Atmospheric parameters and carbon abundance for hot DB white dwarfs

TL;DR

This study analyzes high-resolution UV spectra of hot DB white dwarfs to determine their atmospheric parameters and element abundances, revealing unusual carbon enrichment and exploring implications for white dwarf evolution.

Contribution

It provides the first detailed atmospheric analysis of hot DB white dwarfs near 25000K, highlighting their carbon enrichment and discussing potential evolutionary links to hot DQ stars.

Findings

Detection of photospheric carbon in two hot DBs

High C/Si ratio limits in these stars

Unresolved origin of hot DQ stars remains

Abstract

Atmospheric parameters for hot DB (helium atmosphere) white dwarfs near effective temperatures of 25000K are extremely difficult to determine from optical spectroscopy. This is particularly unfortunate, because this is the range of variable DBV or V777 Her stars. Accurate atmospheric parameters are needed to help or confirm the asteroseismic analysis of these objects. Another important aspect is the new class of white dwarfs - the hot DQ - detected by Dufour et al. (2007), with spectra dominated by carbon lines. The analysis shows that their atmospheres are pure carbon. The origin of these stars is not yet understood, but they may have an evolutionary link with the hotter DBs as studied here. Our aim is to determine accurate atmospheric parameters and element abundances and study the implications for the evolution white dwarfs of spectral classes DB and hot DQ. High resolution UV spectra of five DBs are studied with model atmospheres. We determine stellar parameters and abundances or upper limits of C and Si. These objects are compared with cooler DBs below 20000K. We find photospheric C and no other heavy elements - with extremely high limits on the C/Si ratio - in two of the five hot DBs. We compare various explanations for this unusual composition, which have been proposed in the literature: accretion of interstellar or circumstellar matter, radiative levitation, carbon dredge-up from deeper interior below the helium layer, and a residual stellar wind. None of these explanations is completely satisfactory, and the problem of the origin of the hot DQ remains an open question.