EDP Sciences
Free Access
Volume 429, Number 1, January I 2005
Page(s) 297 - 308
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20041688
Published online 13 December 2004

A&A 429, 297-308 (2005)
DOI: 10.1051/0004-6361:20041688

Depletion in post-AGB stars with a dusty disc. II.

T. Maas1, 2, H. Van Winckel2 and T. Lloyd Evans3

1  Department of Astronomy, University of Texas, Austin, TX 78712, USA
    e-mail: thomas@astro.as.utexas.edu
2  Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
3  School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife, Scotland KY16 9SS, UK

(Received 19 July 2004 / Accepted 30 August 2004)

We present a chemical abundance analysis on the basis of high signal-to-noise and high resolution spectra for 12 stars of our newly defined sample. The selection criterion for the stars of this sample was their position in the "RV Tauri" box in the [12]-[25], [25]-[60] two-colour diagram. An additional requisite was the presence of a near-IR excess. We found that the photospheres of nine stars are affected by the depletion process. Since the most likely origin of the near-IR excess is a disc, this strongly suggests that the phenomenon of depletion and the presence of a disc are linked. Among the depleted stars we find different depletion patterns. In seven stars elements with a condensation temperature below 1500 K are not or only slightly affected. Large underabundances are measured only for most elements with a condensation temperature above 1500 K.

Key words: stars: abundances -- stars: AGB and post-AGB -- stars: evolution -- stars: binaries: spectroscopic

SIMBAD Objects

© ESO 2004

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