All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1324fig1.eps} \end{figure}$ Figure 1: The equilibrium radial distribution of gas surface density (the solid line), the initial rotation curve (the dashed line), and the Gaussian vertical scale height of gas distribution (the dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1324fig2.eps} \end{figure}$ Figure 2: Temporal evolution of the gas volume density distribution after the release of $2\times 10^{53}$ erg of thermal energy at z=0,r=0 pc. The upper panels correspond to 200 consecutive SN explosions over 30 Myr, while the lower panels show the impact of a single hypernova of the same total energy of $2.0\times 10^{53}$ erg. The scale bar is in gm cm^-3.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fig3.eps} \end{figure}$ Figure 3: The same as Fig. 2, but for the energy input of $5\times 10^{53}$ erg.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1324fig4.eps} \end{figure}$ Figure 4: The same as Fig. 2, but for the energy input of 10⁵⁴ erg.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1324fig5.eps} \end{figure}$ Figure 5: The vertical cut through the distribution of the gas volume density produced by 500 consecutive SNe at t=27 Myr ( the left panel) and single hypernova of the same total energy of $5.0\times 10^{53}$ erg ( the right panel). The gas velocity field is shown by the arrows.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1324fig6.eps} \end{figure}$ Figure 6: The contrast in the HI column density between the ring and the central depression ${\cal K}=N_{\rm r}({\rm HI})/N_{\rm c}\rm (HI)$ as a function of the ring radius. The solid lines show the contrast $\cal K$ produced by multiple SNe, whereas the dashed lines show that produced by a single hypernova of the same total energy. An inclination angle of $5^\circ$ is assumed. The energy input is indicated in the right upper corner of each panel. The dashed-dotted and dotted lines in the lower panel give the contrast $\cal K$ for an inclination angle of $45^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fig7.eps} \end{figure}$ Figure 7: The pV-diagrams of the shell created by 500 consecutive SNe. The pV-cuts are taken along the major axis of the model galaxy viewed at an angle of $5^\circ$ . The evolutionary time of the shell is indicated in the right upper corner. The quantity $S_{\rm HI}$ is plotted in all model pV-diagrams.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fig8.eps} \end{figure}$ Figure 8: The pV-diagrams of the shell produced by a single hypernova of the total energy of $5.0\times 10^{53}$ erg. The pV-cuts are taken along the major axis of the model galaxy viewed at an inclination angle of $5^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fig9.eps} \end{figure}$ Figure 9: The same as Fig. 8, but for a single hypernova of the total energy of 10⁵⁴ erg.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fg10.eps} \end{figure}$ Figure 10: The pV-diagrams of the shell created by 1000 consecutive SNe. The pV-cuts are taken along the minor ( the left panels) and the major ( the right panels) axis of the model galaxy viewed at an angle of $45^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg11.eps} \end{figure}$ Figure 11: The same as in Fig. 10, but for a single hypernova of the same total energy of 10⁵⁴ erg. The pV-cuts taken along the minor axis of the hypernova-driven shell show the characteristic S-shaped structure due to an expansion in the vertical direction.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fg12.eps} \end{figure}$ Figure 12: Integrated HI emission of Ho I. In the bottom left corner we show the half-power beam (8 $.\!\!^{\prime\prime}$ 2 $\times$ 7.0 $.\!\!^{\prime\prime}$ ). The grayscale represents the HI column density. The data have been obtained from the Very Large Array observations (Ott et al. 2001).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1324fg13.eps} \end{figure}$ Figure 13: The integrated HI image of the ring produced by 500 consecutive SNe. The inclination angle is indicated in the right upper corner. The scale bar is in cm^-2. The origin of narrow rings is an assumption of axisymmetry in our numerical simulations.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1324fg14.eps} \end{figure}$ Figure 14: Off-plane explosions. Temporal evolution of the gas volume density distribution after the release of $1.0\times 10^{54}$ erg of thermal energy at r=0,z=100 pc. The upper panels correspond to 1000 consecutive SN explosions over 30 Myr, while the lower panels show the impact of a single hypernova of the same total energy of 10⁵⁴ erg. The scale bar is in gm cm^-3.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg15.eps} \end{figure}$ Figure 15: Off-plane explosion. The pV-diagrams of the shell created by a single hypernova of the total energy of 10⁵⁴ erg. The pV-cuts are taken along the major axis of the model galaxy viewed at an inclination angle of $5^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg16.eps} \end{figure}$ Figure 16: The distribution of the gas volume density created by the collision of a cloud of $M_{\rm\scriptstyle HVC} = 2.5 \times 10^6~M_\odot$ and $v_{\rm\scriptstyle HVC}=200$ km s^-1 with the galactic gas disk.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg17.eps} \end{figure}$ Figure 17: The integrated HI image of the gas volume density distribution shown in Fig. 16. An inclination angle of $5^\circ$ is adopted. The scale bar is in cm^-2.