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Magnetohydrodynamic code for gravitationally-stratified media

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Figure

Fig. 1. Standard Riemann shock tube problemsnapshot at time t = 0.2. The density, velocity,thermal energy density per unit mass and pres-sure are shown.
Fig. 3. Snapshot of Brio & Wu problem, takenat the timepressure, and the t = 0.11. Density, velocity, thermal y component of magnetic fieldare shown.
Fig. 4. Snapshot of the plasma density of the Ország-Tang vortex prob-lem simulation at t = 0.5.
Fig. 7. Snapshot of the vertical velocity structure of the simulation ofthe wave propagation and conversion in the non-magnetic solar chro-mosphere and corona taken at t = 230 s
+2

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