The Detached Haze Layer Of Titan Observed By Cassini/iss Images

Details The Detached Haze Layer Of Titan Observed By Cassini/iss Images The Detached Haze Layer Of Titan Observed By Cassini/iss Images

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.5809c&link_type=abstract

American Astronomical Society, DPS meeting #42, #58.09; Bulletin of the American Astronomical Society, Vol. 42, p.1083

Astronomy and Astrophysics

Astronomy

Scientific paper

After ISS on Voyager, in 1980 and 1981, the ISS instrument onboard Cassini observed an optically thin detached haze layer over the main thick haze layer of Titan. About one Titan year after its first detection, it surprisingly culminates 150 km higher than in 1980. It also appears layered in fine structures probably triggered by waves. This layer is though to be produced by the large scale circulation. The size and the composition of the aerosols forming this layer, and the structure of the layer itself are important clues to understand the atmosphere circulation and the formation the aerosols from the complex photochemistry.
To characterize the detached haze layer, we used large phase angle images acquired by Cassini probe with the ISS camera at different dates between 2005 and 2009, at seven different phase angles (from 112° to 161°) and with two different filters. This set of observations reveals a strong forward peak of the aerosol phase function, similar to what was observed by Voyager. Our analysis shows that the signal is consistent with particles in the range 0.2 to 0.3 [[Unsupported Character - Symbol Font μ]]m. Assuming fractal aggregates made of monomers of radius rm = 0.05 [[Unsupported Character - Symbol Font μ]]m, we find that aggregates should be composed of several tens of monomers. In our presentation we will describe in detail our results and the important consequences that can be drawn concerning the circulation, the aerosol size distribution and we will discuss the connection with chemical aspects.

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