Atomic Diffusion and ο Leonis

Details Atomic Diffusion and ο Leonis Atomic Diffusion and ο Leonis

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...623..442m&link_type=abstract

The Astrophysical Journal, Volume 623, Issue 1, pp. 442-446.

Astronomy and Astrophysics

Astronomy

11

Stars: Binaries: General, Convection, Diffusion, Stars: Chemically Peculiar, Stars: General

Scientific paper

Evolutionary models for stars of 1.85, 1.89, 1.97, 2.12, and 2.24 Msolar are calculated, taking all effects of atomic diffusion into account. The stars of 1.97 and 2.24 Msolar are shown to reproduce the position in the H-R diagram of the two components of ο Leonis at an age of 706 Myr. ο Leo A is at Teff~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 ο 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 ο Leo A.

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