  Using detrended fluctuation analysis (DFA) and rescaled range (R/S) analysis,
we investigate the scaling properties of EUV intensity fluctuations of
low-latitude coronal holes (CHs) and neighboring quiet-Sun (QS) regions in
signals obtained with the Solar Dynamics Observatory/Atmospheric Imaging
Assembly (SDO/AIA) instrument. Contemporaneous line-of-sight SDO/Helioseismic
and Magnetic Imager (HMI) magnetic fields provide a context for the physical
environment. We find that the intensity fluctuations in the time series of EUV
images present at each spatial point a scaling symmetry over the range $\sim
20$ min to $\sim$ 1 hour. Thus we are able to calculate a generalized Hurst
exponent and produce image maps, not of physical quantities like intensity or
temperature, but of a single dynamical parameter that sums up the statistical
nature of the intensity fluctuations at each pixel. In quiet-Sun (QS) regions
and in coronal holes (CHs) with magnetic bipoles, the scaling exponent ($1.0 <
\alpha \leq 1.5$) corresponds to anti-correlated turbulent-like processes. In
coronal holes, and in quiet-Sun regions primarily associated with (open)
magnetic field of dominant polarity, the generalized exponent (0.5 $< \alpha <$
1) corresponds to positively-correlated (persistent) processes. We identify a
tendency for $\alpha$ $\sim$ $1$ near coronal hole boundaries and in other
regions in which open and closed magnetic fields are in proximity. This is a
signature of an underlying $1/f$ type process that is characteristic for
self-organized criticality and shot-noise models.
