Abstract:
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 highspeed quasi-periodic upflows, their dissipation, and
the detection of damping in Alfv´en waves from the
spectral line width variation are discussed in particular.
