All Figures

$\begin{figure} \par\includegraphics[width=20pc]{7824fig1.eps} \end{figure}$ Figure 1: The evolution of a typical SNR computed using parameters as described in the text. Results are shown from 1000 to 4000 yr as indicated. Shown in the top panel is the ISM magnetic field B (perpendicular to the flow) which gets compressed by a factor $s\approx 4$ . Shown in the second panel is the density $\rho$ . From the origin one can see the reverse shock (RS), the contact discontinuity between the ejected and shocked ISM and the blast wave, forward shock (FS), which propagates in the undisturbed ISM. The position of the RS and FS are indicated by the vertical dashed lines. In the bottom panels the speed v is shown on a logarithmic scale, and therefore -v is shown just below it. Shown here is that at some time the RS starts to move inward, and the speed reverses sign meaning that the flow is now inward toward the center. In the last panel the pressure P is shown.
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In the text

$\begin{figure} \par\includegraphics[width=37pc]{7824fig2.eps} \end{figure}$ Figure 2: The computed FS ( top panel) and RS ( bottom panel) radius as a function of time. Different scenarios are shown corresponding to a SNR expanding in ISM of different densities, e.g. $\rho _{\rm ISM} = 10^{-27}$ g cm^-3 up to $\rho _{\rm ISM} = 10^{-23}$ g cm^-3. Shown on the left panels are SNR scenarios corresponding to an ejecta mass $M_{\rm ej}=3~M_{\odot}$ in the middle panels $M_{\rm ej}=2~M_{\odot}$ and on the right $M_{\rm ej}=1~M_{\odot}$ . The dotted lines in the upper left panel show the Sedov solution where the FS radius increases as t^2/5.
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In the text

$\begin{figure} \par\includegraphics[width=35pc]{7824fig3.eps} \end{figure}$ Figure 3: The effect of different parameters on the RS return time $t_{\rm R}$ . Shown in the left large panel is $t_{\rm R}$ as a function of $\rho _{\rm ISM}$ for $M_{\rm ej}$ = 1, 2, 3, ...., 10 $M_{\odot }$ . Shown on the top right panel is the dependence of $t_{\rm R}$ on $M_{\rm ej}$ for all different $\rho _{\rm ISM}$ scenarios. The middle panel on the right show the dependence of $t_{\rm R}$ on the ejection energy $E_{\rm ej}$ and the bottom right panel the dependence on the adiabatic index $\gamma$ .
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In the text

$\begin{figure} \par\includegraphics[width=17pc]{7824fig4.eps} \end{figure}$ Figure 4: Time before the RS starts to move inward toward the origin $t_{\rm c}$ as a function of $t_{\rm R}$ for all computations as shown in Fig. 2. Shown by the solid line is $t_{\rm c}=0.5t_{\rm R}$ .
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In the text

$\begin{figure} \par\includegraphics[width=40pc]{7824fig5.eps} \end{figure}$ Figure 5: A computed SNR (in terms of density) moving from a ISM density of $\rho _{\rm ISM}=10^{-24}$ g cm^-3 to a medium where $\rho _{\rm ISM} = 10^{-23}$ g cm^-3. Shown from top to bottom are different stages in the SNR evolution, e.g. 1000, 3000, 5000 and 7000 yr. Note that a logarithmic scaling is used and that the density is normalized by dividing by 10^-24.
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In the text

$\begin{figure} \par\includegraphics[width=31pc]{7824fig6.eps} \end{figure}$ Figure 6: As in Fig. 5 except now the compressed ISM magnetic field is shown for two different ISM field orientations. Shown on the left of each panel are the field lines and on the right the field magnitude.
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In the text

$\begin{figure} \par\includegraphics[width=40pc]{7824fig7.eps} \end{figure}$ Figure 7: The top panel shown the ISM magnetic field B (for the case where the field is parallel to the interface). Shown in the second panel is the density $\rho$ . The bottom three panels show the speed v and -v and pressure P. Computations are shown from the SNR origin in the direction directly toward the more denser medium (solid line) and directly away in the opposite direction (dotted line). The left panels show parameters at 1000 yr, the middle panel parameters at 1500 yr and the right panel at 2000 yr. The location of the reflected wave is shown by the dashed line in the pressure panels.
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In the text

