All Figures

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{mavillez_fig01.ps} \end{figure}$ Figure 1: Time evolution of the random field component (red), the mean field (green) and total field strength (black).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.6cm,clip]{mavillez_fig02a.... ...m} \includegraphics[angle=-90,width=5.6cm,clip]{mavillez_fig02b.ps} \end{figure}$ Figure 2: Two-dimensional slices through the three-dimensional data cube showing the vertical (perpendicular to the midplane) distribution of the density ( left panel) and magnetic field ( right panel) at time t=221.9 Myr. The mean field in the midplane is $3.1~\mu$ G. The z-scale above 0.5 and below -0.5 kpc is shrunk (in order to fit the paper size) and thus, the distribution of the labels is not uniform. Red in the density map refers to lowest density (and thus highest temperature if in pressure equilibrium), while dark blue refers to the highest density (and thus lowest temperature). In the magnetic field image red/blue correspond to the highest/lowest strength. The left panel shows the presence of a wiggly and thin disk of cold gas overlayed by a frothy thick disk composed of neutral (light blue) and ionized (greenish) gas. The expansion of superbubbles can be nicely seen, especially in the southern hemisphere. The magnetic field map shows the thin magnetized disk overlayed by loops of field lines, magnetic islands, and clouds wrapped in field lines moving downwards. From these maps it can be immediately seen that the simulations must take into account large heights on either side of the midplane, allowing for the setup of the disk-halo-disk circulation.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{mavillez_fig03a.... ...m} \includegraphics[angle=-90,width=7.8cm,clip]{mavillez_fig03d.ps} \end{figure}$ Figure 3: Two-dimensional slices through the three-dimensional data set at z=0 (Galactic midplane), showing density ( top left panel), temperature ( top right panel), pressure Phys. Rev. E/k ( bottom left panel), and magnetic field ( bottom right panel) after 358 Myr of evolution. Colour bars indicate the logarithmic scale of each quantity. Red refers to lowest density, highest temperature and pressure, while dark blue refers to the highest density and lowest temperature and pressure. In the magnetic field image red/blue correspond to the highest/lowest strength. Direct visual inspection shows a strong inverse spatial correlation between gas density and temperature (although the pressure diagram is still far from uniform), whereas the correlation between magnetic field strength and gas density is only present for the cold dense regions. For higher temperature regions this correlation becomes rather poor and vanishes completely for the hot gas (s. Fig. 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{mavillez_fig04.ps} \end{figure}$ Figure 4: Scatter plot of B versus $\rho$ for ${T}\leq 200$ (black), $200<{T}\leq 10^{3.9}$ (orange), $10^{3.9}<{T}\leq 10^{4.2}$ (blue), $10^{4.2}<{T}\leq 10^{5.5}$ K (green), and T>10^5.5 K (red) regimes at 300 Myr of disk evolution. The points in the plot are sampled at intervals of four points in each direction. Note that during the evolution of the system the field strength broadened its distribution spanning two orders of magnitude after 300 Myr.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{mavillez_fig05.ps} \end{figure}$ Figure 5: Comparison of the averages $\langle P_{\rm ram}\rangle$ (green), $\langle P_{\rm th}\rangle$ (black), and $\langle P_{\rm mag}\rangle$ (red) as function of the temperature (in the simulated disk $\left \vert z\right \vert\leq 250$ pc) averaged over temperature bins of $\Delta \log {T}=0.1$ K.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{mavillez_fig06a.ps}\vspace*{... ...ce*{2.5mm} \par\includegraphics[width=7cm,clip]{mavillez_fig06c.ps} \end{figure}$ Figure 6: Averaged volume weighted histograms of the thermal ( top panel), magnetic ( middle panel) and total ( bottom panel) pressures for the different temperature regimes in the ISM. The total distribution of each pressure is shown by the dashed black line. The histograms have been calculated using 51 snapshots with a time interval of 1 Myrbetween 350 and 400 Myr.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{mavillez_fig07a.ps}\hspace... ...pace*{5.5mm} \includegraphics[width=6.7cm,clip]{mavillez_fig07d.ps} \end{figure}$ Figure 7: Averaged volume weighted histograms of the density for the different temperature regimes of the disk gas (the full distribution is shown by the dashed line) in the top panels and averaged temperature histograms in the bottom panels for the MHD run ( left column) and the HD run ( right column). The histograms have been calculated using 51 snapshots with a time interval of 1 Myr between 350 and 400 Myr.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{mavillez_fig08a.ps}\vspace*{5mm} \par\includegraphics[width=7cm,clip]{mavillez_fig08b.ps} \end{figure}$ Figure 8: Time history of the volume occupation fractions of the different temperature regimes for the MHD ( top panel) and HD ( bottom panel) runs.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{mavillez_fig09a.ps}\vspace*{... ...pace*{6mm} \par\includegraphics[width=7cm,clip]{mavillez_fig09c.ps} \end{figure}$ Figure 9: Top and middle panels show the histories of the mass fractions of the different thermal regimes for the magnetized ( top) and unmagnetized ( middle) ISM. Bottom panel shows the history of the fraction of mass of the WNM gas having $500 <{T}\leq 5000$ K in the disk for the HD (red) and MHD (black) runs.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{mavillez_fig10a.ps}\vspace*{5mm} \par\includegraphics[width=7.2cm,clip]{mavillez_fig10b.ps} \end{figure}$ Figure 10: History of the root mean square velocity of the differenttemperature regimes of the disk gas in the MHD ( top panel) and HD( bottom panel) runs.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{mavillez_fig01.ps} \end{figure}$	Figure 1: Time evolution of the random field component (red), the mean field (green) and total field strength (black).
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{mavillez_fig05.ps} \end{figure}$	Figure 5: Comparison of the averages $\langle P_{\rm ram}\rangle$ (green), $\langle P_{\rm th}\rangle$ (black), and $\langle P_{\rm mag}\rangle$ (red) as function of the temperature (in the simulated disk $\left \vert z\right \vert\leq 250$ pc) averaged over temperature bins of $\Delta \log {T}=0.1$ K.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{mavillez_fig06a.ps}\vspace{... ...ce{2.5mm} \par\includegraphics[width=7cm,clip]{mavillez_fig06c.ps} \end{figure}$	Figure 6: Averaged volume weighted histograms of the thermal ( top panel), magnetic ( middle panel) and total ( bottom panel) pressures for the different temperature regimes in the ISM. The total distribution of each pressure is shown by the dashed black line. The histograms have been calculated using 51 snapshots with a time interval of 1 Myrbetween 350 and 400 Myr.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{mavillez_fig08a.ps}\vspace*{5mm} \par\includegraphics[width=7cm,clip]{mavillez_fig08b.ps} \end{figure}$	Figure 8: Time history of the volume occupation fractions of the different temperature regimes for the MHD ( top panel) and HD ( bottom panel) runs.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{mavillez_fig09a.ps}\vspace{... ...pace{6mm} \par\includegraphics[width=7cm,clip]{mavillez_fig09c.ps} \end{figure}$	Figure 9: Top and middle panels show the histories of the mass fractions of the different thermal regimes for the magnetized ( top) and unmagnetized ( middle) ISM. Bottom panel shows the history of the fraction of mass of the WNM gas having $500 <{T}\leq 5000$ K in the disk for the HD (red) and MHD (black) runs.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{mavillez_fig10a.ps}\vspace*{5mm} \par\includegraphics[width=7.2cm,clip]{mavillez_fig10b.ps} \end{figure}$	Figure 10: History of the root mean square velocity of the differenttemperature regimes of the disk gas in the MHD ( top panel) and HD( bottom panel) runs.
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