  For the period of 1997-2006, coronal holes detected in the SOHO/EIT 195 $\AA$
full disk calibrated images are used to compute the rotation rates of high
latitude and near polar coronal holes and, their latitudinal variation is
investigated. We find that, for different latitude zones between $80^{o}$ north
and $75^{o}$ south, for all their area, the number of days observed on the
solar disk, and their latitudes, coronal holes rotate rigidly. Estimated
magnitudes of sidereal rotation rate of the coronal holes are: $13.051 \pm
0.206$ deg/day for the equator, $12.993 \pm 0.064$ deg/day in the region of
higher latitudes and, $12.999 \pm 0.329$ deg/day near the polar regions. For
all the latitudes and the area, we have also investigated the annual variation
of rotation rates of these coronal holes. We find that, for all the years,
coronal holes rotate rigidly and their magnitude of equatorial, high latitude
and polar region rotation rates are independent of magnitude of solar activity.
