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The Nitrogen Spectra of WN Stars: The WN6 “Standard” Star HD 192163 (WR136)

Published online by Cambridge University Press:  03 August 2017

U. Wessolowski ,
W.-R. Hamann  and
W. Schmutz
U. Wessolowski
Affiliation:
1 Institut für Theoretische Physik und Sternwarte der Universität Olshausenstraße 40, D-2300 Kiel 1, FRG
W.-R. Hamann
Affiliation:
1 Institut für Theoretische Physik und Sternwarte der Universität Olshausenstraße 40, D-2300 Kiel 1, FRG
W. Schmutz
Affiliation:
2 Joint Institute for Laboratory Astrophysics University of Colorado, Boulder, CO 80309-0440, USA

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Hitherto our quantitative analyses of WR spectra [2][5] have been based on pure-helium models [1][6]. Now we further improved our non-LTE calculations by including a complex model atom of nitrogen (90 energy levels, 351 line transitions; with low-temperature dielectronic recombination) into our model atmospheres in order to synthesize adequately the spectra of WN subtypes (Wessolowski et al., in preparation). Together with the nitrogen (the most important “metal” in WN atmospheres), we introduced an improved temperature structure into our model calculations [3], now accounting for non-grey radiative equilibrium instead of the grey approximation applied so far. Moreover we took into account the line overlap of the considered elements (here: helium, nitrogen) and also their blanketing effects on the continuous radiation field.

References

References:

[1] Hamann, W.-R., Schmutz, W.: 1987, Astron. Astrophys. 174, 173 Google Scholar
[2] Hamann, W.-R., Schmutz, W., Wessolowski, U.: 1988, Astron. Astrophys. 194, 190 Google Scholar
[3] Hamann, W.-R., Wessolowski, U.: 1990, Astron. Astrophys. 227, 171 Google Scholar
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[6] Wessolowski, U., Schmutz, W., Hamann, W.-R.: 1988, Astron. Astrophys. 194, 160 Google Scholar