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1324fg18.eps} \end{figure}$ Figure 18: The pV-diagrams of the gas volume density distribution shown in Fig. 16. The pV-cuts are taken along the major axis of the projected galaxy. An inclination angle of $5^\circ$ is assumed.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1324fig1.eps} \end{figure}$	Figure 1: The equilibrium radial distribution of gas surface density (the solid line), the initial rotation curve (the dashed line), and the Gaussian vertical scale height of gas distribution (the dotted line).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1324fig2.eps} \end{figure}$	Figure 2: Temporal evolution of the gas volume density distribution after the release of $2\times 10^{53}$ erg of thermal energy at z=0,r=0 pc. The upper panels correspond to 200 consecutive SN explosions over 30 Myr, while the lower panels show the impact of a single hypernova of the same total energy of $2.0\times 10^{53}$ erg. The scale bar is in gm cm^-3.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fig3.eps} \end{figure}$	Figure 3: The same as Fig. 2, but for the energy input of $5\times 10^{53}$ erg.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1324fig4.eps} \end{figure}$	Figure 4: The same as Fig. 2, but for the energy input of 10⁵⁴ erg.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1324fig5.eps} \end{figure}$	Figure 5: The vertical cut through the distribution of the gas volume density produced by 500 consecutive SNe at t=27 Myr ( the left panel) and single hypernova of the same total energy of $5.0\times 10^{53}$ erg ( the right panel). The gas velocity field is shown by the arrows.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fig7.eps} \end{figure}$	Figure 7: The pV-diagrams of the shell created by 500 consecutive SNe. The pV-cuts are taken along the major axis of the model galaxy viewed at an angle of $5^\circ$ . The evolutionary time of the shell is indicated in the right upper corner. The quantity $S_{\rm HI}$ is plotted in all model pV-diagrams.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fig8.eps} \end{figure}$	Figure 8: The pV-diagrams of the shell produced by a single hypernova of the total energy of $5.0\times 10^{53}$ erg. The pV-cuts are taken along the major axis of the model galaxy viewed at an inclination angle of $5^\circ$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fig9.eps} \end{figure}$	Figure 9: The same as Fig. 8, but for a single hypernova of the total energy of 10⁵⁴ erg.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fg10.eps} \end{figure}$	Figure 10: The pV-diagrams of the shell created by 1000 consecutive SNe. The pV-cuts are taken along the minor ( the left panels) and the major ( the right panels) axis of the model galaxy viewed at an angle of $45^\circ$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg11.eps} \end{figure}$	Figure 11: The same as in Fig. 10, but for a single hypernova of the same total energy of 10⁵⁴ erg. The pV-cuts taken along the minor axis of the hypernova-driven shell show the characteristic S-shaped structure due to an expansion in the vertical direction.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1324fg12.eps} \end{figure}$	Figure 12: Integrated HI emission of Ho I. In the bottom left corner we show the half-power beam (8 $.\!\!^{\prime\prime}$ 2 $\times$ 7.0 $.\!\!^{\prime\prime}$ ). The grayscale represents the HI column density. The data have been obtained from the Very Large Array observations (Ott et al. 2001).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1324fg13.eps} \end{figure}$	Figure 13: The integrated HI image of the ring produced by 500 consecutive SNe. The inclination angle is indicated in the right upper corner. The scale bar is in cm^-2. The origin of narrow rings is an assumption of axisymmetry in our numerical simulations.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1324fg14.eps} \end{figure}$	Figure 14: Off-plane explosions. Temporal evolution of the gas volume density distribution after the release of $1.0\times 10^{54}$ erg of thermal energy at r=0,z=100 pc. The upper panels correspond to 1000 consecutive SN explosions over 30 Myr, while the lower panels show the impact of a single hypernova of the same total energy of 10⁵⁴ erg. The scale bar is in gm cm^-3.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg15.eps} \end{figure}$	Figure 15: Off-plane explosion. The pV-diagrams of the shell created by a single hypernova of the total energy of 10⁵⁴ erg. The pV-cuts are taken along the major axis of the model galaxy viewed at an inclination angle of $5^\circ$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg16.eps} \end{figure}$	Figure 16: The distribution of the gas volume density created by the collision of a cloud of $M_{\rm\scriptstyle HVC} = 2.5 \times 10^6~M_\odot$ and $v_{\rm\scriptstyle HVC}=200$ km s^-1 with the galactic gas disk.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1324fg17.eps} \end{figure}$	Figure 17: The integrated HI image of the gas volume density distribution shown in Fig. 16. An inclination angle of $5^\circ$ is adopted. The scale bar is in cm^-2.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1324fg18.eps} \end{figure}$	Figure 18: The pV-diagrams of the gas volume density distribution shown in Fig. 16. The pV-cuts are taken along the major axis of the projected galaxy. An inclination angle of $5^\circ$ is assumed.
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