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$\begin{figure} \par\includegraphics[width=12cm,clip]{Fg041_fig1.ps} \end{figure}$ Figure 1: Response of the gaseous disk of a galaxy to a tidal interaction. The collision parameters are those of run 2 (see Table 1). Dark haloes are initially truncated at three times the optical radius of the galaxies. The gas column-density is plotted in grayscale. The center of the second galaxy is represented by the star symbol. More than ten gravitational clumps collapse along the tail with masses of 10⁷ to 10⁸ $M_{\hbox {$\odot $ }}$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{Fg041_fig2.ps} \end{figure}$ Figure 2: Same run as in Fig. 1, with the truncation radius of the dark haloes extended up to 10 times the radius of the stellar disks. Gas accumulations of 10⁹ solar masses are formed at the tip of each tidal tail. One of them quickly falls into the disturbing galaxy, while the other one forms a gravitationally bound object that orbits at large radii on a nearly circular path.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Fg041_fig3a.eps} \includegraphics[width=8cm,clip]{Fg041_fig3b.eps} \end{figure}$ Figure 3: Same run as in Fig. 2 observed at t=600 Myr. The initial disk plane is seen face-on (top) and edge-on (bottom). Two tidal dwarf galaxies (A and G) are formed near the extremity of the tails, with respective masses of 1.1 and $1.3\times 10^9$ $M_{\hbox {$\odot $ }}$ . The smaller gravitational clumps distributed along the tails (B to F) have masses from $3\times 10^7$ $M_{\hbox {$\odot $ }}$ to $11\times 10^7$ $M_{\hbox {$\odot $ }}$ . The initial gas mass in the disk was 10¹⁰ $M_{\hbox {$\odot $ }}$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{Fg041_fig2.ps} \end{figure}$	Figure 2: Same run as in Fig. 1, with the truncation radius of the dark haloes extended up to 10 times the radius of the stellar disks. Gas accumulations of 10⁹ solar masses are formed at the tip of each tidal tail. One of them quickly falls into the disturbing galaxy, while the other one forms a gravitationally bound object that orbits at large radii on a nearly circular path.
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