The far-ultraviolet spectra of "cool" PG1159 stars

Abstract

We present a comprehensive study of Far Ultraviolet Spectroscopic Explorer (FUSE) spectra (912-1190 A) of two members of the PG1159 spectral class, which consists of hydrogen-deficient (pre-) white dwarfs with effective temperatures in the range Teff = 75,000-200,000 K. As two representatives of the cooler objects, we have selected PG1707+427 (Teff = 85,000 K) and PG1424+535 (Teff = 110,000 K), complementing a previous study of the hotter prototype PG1159-035 (Teff = 140,000 K). The helium-dominated atmospheres are strongly enriched in carbon and oxygen, therefore, their spectra are dominated by lines from C III-IV and O III-VI, many of which were never observed before in hot stars. In addition, lines of many other metals (N, F, Ne, Si, P, S, Ar, Fe) are detectable, demonstrating that observations in this spectral region are most rewarding when compared to the near-ultraviolet and optical wavelength bands. We perform abundance analyses of these species and derive upper limits for several undetected light and heavy metals including iron-group and trans-iron elements. The results are compared to predictions of stellar evolution models for neutron-capture nucleosynthesis and good agreement is found.

Accepted for publication in A&A

References in corpus (3)

• Discovery of photospheric argon in very hot central stars of planetary nebulae and white dwarfs
• High-resolution ultraviolet spectroscopy of PG1159-035 with HST and FUSE
• Stellar laboratories IV. New Ga IV, Ga V, and Ga VI oscillator strengths and the gallium abundance in the hot white dwarfs G191-B2B and RE0503-289

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