  A Circumnuclear Disk (CND) of molecular gas occupies the central few parsecs
of the Galactic Center. It is likely subject to turbulent disruptions from
violent events in its surrounding environment, but the effect of such
perturbations has not yet been investigated in detail. Here we perform 3D,
N-body/smoothed particle hydrodynamic (SPH) simulations with an adapted general
turbulence driving method to investigate the CND's structural evolution, in
particular its reaction to varied scales of injected turbulence. We find that,
because of shear flow in the disk, transient arcs of gas (streams) naturally
arise when turbulence is driven on large scales (up to $\sim4$~pc), as might
occur when a supernova blast wave encounters the CND. Because energetic events
arise naturally and often in the central parsecs of our Galaxy, this result
suggests that the transient structures that characterize the CND do not imply
that the CND itself is a transient structure. We also note that features
similar to the density concentrations, or ``clumps'', detailed in literature
emerge when we account for the observed orientation of the disk and for the
spatial resolution of observations. As such, clumps could be an artifact of
observational limitations.
