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We studied the solar surface flows (differential rotation and meridionalcirculation) using a magnetic element feature tracking technique by which thesurface velocity is obtained using magnetic field data. We used theline-of-sight magnetograms obtained by the Helioseismic and Magnetic Imageraboard the Solar Dynamics Observatory from 01 May 2010 to 16 August 2017(Carrington rotations 2096 to 2193) and tracked the magnetic element featuresevery hour. Using our method, we estimated the differential rotation velocityprofile. We found rotation velocities of $\sim$ 30 and -170 m s$^{-1}$ atlatitudes of 0$^{\circ}$ and 60$^{\circ}$ in the Carrington rotation frame,respectively. Our results are consistent with previous results obtained byother methods, such as direct Doppler, time-distance helioseismology, or crosscorrelation analyses. We also estimated the meridional circulation velocityprofile and found that it peaked at $\sim$12 m s$^{-1}$ at a latitude of45$^{\circ}$, which is also consistent with previous results. The dependence ofthe surface flow velocity on the magnetic field strength was also studied. Inour analysis, the magnetic elements having stronger and weaker magnetic fieldslargely represent the characteristics of the active region remnants and solarmagnetic networks, respectively. We found that magnetic elements having astrong (weak) magnetic field show faster (slower) rotation speed. On the otherhand, magnetic elements having a strong (weak) magnetic field show slower(faster) meridional circulation velocity. These results might be related to theSun's internal dynamics.

Effect of Magnetic Field Strength on Solar Differential Rotation and Meridional Circulation