Numerical Simulation of Coronal Waves Interacting with Coronal Holes: III. Dependence on Initial Amplitude of the Incoming Wave

Abstract

We performed 2.5D magnetohydrodynamic (MHD) simulations showing the propagation of fast-mode MHD waves of different initial amplitudes and their interaction with a coronal hole (CH), using our newly developed numerical code. We find that this interaction results in, first, the formation of reflected, traversing and transmitted waves (collectively, secondary waves) and, second, in the appearance of stationary features at the CH boundary. Moreover, we observe a density depletion that is moving in the opposite direction to the incoming wave. We find a correlation between the initial amplitude of the incoming wave and the amplitudes of the secondary waves as well as the peak values of the stationary features. Additionally, we compare the phase speed of the secondary waves and the lifetime of the stationary features to observations. Both effects obtained in the simulation, the evolution of secondary waves, as well as the formation of stationary fronts at the CH boundary, strongly support the theory that coronal waves are fast-mode MHD waves.

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• Geometrical properties of the interaction between oblique incoming coronal waves and coronal holes
• A new method for estimating global coronal wave properties from their interaction with solar coronal holes
• Construction of coronal hole and active region magnetohydrostatic solutions in two dimensions: Force and energy balance