Can Enhanced Diffusion Improve Helioseismic Agreement for Solar Models with Revised Abundances?

Details Can Enhanced Diffusion Improve Helioseismic Agreement for Solar Models with Revised Abundances? Can Enhanced Diffusion Improve Helioseismic Agreement for Solar Models with Revised Abundances?

2005-02-17

arxiv.org/abs/astro-ph/0502364v2

Astrophys.J. 627 (2005) 1049-1056

Astronomy and Astrophysics

Astrophysics

Version 2: 24 pages, 3 figures; Accepted to ApJ with omission of g-mode predictions and discussion that are included in this p

Scientific paper

10.1086/430438

Recent solar photospheric abundance analyses (Asplund et al. 2004, 2005; Lodders 2003) have revised downward the C, N, O, Ne, and Ar abundances by 0.15 to 0.2 dex compared to previous determinations of Grevesse & Sauval (1998). With these revisions, the photospheric Z/X decreases to 0.0165 (0.0177 Lodders), and Z to ~0.0122 (0.0133 Lodders). A number of papers report that solar models evolved with standard opacities and diffusion treatment using these new abundances give poor agreement with helioseismic inferences. Here we explore evolved solar models with varying diffusion treatments to reduce the photospheric abundances while keeping the interior abundances about the same as earlier standard models. While enhanced diffusion improves agreement with some helioseismic constraints compared to a solar model evolved with the new abundances using nominal input physics, the required increases in thermal diffusion rates are unphysically large, and none of the variations tried restores the good agreement attained using the earlier abundances. A combination of modest opacity increases, diffusion enhancements, and abundance increases near the level of the uncertainties, while somewhat contrived, remains the most physically plausible means to restore agreement with helioseismology. The case for enhanced diffusion would be improved if the inferred convection-zone helium abundance could be reduced; we recommend reconsidering this derivation in light of new equations of state with modified abundances and other improvements. We also recommend considering, as a last resort, diluting the convection zone, which contains only 2.5% of the sun's mass, by accretion of material depleted in these more volatile elements C, N, O, Ne, & Ar after the sun arrived on the main sequence.

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