Volume 381, Number 3, JanuaryIII 2002
|Page(s)||971 - 981|
|Section||Interstellar and circumstellar matter|
|Published online||15 January 2002|
The accretion/diffusion theory for λ Bootis stars in the light of spectroscopic data
Institute for Astronomy (IfA), University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria e-mail: firstname.lastname@example.org
2 Department of Astronomy, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106-7215, USA
3 Zentraler Informatikdienst der Universität Wien, Universitätsstrasse 7, 1010 Vienna, Austria e-mail: email@example.com
Corresponding author: U. Heiter, firstname.lastname@example.org
Accepted: 25 October 2001
Most of the current theories suggest the λ Bootis phenomenon to originate from an interaction between the stellar surface and its local environment. In this paper, we compare the abundance pattern of the λ Bootis stars to that of the interstellar medium and find larger deficiencies for Mg, Si, Mn and Zn than in the interstellar medium. A comparison with metal poor post-AGB stars showing evidence for circumstellar material indicates a similar physical process possibly being at work for some of the λ Bootis stars, but not for all of them. Despite the fact that the number of spectroscopically analysed λ Bootis stars has considerably increased in the past, a test of predicted effects with observations shows current abundance and temperature data to be still controversial.
Key words: stars: abundances / stars: atmospheres / stars: chemically peculiar / stars: early-type / ISM: abundances
© ESO, 2002
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