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Figure 1:
Test models A and B (
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Figure 2:
"Hot'' test models C and D (
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Figure 3: Test calculations: ground-state populations of the included iron-group ions vs. atomic density as depth index for models A, B, and C. Top panel: the "cool'' models A (black) and B (grey) show ionization stages up to Fe XIV. The model atom for Model A which only includes ions up to Fe X is clearly insufficient. For both models, the M-shell ions (Fe IX-Fe XVII) are strongly concentrated towards the inner boundary. Bottom panel: the "hot'' Model C shows M-shell ions already at lower densities. Ionization stages up to Fe XVI are excited. |
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Figure 4: Model spectra around O VI 3811/34 for different clumping structures. For Model D our standard approach is used (see text). For Model D2 clumping is initiated farther out in the wind whereas for Model D1 a constant clumping factor is assumed. The O VI emission reacts strongly to the clumping structure. The farther out clumping is initiated the stronger O VI becomes. For Model D2 the continuum level is also affected. |
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Figure 5:
Hydrodynamic model: comparison of the synthetic spectrum (thick line, grey)
with the observed spectrum of WR 111 (thin line). Prominent spectral lines
are identified. After correction for interstellar extinction, the observed
flux and the model flux are both divided by the model continuum.
Additionally, a correction for interstellar Ly ![]() |
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Figure 6:
Hydrodynamic model: Emergent flux distribution (grey) compared with the
observed flux of WR 111 (dashed black line) including optical and infrared
photometry (labeled blocks). A distance modulus of 11.0 mag
(
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Figure 7:
Wind acceleration as in Fig. 1, but for the self-consistent
hydrodynamic model. The grey line indicates the acceleration
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Figure 8:
Velocity structure of the hydrodynamic model (black) compared to
different ![]() ![]() |
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Figure 9:
The effective force multiplier parameter ![]() ![]() ![]() |
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