The far-ultraviolet spectra of "cool" PG1159 stars

TL;DR

This study analyzes far-ultraviolet spectra of two cool PG1159 stars, revealing detailed chemical compositions and comparing findings with stellar evolution models, thus enhancing understanding of hydrogen-deficient pre-white dwarfs.

Contribution

It provides the first detailed abundance analysis of cooler PG1159 stars in the far-ultraviolet, expanding knowledge of their chemical compositions and evolutionary status.

Findings

Detection of numerous metal lines, including many observed for the first time in hot stars.

Derived elemental abundances consistent with stellar evolution models for neutron-capture nucleosynthesis.

Established upper limits for undetected elements, informing future spectral studies.

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.