Abstract
Theoretical λ CDM cosmological models predict a much larger number of low mass dark matter haloes than has been observed in the Local Group of galaxies. One possible explanation is the increased difficulty of detecting these haloes if most of the visible matter is lost at early evolutionary phases through galactic winds. In this work we study the current models of triggering galactic winds in dwarf spheroidal galaxies (dSph) from supernovae, and study, based on 3D hydrodynamic numerical simulations, the correlation of the mass loss rates and important physical parameters as the dark matter halo mass and the star formation rate. We find that the existence of winds is ubiquitous, independent on the gravitational potential, as would be expected. This because our simulations revealed that the Rayleigh-Taylor Instability (RTI) may play a major role on pushing matter out of these systems, even for very massive haloes. However, as already reported in previous works we have found a correlation between the mass loss rate and both the halo mass and the rate of supernovae. Besides, the epoch in which most of the baryon galactic matter is removed from the galaxy varies depends on those quantities. This result, combined to the importance of the RTI in each model, may change our understanding about the chemical evolution of dwarf galaxies, as well as in the heavy element contamination of the intergalactic medium at high redshifts.
