EDP Sciences Journals List
Advanced Search
Subscriber Authentication Point
Home All issues Volume 378/2 Article
Free access article

Issue A&A
Volume 378, Number 2, November I 2001
Page(s) 546 - 555
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20011238



A&A 378, 546-555 (2001)
DOI: 10.1051/0004-6361:20011238

Non-linear radiative models of post-AGB stars: Application to HD 56126

A. B. Fokin1, 2, A. Lèbre2, H. Le Coroller3 and D. Gillet3

1  Institute of Astronomy of the Russian Academy of Sciences, 48 Pjatnitskaya Str., Moscow 109017, Russia
2  Groupe de Recherche en Astronomie et Astrophysique du Languedoc-UMR 5024/ISTEEM (CNRS), Université Montpellier II, Place E. Bataillon, 34095 Montpellier Cedex 05, France
3  Observatoire de Haute-Provence (CNRS), 04870 Saint-Michel-l'Observatoire, France

(Received 19 June 2001 / Accepted 20 August 2001 )

Abstract
In order to study in a general manner the pulsations of the post-AGB stars we performed a grid of non-linear radiative low-mass, high-luminosity models in a wide range of Teff, L and M. Theoretical bolometric light curves and radial velocity curves were computed as well as their associated power spectra. We have also examined the behaviour of these models according to the stellar mass, the chemical composition and the opacity tables we have used in the code. Concerning the carbon rich post-AGB star HD 56126, the models best found to fit its observational characteristics are X = 0.7, Z = 0.004, M = 0.8 $M_\odot$, L = 6000-7000 $L_\odot$ and Teff $\le$ 5850 K. Models computed with smaller mass fail to reproduce both the period and the pulsational amplitude of HD 56126, which is quite different from the pulsational amplitude of the RV Tauri stars. The previously analysed spectroscopic and photometric variations of HD 56126 appear to be consistent with a non-regular radial pulsation where the dominant pulsation mode is the first overtone. In the course of the pulsation, moderate shock waves are repeatedly generated and they propagate throughout the stellar atmosphere. They provoke a complex, asynchronous motion of the outer layers.


Key words: stars: atmospheres -- stars: AGB and post-AGB -- line: profiles -- stars: oscillations -- stars: fundamental parameters -- stars: individual: HD 56126

Offprint request: A. Lèbre, lebre@graal.univ-montp2.fr

SIMBAD Objects



© ESO 2001


What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access. An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.
  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account. In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.