Numerical Simulation of Coronal Waves Interacting with Coronal Holes: III. Dependence on Initial Amplitude of the Incoming Wave. (arXiv:1811.12735v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Piantschitsch_I/0/1/0/all/0/1">Isabell Piantschitsch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vrsnak_B/0/1/0/all/0/1">Bojan Vrsnak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hanslmeier_A/0/1/0/all/0/1">Arnold Hanslmeier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemmerer_B/0/1/0/all/0/1">Birgit Lemmerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veronig_A/0/1/0/all/0/1">Astrid Veronig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_Perez_A/0/1/0/all/0/1">Aaron Hernandez-Perez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calogovic_J/0/1/0/all/0/1">Jasa Calogovic</a>
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.
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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