  Coronal holes are the dark patches in the solar corona associated with
relatively cool, less dense plasma and unipolar fields. The fast component of
the solar wind emanates from these regions. Several observations reveal the
presence of magnetohydrodynamic (MHD) waves in coronal holes which are believed
to play a key role in the acceleration of fast solar wind. The recent advent of
high-resolution instruments had brought us many new insights on the properties
of MHD waves in coronal holes which are reviewed in this article. The advances
made in the identification of compressive slow MHD waves in both polar and
equatorial coronal holes, their possible connection with the recently
discovered high- speed quasi-periodic upflows, their dissipation, and the
detection of damping in Alfven waves from the spectral line width variation are
discussed in particular.
