  For the years 2001-2008, we use full-disk, SOHO/EIT 195 $\AA$ calibrated
images to determine latitudinal and day to day variations of the rotation rates
of coronal holes. We estimate the weighted average of heliographic coordinates
such as latitude and longitude from the central meridian on the observed solar
disk. For different latitude zones between $40^{o}$ north - $40^{o}$ south, we
compute rotation rates, and find that, irrespective of their area, number of
days observed on the solar disk and latitudes, coronal holes rotate rigidly.
Combined for all the latitude zones, we also find that coronal holes rotate
rigidly during their evolution history. In addition, for all latitude zones,
coronal holes follow a rigid body rotation law during their first appearance.
Interestingly, average first rotation rate ($\sim 438 nHz$) of the coronal
holes, computed from their first appearance on the solar disk, match with
rotation rate of the solar interior only below the tachocline.
