EDP Sciences
Free Access
Volume 368, Number 1, March II 2001
Page(s) 250 - 266
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20000572

A&A 368, 250-266 (2001)
DOI: 10.1051/0004-6361:20000572

Atmospheric abundances in post-AGB candidates of intermediate temperature

A. Arellano Ferro1, Sunetra Giridhar2 and P. Mathias3

1  Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, México D.F., CP 04510, México
2  Indian Institute of Astrophysics, Bangalore 560034, India
    e-mail: giridhar@iiap.ernet.in
3  Observatoire de la Côte d'Azur, Département Fresnel, UMR 6528, BP 4229, 06304 Nice Cedex 04, France
    e-mail: mathias@obs-nice.fr

(Received 23 August 2000 / Accepted 19 December 2000)

Detailed atmospheric abundances have been calculated for a sample of A-G supergiant stars with IR fluxes and/or high galactic latitudes. HD 172481 and HD 158616 show clear indications of being post-AGB stars that have experienced third dredge-up. HD 158616 is carbon-rich while the abundance pattern of HD 172481 and its large Li enhancement gives support to the hot bottom burning scenario that explains paucity of carbon-rich stars among AGB stars. HD 172324 is very likely a hot post-AGB star that shows a strong carbon deficiency. HD 725, HD 218753 and HD 331319 also appear to be evolved objects between the red giant and the AGB. HD 9167, HD 173638 with a few exceptions, reflect solar abundances and no signs of post red giant evolution. They are most likely young massive disk supergiants. Further analysis of proto-Planetary Nebula HDE 341617 reveals that He lines show signs of velocity stratification. The emission lines have weakened considerably since 1993. The envelope expands at 19 km s-1 relative to the star. Atmospheric abundances, evolutionary tracks and isochrones are used to estimate masses and ages of all stars in the sample.

Key words: stars: post-AGB -- stars: chemically peculiar -- stars: evolution

Offprint request: A. Arellano Ferro armando@astroscu.unam.mx

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© ESO 2001