LABORATORY STUDIES OF ORGANIC-CHEMISTRY IN PLANETARY-ATMOSPHERES - FROM SIMULATION EXPERIMENTS TO SPECTROSCOPIC DETERMINATIONS

Possible approaches to the study of organic chemistry in planetary atm ospheres are threefold: they comprise theoretical modeling, simulation experiments, and observational programs. Because of their respective merits and limitations, these approaches are quite complementary, and their simultaneous improvement is the way to progress further in the f ield. All three ask for laboratory work, and the lack, or limited accu racy, of laboratory data is the main restriction to future improvement . Together with the development of theoretical modeling (based on chem ical kinetics and depending on laboratory studies of reaction pathways and rate constants) laboratory simulation remains a powerful techniqu e. Despite the inaccurate reproduction of all planetary conditions, th is experimental approach yields precious information on the nature of middle and higher order molecular weight organics that can be expected in an atmosphere of a given overall composition; and there is, in gen eral, good agreement between the data obtained from simulations and th ose derived from observations. Indeed, several of the organic species highlighted in such experiments, and their relative abundances, are co mpatible with those detected in related planetary atmospheres. This is shown in the particular case of Titan. Thus experimental results furn ish information on the nature of organics to be searched for in planet ary atmospheres, while, in turn, the detection of such candidates and possible indications of their concentration profiles, or the setting o f upper limits to their abundancies, constrain the kinetic approach. G iven the lists of candidates from simulation experiments, experimental programs for a systematic determination of spectroscopic characterist ics, including frequencies and band or line intensities, of the likely organics in planetary atmospheres, have to be developed. As an exampl e, experimental requirements and current results, both in the IR and t he UV range, are presented concerning Titan's atmosphere in view of th e Cassini-Huygens mission.