Uncertainties in (E)UV model atmosphere fluxes

Details Uncertainties in (E)UV model atmosphere fluxes Uncertainties in (E)UV model atmosphere fluxes

2008-02-13

arxiv.org/abs/0802.1773v1

Astronomy and Astrophysics

Astrophysics

3 pages, 5 figures

Scientific paper

10.1051/0004-6361:200809430

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. Systematic differences may occur due to a code-specific cutoff frequency of the H I 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 A for stars with effective temperatures below about 30000K only, if the same cutoff frequency is chosen. 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. 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.

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