  Coronal bright points (CBP) are ubiquitous small brightenings in the solar
corona associated with small magnetic bipoles. We derive the solar differential
rotation profile by tracing the motions of CBPs detected by the Atmospheric
Imaging Assembly (AIA) instrument aboard the Solar Dynamics Observatory (SDO).
We also investigate problems related to detection of coronal bright points
resulting from instrument and detection algorithm limitations. To determine the
positions and identification of coronal bright points we used a segmentation
algorithm. A linear fit of their central meridian distance and latitude versus
time was utilised to derive velocities. We obtained 906 velocity measurements
in a time interval of only 2 days. The differential rotation profile can be
expressed as $\omega_{rot} = (14.47\pm 0.10 + (0.6\pm 1.0)\sin^{2}(b) +
(-4.7\pm 1.7)\sin^{4}(b))$\degr day$^{-1}$. Our result is in agreement with
other work and it comes with reasonable errors in spite of the very short time
interval used. This was made possible by the higher sensitivity and resolution
of the AIA instrument compared to similar equipment as well as high cadence.
The segmentation algorithm also played a crucial role by detecting so many
CBPs, which reduced the errors to a reasonable level. Data and methods
presented in this paper show a great potential to obtain very accurate velocity
profiles, both for rotation and meridional motion and, consequently, Reynolds
stresses. The amount of coronal bright point data that could be obtained from
this instrument should also provide a great opportunity to study changes of
velocity patterns with a temporal resolution of only a few months. Other
possibilities are studies of evolution of CBPs and proper motions of magnetic
elements on the Sun.
