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Aerosols in Titan's atmosphere play an important role in determining its thermal structure. They also serve as sinks for organic vapours and can act as condensation nuclei for the formation of clouds, where the condensation efficiency will depend on the chemical composition of the aerosols. So far, however, no direct information has been available on the chemical composition of these particles. Here we report an in situ chemical analysis of Titan's aerosols by pyrolysis at 600 °C. Ammonia (NH3) and hydrogen cyanide (HCN) have been identified as the main pyrolysis products. This clearly shows that the aerosol particles include a solid organic refractory core. NH3 and HCN are gaseous chemical fingerprints of the complex organics that constitute this core, and their presence demonstrates that carbon and nitrogen are in the aerosols. [ABSTRACT FROM AUTHOR]

In the framework of the cometary sampling and composition (COSAC) experiment of the European Space Agency (ESA) Rosetta space mission to a comet, a new generation of porous polymer porous-layer open tubular (PLOT) columns has been investigated with the aim of separating the light organic compounds targeted by the experiment within the constraints of the operating conditions used in space. Both styrene-divinylbenzene and ethylene glycol-dimethyl acrylate-divinylbenzene porous polymers can be used to separate most of the target compounds, but the latter was selected because of its better separating properties. The most appropriate column characteristics were found to be 10 m length, 0.18 mm internal diameter, and 1–2 μm layer thickness, despite the low sample-loading capacity of such a column, which impairs its chromatographic performance. The influence of column overloading on retention properties and efficiency was, therefore, studied. To achieve the separation with optimum sensitivity, and within the in-situ time allowed for the analysis, it was also demonstrated that the maximum allowed temperature and reduced outlet pressure are required. Finally, it was shown that in the presence of water, the most abundant volatile compound in comets the separating properties of the studied columns are conserved. This paper thus demonstrates the suitability of the porous polymer PLOT column selected for the COSAC experiment and requirements for use in space; it is the first porous polymer PLOT column to be used in space exploration. [ABSTRACT FROM AUTHOR]

Due to its abundance and unique properties, water is a major actor in the formation and evolution of many planetary surfaces as well as a sensitive and reliable tracer of past geologic and climatic processes. Water ice is found in variable abundance at the surfaces of many Solar System objects, from the floor of permanently shadowed craters at the poles of Mercury to large fractions of the surfaces of several trans-Neptunian objects. With few exceptions, water is not found in pure form but associated to contaminants of various nature and concentration. These associations and the nature of the mixing and segregation processes that affect and control them are key for our understanding of some of the most important aspects of planetary evolution processes. The observation and characterization of water ice at the surface of Solar System objects is therefore among the primary scientific objectives of many space missions. The quantitative interpretation of remote sensing data in terms of surface composition and physical properties requires the use of complex physical models that rely on experimental data in two different ways. First, the models require as inputs the fundamental properties of the pure materials, such as the optical or dielectric constant. Second, the models can only be fully tested if their results are confronted to actual measurements performed on samples whose complexity comes close to the one encountered on natural planetary surfaces but which are nevertheless well-enough characterized to serve as reference. Such measurements are challenging as macroscopic ice-rich samples prepared as analogues of icy planetary surfaces tend to be unstable, the ice component being prone to metamorphism and phase change. The questions of the reproducibility of the samples and the relevance of the measurements are therefore critical. The Ice Laboratory at the University of Bern has been set up in 2010 to overcome some of these difficulties. We have developed protocols to prepare, store, handle and characterize various associations of ice with mineral and organics contaminants as analogues of different types of icy Solar System surfaces. The aims of this article are to present the context and background for our investigations, describe these protocols and associated hardware in a comprehensive way, provide quantitative characterization of the samples obtained using these protocols and summarize the main results obtained so far by experimenting with these samples. The current state and possible future evolutions of this project are then discussed in the context of the next generation of space missions to visit icy objects in the Solar System and longer term perspectives on future observations of protoplanetary discs and exoplanetary systems. [ABSTRACT FROM AUTHOR]

Biemann et al. calls into question our preliminary interpretations of our experimental results. A comparison of laboratory and flight measurements should settle the uncertainties he raises. In addition to evaluating instrumental characteristics such as the 'piston effect', a technique we used for injecting oven-gas content for gas chromatography–mass spectrometry (GC–MS), such studies should enable a wide range of possible compositions for Titan's aerosols to be investigated. Our aerosol collection and pyrolysis (ACP) measurements in Titan's atmosphere can then be revisited. [ABSTRACT FROM AUTHOR]