All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{figures/0071fig1.eps}\end{figure}$ Figure 1: Overview of the ISM model: equilibrium plots of a) temperature T, b) electron fraction x_e and c) pressure P as a function of density n for two different values of the UV field G₀, drawn line: G₀=1, dotted: G₀=10 ( $\times$ 1.6 $\times$ $10^{-3}~{\rm ergs~cm^{-2}~s^{-1}}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{figures/0071fig2.ps} \end{figure}$ Figure 2: Simulated dwarf galaxy after $\approx$ 1 Gyr. Shown are UBV composite pictures overplotted with HI density contours at different times. Last frame shows the central regions at $t= 1165~{\rm Myr}$ . HI contour levels are at $N_{{\rm HI}}= 10^{20}$ , 2.1 $\times$ 10²⁰, 3.6 $\times$ 10²⁰ and 2 $\times$ $10^{21}~{\rm cm^{-2}}$ . (This figure is available in color in electronic form.)
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In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{figures/0071fig3.eps} \end{figure}$ Figure 3: HI surface density & velocity dispersion map in quiescent phase ( left, taken at 1165 Myr) and in burst phase ( right, at 1211 Myr).
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{figures/0071fig4.ps} \end{figure}$ Figure 4: Star Formation History of a simulated dwarf galaxy. Upper panel: density plot of the azimutally averaged star formation rate. Lower panel: total star formation rate. The dotted line indicates the SFR for a run with $50\%$ reduced feedback strength.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{figures/0071fig5.ps} \end{figure}$ Figure 5: Radial profile of the mean star formation density (drawn line, dotted lines are exponentials with scalelengths of 0.25 and 1. kpc).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{figures/0071fig6.ps} \end{figure}$ Figure 6: distribution of ${\rm SFR/\langle SFR} \rangle_t$ for a sample of isolated dwarfs (squares with error bars), a simulation with full feedback (drawn line) and a simulation with $50\%$ feedback (dotted line). Data is taken from Van Zee (2001).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{figures/0071fig1.eps}\end{figure}$	Figure 1: Overview of the ISM model: equilibrium plots of a) temperature T, b) electron fraction x_e and c) pressure P as a function of density n for two different values of the UV field G₀, drawn line: G₀=1, dotted: G₀=10 ( $\times$ 1.6 $\times$ $10^{-3}~{\rm ergs~cm^{-2}~s^{-1}}$ ).
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$\begin{figure} \par\includegraphics[width=16.2cm,clip]{figures/0071fig3.eps} \end{figure}$	Figure 3: HI surface density & velocity dispersion map in quiescent phase ( left, taken at 1165 Myr) and in burst phase ( right, at 1211 Myr).
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$\begin{figure} \par\includegraphics[width=16.7cm,clip]{figures/0071fig4.ps} \end{figure}$	Figure 4: Star Formation History of a simulated dwarf galaxy. Upper panel: density plot of the azimutally averaged star formation rate. Lower panel: total star formation rate. The dotted line indicates the SFR for a run with $50\%$ reduced feedback strength.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{figures/0071fig5.ps} \end{figure}$	Figure 5: Radial profile of the mean star formation density (drawn line, dotted lines are exponentials with scalelengths of 0.25 and 1. kpc).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{figures/0071fig6.ps} \end{figure}$	Figure 6: distribution of ${\rm SFR/\langle SFR} \rangle_t$ for a sample of isolated dwarfs (squares with error bars), a simulation with full feedback (drawn line) and a simulation with $50\%$ feedback (dotted line). Data is taken from Van Zee (2001).
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