Led by Professor Stephen Moggach, the Space Crystallography Node aims to determine the crystal structures of molecular co-crystals that are likely to form on the surface of Titan – Saturn’s largest moon.
Titan has geological features that are somewhat similar to those found on Earth, with seas, lakes and sweeping dunes. Unlike the Earth, however, the temperature hardly varies, sitting at a constant value of around 92K. In addition, the surface composition is quite different to the Earth, and dominated by molecular materials, much of which are photochemically produced in the moon’s atmosphere. These range from simple compounds such as ethane and acetylene, to more complex molecules (e.g. methylcyanoacetylene). These more complex molecular compounds first form as a haze layer in Titan’s atmosphere, before being deposited onto the surface.
Interestingly, because of the active weather system on Titan, these deposited ‘pure’ compounds can mix by being buried in subsequent layers of organic material, or by dissolution in the liquid hydrocarbon seas, and could lead to the formation of molecular co-crystals.
Professor Moggach’s team has recently been awarded a LIEF grant to enable the purchase of a Differential Scanning Calorimetry (DSC), which will will allow them to look at materials between -170 to 600 degrees. This is a key piece of equipment allowing them to look at planetary science co-crystals on this Titan project.
