A wind origin for Titan's haze structure

P. Rannou (), F. Hourdin and C. P. McKay
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P. Rannou: Université de Paris 6/Université de Versailles-St-Quentin
F. Hourdin: Université de Paris 6
C. P. McKay: NASA-Ames Research Center

Nature, 2002, vol. 418, issue 6900, 853-856

Abstract: Abstract Titan, the largest moon of Saturn, is the only satellite in the Solar System with a dense atmosphere. Titan's atmosphere is mainly nitrogen with a surface pressure of 1.5 atmospheres and a temperature of 95 K (ref. 1). A seasonally varying2 haze, which appears to be the main source of heating and cooling that drives atmospheric circulation3,4, shrouds the moon. The haze has numerous features that have remained unexplained. There are several layers5, including a ‘polar hood’6,7,8, and a pronounced hemispheric asymmetry2. The upper atmosphere rotates much faster than the surface of the moon9,10, and there is a significant latitudinal temperature asymmetry at the equinoxes11,12. Here we describe a numerical simulation of Titan's atmosphere, which appears to explain the observed features of the haze. The critical new factor in our model is the coupling of haze formation with atmospheric dynamics, which includes a component of strong positive feedback between the haze and the winds.

Date: 2002
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DOI: 10.1038/nature00961

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