The timescale for HCN remaining unreacted following its established formation in the atmosphere is unknown. However, low temperature 85 conditions coupled with relatively low intensity solar flux at the surface (0.1% of Earth ( )) make partial deposition of unreacted HCN plausible. Below 170 K, HCN crystallizes in the orthorhombic space group Imm2 (Fig. ) . This highly non-isotropic 90 structure is composed of strongly hydrogen bonded chains, which, in turn, are relatively weakly interacting amongst each other and stacked in a close-packed fashion (Fig. ). Here we share evidence, experimental and computational, in favor of molecular intermixing between solid HCN and small hydrocarbons, the latter normally liquid at Titan's surface. Based on this evidence we posit that hydrocarbons can intercalate and actively diffuse through an HCN lattice (Fig. ). Because it is challenging to ascertain the degree of order in the systems we study, both cocrystals and solid solutions may be suitable descriptions of these rare examples of attracting opposites.