Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..584k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 15, 1984, p. 584-590. Research supported by the L. Deutscher Foun
Astronomy and Astrophysics
Astrophysics
3
Stellar Cores, Stellar Oscillations, Thermal Diffusion, Carbon Stars, Convection, Gaseous Diffusion, Giant Stars, Stellar Composition, Stellar Envelopes, Stellar Evolution, Stellar Structure, Thermonuclear Reactions
Scientific paper
The effect of diffusion on the evolution of a thermally pulsating star of six solar masses, at different core-mass values in the range 0.8-1.0 solar mass is investigated. The diffusion equations, including terms for concentration, pressure, and temperature are solved for mixture of three gases: H, He, and a third component representative of all heavier elements. Diffusion is negligible in the homogeneous envelope and in the almost homogeneous core. The diffusion time scale becomes relatively short in the double-shell region between the core and the envelope. In this region, nuclear reactions and convection are much more rapid than diffusion. Diffusive equilibrium is quickly established in a certain region within the double-shell zone, due to the fact that diffusion resulting from composition gradients is opposed by pressure diffusion and thermal diffusion. The composition profiles eventually become frozen if temperature and density profiles remain unchanged.
Kovetz Attay
Prialnik Dina
Shaviv Giora
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