Atomic diffusion and o Leonis

doi:10.1086/427919

Atomic diffusion and o Leonis

2005-04-10

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DOI：10.1086/427919

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Abstract

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Evolutionary models for stars of 1.85, 1.89, 1.97, 2.12, and 2.24 M-. are calculated, taking all effects of atomic diffusion into account. The stars of 1.97 and 2.24 M-. are shown to reproduce the position in the H-R diagram of the two components of o Leonis at an age of 706 Myr. o Leo A is at T-eff similar to 6100 K, much cooler than most known Am stars. The abundance anomalies predicted for this star are also in agreement with observations. It is rapidly evolving toward the giant branch but was caught just before mixing wiped out its abundance anomalies. The model is the same as that used by Richer and coworkers for AmFm stars, and no adjustment of parameters was made for the calculations presented here. The anomalies observed on o Leo are a strong argument in favor of that model for AmFm stars. The earlier model considered for Am stars implied anomalies over a much smaller fraction of the mass of Am stars and appears excluded by the anomalies observed on o Leo A.

Keywords:

binaries : general

convection

diffusion

stars : chemically peculiar

stars : general

Atomic diffusion and o Leonis

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