| Issue |
A&A
Volume 579, July 2015
|
|
|---|---|---|
| Article Number | A122 | |
| Number of page(s) | 8 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/201526029 | |
| Published online | 15 July 2015 | |
Convective settling in main sequence stars: Li and Be depletion
Max Planck Institute for Astrophysics, Karl-Schwarzschildstr. 1, 85748 Garching, Germany
e-mail: robo@mpa-garching.mpg.de
Received: 5 March 2015
Accepted: 25 May 2015
The process of convective settling is based on the assumption that a small fraction of the low-entropy downflows sink from the photosphere down to the bottom of the star’s envelope convection zone retaining a substantial entropy contrast. We have previously shown that this process could explain the slow Li depletion observed in the Sun. We construct a parametric model of convective settling to investigate the dependence of Li and Be depletion on stellar mass and age. Our model is generally in good agreement with the Li abundances measured in open clusters and solar twins, although it seems to underestimate the Li depletion in the first ~1 Gyr. The model is also compatible with the Be abundances measured in a sample of field stars.
Key words: convection / stars: evolution / stars: abundances
© ESO, 2015
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