  Developing an understanding of how magnetic fields can become entangled in a
prominence is important for predicting a possible eruption. This work
investigates the kinetic energy and vorticity associated with plasma motion
residing inside quiescent prominences (QPs). These plasma flow characteristics
can be utilized to improve our understanding of how the prominence maintains a
stable magnetic field configuration. Three different contrast-enhanced solar
prominence observations from Hinode/Solar Optical Telescope were used to
construct velocity maps -- in the plane of the sky -- via a Fourier local
correlation tracking program. The resulting velocities were then used to
perform the first ever analysis of the two-dimensional kinetic energy and
enstrophy spectra of a prominence. Enstrophy is introduced here as a means of
quantifying the vorticity that has been observed in many QPs. The kinetic
energy power spectral density (PSD) produced indices ranging from -1.00 to
-1.60. There was a consistent anisotropy in the kinetic energy spectrum of all
three prominences examined. Examination of the intensity PSD reveals that a
different scaling relationship exists between the observed prominence structure
and velocity maps. All of the prominences exhibited an inertial range of at
least $0.8 \leq k\leq 2.0\; \textrm{rads} \: \textrm{Mm}^{-1}$. Quasi-periodic
oscillations were also detected in the centroid of the velocity distributions
for one prominence. Additionally, a lower limit was placed on the kinetic
energy density ($\epsilon \, \sim 0.22-7.04\: \mathrm{km}^{2}\textrm{s}^{-2}$)
and enstrophy density ($\omega \, \sim 1.43-13.69\: \times 10^{-16} \,
\textrm{s}^{-2}$) associated with each prominence.
