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 .
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 which has been observed in many quiescent prominences .
The kinetic energy power spectral density 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 power spectral density 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 .