  gamma Draconis, a K5III star, showed radial velocity (RV) variations
consistent with a 10.7 Jupiter mass planet from 2003-2011. After 2011, the
periodic signal decayed, then reappeared with a phase shift. Hatzes et al.
(2018) suggested that gamma Dra's RV variations could come from oscillatory
convective modes, but did not fit a mathematical model. Here we assess whether
a quasi-periodic Gaussian process (GP)---appropriate when spots with finite
lifetimes trace underlying periodicity---can explain the RVs. We find that a
model with only one quasiperiodic signal is not adequate: we require a second
component to fit the data. The best-fit model has quasi-periodic oscillations
with P1 = 705 days and P2 = 15 days. The 705-day signal may be caused by
magnetic activity. The 15-day period requires further investigation.
