Line blanketing by iron group elements in Non-LTE model atmospheres for hot stars

Details Line blanketing by iron group elements in Non-LTE model atmospheres for hot stars Line blanketing by iron group elements in Non-LTE model atmospheres for hot stars

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...278..199d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 278, no. 1, p. 199-208

Astronomy and Astrophysics

Astrophysics

94

Atmospheric Models, Ferrous Metals, Line Spectra, O Stars, Radiative Transfer, Stellar Atmospheres, Local Thermodynamic Equilibrium, Stellar Models

Scientific paper

We present the first metal line blanketed non-Local Thermodynamic Equilibrium (LTE) model atmospheres for O stars which include 130,000 lines of the iron group elements scandium through nickel, a subset from Kurucz' (1991) line list, fully self-consistently. It is shown that even the treatment of the complete line list (greater than 106 lines) in NLTE models poses no longer any fundamental problem. The numerical solution of the metal line blanketing problem consists of an opacity sampling technique within the framework of the Accelerated Lambda Iteration method. Exploratory models with different parameters were successfully constructed, e.g. for hot subdwarfs and central stars of planetary nebulae as well as for white dwarfs. We discuss the blanketing effects of metal lines (1) onto the atmospheric stratification, (2) onto UV and EUV fluxes, (3) onto the emergent H and He line profiles, and (4) the potential of iron lines as sensitive temperature indicators. The models are used to interprete EUV observations of the white dwarf G191-B2B and UV spectra of the hot sdO star BD+28 deg 4211.

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