All Figures

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{2190fig1.eps}\end{figure}$ Figure 1: The network of processes connecting the different gaseous and stellar components. Clouds are the sites of SF. Stars return mass and inject energy into the multi-phase ISM. The two gas phases exchange mass and momentum by means of condensation or evaporation (C/E) and drag. The energy dissipation is due to radiative cooling and cloud-cloud collisions.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2190fig2.eps}\end{figure}$ Figure 2: The SF scheme: (t₀) inactive cloud (no SF); (t₁) an embedded star cluster formed with a local SF efficiency; (t₂) the cloud fragmented by SNII energy input.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{2190fig3.ps} \end{figure}$ Figure 3: The evolution of stellar surface density (at $1~\ensuremath{{\rm Gyr}}$ and $3~\ensuremath{{\rm Gyr}}$ ). The stellar disk becomes slightly thicker with time but is otherwise stable with weak transient spiral patterns. The surface density plots (Figs. 3 and 4) were computed using the NEMO Stellar Dynamics Toolbox (Teuben 1995). The particles were binned in a grid with a cell size of $40~\ensuremath{{\rm pc}}$ . The resulting map was then smoothed with a Gaussian kernel with ${\it FWHM} = 1~\ensuremath{{\rm kpc}}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.15cm,clip]{2190fig4.ps} \end{figure}$ Figure 4: The evolution of cloud surface density (at $1~\ensuremath{{\rm Gyr}}$ and $3~\ensuremath{{\rm Gyr}}$ ). The cloud disk is stable, but the overall surface density slowly decreases. For details on how the surface density was computed see Fig. 3.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.65cm,clip]{2190fig5.ps} \end{figure}$ Figure 5: The of evolution of gas density (at $1~\ensuremath{{\rm Gyr}}$ and $3~\ensuremath{{\rm Gyr}}$ ). In each panel the xy- ( bottom), xz-projection ( top), and density scale are shown. Starting from a homogenous distribution, the diffuse gas collapses and forms a thin gas disk within $1~\ensuremath{{\rm Gyr}}$ . While the mass of the gaseous disk is nearly constant, its radius is growing slowly. Densities in the disk are of the order of $1~\ensuremath{{\rm cm}^{-3}}$ . The halo has densities from $10^{-4}~\ensuremath{{\rm cm}^{-3}}$ to $10^{-6}~\ensuremath{{\rm cm}^{-3}}$ . Densities were computed on a 100 $\times$ 100-grid using the SPH formalism.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.55cm,clip]{2190fig6.ps} \end{figure}$ Figure 6: The evolution of gas temperature (at $1~\ensuremath{{\rm Gyr}}$ and $3~\ensuremath{{\rm Gyr}}$ ). In each panel the xy- ( bottom), xz-projection ( top), and temperature scale are shown. After the initial collapse, the diffuse gas forms a disk at about $10^4~\ensuremath{{\rm K}}$ . The central part of the disk, as well as small bubbles in the outer parts, are heated by SNII to $10^6~\ensuremath{{\rm K}}$ . The halo gas it at $10^6{-}10^7~\ensuremath{{\rm K}}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.85cm,clip]{2190fig7.ps} \end{figure}$ Figure 7: The evolution of the SFR with time (full line). The SFR decreases with time due to consumption of cloud mass. The average SFR (dashed line) is $\approx$ $1.6~\ensuremath{{M}_{\odot}} ~\ensuremath{~{\rm yr}^{-1}}$ . The dotted line is the result of a simple analytic model accounting for the depletion of the cloudy medium by SF.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.8cm,clip]{2190fig8.ps}\end{figure}$ Figure 8: The evolution of SF efficiency. SFE is up to 0.4 in the centre of the galaxy. The average over the whole disk is about 0.06.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.65cm,clip]{2190fig9.ps} \end{figure}$ Figure 9: The open diamonds show the SFR per $\ensuremath {{\rm pc}^2}$ averaged over $100~\ensuremath{{\rm Myr}}$ as a function of cloud surface density. The full line is a recent determination of the Schmidt Law by Kennicutt (1998) with a slope of -1.4. The vertical dashed line indicates a cut-off density for SF in disk galaxies that was also found by Kennicutt (1998).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{2190fi10.ps} \end{figure}$ Figure 10: The cloud mass spectrum. The different lines correspond to the mass spectrum after $1~\ensuremath{{\rm Gyr}}$ (dotted), $2~\ensuremath{{\rm Gyr}}$ (dashed), and $3~\ensuremath{{\rm Gyr}}$ (full) of evolution. The fitted power-law mass function is with $\alpha \approx -2.0$ comparable to the observed mass spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{2190fig1.eps}\end{figure}$	Figure 1: The network of processes connecting the different gaseous and stellar components. Clouds are the sites of SF. Stars return mass and inject energy into the multi-phase ISM. The two gas phases exchange mass and momentum by means of condensation or evaporation (C/E) and drag. The energy dissipation is due to radiative cooling and cloud-cloud collisions.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2190fig2.eps}\end{figure}$	Figure 2: The SF scheme: (t₀) inactive cloud (no SF); (t₁) an embedded star cluster formed with a local SF efficiency; (t₂) the cloud fragmented by SNII energy input.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.15cm,clip]{2190fig4.ps} \end{figure}$	Figure 4: The evolution of cloud surface density (at $1~\ensuremath{{\rm Gyr}}$ and $3~\ensuremath{{\rm Gyr}}$ ). The cloud disk is stable, but the overall surface density slowly decreases. For details on how the surface density was computed see Fig. 3.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=7.85cm,clip]{2190fig7.ps} \end{figure}$	Figure 7: The evolution of the SFR with time (full line). The SFR decreases with time due to consumption of cloud mass. The average SFR (dashed line) is $\approx$ $1.6~\ensuremath{{M}_{\odot}} ~\ensuremath{~{\rm yr}^{-1}}$ . The dotted line is the result of a simple analytic model accounting for the depletion of the cloudy medium by SF.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=7.8cm,clip]{2190fig8.ps}\end{figure}$	Figure 8: The evolution of SF efficiency. SFE is up to 0.4 in the centre of the galaxy. The average over the whole disk is about 0.06.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=7.65cm,clip]{2190fig9.ps} \end{figure}$	Figure 9: The open diamonds show the SFR per $\ensuremath {{\rm pc}^2}$ averaged over $100~\ensuremath{{\rm Myr}}$ as a function of cloud surface density. The full line is a recent determination of the Schmidt Law by Kennicutt (1998) with a slope of -1.4. The vertical dashed line indicates a cut-off density for SF in disk galaxies that was also found by Kennicutt (1998).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.1cm,clip]{2190fi10.ps} \end{figure}$	Figure 10: The cloud mass spectrum. The different lines correspond to the mass spectrum after $1~\ensuremath{{\rm Gyr}}$ (dotted), $2~\ensuremath{{\rm Gyr}}$ (dashed), and $3~\ensuremath{{\rm Gyr}}$ (full) of evolution. The fitted power-law mass function is with $\alpha \approx -2.0$ comparable to the observed mass spectrum.
Open with DEXTER