Isabelle Couturier-Tamburelli

Photochemical activity of Titan's low-altitude condensed haze

Titan, the largest moon of Saturn and similar to Earth in many aspects, has unique orange-yellow colour that comes from its atmospheric haze, whose formation and dynamics are far from well understood. Present models assume that Titans tholin-like haze formation occurs high in atmosphere through gas-phase chemical reactions initiated by high-energy solar radiation. Here we address an important question: Is the lower atmosphere of Titan photochemically active or inert? We demonstrate that indeed tholin-like haze formation could occur on condensed aerosols throughout the atmospheric column of Titan. Detected in Titans atmosphere, dicyanoacetylene (C₄N₂) is used in our laboratory simulations as a model system for other larger unsaturated condensing compounds. We show that C4N2 ices undergo condensed-phase photopolymerization (tholin formation) at wavelengths as long as 355 nm pertinent to solar radiation reaching a large portion of Titans atmosphere, almost close to the surface.

Simulation of Titan’s atmospheric photochemistry - Formation of non-volatile residue from polar nitrile ices

We studied the photochemistry of frozen ice of a polar Titan’s atmospheric molecule cyanodiacetylene (HC5N) to determine the possible contribution of this compound to the lower altitude photochemistry of haze layers found on Titan. We used infrared analysis to examine the residue produced by irradiation of solid HC5N at > 300 nm. The resulting polymer is orange-brown in color. Based on theoretical analysis and the general tendency of HC5N and C4N2 to undergo similar ice photochemistry at longer wavelengths accessible in Titan’s lower atmosphere, we conclude that Titan’s lower atmosphere is photochemically active in the regions of cloud, ice, and aerosol formation. C4N2 is a symmetric molecule with no net dipole moment whereas, HC5N has a large dipole moment of 4 D. Consequently, though both these molecules have very similar molecular weight and size, their sublimation temperatures are di erent, HC5N subliming around 170 K compared to 160 K for C4N2. Based on our studies we conclude that in Titan’s atmosphere the cyanoacetylene class of molecules (HCN, HC3N, HC5N, etc.) would condense first followed by the dicyanoacetylenes (C2N2, C4N2, C6N2, etc.), leading to fractionation of di erent class of molecules. From the fluxes used in the laboratory and depletion of the original HC5N signals, we estimate Titan’s haze ice photochemistry involving polar nitriles to be significant and very similar to their non-polar counterparts.