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Fig. 12


Pressure temperature profiles at the substellar point of the four planets studied here. The short dash portion of the profiles are the 1.4 μm photospheric pressures. The long-dash portions represent what the photospheric pressures would be if water dissociation were not taken into account. The background and the black contour lines show the water abundance for a solar composition gas as a function of pressure and temperature. The dashed-dot brown contour lines are the contour lines of the ratio between the opacities of molecules (mainly H2 O and TiO) and the bound-free opacity of H calculated at1.25 μm. At higher temperatures and lower pressures than the line labeled “1”, H is an important opacity source in the atmosphere.

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