Astron. Astrophys. 363, 1051-1054 (2000)

3. Physical quantities of models and temperature structure

The physical quantities of models from Tlusty are given in the form of temperature, electron number density and particle number density vs. depth-mass variable or Rosseland optical depth.

Converting the electron and particle densities to pressure, it is easy to construct the T-p diagram to compare the models of different helium abundances (Fig. 1). The line-blanketing is very critical for cool models and Fig. 1 and Fig. 2 allow one to evaluate the line blanketing effect in our coolest model. While there are some differences in the temperature vs. mass depth variable scale (Fig. 2), probably due to backwarming in the fully line-blanketed LTE model, the overal differences in NLTE and the blanketed LTE model quantities in the visual continuum forming regions (Fig. 1) are very small and the line blanketing in our model is in practice appropriate.

Fig. 1. The temperature-pressure diagram in logarithmic scale for =15000K and log g=4.0. Solid line- LTE model with n(He)=0.1 and dotted line- NLTE model, dashed line-NLTE model and n(He)=1, dash dot dot dot line-Kurucz model and n(He)=0.1. The asterisk stands for depth point with T=Teff.

Fig. 2. The temperature-mass depth variable in logarithmic scale for model =15000K and log g=4.0. Solid line- LTE model with n(He)=0.1 and dotted line- NLTE model, dashed line-NLTE model and n(He)=1., dash dot dot dot line-Kurucz LTE model model and n(He)=0.1. The asterisk stands for depth point with T=Teff.

© European Southern Observatory (ESO) 2000

Online publication: December 5, 2000
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