The detectability of Titan's surface in the near-infrared

Statistics – Computation

Scientific paper

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Atmospheric Composition, Atmospheric Models, Atmospheric Scattering, Near Infrared Radiation, Planetary Surfaces, Radiation Detectors, Satellite Atmospheres, Spectral Reflectance, Surface Properties, Titan, Albedo, Haze, Scattering Functions

Scientific paper

The extent to which the surface of Titan, which is not visible in visual radiation, might be detectable in the near infrared was studied. Multiple scattering computations of the radiation reflected by Titan at 1.58 micrometers (in a methane window), and, as a comparison, at 0.635 micrometers were performed. A three layer optical model of Titan's atmosphere was used: an organic haze layer at the top, next a methane cloud layer, and a nitrogen gas layer at the bottom. Constrained by the geometric albedo and the haze scattering properties at both wavelengths, it was found that the atmosphere must be relatively thin at 1.58 micrometers (optical thickness approximately = 0.5). The presence of a backward peak in the scattering function of the cloud particles influenced the computed geometric albedo strongly. It was found that the surface must be brighter in the near IR than in the visual. Furthermore, it was found that surface features with strong contrast might be rather easily detectable at wavelengths equal to 1.58 micrometers.

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