Stellar Models with Microscopic Diffusion and Rotational Mixing I: Application to the Sun

Details Stellar Models with Microscopic Diffusion and Rotational Mixing I: Application to the Sun Stellar Models with Microscopic Diffusion and Rotational Mixing I: Application to the Sun

1994-08-17

arxiv.org/abs/astro-ph/9408058v1

Astrophys.J. 441 (1995) 865

Astronomy and Astrophysics

Astrophysics

16 pages, uuencoded postscript, also available by anonymous ftp to ftp.cita.utoronto.ca in: /cita/brian/papers/sun.ps submitte

Scientific paper

10.1086/175408

The Yale stellar evolution code has been modified to include the combined effects of diffusion and rotational mixing on $^1$H, $^4$He and the trace elements $^3$He, $^6$Li, $^7$Li, and $^9$Be. The interaction between rotational mixing and diffusion is studied by calculating a number of calibrated solar models. The rotational mixing inhibits the diffusion in the outer parts of the models, leading to a decrease in the envelope diffusion by 25 -- 50\%. Conversely, diffusion leads to gradients in mean molecular weight which can inhibit the rotational mixing. The degree to which gradients in mean molecular weight inhibits the rotational mixing is somewhat uncertain. A comparison to the observed solar oblateness suggests that gradients in the mean molecular weight play a smaller role in inhibiting the rotational mixing previously believed. This is reinforced by the fact that the model with the standard value for the inhibiting effect of mean molecular weight on the rotational mixing depletes no Li on the main sequence. This is in clear contrast to the observations. A reduction in the inhibiting effect of mean molecular weight gradients by a factor of ten leads to noticeable main sequence Li depletion.

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