AmFm Stars as a Test of Rotational Mixing Models

Details AmFm Stars as a Test of Rotational Mixing Models AmFm Stars as a Test of Rotational Mixing Models

Jul 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...645..634t&link_type=abstract

The Astrophysical Journal, Volume 645, Issue 1, pp. 634-651.

Astronomy and Astrophysics

Astronomy

21

Hydrodynamics, Stars: Rotation

Scientific paper

Stellar evolution models have been calculated for stars of 1.7-2.5 Msolar with both the Geneva-Toulouse and Montreal codes. In the Geneva-Toulouse code, the internal evolution of angular momentum is calculated self-consistently along with the transport of a few species. In the Montreal code, the transport of 24 species is treated in detail, taking into account radiative accelerations, thermal diffusion, and gravitational settling, along with the turbulent diffusion coefficients calculated in the Geneva-Toulouse code. It is verified that the two codes lead to very similar internal structure for a given mass. The calculated surface abundances are compared to abundance anomalies observed on AmFm stars. It is found that with approximately the same parameters as used for other types of stars, the Geneva-Toulouse code leads to turbulent transport coefficients that produce abundance anomalies consistent with the observed ones for HD 73045, HD 23610, and Sirius. Taking into account the effect of the anisotropy of turbulence on vertical transport plays an important role, although the level of anisotropy in stellar envelopes is very uncertain; this effect is usually neglected in calculations. The stabilizing effect of the mean molecular weight gradient can also be important. The current level of accuracy of observed abundances only permits to choose within a one-parameter family of models. To distinguish between turbulent models with different interior profiles, an accuracy of 0.03 dex is required of abundance determinations, a level of accuracy that is not currently achieved. It is also shown that taking into account the pre-main-sequence evolution of the rotation profile leads to an important reduction in the Ω dependence of turbulent transport for slow rotators.

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