Issue |
A&A
Volume 433, Number 2, April II 2005
|
|
---|---|---|
Page(s) | 641 - 645 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361:20042258 | |
Published online | 22 March 2005 |
Fluorine in extremely hot post-AGB stars: Evidence for nucleosynthesis*
1
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany e-mail: werner@astro.uni-tuebingen.de
2
Dr.-Remeis-Sternwarte, Universität Erlangen-Nürnberg, Sternwartstraße 7, 96049 Bamberg, Germany
3
Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA
Received:
26
October
2004
Accepted:
30
November
2004
We have discovered lines of highly ionized fluorine ( and
) in the far-UV spectra of extremely hot
(
= 85 000–150 000 K) post-AGB stars. Our sample comprises H-rich
central stars of planetary nebulae as well as H-deficient PG1159 stars. We
performed non-LTE calculations and find strong F overabundances (up to 10-4
by mass, i.e., 250 times solar) in a number of PG1159 stars, while F is
essentially solar in the H-rich stars. Since PG1159 stars are believed to
exhibit intershell matter of the preceding AGB phase on their surface, their
chemical analyses allow for a direct insight into nucleosynthesis processes
during the AGB phase. The high F abundances in PG1159 stars confirm the
conclusion from abundance determinations in giants, that F is synthesized in AGB
stars and that the F enrichment in the intershell must be very high.
Key words: stars: abundances / stars: evolution / stars: AGB and post-AGB / stars: white dwarfs
© ESO, 2005
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