Convective flows are known as the prime means of transporting magnetic fields on the solar surface .
Thus , small magnetic structures are good tracers of the turbulent flows .
We study the migration and dispersal of magnetic bright features ( MBFs ) in intergranular areas observed at high spatial resolution with Sunrise /IMaX .
We describe the flux dispersal of individual MBFs as a diffusion process whose parameters are computed for various areas in the quiet Sun and the vicinity of active regions from seeing-free data .
We find that magnetic concentrations are best described as random walkers close to network areas ( diffusion index , \gamma = 1.0 ) , travelers with constant speeds over a supergranule ( \gamma = 1.9 - 2.0 ) , and decelerating movers in the vicinity of flux emergence and/or within active regions ( \gamma = 1.4 - 1.5 ) .
The three types of regions host MBFs with mean diffusion coefficients of 130 km ^ { 2 } s ^ { -1 } , 80 - 90 km ^ { 2 } s ^ { -1 } , and 25 - 70 km ^ { 2 } s ^ { -1 } , respectively .
The MBFs in these three types of regions are found to display a distinct kinematic behavior at a confidence level in excess of 95 % .