Iron deficiency in hot hydrogen-deficient post-AGB stars

Details Iron deficiency in hot hydrogen-deficient post-AGB stars Iron deficiency in hot hydrogen-deficient post-AGB stars

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9758w&link_type=abstract

HST Proposal ID #9758

Physics

Hst Proposal Id #9758 Hot Stars

Scientific paper

The first attempt to measure the iron abundance in hot hydrogen-deficient post-AGB stars arrived at a surprising result. From the non-detection of iron lines in FUSE spectra of three extremely hot {Teff>100, 000K} PG1159-type central stars of the planetary nebulae, we found that iron is deficient by at least one order of magnitude. We propose HST/STIS observations of three hydrogen-deficient post-AGB stars, each representing the UV-brightest member of a spectroscopic subclass. High-resolution UV spectroscopy will reveal the origin of the iron deficiency. The determination of the Fe/Ni abundance ratio can decide if dust fractionation in the former AGB star atmosphere or s-process neutron-capture in the interior helium-buffer layer is responsible for the iron depletion. In the latter case we can verify our understanding of the "born-again'' star phenomenon and of the s-process synthesis of trans-iron elements in low-mass AGB stars.

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