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Consistent Solar Evolution Model Including Diffusion and Radiative Acceleration Effects
The solar evolution has been calculated including all the effects of the diffusion of helium and heavy elements. Monochromatic opacities are used to calculate radiative accelerations and Rosseland
Implications of WMAP Observations on Li Abundance and Stellar Evolution Models
The Wilkinson Microwave Anisotropy Probe (WMAP) determination of the baryon-to-photon ratio implies, through big bang nucleosynthesis, a cosmological Li abundance larger, by a factor of 2-3, than the
Diffusion in white dwarfs - New results and comparative study
On presente de nouvelles estimations des echelles de temps de diffusion des elements lourds dans les naines blanches
Diffusion coefficients for stellar plasmas
On presente une methode approximee de calcul des coefficients de diffusion pour des plasmas denses caracteristiques des enveloppes de naines blanches
Models of Metal-Poor Stars with Gravitational Settling and Radiative Accelerations
Isochrones for ages between 12 and 18 Gyr have been derived from the evolutionary tracks presented in Paper I (Richard et al.) for masses from 0.5 to 1.0 Mand initial chemical abundances
Models of metal poor stars with gravitational settling and radiative accelerations: I. evolution and abundance anomalies
Evolutionary models have been calculated for Population II stars of 0.5-1.0 M? from the pre-main sequence to the lower part of the giant branch. Rosseland opacities and radiative accelerations were
The Evolution of AmFm Stars, Abundance Anomalies, and Turbulent Transport
Stellar evolution models of stars of 1.45-3.0 M☉ have been calculated, including the atomic diffusion of metals and radiative accelerations for all species in the OPAL opacities. As the abundances
Models for solar abundance stars with gravitational settling and radiative accelerations: Application to M67 and NGC 188
Evolutionary models taking into account radiative accelerations, thermal diffusion, and gravitational settling for 28 elements, including all those contributing to OPAL stellar opacities, have been
Models of Metal-poor Stars with Gravitational Settling and Radiative Accelerations. III. Metallicity Dependence
Evolutionary models have been calculated for Population II stars of 0.5-1.2 Mfrom the pre-main sequence to the lower part of the giant branch. Models were calculated for Z ¼ 0:017 � 10 � 4 to 0.0068
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