  We used our newly developed magnetohydrodynamic (MHD) code to perform 2.5D
simulations of a fast-mode MHD wave interacting with coronal holes (CH) of
varying Alfv\'en speed which result from assuming different CH densities. We
find that this interaction leads to effects like reflection, transmission,
stationary fronts at the CH boundary and the formation of a density depletion
that moves in the opposite direction to the incoming wave. We compare these
effects with regard to the different CH densities and present a comprehensive
analysis of morphology and kinematics of the associated secondary waves. We
find that the density value inside the CH influences the phase speed as well as
the amplitude values of density and magnetic field for all different secondary
waves. Moreover, we observe a correlation between the CH density and the peak
values of the stationary fronts at the CH boundary. The findings of reflection
and transmission on the one hand and the formation of stationary fronts caused
by the interaction of MHD waves with CHs on the other hand, strongly support
the theory that large scale disturbances in the corona are fast-mode MHD waves.
