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We focus on Hinode Solar Optical Telescope (SOT) calcium II H-lineobservations of a solar quiescent prominence (QP) that exhibits highly variabledynamics suggestive of turbulence. These images capture a sufficient range ofscales spatially ($\sim$0.1-100 arc seconds) and temporally ($\sim$16.8 s - 4.5hrs) to allow the application of statistical methods used to quantify finiterange fluid turbulence. We present the first such application of thesetechniques to the spatial intensity field of a long lived solar prominence.Fully evolved inertial range turbulence in an infinite medium exhibitsmultifractal \emph{scale invariance} in the statistics of its fluctuations,seen as power law power spectra and as scaling of the higher order moments(structure functions) of fluctuations which have non-Gaussian statistics;fluctuations $\delta I(r,L)=I(r+L)-I(r)$ on length scale $L$ along a givendirection in observed spatial field $I$ have moments that scale as $<\deltaI(r,L)^p>\sim L^{\zeta(p)}$. For turbulence in a system that is of finite size,or that is not fully developed, one anticipates a generalized scale invarianceor extended self-similarity (ESS) $<\delta I(r,L)^p>\sim G(L)^{\zeta(p)}$. Forthese QP intensity measurements we find scaling in the power spectra and ESS.We find that the fluctuation statistics are non-Gaussian and we use ESS toobtain ratios of the scaling exponents $\zeta(p)$: these are consistent with amultifractal field and show distinct values for directions longitudinal andtransverse to the bulk (driving) flow. Thus, the intensity fluctuations of theQP exhibit statistical properties consistent with an underling turbulent flow.

Turbulent characteristics in the intensity fluctuations of a solar quiescent prominence observed by the \textit{Hinode} Solar Optical Telescope