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

Numerical Simulation of Coronal Waves Interacting with Coronal Holes: II. Dependence on Alfv\'en Speed Inside the Coronal Hole