  Context. It is possible to detect and track coronal bright points (CBPs) in
SDO/AIA images. Combination of high resolution and high cadence provides a
wealth of data that can be used to determine velocity flows on the solar
surface with very high accuracy. Aims. We derived a very accurate solar
rotation profile and investigated meridional flows, torsional oscillations and
horizontal Reynolds stress based on $\approx$6 months of SDO/AIA data. Methods.
We used a segmentation algorithm to detect CBPs in SDO/AIA images. We also used
invariance of the solar rotation profile with central meridian distance (CMD)
to determine the height of CBPs in 19.3 nm channel. Results. Best fit solar
rotation profile is given by $\omega(b)=(14.4060\pm0.0051 +
(-1.662\pm0.050)\sin^{2}b + (-2.742\pm0.081)\sin^{4}b)${\degr} day$^{-1}$.
Height of CBPs in SDO/AIA 19.3 nm channel was found to be $\approx$6500 km.
Meridional motion is predominantly poleward for all latitudes, while solar
velocity residuals show signs of torsional oscillations. Horizontal Reynolds
stress was found to be small compared to similar works, but still showing
transfer of angular momentum towards the solar equator. Conclusion. Most of the
results are consistent with Doppler measurements rather than tracer
measurements. Fairly small calculated value of horizontal Reynolds stress might
be due to the particular phase of the solar cycle. Accuracy of the calculated
rotation profile indicates that it is possible to measure changes in the
profile as the solar cycle evolves. Analysis of further SDO/AIA CBP data will
also help in better understanding of the temporal behaviour of the rotation
velocity residuals, meridional motions and Reynolds stress.
