  We developed a new numerical code that is able to perform 2.5D simulations of
a magnetohydrodynamic (MHD) wave propagation in the corona, and its interaction
with a low density region, such as a coronal hole (CH). We show that the impact
of the wave on the CH leads to different effects, such as reflection and
transmission of the incoming wave, stationary features at the CH boundary, or
formation of a density depletion. We present a comprehensive analysis of the
morphology and kinematics of primary and secondary waves, that is, we describe
in detail the temporal evolution of density, magnetic field, plasma flow
velocity, phase speed and position of the wave amplitude. Effects like
reflection, refraction and transmission of the wave strongly support the theory
that large scale disturbances in the corona are fast MHD waves and build the
major distinction to the competing pseudo-wave theory. The formation of
stationary bright fronts was one of the main reasons for the development of
pseudo-waves. Here we show that stationary bright fronts can be produced by the
interactions of an MHD wave with a CH. We find secondary waves that are
traversing through the CH and we show that one part of these traversing waves
leaves the CH again, while another part is being reflected at the CH boundary
inside the CH. We observe a density depletion that is moving in the opposite
direction of the primary wave propagation. We show that the primary wave pushes
the CH boundary to the right, caused by the wave front exerting dynamic
pressure on the CH.

Solar and Stellar Astrophysics