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Title:
The mesosphere and lower thermosphere of Titan revealed by Cassini/UVIS stellar occultations
Authors:
Koskinen, T. T.; Yelle, R. V.; Snowden, D. S.; Lavvas, P.; Sandel, B. R.; Capalbo, F. J.; Benilan, Y.; West, R. A.
Affiliation:
AA(Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA), AB(Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA), AC(Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA), AD(Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA), AE(Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA), AF(Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), Universités Paris, Est Creteil et Paris Diderot, 61 Avenue du Général de Gaulle, 94010 Créteil Cedex, France), AG(Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), Universités Paris, Est Creteil et Paris Diderot, 61 Avenue du Général de Gaulle, 94010 Créteil Cedex, France), AH(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA)
Publication:
Icarus, Volume 216, Issue 2, p. 507-534. (Icarus Homepage)
Publication Date:
12/2011
Origin:
ELSEVIER
Abstract Copyright:
Elsevier Inc.
DOI:
10.1016/j.icarus.2011.09.022
Bibliographic Code:
2011Icar..216..507K

Abstract

Stellar occultations observed by the Cassini/UVIS instrument provide unique data that probe the mesosphere and lower thermosphere of Titan at altitudes between 400 and 1400 km. This region is a site of complex photochemistry that forms hydrocarbon and nitrile species, and plays a crucial role in the formation of the organic hazes observed in the stratosphere, but has yet to be adequately characterized. We analyzed publicly available data obtained between flybys Tb in December 2004 and T58 in July 2009, with an emphasis on two stable occultations obtained during flybys T41 and T53. We derived detailed density profiles for CH4, C2H2, C2H4, C4H2, HCN, HC3N and C6H6 between ˜400 and 1200 km and extinction coefficients for aerosols between 400 and 900 km. Our analysis reveals the presence of extinction layers in the occultation data that are associated with large perturbations in the density profiles of the gaseous species and extinction profiles of the aerosols. These relatively stable features vary in appearance with location and change slowly over time. In particular, we identify a sharp extinction layer between 450 and 550 km that coincides with the detached haze layer. In line with recent images obtained by Cassini/ISS, the altitude of this layer changes rapidly around the equinox in 2009. Our results point to unexpected complexity that may have significant consequences for the dynamics and physical processes taking place in the upper atmosphere of Titan.
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