$\begin{figure} \par\includegraphics[width=40pc]{7824fig8.eps} \end{figure}$ Figure 8: Similar to Fig. 5, except here the SNR moves from a medium with density of $\rho _{\rm ISM}=10^{-24}$ g cm^-3 to a medium where $\rho _{\rm ISM}=10^{-25}$ g cm^-3. In this case densities of $\rho _{\rm ISM}=10^{-24}$ g cm^-3 will be the denser region.
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In the text

$\begin{figure} \par\includegraphics[width=27pc]{7824fig9.eps} \end{figure}$ Figure 9: As in Fig. 6 but for the case where the SNR moves into a less denser region.
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In the text

$\begin{figure} \par\includegraphics[width=40pc]{7824fg10.eps} \end{figure}$ Figure 10: As in Fig. 7 except here the SNR moves into a medium of lesser density. The interface between the two media is a infinite plane situated 5 pc from the initial explosion. Note that in this scenario there is no reflected shock, but a second reverse shock start to form as the FS moves well into the medium of lesser density.
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In the text

$\begin{figure} \par\includegraphics[width=20pc]{7824fg11.eps} \end{figure}$ Figure 11: The pressure P of the SNR in the direction toward the contact discontinuity. The simulation is shown from 2000 yr up to 8000 yr. As time increases a second RS forms and at 8000 yr it starts to move toward the center.
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In the text

$\begin{figure} \par\includegraphics[width=17pc]{7824fig4.eps} \end{figure}$	Figure 4: Time before the RS starts to move inward toward the origin $t_{\rm c}$ as a function of $t_{\rm R}$ for all computations as shown in Fig. 2. Shown by the solid line is $t_{\rm c}=0.5t_{\rm R}$ .
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$\begin{figure} \par\includegraphics[width=40pc]{7824fig5.eps} \end{figure}$	Figure 5: A computed SNR (in terms of density) moving from a ISM density of $\rho _{\rm ISM}=10^{-24}$ g cm^-3 to a medium where $\rho _{\rm ISM} = 10^{-23}$ g cm^-3. Shown from top to bottom are different stages in the SNR evolution, e.g. 1000, 3000, 5000 and 7000 yr. Note that a logarithmic scaling is used and that the density is normalized by dividing by 10^-24.
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$\begin{figure} \par\includegraphics[width=31pc]{7824fig6.eps} \end{figure}$	Figure 6: As in Fig. 5 except now the compressed ISM magnetic field is shown for two different ISM field orientations. Shown on the left of each panel are the field lines and on the right the field magnitude.
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$\begin{figure} \par\includegraphics[width=40pc]{7824fig8.eps} \end{figure}$	Figure 8: Similar to Fig. 5, except here the SNR moves from a medium with density of $\rho _{\rm ISM}=10^{-24}$ g cm^-3 to a medium where $\rho _{\rm ISM}=10^{-25}$ g cm^-3. In this case densities of $\rho _{\rm ISM}=10^{-24}$ g cm^-3 will be the denser region.
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$\begin{figure} \par\includegraphics[width=27pc]{7824fig9.eps} \end{figure}$	Figure 9: As in Fig. 6 but for the case where the SNR moves into a less denser region.
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$\begin{figure} \par\includegraphics[width=40pc]{7824fg10.eps} \end{figure}$	Figure 10: As in Fig. 7 except here the SNR moves into a medium of lesser density. The interface between the two media is a infinite plane situated 5 pc from the initial explosion. Note that in this scenario there is no reflected shock, but a second reverse shock start to form as the FS moves well into the medium of lesser density.
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$\begin{figure} \par\includegraphics[width=20pc]{7824fg11.eps} \end{figure}$	Figure 11: The pressure P of the SNR in the direction toward the contact discontinuity. The simulation is shown from 2000 yr up to 8000 yr. As time increases a second RS forms and at 8000 yr it starts to move toward the center.
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