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The influence of non isotropic scattering of thermal radiation on spectra of brown dwarfs and hot exoplanets

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Figure

Fig. 1. Mean particle sizes, number densities and temperature profiles(aries of the four particle types that we define for our radiative transfercalculations (see text and Fig.(2for our two model atmospheres
Table 1. Assumed particle sizes (μm) for the four different particle typesin the two model atmospheres.
Fig. 4. As Fig. 3, except for the 2000 K model atmosphere.
Fig. 5. Brightness temperature spectra for the 1500 K case. The solidcluded. The dashed line shows the spectrum for purely absorbing par-ticle, but same optical thickness (single-scattering albedo, or ssa in thelegend, of zero)
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