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The crystallography of Pluto

Christoph G. SalzmannAlexander Rosu-Finsen
[Pluto]

Far beyond the realm of the mighty gas giant Neptune lies the icy world of Pluto. Originally believed to be an inactive and desolate dwarf planet at the outer rim of our Solar system, the New Horizons spacecraft recently revealed Pluto to be a ‘scientific wonderland’ with complex surface geology (Moore et al., 2016; Hall, 2020) and atmospheric chemistry (Wong et al., 2017). Writing in IUCrJ, Maynard-Casely and co-workers have now investigated two of the most abundant Plutonian minerals, solid nitrogen and methane, with powder neutron diffraction (Maynard-Casely et al., 2020). The new results on the thermal-expansion properties, phase-transition behaviours and crystal structures of these materials will be key to understanding the active geology of our distant neighbour. This work also represents an important contribution towards advancing the emerging field of ‘small-molecule geology’ which is concerned with materials that are gases or liquids under Earth conditions but rock-forming minerals at greater distances from the Sun.

The surface of Pluto is a sight to behold. Rugged mountain ranges taller than Mount Everest give way to cracks deeper than the Grand Canyon and flat plains such as Sputnik Planitia which is part of Pluto’s famous ‘heart’ region shown in Fig. 1(a) (Moore et al., 2016). Solid nitrogen has been suggested to be the dominating mineral of this plain and fascinating polygonal surface patterns indicate active convection processes (Grundy et al., 2016). The crystal structure of β-nitrogen displays orientational disorder of the N2 molecules which are arranged in a hexagonal close-packed fashion [see Fig. 1(b)] (Streib et al., 1962; Press et al., 1982). This makes β-nitrogen a so-called ‘plastic’ phase which is a class of mechanically soft materials and therefore consistent with the convection processes of Pluto’s plains. Maynard-Casely and co-workers present accurate density data of β-nitrogen and follow the phase transition to α-nitrogen which is the stable phase below 38 K (Maynard-Casely et al., 2020). In α-nitrogen, the nitrogen molecules display defined orientations and the authors now show that its crystal structure is best described by the Pa3 space group thereby resolving a long-standing debate. The phase transition from β- to α-nitrogen takes place in a temperature range relevant for Pluto, and it can be speculated that the associated density change and most likely hardening of the material are important factors for Pluto’s glaciology.

 
[Fig. 1]Figure 1. Pluto and the crystal structures of two of its most important minerals. (a) Photographic image of Pluto taken by the New Horizons spacecraft (Source: NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute/Alex Parker. Published: July 23, 2018). (b, c) Crystal structures of β-nitrogen (Streib et al., 1962, Press et al., 1982) and methane I (Press, 1972) shown with random orientations of the N2 and CH4 molecules, and using 3×3×2 and 2×2×2 supercells, respectively.

Solid methane is expected to exist as phase I on Pluto which is, just like β-nitrogen, a plastic phase with orientational disorder of the CH4 molecules that are packed in a face-centred cubic structure [see Fig. 1(c)] (Press, 1972). Again, Maynard-Casely and coworkers determined accurate density values for methane I which is, due to its high hydrogen content, a significantly lighter material than solid nitrogen. To their credit, the work was carried out with protiated methane, the form of methane expected to exist on Pluto, and not the deuterated analogue (CD4) which would have offered tremendous advantages from the neutron diffraction point of view. Although not relevant for Pluto, they also followed the phase transition to methane II at low temperatures and observed hints of the intriguing phenomenon of negative thermal expansion. Above 65 K, they found that methane I transforms from a fine powder to large crystalline grains. Skyscraper-sized shards on Pluto are thought to consist of solid methane (Hall, 2020) and the observed changes in crystal size upon heating may provide an explanation for their formation.

Water ice is another important mineral on Pluto. Unlike solid nitrogen and methane, its density changes very little in the temperature range relevant for Pluto (Fortes, 2018) and it is a much harder material due to hydrogen bonding between the H2O molecules (Salzmann, 2019). Hence, water ice is Pluto’s ‘bedrock’ material and the major constituent of its tall mountain ranges (Grundy et al., 2016). The likely form of water ice to exist on Pluto is the familiar hexagonal ice Ih. However, it has also been speculated that the ferroelectric low-temperature phase ice XI may exist (Fukazawa et al., 2006).

Future work will focus on accurately measuring the mechanical properties of Pluto’s minerals. Moving beyond the traditional fitting of Bragg diffraction data, total scattering studies and the analysis of pair-distribution functions can be expected to provide detailed insights into the local structures of the orientationally disordered nitrogen and methane phases. The interplay and mixing of the various minerals will need to be investigated in more detail as well. This will include the formation of solid solutions and the formation of clathrate hydrates in which cages of water molecules trap guest species such as nitrogen or methane molecules. Most recently, it has been suggested that a layer of clathrate hydrates may provide the thermal insulation required to stabilize a subsurface ocean on Pluto (Kamata et al., 2019). Pluto clearly still harbours many secrets and following the work of Maynard-Casely and co-workers, crystallography will certainly continue to be a major tool for understanding its geology. But also, considering how long it takes to reach Pluto, we should really send another spacecraft very soon to further explore this fascinating world.

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This article was originally published in IUCrJ (2020). 7, 782783

29 September 2020

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