The Saturnian moon Titan has a thick, organic-rich atmosphere,
and condensed phases of small organic molecules are anticipated to
be stable on its surface. Of particular importance are crystalline
phases of organics, known as cryominerals, which can play important
roles in surface chemistry and geological processes on Titan. Many
of these cryominerals could exhibit rich phase behavior, especially
multicomponent cryominerals whose component molecules have multiple
solid phases. One such cryomineral is the acetylene:ammonia (1:1)
co-crystal, and here we use density functional theory-based ab initio
molecular dynamics simulations to quantify its structure and dynamics
at Titan conditions. We show that the acetylene:ammonia (1:1) co-crystal
is a plastic co-crystal (or rotator phase) at Titan conditions because
the ammonia molecules are orientationally disordered. Moreover, the
ammonia molecules within this co-crystal rotate on picosecond time
scales, and this rotation is accompanied by the breakage and reformation
of hydrogen bonds between the ammonia hydrogens and the π-system
of acetylene. The robustness of our predictions is supported by comparing
the predictions of two density functional approximations at different
levels of theory, as well as through the prediction of infrared and
Raman spectra that agree well with experimental measurements. We anticipate
that these results will aid in understanding geochemistry on the surface
of Titan.