Stellar laboratories. V. The Xe vi ultraviolet spectrum and the xenon abundance in the hot DO-type white dwarf RE 0503-289
Abstract
Context. For the spectral analysis of spectra of hot stars with a high resolution and high signal-to-noise ratio (S/N), advanced non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that are used for their calculation.
Aims: Reliable Xe vi oscillator strengths are used to identify Xe lines in the ultraviolet spectrum of the DO-type white dwarf
Methods: We publish newly calculated oscillator strengths that are based on a recently measured Xe vi laboratory line spectrum. These strengths were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models to analyze Xe vi lines exhibited in high-resolution and high S/N UV observations of
Results: We identify three hitherto unknown Xe vi lines in the ultraviolet spectrum of
Conclusions: Reliable measurements and calculations of atomic data are prerequisite for stellar-atmosphere modeling. Observed Xe vi line profiles in the ultraviolet spectrum of the white dwarf
- Publication:
-
Astronomy and Astrophysics
- Pub Date:
- May 2015
- DOI:
- 10.1051/0004-6361/201526078
- arXiv:
- arXiv:1504.01991
- Bibcode:
- 2015A&A...577A..88R
- Keywords:
-
- atomic data;
- line: identification;
- stars: abundances;
- stars: atmospheres;
- stars: individual: RE0503-289;
- white dwarfs;
- Astrophysics - Solar and Stellar Astrophysics;
- Physics - Atomic Physics
- E-Print:
- 3 pages, 4 figures