http://arxiv.org/abs/1504.01991
For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation.
Reliable Xe VI oscillator strengths are used to identify Xe lines in the ultraviolet spectrum of the DO-type white dwarf RE0503-289 and to determine its photospheric Xe abundance.
Based on a recently measured Xe VI laboratory line spectrum, newly calculated oscillator strengths were published. These were used to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for the analysis of Xe VI lines exhibited in high-resolution and high-S/N UV observations of RE0503-289.
We identified three hitherto unknown Xe VI lines in the ultraviolet spectrum of RE0503-289 and confirmed its previously measured photospheric Xe abundance (-4.2 +/- 0.6 by mass).
Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. Observed Xe VI line profiles in the ultraviolet spectrum of the white dwarf RE0503-289 were well reproduced with the newly calculated Xe VI oscillator strengths.
T. Rauch, D. Hoyer, P. Quinet, et. al.
Thu, 9 Apr 15
1/52
Comments: 3 pages, 4 figures
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