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The Sun features on its surface typical flow patterns called the granulation,mesogranulation, and supergranulation. These patterns arise due to convectiveflows transporting energy from the interior of the Sun to its surface. In thispaper we will shed light on the interaction between the convective flows inlarge-scale cells as well as the large-scale magnetic fields in active regions,and investigate in detail the statistical distribution of flow velocitiesduring the evolution and formation of National Oceanic and AtmosphericAdministration (NOAA) active region 11190. To do so, we employed localcorrelation tracking methods on data obtained by the Solar Dynamics Observatory(SDO) spacecraft in the continuum as well as on processed line-of-sight (LOS)magnetograms. We find that the flow fields in an active region can be modelledby a two-component distribution. One component is very stable, follows aRayleigh distribution, and can be assigned to the background flows, whilst theother component is variable in strength and velocity range and can beattributed to the flux emergence visible both in the continuum maps as well asmagnetograms. Generally, the plasma flows, as seen by the distribution of themagnitude of the velocity, follow a Rayleigh distribution even through the timeof formation of active regions. However, at certain moments of large-scale fastflux emergence, a second component featuring higher velocities is formed in thevelocity magnitudes distribution. The plasma flows are generally highlycorrelated to the motion of magnetic elements and vice versa except during thetimes of fast magnetic flux emergence as observed by rising magnetic elements.At these times, the magnetic fields are found to move faster than thecorresponding plasma.

Photospheric plasma and magnetic field dynamics during the formation of solar AR 11190