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Developing an understanding of how magnetic fields can become entangled in aprominence is important for predicting a possible eruption. This workinvestigates the kinetic energy and vorticity associated with plasma motionresiding inside quiescent prominences (QPs). These plasma flow characteristicscan be utilized to improve our understanding of how the prominence maintains astable magnetic field configuration. Three different contrast-enhanced solarprominence observations from Hinode/Solar Optical Telescope were used toconstruct velocity maps -- in the plane of the sky -- via a Fourier localcorrelation tracking program. The resulting velocities were then used toperform the first ever analysis of the two-dimensional kinetic energy andenstrophy spectra of a prominence. Enstrophy is introduced here as a means ofquantifying the vorticity that has been observed in many QPs. The kineticenergy power spectral density (PSD) produced indices ranging from -1.00 to-1.60. There was a consistent anisotropy in the kinetic energy spectrum of allthree prominences examined. Examination of the intensity PSD reveals that adifferent scaling relationship exists between the observed prominence structureand velocity maps. All of the prominences exhibited an inertial range of atleast $0.8 \leq k\leq 2.0\; \textrm{rads} \: \textrm{Mm}^{-1}$. Quasi-periodicoscillations were also detected in the centroid of the velocity distributionsfor one prominence. Additionally, a lower limit was placed on the kineticenergy 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.

Analysis of Flows Inside Quiescent Prominences as Captured by Hinode/Solar Optical Telescope