Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{MS3707f1.eps} \end{figure}$ Figure 1: The evolution of the dynamo coefficient $\alpha _{xx}$ for the model D1; the height above the galactic plane is z=300 pc for different time steps.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f2.eps} \end{figure}$ Figure 2: The time evolution of the dynamo coefficient $\alpha _{xx}$ for the models D1 (right) and B1 (left) at three chosen heights above the disk plane for the high (HR, solid lines) and low (LR, dotted lines) resolution models.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f3.eps} \end{figure}$ Figure 3: The time evolution of the dynamo coefficients $\alpha _{yy}$ for the models B1 (left) and D1 (right) at three chosen heights above the disk plane for the high resolution models. The curves are described in the insets.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f4.eps} \end{figure}$ Figure 4: The time evolution of the dynamo coefficient $\alpha _{zz}$ (left) and the diffusion coefficient $\eta _{\rm T}$ (right) for both models at three chosen heights above the disk plane for the high resolution models. The curves are described in the inset.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f5.eps} \end{figure}$ Figure 5: The time evolution of three dynamo coefficients: $\alpha ^A_{yx}$ (solid lines), $\alpha _{yx}$ (dashed-dotted lines) and $\alpha _{xy}$ (dashed lines) for the model B1 (the left panel) and D1 (the right panel) at z=700 pc. The curves are described in the insets.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f6.eps} \end{figure}$ Figure 6: The time evolution of the natural logarithm of the mean square velocity (left) and the chosen dynamo coefficients (right) for both models at 700 pc height above the galactic plane for the high resolution models. The curves are described in the insets.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f7.eps} \end{figure}$ Figure 7: The time evolution of the dynamo coefficient $\alpha _{xx}$ (left) and $\alpha _{yy}$ (right) for the model B1 (solid lines) and B2 (dashed-dotted lines) at z=700 pc. The experiment B1 has two times stronger the initial magnetic field than B2.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{MS3707f8.eps} \end{figure}$ Figure 8: The time evolution of the dynamo coefficient $\alpha _{zz}$ (left) and the diffusion coefficient $\eta _{\rm T}$ (right) for the model B1 (solid lines) and B2 (dashed-dotted lines) at z=700 pc. The experiment B1 has a two times stronger initial magnetic field than B2.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{MS3707f9.eps} \end{figure}$ Figure 9: The time evolution of three dynamo coefficients: $\alpha ^A_{yx}$ (solid lines), $\alpha _{yx}$ (dashed-dotted lines) and $\alpha _{xy}$ (dashed lines) for the model B1 (the left panel) and B2 (the right panel) at z=700 pc. The experiment B1 has a two times stronger initial magnetic field than B2.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{MS3707f1.eps} \end{figure}$	Figure 1: The evolution of the dynamo coefficient $\alpha _{xx}$ for the model D1; the height above the galactic plane is z=300 pc for different time steps.
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$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f2.eps} \end{figure}$	Figure 2: The time evolution of the dynamo coefficient $\alpha _{xx}$ for the models D1 (right) and B1 (left) at three chosen heights above the disk plane for the high (HR, solid lines) and low (LR, dotted lines) resolution models.
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$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f3.eps} \end{figure}$	Figure 3: The time evolution of the dynamo coefficients $\alpha _{yy}$ for the models B1 (left) and D1 (right) at three chosen heights above the disk plane for the high resolution models. The curves are described in the insets.
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$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f4.eps} \end{figure}$	Figure 4: The time evolution of the dynamo coefficient $\alpha _{zz}$ (left) and the diffusion coefficient $\eta _{\rm T}$ (right) for both models at three chosen heights above the disk plane for the high resolution models. The curves are described in the inset.
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$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f5.eps} \end{figure}$	Figure 5: The time evolution of three dynamo coefficients: $\alpha ^A_{yx}$ (solid lines), $\alpha _{yx}$ (dashed-dotted lines) and $\alpha _{xy}$ (dashed lines) for the model B1 (the left panel) and D1 (the right panel) at z=700 pc. The curves are described in the insets.
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$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f6.eps} \end{figure}$	Figure 6: The time evolution of the natural logarithm of the mean square velocity (left) and the chosen dynamo coefficients (right) for both models at 700 pc height above the galactic plane for the high resolution models. The curves are described in the insets.
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$\begin{figure} \par\includegraphics[width=11.8cm,clip]{MS3707f7.eps} \end{figure}$	Figure 7: The time evolution of the dynamo coefficient $\alpha _{xx}$ (left) and $\alpha _{yy}$ (right) for the model B1 (solid lines) and B2 (dashed-dotted lines) at z=700 pc. The experiment B1 has two times stronger the initial magnetic field than B2.
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$\begin{figure} \par\includegraphics[width=11.6cm,clip]{MS3707f8.eps} \end{figure}$	Figure 8: The time evolution of the dynamo coefficient $\alpha _{zz}$ (left) and the diffusion coefficient $\eta _{\rm T}$ (right) for the model B1 (solid lines) and B2 (dashed-dotted lines) at z=700 pc. The experiment B1 has a two times stronger initial magnetic field than B2.
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$\begin{figure} \par\includegraphics[width=11.6cm,clip]{MS3707f9.eps} \end{figure}$	Figure 9: The time evolution of three dynamo coefficients: $\alpha ^A_{yx}$ (solid lines), $\alpha _{yx}$ (dashed-dotted lines) and $\alpha _{xy}$ (dashed lines) for the model B1 (the left panel) and B2 (the right panel) at z=700 pc. The experiment B1 has a two times stronger initial magnetic field than B2.
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