Volume 481, Number 3, April III 2008
|Page(s)||807 - 809|
|Published online||18 February 2008|
Uncertainties in (E)UV model atmosphere fluxes
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany e-mail: firstname.lastname@example.org
Accepted: 4 February 2008
Context. During the comparison of synthetic spectra calculated with two NLTE model atmosphere codes, namely TMAP and TLUSTY, we encounter systematic differences in the EUV fluxes due to the treatment of level dissolution by pressure ionization.
Aims. In the case of Sirius B, we demonstrate an uncertainty in modeling the EUV flux reliably in order to challenge theoreticians to improve the theory of level dissolution.
Methods. We calculated synthetic spectra for hot, compact stars using state-of-the-art NLTE model-atmosphere techniques.
Results. Systematic differences may occur due to a code-specific cutoff frequency of the Lyman bound-free opacity. This is the case for TMAP and TLUSTY. Both codes predict the same flux level at wavelengths lower than about 1500 Å for stars with effective temperatures (Teff) below about 30 000 K only, if the same cutoff frequency is chosen.
Conclusions. The theory of level dissolution in high-density plasmas, which is available for hydrogen only should be generalized to all species. Especially, the cutoff frequencies for the bound-free opacities should be defined in order to make predictions of UV fluxes more reliable.
Key words: atomic data / stars: atmospheres / stars: individual: HZ 43 / stars: individual: Sirius B / stars: white dwarfs / ultraviolet: stars / X-rays: stars
© ESO, 2008
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