  We studied the solar surface flows (differential rotation and meridional
circulation) using a magnetic element feature tracking technique by which the
surface velocity is obtained using magnetic field data. We used the
line-of-sight magnetograms obtained by the Helioseismic and Magnetic Imager
aboard the Solar Dynamics Observatory from 01 May 2010 to 16 August 2017
(Carrington rotations 2096 to 2193) and tracked the magnetic element features
every hour. Using our method, we estimated the differential rotation velocity
profile. We found rotation velocities of $\sim$ 30 and -170 m s$^{-1}$ at
latitudes of 0$^{\circ}$ and 60$^{\circ}$ in the Carrington rotation frame,
respectively. Our results are consistent with previous results obtained by
other methods, such as direct Doppler, time-distance helioseismology, or cross
correlation analyses. We also estimated the meridional circulation velocity
profile and found that it peaked at $\sim$12 m s$^{-1}$ at a latitude of
45$^{\circ}$, which is also consistent with previous results. The dependence of
the surface flow velocity on the magnetic field strength was also studied. In
our analysis, the magnetic elements having stronger and weaker magnetic fields
largely represent the characteristics of the active region remnants and solar
magnetic networks, respectively. We found that magnetic elements having a
strong (weak) magnetic field show faster (slower) rotation speed. On the other
hand, magnetic elements having a strong (weak) magnetic field show slower
(faster) meridional circulation velocity. These results might be related to the
Sun's internal dynamics.
