Hydrogen-helium-diffusion in solar models

Details Hydrogen-helium-diffusion in solar models Hydrogen-helium-diffusion in solar models

Oct 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...205..125w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 205, no. 1-2, Oct. 1988, p. 125-128.

Physics

23

Gaseous Diffusion, Helium Hydrogen Atmospheres, Solar Physics, Stellar Evolution, Stellar Models, Diffusion Coefficient, Main Sequence Stars, Stellar Mass

Scientific paper

The effect of diffusion on stellar evolution is shown by comparing solar models without, with and with artificially increased diffusion. The diffusion equation includes temperature diffusion and pressure diffusion as well as concentration diffusion. The numerical calculations demonstrate that the main contribution to diffusion inside a star is pressure diffusion. Therefore the effect of diffusion is an enrichment of helium in the center and of hydrogen at the surface of the star. Consequences for models of the present-day sun that include diffusion compared to a model without diffusion are decreased values of the initial helium abundances (Y0 = 0.268 and 0.264 instead of 0.270) and increased mixing length parameters (α = 1.75 and 1.96 instead of 1.64).

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