West, R., Cassler, B., Snow, J., Dumont, P., Turtle, E., McEwen, A., Mitchell, C., Porco, C. (2006). "Fine-Scale Structure in Titan's High Haze." Eos Trans. AGU 87(52), Fall Meet. Suppl., Abstract P21B-01.


Images of Titan's limb from the Cassini Imaging Science Subsystem reveal layer structures not previously seen. These are most apparent in the north polar hood at latitudes above 60 degrees. Within this region many (~10) layers can be seen between about 300 and 500 km altitude, and structural changes are apparent in a movie of 36 images taken over a 2-hour period. At altitudes less than 60 degrees a `detached' haze is readily seen near the 500 km level (2 micro-bar pressure). The altitude of this layer does not vary with latitude, unlike the detached haze seen in the Voyager images, and it is about 150 km higher than that seen in the Voyager images. Because of rapid sedimentation rates it is difficult to understand how this layer can be maintained over the course of more than two years as observed by Cassini and for even longer periods as indicated by stellar occultations, unless it is produced by a condensate forming at or near a local temperature minimum. At high resolution sub-layers within this layer can be seen. We show the results of retrievals of haze extinction coefficients at a resolution of 5 km.