All Figures

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian1.eps} \end{figure}$ Figure 1: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 450 Myr (left). The galaxy's closest approach to the cluster center is at t=500 Myr. Magnetic field vectors and gas density in the log scale in the plane perpendicular to the galactic disk at $t \sim$ 450 Myr (right). The galaxy moves to the south-east in both figures.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian2.eps} \end{figure}$ Figure 2: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 550 Myr (left). Magnetic field vectors and gas density in the log scale in the plane perpendicular to the galactic disk at $t \sim$ 550 Myr (right). The galaxy moves to the south-east in both figures.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian3.eps} \end{figure}$ Figure 3: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 650 Myr (left) and in the plane perpendicular to the galactic disk at $t \sim$ 650 Myr (right). The galaxy moves to the south-east in both figures.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian4.eps} \end{figure}$ Figure 4: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 750 Myr (left). Magnetic field vectors and gas density in the log scale in the plane perpendicular to the galactic disk at $t \sim$ 750 Myr (right).
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian5.eps} \end{figure}$ Figure 5: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 850 Myr (left) and in the plane perpendicular to the galactic disk at $t \sim$ 850 Myr (right).
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian6.eps} \end{figure}$ Figure 6: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 950 Myr (left) and in the plane perpendicular to the galactic disk at $t \sim$ 950 Myr (right).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{otmian7.eps} \end{figure}$ Figure 7: The evolution of the total magnetic energy normalized by its initial value as a function of time. Thin solid line: within a thick disk, uniform diffusion (case A). Thin dashed line: within a thick disk, non-uniform diffusion (case B). Thick solid line: within the whole computational box, uniform diffusion (case A). Thick dashed line: within the whole computational box, non-uniform diffusion (case B). Thick dotted line: within the whole computational box, without diffusion (case C). Thick dash-dotted line: within the whole computational box, 5 times lower diffusion than case A (case D).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{otmian8.ps} \end{figure}$ Figure 8: The evolution of the total magnetic energy normalized by its initial value as a function of time. Dashed line: uniform diffusion (case A), low cloud-cloud collision rate. Solid line: uniform diffusion, 6 times higher cloud-cloud collision rate.
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In the text

$\begin{figure} \par\includegraphics[width=11.1cm,clip]{otmian9.eps} \end{figure}$ Figure 9: Evolution of the polarized intensity at the chosen time steps. Contours: polarized intensity in logarithmic scale. The magnetic field vectors are superimposed onto the gas surface density (greyscale) in logarithmic scale. The timestep of snapshots is written in the lower left corner of each snapshot. The assumed beamsize is 10''.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{otmian10.eps} \end{figure}$ Figure 10: The radial velocity vectors superimposed onto the magnetic field strength in the galactic plane at the time step of t= 450 Myr.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{otmian11.eps} \end{figure}$ Figure 11: Velocity vectors superimposed onto the magnetic field strength (greyscales) at t= 650 Myr. Left panel: the radial velocity component in the galactic plane. Right panel: the full velocity in the plane perpendicular to the galactic disk.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian1.eps} \end{figure}$	Figure 1: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 450 Myr (left). The galaxy's closest approach to the cluster center is at t=500 Myr. Magnetic field vectors and gas density in the log scale in the plane perpendicular to the galactic disk at $t \sim$ 450 Myr (right). The galaxy moves to the south-east in both figures.
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$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian2.eps} \end{figure}$	Figure 2: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 550 Myr (left). Magnetic field vectors and gas density in the log scale in the plane perpendicular to the galactic disk at $t \sim$ 550 Myr (right). The galaxy moves to the south-east in both figures.
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$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian3.eps} \end{figure}$	Figure 3: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 650 Myr (left) and in the plane perpendicular to the galactic disk at $t \sim$ 650 Myr (right). The galaxy moves to the south-east in both figures.
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$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian4.eps} \end{figure}$	Figure 4: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 750 Myr (left). Magnetic field vectors and gas density in the log scale in the plane perpendicular to the galactic disk at $t \sim$ 750 Myr (right).
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$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian5.eps} \end{figure}$	Figure 5: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 850 Myr (left) and in the plane perpendicular to the galactic disk at $t \sim$ 850 Myr (right).
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$\begin{figure} \par\includegraphics[width=15.6cm,clip]{otmian6.eps} \end{figure}$	Figure 6: Magnetic field vectors and gas density in the log scale in the midplane at $t \sim$ 950 Myr (left) and in the plane perpendicular to the galactic disk at $t \sim$ 950 Myr (right).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{otmian8.ps} \end{figure}$	Figure 8: The evolution of the total magnetic energy normalized by its initial value as a function of time. Dashed line: uniform diffusion (case A), low cloud-cloud collision rate. Solid line: uniform diffusion, 6 times higher cloud-cloud collision rate.
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$\begin{figure} \par\includegraphics[width=11.1cm,clip]{otmian9.eps} \end{figure}$	Figure 9: Evolution of the polarized intensity at the chosen time steps. Contours: polarized intensity in logarithmic scale. The magnetic field vectors are superimposed onto the gas surface density (greyscale) in logarithmic scale. The timestep of snapshots is written in the lower left corner of each snapshot. The assumed beamsize is 10''.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{otmian10.eps} \end{figure}$	Figure 10: The radial velocity vectors superimposed onto the magnetic field strength in the galactic plane at the time step of t= 450 Myr.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{otmian11.eps} \end{figure}$	Figure 11: Velocity vectors superimposed onto the magnetic field strength (greyscales) at t= 650 Myr. Left panel: the radial velocity component in the galactic plane. Right panel: the full velocity in the plane perpendicular to the galactic disk.
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