  To explore the magnetic flux dispersion in the undisturbed solar photosphere,
magnetograms acquired by Helioseismic and Magnetic Imager (HMI) onboard the
Solar Dynamic Observatory (SDO) were utilized. Two areas, a coronal hole area
(CH) and an area of super-granulation pattern, SG, were analyzed. We explored
the displacement and separation spectra and the behavior of the turbulent
diffusion coefficient, $K$. The displacement and separation spectra are very
similar to each other. Small magnetic elements (of size 3-100 squared pixels
and the detection threshold of 20 Mx sm$^{-2}$) in both CH and SG areas
disperse in the same way and they are more mobile than the large elements (of
size 20-400 squared pixels and the detection threshold of 130 Mx sm$^{-2}$).
The regime of super-diffusivity is found for small elements ($\gamma \approx
1.3 $ and $K$ growing from $\sim$100 to $\sim$ 300 km$^2$ s$^{-1}$). Large
elements in the CH area are scanty and show super-diffusion with $\gamma
\approx 1.2$ and $K$ = (62-96) km$^2$ s$^{-1}$ on rather narrow range of
500-2200 km. Large elements in the SG area demonstrate two ranges of linearity
and two diffusivity regimes: sub-diffusivity on scales (900-2500) km with
$\gamma=0.88$ and $K$ decreasing from $\sim$130 to $\sim$100 km$^2$ s$^{-1}$,
and super-diffusivity on scales (2500-4800) km with $\gamma \approx 1.3$ and
$K$ growing from $\sim$140 to $\sim$200 km$^2$ s$^{-1}$. Comparison of our
results with the previously published shows that there is a tendency of
saturation of the diffusion coefficient on large scales, i.e., the turbulent
regime of super-diffusivity is gradually replaced by normal diffusion.
