Surface-atmosphere interactions on Titan compared with those on the pre-biotic Earth.
The surface and atmosphere of Titan constitute a system which is potentially as complex as that of the Earth, with the possibility of precipitation, surface erosion due to liquids, chemistry in large surface or subsurface hydrocarbon reservoirs, surface expressions of internal activity, and occasional major impacts leading to crustal melting.  While none of the above have been observed as yet, the composition, density and thermal properties of Titan's atmosphere make it uniquely suited in the outer solar system as a place where such processes may occur.  The one attribute of the Earth not expected on Titan is biological activity, which has had a profound effect on the evolution of the Earth's surface-atmosphere system.  The earliest environment of Titan could have been warm enough for liquid ammonia-water solutions to exist on or near surface; pre-biotic organic processes may have taken place in such an environment.  After a few hundred million years surface ammonia-water would have disappeared.  Therefore, study of Titan through the Cassini-Huygens mission, planned for launch in 1997, primarily affords the opportunity to understand planet-wide surface-atmosphere interactions in the presence of fluids but in the absence of life.  More speculative is the possibility that endogenic and exogenic heating continue to provide short-lived environments on Titan wherein pre-biotic organic processes in the presence of water happen.
Lunine
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Lunar and Planetary Laboratory, University of Arizona, Tucson 85721, USA.
McKay
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CP
D001272:Atmosphere / Q000032:analysis*; D002980:Climate; D018534:Earth, Planet; D019418:Evolution, Chemical; D019419:Evolution, Planetary; D005118:Extraterrestrial Environment; D006838:Hydrocarbons; D008697:Methane; D008962:Models, Theoretical; D009792:Oceans and Seas; D018539:Saturn; D013696:Temperature
D006838:Hydrocarbons; D008697:Methane