All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2896fig0.ps} \end{figure}$ Figure 1: Initial geometry of the shock-cloud interaction. The cloud is centered at (x,y,z)=(0,0,0). The shock is moving upwards through the ISM with velocity w (see text). Only one quarter of the volume shown is modeled numerically as indicated by a gray patch covering upper right portion of the top face of the domain.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2896fig1.ps} \end{figure}$ Figure 2: $\chi -{\cal M}$ parameter space. The lines are derived for length-scale l = 1 pc and mark the density contrast for which $[\tau _{\rm cond}]_{\rm psh} = \tau _{\rm cc}$ (dotted line), $[\tau _{\rm rad}]_{\rm cl} = \tau _{\rm cc}$ (dashed line), and $[\tau _{\rm rad}]_{\rm cl} = [\tau _{\rm cond}]_{\rm psh}$ (solid line). The crosses mark the two cases investigated.
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In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{fig3_aa2896-05.eps} % \end{figure}$ Figure 3: 3-D visualizations of the mass density evolution during the shock-cloud interaction at selected times in units of $\tau _{\rm cc}$ . The gray scale shows the density distributions, in log scale. The box is $4\times 4\times 6$ pc³. The calculation is the one neglecting the thermal conduction and the radiative losses and at the highest spatial resolution (run HY2, see Table 2).
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{fig4_aa2896-05.eps} \end{figure}$ Figure 4: 2-D sections in the (x,z) plane of the mass density distribution (gm cm^-3), in log scale, in the simulations HY2 ( left half panels) and HTR50 ( right half panels), sampled at the labeled times in units of $\tau _{\rm cc}$ . The velocity arrows scale linearly with respect to the reference velocity shown in the upper left panel and corresponding to 500 km s^-1. The contour encloses the cloud material.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{fig5_aa2896-05.eps} \end{figure}$ Figure 5: As in Fig. 4 for the plasma temperature distribution (MK).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2896fig5.ps} % \end{figure}$ Figure 6: Mass density ( left panels) and temperature ( right panels) profiles along the symmetry axis, z, in the runs HY2 (solid lines) and HTR50 (dotted lines) at selected times in units of $\tau _{\rm cc}$ . The arrows mark the reflected (A), transmitted (B) and primary (C) shocks for the two simulations.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{fig7_aa2896-05.eps} % \end{figure}$ Figure 7: As Fig. 4 for the Mach 30 case. Note that the velocity field calculated in the run HY2 has been scaled by the factor 3/5, according to the Mach scaling (see Eq. (17)). The velocity arrows scale linearly with respect to the reference velocity shown in the upper left panel and corresponding to 300 km s^-1. The contour encloses the cloud material.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{fig8_aa2896-05.eps} % \end{figure}$ Figure 8: As Fig. 5 for the Mach 30 case. The velocity field and the temperature distribution calculated in the run HY2 have been scaled by the factor 3/5 and (3/5)², respectively, according to the Mach scaling (see Eq. (17)).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2896fig8.ps}\end{figure}$ Figure 9: Mass fraction of the initial cloud material dominated by the radiative losses (dashed line) or by the thermal conduction (dotted line) in run HTR30.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2896fig9.ps} \end{figure}$ Figure 10: Evolution of the global properties of the gas cloud defined in Sect. 3.4 for runs HY1 and HY2 which neglect the thermal conduction and the radiation (dashed and solid lines), and for runs HTR50 and HTR30, which instead include the thermal conduction and the radiation (dotted and dash-dotted lines).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2896fap1.ps} \end{figure}$ Figure A.1: Comparison of the temperature distributions along the direction of propagation as computed numerically with the FLASH code (solid lines), sampled every 0.5 s, with the corresponding analytic solutions (dashed lines).

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2896fig0.ps} \end{figure}$	Figure 1: Initial geometry of the shock-cloud interaction. The cloud is centered at (x,y,z)=(0,0,0). The shock is moving upwards through the ISM with velocity w (see text). Only one quarter of the volume shown is modeled numerically as indicated by a gray patch covering upper right portion of the top face of the domain.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2896fig1.ps} \end{figure}$	Figure 2: $\chi -{\cal M}$ parameter space. The lines are derived for length-scale l = 1 pc and mark the density contrast for which $[\tau _{\rm cond}]_{\rm psh} = \tau _{\rm cc}$ (dotted line), $[\tau _{\rm rad}]_{\rm cl} = \tau _{\rm cc}$ (dashed line), and $[\tau _{\rm rad}]_{\rm cl} = [\tau _{\rm cond}]_{\rm psh}$ (solid line). The crosses mark the two cases investigated.
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$\begin{figure} \par\includegraphics[width=15.4cm,clip]{fig3_aa2896-05.eps} % \end{figure}$	Figure 3: 3-D visualizations of the mass density evolution during the shock-cloud interaction at selected times in units of $\tau _{\rm cc}$ . The gray scale shows the density distributions, in log scale. The box is $4\times 4\times 6$ pc³. The calculation is the one neglecting the thermal conduction and the radiative losses and at the highest spatial resolution (run HY2, see Table 2).
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$\begin{figure} \par\includegraphics[width=15.8cm,clip]{fig5_aa2896-05.eps} \end{figure}$	Figure 5: As in Fig. 4 for the plasma temperature distribution (MK).
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$\begin{figure} \par\includegraphics[width=12cm,clip]{2896fig5.ps} % \end{figure}$	Figure 6: Mass density ( left panels) and temperature ( right panels) profiles along the symmetry axis, z, in the runs HY2 (solid lines) and HTR50 (dotted lines) at selected times in units of $\tau _{\rm cc}$ . The arrows mark the reflected (A), transmitted (B) and primary (C) shocks for the two simulations.
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$\begin{figure} \par\includegraphics[width=15.8cm,clip]{fig7_aa2896-05.eps} % \end{figure}$	Figure 7: As Fig. 4 for the Mach 30 case. Note that the velocity field calculated in the run HY2 has been scaled by the factor 3/5, according to the Mach scaling (see Eq. (17)). The velocity arrows scale linearly with respect to the reference velocity shown in the upper left panel and corresponding to 300 km s^-1. The contour encloses the cloud material.
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$\begin{figure} \par\includegraphics[width=15.8cm,clip]{fig8_aa2896-05.eps} % \end{figure}$	Figure 8: As Fig. 5 for the Mach 30 case. The velocity field and the temperature distribution calculated in the run HY2 have been scaled by the factor 3/5 and (3/5)², respectively, according to the Mach scaling (see Eq. (17)).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2896fig8.ps}\end{figure}$	Figure 9: Mass fraction of the initial cloud material dominated by the radiative losses (dashed line) or by the thermal conduction (dotted line) in run HTR30.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{2896fig9.ps} \end{figure}$	Figure 10: Evolution of the global properties of the gas cloud defined in Sect. 3.4 for runs HY1 and HY2 which neglect the thermal conduction and the radiation (dashed and solid lines), and for runs HTR50 and HTR30, which instead include the thermal conduction and the radiation (dotted and dash-dotted lines).
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