Three-Dimensional Propagation of Magnetohydrodynamic Waves in the Solar Chromosphere and Corona

We study the three-dimensional magnetohydrodynamic (MHD) wave
propagation in the solar atmosphere consisting of the chromosphere and corona. Pressure enhancement and velocity shear are implemented simultaneously at the bottom of the chromosphere. The global propagation of the incurred MHD waves, including fast- and slow-mode magnetoacoustic waves as well as Alfvén wave, can be identified. Wave front positions obtained numerically with respect to specific waves fit well with those calculated with local MHD wave speeds.