  Massive, evolved stars play a crucial role in the metal-enrichment, dust
budget, and energetics of the interstellar medium, however, the details of
their evolution are uncertain because of their rarity and short lifetimes
before exploding as supernovae. Discrepancies between theoretical predictions
from single-star evolutionary models and observations of massive stars have
evoked a shifting paradigm that implicates the importance of binary
interaction. We present mid- to far-infrared observations from the
Stratospheric Observatory for Infrared Astronomy (SOFIA) of a conical "helix"
of warm dust ($\sim180$ K) that appears to extend from the Wolf-Rayet star
WR102c. Our interpretation of the helix is a precessing, collimated outflow
that emerged from WR102c during a previous evolutionary phase as a rapidly
rotating luminous blue variable. We attribute the precession of WR102c to
gravitational interactions with an unseen compact binary companion whose
orbital period can be constrained to $800\,\mathrm{d}<P<1400$ d from the
inferred precession period, $\tau_p\sim1.4\times10^4$ yr, and limits imposed on
the stellar and orbital parameters of the system. Our results concur with the
range of orbital periods ($P\lesssim1500$ d) where spin-up via mass exchange is
expected to occur for massive binary systems.
