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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
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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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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
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