star during its life on the main sequence. The average C-13 concentration produced leads, at the time of appearance of the deep surface convective zone during the giant phase, to surface (C-12/C-13) abundance ratios close to the observed ratios. For a turbulent diffusion coefficient D = 200 nu, where nu is the microscopic viscosity, one obtains the following values of the mass (in solar units) and the surface abundance ratio: (1, 8.9); (1.6, 18.2); (2, 24.5). The value of Di is in agreement with that obtained previously by Schatzman (1977).

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