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Titan’s atmospheric methane most likely originates from lakes at the surface and subsurface reservoirs. Accordingly, it has been commonly assumed that Titan’s tropopause region, where the vertical temperature profile is a minimum, acts as a cold trap for convecting methane, leading to the expectation that the formation of methane clouds in Titan’s stratosphere would be rare. The additional assumption...
Up to now, there has been no corroboration from Cassini CIRS of the Voyager IRIS-discovery of cyanoacetylene (HC 3 N) ice in Titan’s thermal infrared spectrum. We report the first compelling spectral evidence from CIRS for the ν 6 HC 3 N ice feature at 506cm −1 at latitudes 62°N and 70°N, from which we derive particle sizes and column abundances in Titan’s lower stratosphere...
Titan's haze is optically thick in the visible, with an optical depth at 0.5μm of about three. The haze varies with latitude in a seasonal cycle and has a detached upper layer. Microphysical models, photochemical models, and laboratory simulations all imply that the production rate of the haze is in the range of 0.5-2x10 -14 gcm -2 s -1 . Given the rate...
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