$\begin{figure} \par\includegraphics[width=12cm,clip]{9800fig1.eps}\end{figure}$ Figure 1: Standard Riemann shock tube problem snapshot at time t=0.2. The density, velocity, thermal energy density per unit mass and pressure are shown.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9800fig2.eps}\end{figure}$ Figure 2: Strong shock tube problem snapshot, taken at the time t=0.12. Density, velocity, thermal energy density per unit mass and pressure are shown.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9800fig3.eps}\end{figure}$ Figure 3: Snapshot of Brio & Wu problem, taken at the time t=0.11. Density, velocity, thermal pressure, and the y component of magnetic field are shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9800fig5.eps}\end{figure}$ Figure 5: Strong shock front caused by the explosion with energy $e=10^{48}~{\rm J}$ in non-uniform media. The figure shows the shape of the shock at the time $t \sim 30~000~{\rm years}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9800fig6.eps}\end{figure}$ Figure 6: Two-dimensional shape of the shock front. The explosion, which caused the shock wave, is marked by cross at the point with the coordinates $\left (0,-0.5\right )$ in the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9800fig7.eps}\end{figure}$ Figure 7: Snapshot of the vertical velocity structure of the simulation of the wave propagation and conversion in the non-magnetic solar chromosphere and corona taken at $t=230~{\rm s}$ . Conversion of the linear waves into non-linear ones is seen at the height above $z=2000~{\rm km}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9800fig8.eps}\end{figure}$ Figure 8: Vertical velocity profile, taken at the centre of the simulation box, from the simulation of the wave conversion in the solar corona taken at $t=230~{\rm s}$ . The conversion of linear waves into non-linear occurs at $z=2000~{\rm km}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9800fig9.eps}\end{figure}$ Figure 9: Snapshot from the simulation of the wave propagation and conversion in magnetic solar chromosphere and corona taken at $t=209~{\rm s}$ . The magnetic field, which is sketched by a cylinder in the figure, acts as a waveguide and suppresses the energy propagation outside the magnetic flux concentration.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9800fi10.eps}\end{figure}$ Figure 10: Vertical velocity profile taken at the centre of the simulation box from the simulation of the wave conversion in the solar corona taken at $t=209~{\rm s}$ . The conversion of linear waves into non-linear occurs at $z=2000~{\rm km}$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9800fig1.eps}\end{figure}$	Figure 1: Standard Riemann shock tube problem snapshot at time t=0.2. The density, velocity, thermal energy density per unit mass and pressure are shown.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{9800fig2.eps}\end{figure}$	Figure 2: Strong shock tube problem snapshot, taken at the time t=0.12. Density, velocity, thermal energy density per unit mass and pressure are shown.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{9800fig3.eps}\end{figure}$	Figure 3: Snapshot of Brio & Wu problem, taken at the time t=0.11. Density, velocity, thermal pressure, and the y component of magnetic field are shown.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9800fig4.eps}\end{figure}$	Figure 4: Snapshot of the plasma density of the Ország-Tang vortex problem simulation at t=0.5.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9800fig5.eps}\end{figure}$	Figure 5: Strong shock front caused by the explosion with energy $e=10^{48}~{\rm J}$ in non-uniform media. The figure shows the shape of the shock at the time $t \sim 30~000~{\rm years}$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9800fig6.eps}\end{figure}$	Figure 6: Two-dimensional shape of the shock front. The explosion, which caused the shock wave, is marked by cross at the point with the coordinates $\left (0,-0.5\right )$ in the figure.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9800fig7.eps}\end{figure}$	Figure 7: Snapshot of the vertical velocity structure of the simulation of the wave propagation and conversion in the non-magnetic solar chromosphere and corona taken at $t=230~{\rm s}$ . Conversion of the linear waves into non-linear ones is seen at the height above $z=2000~{\rm km}$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9800fig8.eps}\end{figure}$	Figure 8: Vertical velocity profile, taken at the centre of the simulation box, from the simulation of the wave conversion in the solar corona taken at $t=230~{\rm s}$ . The conversion of linear waves into non-linear occurs at $z=2000~{\rm km}$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9800fig9.eps}\end{figure}$	Figure 9: Snapshot from the simulation of the wave propagation and conversion in magnetic solar chromosphere and corona taken at $t=209~{\rm s}$ . The magnetic field, which is sketched by a cylinder in the figure, acts as a waveguide and suppresses the energy propagation outside the magnetic flux concentration.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9800fi10.eps}\end{figure}$	Figure 10: Vertical velocity profile taken at the centre of the simulation box from the simulation of the wave conversion in the solar corona taken at $t=209~{\rm s}$ . The conversion of linear waves into non-linear occurs at $z=2000~{\rm km}$ .
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