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Figure 1: Common geometrical setups of a model PDR. The surface of any plane-parallel or spherical cloud is illuminated either a) uni-directional or b) isotropically. |
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Figure 2:
Comparison of attenuation of the mean intensity for the case of an
uni-directional and isotropically illuminated medium.
The solid line gives the attenuation due to uni-directional illumination, while
the dashed line gives the attenuation for an isotropic FUV radiation where ![]() |
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Figure 3:
H2 photo-dissociation rates resulting from uni-directional FUV illuminated clouds compared to an isotropic illumination. The results from isotropic models are plotted vs. the perpendicular ![]() ![]() |
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Figure 4:
The influence of the cosmic ray ionization rate
on the chemical structure of a model cloud. The left panel shows results for
Model F1 (n=103 cm-3, ![]() ![]() |
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Figure 5:
Comparison between model codes with (dashed line) and without (solid line)
excited molecular hydrogen, H2*. The abundance profile of CH is plotted for both models against
![]() ![]() |
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Figure 6:
The density profile of atomic carbon for the benchmark model F2 (low density, high FUV,
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Figure 7:
Model F1 (n=103 cm-3, ![]() |
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Figure 8:
Model F1 (n=103 cm-3, ![]() |
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Figure 9:
Model F1 (n=103 cm-3, ![]() ![]() |
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Figure 10:
Model F4 (
n=105.5 cm-3, ![]() |
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Figure 11:
Model F4 (
n=105.5 cm-3, ![]() |
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Figure 12:
Model V2 (n=103 cm-3, ![]() |
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Figure 13:
Model V2 (n=103 cm-3, ![]() |
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Figure 14:
Model V2 (n=103 cm-3, ![]() |
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Figure 15:
Model V2 (n=103 cm-3, ![]() ![]() ![]() ![]() |
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Figure 16:
Model V2 (n=103 cm-3, ![]() ![]() ![]() |
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