2004/10/28 by K. Werner, Werner, K., T. Rauch +4
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Gamma-ray bursts and supernovae #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0410689
3 pages, to appear in "Astrophysics in the FUV: Five years of discovery with FUSE", ed. Sonneborn, Moos, Andersson, ASP Conf. Series
arxiv created 2004/10/28 · openalex publication_date 2004/10/28 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
FUSE spectroscopy has proved that extremely hot hydrogen-deficient post-AGB stars (PG1159 stars) display matter on their surface that usually remains hidden in the region between the H- and He-burning shells of the former AGB star. Hence, the spectral analysis of PG1159 stars allows to study directly the chemistry of this intershell region which is the outcome of complicated burning and mixing processes during AGB evolution. Detailed abundance determinations provide constraints for these processes which are still poorly understood. With FUSE we have discovered high neon and fluorine overabundances. There is also a significant iron deficiency, which may be caused by s-process neutron capture transforming iron into heavier elements.