Volume 531, July 2011
|Number of page(s)||6|
|Published online||04 July 2011|
Iron abundance in the prototype PG 1159 star, GW Vir pulsator PG 1159 − 035, and related objects⋆
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls Universität Tübingen, Sand 1, 72076 Tübingen, Germany
2 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Received: 31 March 2011
Accepted: 3 May 2011
We performed an iron abundance determination of the hot, hydrogen deficient post-AGB star PG 1159 − 035, which is the prototype of the PG 1159 spectral class and the GW Vir pulsators, and of two related objects (PG 1520 + 525, PG 1144 + 005), based on the first detection of Fe viii lines in stellar photospheres. In another PG 1159 star, PG 1424 + 535, we detect Fe vii lines. In all four stars, each within Teff = 110 000−150 000 K, we find a solar iron abundance. This result agrees with our recent abundance analysis of the hottest PG 1159 stars (Teff = 150 000−200 000 K) that exhibit Fe x lines. On the whole, we find that the PG 1159 stars are not significantly iron deficient, in contrast to previous notions.
Key words: stars: abundances / stars: atmospheres / stars: evolution / stars: AGB and post-AGB / white dwarfs
Based on observations made with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer. FUSE was operated for NASA by the Johns Hopkins University under NASA contract NAS5-32985. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26666.
© ESO, 2011
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