Resumen
We evaluate the minimum energy input rate that starbursts require for expelling their newly processed matter from their host galaxies. To this end we first review the main facts about the power expected from correlated massive stars and the hydrodynamics that they induce in their host ISM. Our estimate of the minimum energy input rate required for mass ejection into the intergalactic medium results from special consideration of the pressure caused by the environment in which a galaxy is situated, as well as to the intrinsic rotation of the gaseous component. We account for these factors and for a massive dark matter distribution, and develop a self-consistent solution for the interstellar matter gas distribution. Our results are in excellent agreement with the results of Mac Low & Ferrara (1999) for galaxies with a flattened disk-like ISM density distribution and a low intergalactic gas pressure (P[IGM]/k <= 1 cm-3 K). However, our solution also requires a much larger energy input rate threshold when one takes into consideration both a larger intergalactic pressure and the possible existence of a low-density, non-rotating, extended gaseous halo component. The steps towards mixing of heavy elements with the ISM and the time scales required are also here reviewed.
