Numerical calculations of the longevity of impact oases on Titan

A promising setting for the formation of interesting prebiotic molecules on Titan is the transient liquid water environment formed by a comet impact, as originally suggested by Thompson and Sagan (1992, in: Symposium on Titan, ESA SP, vol. 338, p. 167). The impact melt (water or a water-ammonia mixture) generated in such an event can react with the abundant photochemical hydrocarbons and nitriles deposited on the surface of Titan to form more complex molecules such as purines and amino acids. We use a finite- difference thermal conduction code to calculate how long it takes for realistic liquid deposits in crater floors to freeze in the Titan environment. Our results suggest that 15 km diameter craters can sustain liquid water or water-ammonia environments for ~[10.sup.2] - [10.sup.3] yr and 150 km craters can sustain them for ~[10.sup.3] - [10.sup.4] yr. We discuss the implications of these timescales for organic chemistry on Titan. Keywords: Titan; Cratering; Impact processes; Prebiotic environments; Prebiotic chemistry