Chemodynamical Simulations of Dwarf Galaxy Evolution
Figure 3
The density (a and b) and temperature (c and d) distributions after 180 Myr of evolution of two model galaxies. Strips on the right of each panel show the density and temperature scales. In one case (a and c), the upper mass in each formed star cluster depends on the total cluster mass (truncated IMF). In the other case (b and d), the upper IMF mass is always the same, irrespective of the mass of the star cluster. It is to notice that the temperature of the gas outside the galaxy has been set to 106 K. The temperature in the central region is hotter in the filled IMF model because of the larger amount of energy provided by SNeII.
