Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.8cm, clip]{0021fig1.ps} \end{figure}$ Figure 1: a) The solid lines delineate the inner and outer radii of the shell expanding in a galaxy with h=500 pc. The dotted line gives the radius of the shell as predicted from the $R \propto (L/\rho)^{1/5}\: t^{3/5}$ law for the SN-driven expansion at t<35 Myr (Castor et al. 1975) and fromthe $R\propto t^{1/3}$ law for the "snow-plow" expansion at t>35 Myr. b) The same for h=210 pc. The dotted line gives the radius of the shell as predicted from the $R\propto t^{1/3}$ law for a cylindrical "snowplow'' expansion at t>13.5 Myr, the dashed line shows a spherical "snowplow'' $R\propto t^{1/4}$ expansion.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm, clip]{0021fig2.ps} \end{figure}$ Figure 2: Relative column density in the ring versus its radius: dashed, solid, and dotted lines represent h= 210, 500, and 700 pc, respectively; open circles correspond to $\Sigma_{\rm g0}=15.2~M_\odot$ pc^-2, filled circles - $\Sigma_{\rm g0}=10.7~M_\odot$ pc^-2.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm, clip]{0021fig3.ps} \end{figure}$ Figure 3: Mass-weighted z-velocity profiles versus projected distance from the geometrical center of the shells. Solid and dotted lines represent the shells with the radii of 0.5 and 0.7 kpc, respectively. Open squares - h=210 pc, t=18 Myr; open triangles - h=370 pc, t=13.5 Myr; open circles - h=500 pc, t=13.5 Myr. Filled squares - h=210 pc, t=36 Myr; filled triangles - h=370 pc, t=31 Myr; filled circles - h=500 pc, t=29 Myr. The unperturbed HI surface density is $\Sigma_{\rm g0}=10.7 \: M_{\odot}$ pc^-2.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm, clip]{0021fig4.ps} \end{figure}$ Figure 4: The HI spectrum of an expanding shell produced by 100 successive SNe located 100 pc above the midplane in a galaxy with a) h=500 pc, b) h=210 pc. The HI spectra are numerically obtained for a 1 kpc diameter beam centered on the shell at three different times in Myr as indicated in each frame.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm, clip]{0021fig5.ps} \end{figure}$ Figure 5: The peak z-velocity versus HI intensity for different gas scale heights and locations of SN explosions above the midplane: dashed line - h=210 pc, SNe at $z_\ast =100$ pc; dotted line - h=370 pc, SNe at $z_\ast =100$ pc; solid line with filled squares - h=500 pc, SNe at $z_\ast =100$ pc; solid line with open squares - h=500 pc, SNe at $z_\ast =50$ pc. Different evolutionary stages of the shells are labeled in Myr.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm, clip]{0021fig6.ps} \end{figure}$ Figure 6: Comparison of the total hydrogen column density and the observed HI in Ho II: solid line - observed HI (Puche et. al. 1992), dashed line shows total column density $N_0({\rm H})$ from (10) with h=625 pc, dotted line - $N_0({\rm H})$ with h=625+18.6(R-1)².
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm, clip]{0021fig2.ps} \end{figure}$	Figure 2: Relative column density in the ring versus its radius: dashed, solid, and dotted lines represent h= 210, 500, and 700 pc, respectively; open circles correspond to $\Sigma_{\rm g0}=15.2~M_\odot$ pc^-2, filled circles - $\Sigma_{\rm g0}=10.7~M_\odot$ pc^-2.
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$\begin{figure} \par\includegraphics[width=7.7cm, clip]{0021fig4.ps} \end{figure}$	Figure 4: The HI spectrum of an expanding shell produced by 100 successive SNe located 100 pc above the midplane in a galaxy with a) h=500 pc, b) h=210 pc. The HI spectra are numerically obtained for a 1 kpc diameter beam centered on the shell at three different times in Myr as indicated in each frame.
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$\begin{figure} \par\includegraphics[width=8.8cm, clip]{0021fig6.ps} \end{figure}$	Figure 6: Comparison of the total hydrogen column density and the observed HI in Ho II: solid line - observed HI (Puche et. al. 1992), dashed line shows total column density $N_0({\rm H})$ from (10) with h=625 pc, dotted line - $N_0({\rm H})$ with h=625+18.6(R-1)².
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